{"survey_paper_info": {"1": {"id": "1312.3455v2", "title": "Low Latency Datacenter Networking: A Short Survey", "url": "http://arxiv.org/pdf/1312.3455v2", "date": "2014-07-31 08:36:28", "abs": "Datacenters are the cornerstone of the big data infrastructure supporting\nnumerous online services. The demand for interactivity, which significantly\nimpacts user experience and provider revenue, is translated into stringent\ntiming requirements for flows in datacenter networks. Thus low latency\nnetworking is becoming a major concern of both industry and academia.\n We provide a short survey of recent progress made by the networking community\nfor low latency datacenter networks. We propose a taxonomy to categorize\nexisting work based on four main techniques, reducing queue length,\naccelerating retransmissions, prioritizing mice flows, and exploiting\nmulti-path. Then we review select papers, highlight the principal ideas, and\ndiscuss their pros and cons. We also present our perspectives of the research\nchallenges and opportunities, hoping to aspire more future work in this space.", "cat": "cs.NI", "authors": ["Shuhao Liu", "Hong Xu", "Zhiping Cai"]}, "2": {"id": "1809.08245v1", "title": "A-type stars in the Canada-France Imaging Survey I. The stellar halo of the Milky Way traced to large radius by blue horizontal branch stars", "url": "http://arxiv.org/pdf/1809.08245v1", "date": "2018-09-21 18:00:03", "abs": "We present the stellar density profile of the outer halo of the Galaxy traced\nover a range of Galactocentric radii from $15< R_{GC} < 220$ kpc by blue\nhorizontal branch (BHB) stars. These stars are identified photometrically using\ndeep $u-$band imaging from the new Canada-France-Imaging-Survey (CFIS) that\nreaches 24.5 mag. This is combined with $griz$ bands from Pan-STARRS 1 and\ncovers a total of $\\sim4000$ deg$^2$ of the northern sky. We present a new\nmethod to select BHB stars that has low contamination from blue stragglers and\nhigh completeness. We use this sample to measure and parameterize the three\ndimensional density profile of the outer stellar halo. We fit the profile using\n(i) a simple power-law with a constant flattening (ii) a flattening that varies\nas a function of Galactocentric radius (iii) a broken power law profile. We\nfind that outer stellar halo traced by the BHB is well modelled by a broken\npower law with a constant flattening of $q=0.86 \\pm 0.02$, with an inner slope\nof $\\gamma=4.24 \\pm 0.08$. This is much steeper than the preferred outer\nprofile that has a slope of $\\beta=3.21\\pm 0.07$ after a break radius of\n$r_b=41.4^{+2.5}_{-2.4}$ kpc. The outer profile of the stellar halo trace by\nBHB stars is shallower than that recently measured using RR Lyrae, a surprising\nresult given the broad similarity of the ages of these stellar populations.", "cat": "astro-ph.GA", "authors": ["Guillaume F. Thomas", "Alan W. McConnachie", "Rodrigo A. Ibata", "Patrick C\u00f4t\u00e9", "Nicolas Martin", "Else Starkenburg", "Raymond Carlberg", "Scott Chapman", "S\u00e9bastien Fabbro", "Benoit Famaey", "Nicholas Fantin", "Stephen Gwyn", "Vincent H\u00e9nault-Brunet", "Khyati Malhan", "Julio Navarro", "Annie C. Robin", "Douglas Scott"]}, "3": {"id": "1906.07484v1", "title": "Stellar populations of nine passive spiral galaxies from the CALIFA survey: are they progenitors of S0s?", "url": "http://arxiv.org/pdf/1906.07484v1", "date": "2019-06-18 10:28:52", "abs": "We investigate the stellar population properties of passive spiral galaxies\nin the CALIFA survey. Nine spiral galaxies that have NUV-r > 5 and no/weak\nnebular emission lines in their spectra are selected as passive spirals. Our\npassive spirals lie in the redshift range of 0.001 < z < 0.021 and have stellar\nmass range of 10.2 < log(M_{\\star}/M_{\\odot}) < 10.8. They clearly lie in the\ndomain of early-type galaxies in the WISE IR color-color diagram. We analyze\nthe stellar populations out to two effective radius, using the best-fitting\nmodel to the measured absorption line-strength indices in the Lick/IDS system.\nWe find that stellar populations of the passive spirals span a wide range, even\nin their centers, and hardly show any common trend amongst themselves either.\nWe compare the passive spirals with S0s selected in the same mass range. S0s\ncover a wide range in age, metallicity, and [a/Fe], and stellar populations of\nthe passive spirals are encompassed in the spread of the S0 properties.\nHowever, the distribution of passive spirals are skewed toward higher values of\nmetallicity, lower [a/Fe], and younger ages at all radii. These results show\nthat passive spirals are possibly related to S0s in their stellar populations.\nWe infer that the diversity in the stellar populations of S0s may result from\ndifferent evolutionary pathways of S0 formation, and passive spirals may be one\nof the possible channels.", "cat": "astro-ph.GA", "authors": ["Mina Pak", "Joon Hyeop Lee", "Hyunjin Jeong", "Suk Kim", "Rory Smith", "Hye-Ran Lee"]}, "4": {"id": "2001.07738v2", "title": "Exploring Early and Late Cosmology with Next Generation Surveys", "url": "http://arxiv.org/pdf/2001.07738v2", "date": "2020-05-09 09:33:37", "abs": "Perturbations from inflation evolve into large scale structure of the late\nuniverse, and encode abundant cosmic structure formation physics. We allow\nfreedom in the primordial power spectrum, rather than assuming a power law\nscale dependence, to study its impact on cosmological parameter determination.\nCombining various generations of cosmic microwave background (CMB) data and\ngalaxy redshift survey data, we investigate the constraints on reconstruction\nof the primordial curvature perturbation power spectrum and the late time\ncosmology, especially the sum of neutrino masses. We quantify how each\nsuccessive generation, in CMB and galaxy surveys, provides significant\nimprovements, often by factors of several. By using CMB polarization\ninformation over a broad range of angular scales, and galaxy redshift data in\nmany bins of redshift, one can allow inflationary freedom and still constrain\nparameters comparably to assuming power law dependence. The primordial power\nspectrum can be reconstructed at the subpercent level in a dozen wavenumber\nbins, while simultaneously fitting the sum of neutrino masses to 14 meV.", "cat": "astro-ph.CO", "authors": ["Guilherme Brando", "Eric V. Linder"]}, "5": {"id": "1503.07475v1", "title": "Role of Matrix Factorization Model in Collaborative Filtering Algorithm: A Survey", "url": "http://arxiv.org/pdf/1503.07475v1", "date": "2015-03-25 17:54:43", "abs": "Recommendation Systems apply Information Retrieval techniques to select the\nonline information relevant to a given user. Collaborative Filtering is\ncurrently most widely used approach to build Recommendation System. CF\ntechniques uses the user behavior in form of user item ratings as their\ninformation source for prediction. There are major challenges like sparsity of\nrating matrix and growing nature of data which is faced by CF algorithms. These\nchallenges are been well taken care by Matrix Factorization. In this paper we\nattempt to present an overview on the role of different MF model to address the\nchallenges of CF algorithms, which can be served as a roadmap for research in\nthis area.", "cat": "cs.IR", "authors": ["Dheeraj kumar Bokde", "Sheetal Girase", "Debajyoti Mukhopadhyay"]}, "6": {"id": "0904.4702v3", "title": "Size Bias in Galaxy Surveys", "url": "http://arxiv.org/pdf/0904.4702v3", "date": "2009-08-05 09:03:14", "abs": "Only certain galaxies are included in surveys: those bright and large enough\nto be detectable as extended sources. Because gravitational lensing can make\ngalaxies appear both brighter and larger, the presence of foreground\ninhomogeneities can scatter galaxies across not only magnitude cuts but also\nsize cuts, changing the statistical properties of the resulting catalog. Here\nwe explore this size bias, and how it combines with magnification bias to\naffect galaxy statistics. We demonstrate that photometric galaxy samples from\ncurrent and upcoming surveys can be even more affected by size bias than by\nmagnification bias.", "cat": "astro-ph.CO", "authors": ["Fabian Schmidt", "Eduardo Rozo", "Scott Dodelson", "Lam Hui", "Erin Sheldon"]}, "7": {"id": "2307.14761v1", "title": "Literature Survey on how to cluster and define Living Labs, Real World Laboratories and similar research infrastructures", "url": "http://arxiv.org/pdf/2307.14761v1", "date": "2023-07-27 10:42:31", "abs": "In today's world, where societal challenges in the areas of digitalization,\ndemographic change and sustainability are becoming increasingly complex, new\ninnovation structures are needed to meet these challenges. Living Labs or also\nReal World Laboratories prove to be such. Through their applied methods such as\nco-creation, they integrate users into research, making it more user-centric.\nWhich other research infrastructures exist and how they can be differentiated\nis presented in this paper on the basis of a systematic literature research.\nFurthermore, methods for user integration are examined and provided in the form\nof an overview.", "cat": "cs.SE", "authors": ["Troung Giang Luu", "Tanja Zylowski", "Sascha Alpers", "Andreas Oberweis"]}, "8": {"id": "2203.01464v1", "title": "A Survey of Analysis Methods for Security and Safety verification in IoT Systems", "url": "http://arxiv.org/pdf/2203.01464v1", "date": "2022-03-03 00:29:32", "abs": "Internet of Things (IoT) has been rapidly growing in the past few years in\nall life disciplines. IoT provides automation and smart control to its users in\ndifferent domains such as home automation, healthcare systems, automotive, and\nmany more. Given the tremendous number of connected IoT devices, this growth\nleads to enormous automatic interactions among sizeable IoT apps in their\nenvironment, making IoT apps more intelligent and more enjoyable to their\nusers. But some unforeseen interactions of IoT apps and any potential malicious\nbehaviour can seriously cause insecure and unsafe consequences to its users,\nprimarily non-experts, who lack the required knowledge regarding the potential\nimpact of their IoT automation processes. In this paper, we study the problem\nof security and safety verification of IoT systems. We survey techniques that\nutilize program analysis to verify IoT applications' security and safety\nproperties. The study proposes a set of categorization and classification\nattributes to enhance our understanding of the research landscape in this\ndomain. Moreover, we discuss the main challenges considered in the surveyed\nwork and potential solutions that could be adopted to ensure the security and\nsafety of IoT systems.", "cat": "cs.CR", "authors": ["Lobna Abuserrieh", "Manar H. Alalfi"]}, "9": {"id": "2211.11080v1", "title": "The LOFAR Tied-Array All-Sky Survey: Timing of 35 radio pulsars and an overview of the properties of the LOFAR pulsar discoveries", "url": "http://arxiv.org/pdf/2211.11080v1", "date": "2022-11-20 20:48:35", "abs": "The LOFAR Tied-Array All-Sky Survey (LOTAAS) is the most sensitive untargeted\nradio pulsar survey performed at low radio frequencies (119--151\\,MHz) to date\nand has discovered 76 new radio pulsars, among which the 23.5-s pulsar\nJ0250+5854, up until recently the slowest-spinning radio pulsar known. Here, we\nreport on the timing solutions of 35 pulsars discovered by LOTAAS, which\ninclude a nulling pulsar and a mildly recycled pulsar, and thereby complete the\nfull timing analysis of the LOTAAS pulsar discoveries. We give an overview of\nthe findings from the full LOTAAS sample of 76 pulsars, discussing their pulse\nprofiles, radio spectra and timing parameters. We found that the pulse profiles\nof some of the pulsars show profile variations in time or frequency and while\nsome pulsars show signs of scattering, a large majority display no pulse\nbroadening. The LOTAAS discoveries have on average steeper radio spectra and\nhave longer spin periods ($1.4\\times$) as well as lower spin-down rates\n($3.1\\times$) compared to the known pulsar population. We discuss the cause of\nthese differences, and attribute them to a combination of selection effects of\nthe LOTAAS survey as well as previous pulsar surveys, though can not rule out\nthat older pulsars tend to have steeper radio spectra.", "cat": "astro-ph.HE", "authors": ["E. van der Wateren", "C. G. Bassa", "S. Cooper", "J. -M. Grie\u00dfmeier", "B. W. Stappers", "J. W. T. Hessels", "V. I. Kondratiev", "D. Michilli", "C. M. Tan", "C. Tiburzi", "P. Weltevrede", "A. -S. Bak Nielsen", "T. D. Carozzi", "B. Ciardi", "I. Cognard", "R. -J. Dettmar", "A. Karastergiou", "M. Kramer", "J. K\u00fcnsem\u00f6ller", "S. Os\u0142owski", "M. Serylak", "C. Vocks", "O. Wucknitz"]}, "10": {"id": "1710.08776v2", "title": "A fast, wide-field and distortion-free telescope with curved detectors for surveys at ultra-low surface brightness", "url": "http://arxiv.org/pdf/1710.08776v2", "date": "2017-10-25 14:03:27", "abs": "We present the design of an all-reflective, bi-folded Schmidt telescope aimed\nat surveys of extended astronomical objects with extremely-low surface\nbrightness. The design leads to a high image quality without any diffracting\nspider, along with a large aperture and field of view, with a small central\nobstruction which barely alters the PSF. As an example, we present the design\nof a high-quality, 36 cm diameter, fast ( f /2.5) telescope working in the\nvisible with a large field of view (1.6{\\deg}x 2.6{\\deg}). The telescope can\noperate with a curved detector (or with a flat detector with a field flattener)\nand a set of filters. The entrance mirror is anamorphic and replaces the\nclassical Schmidt entrance corrector plate. We show that this anamorphic\nprimary mirror can be manufactured through stress polishing, avoiding high\nspatial frequency errors, and tested with a simple interferometer scheme. This\nprototype is intended to serve as a fast-track scientific and technological\npathfinder for the future space-based MESSIER mission.", "cat": "astro-ph.IM", "authors": ["Eduard Muslimov", "David Valls-Gabaud", "G\u00e9rard Lema\u00eetre", "Emmanuel Hugot", "Wilfred Jahn", "Simona Lombardo", "Xin Wang", "Pascal Vola", "Marc Ferrari"]}, "11": {"id": "2303.11666v2", "title": "A Survey on Causal Inference for Recommendation", "url": "http://arxiv.org/pdf/2303.11666v2", "date": "2024-07-08 15:55:13", "abs": "Causal inference has recently garnered significant interest among recommender\nsystem (RS) researchers due to its ability to dissect cause-and-effect\nrelationships and its broad applicability across multiple fields. It offers a\nframework to model the causality in recommender systems like confounding\neffects and deal with counterfactual problems such as offline policy evaluation\nand data augmentation. Although there are already some valuable surveys on\ncausal recommendations, they typically classify approaches based on the\npractical issues faced in RS, a classification that may disperse and fragment\nthe unified causal theories. Considering RS researchers' unfamiliarity with\ncausality, it is necessary yet challenging to comprehensively review relevant\nstudies from a coherent causal theoretical perspective, thereby facilitating a\ndeeper integration of causal inference in RS. This survey provides a systematic\nreview of up-to-date papers in this area from a causal theory standpoint and\ntraces the evolutionary development of RS methods within the same causal\nstrategy. Firstly, we introduce the fundamental concepts of causal inference as\nthe basis of the following review. Subsequently, we propose a novel\ntheory-driven taxonomy, categorizing existing methods based on the causal\ntheory employed - namely, those based on the potential outcome framework, the\nstructural causal model, and general counterfactuals. The review then delves\ninto the technical details of how existing methods apply causal inference to\naddress particular recommender issues. Finally, we highlight some promising\ndirections for future research in this field. Representative papers and\nopen-source resources will be progressively available at\nhttps://github.com/Chrissie-Law/Causal-Inference-for-Recommendation.", "cat": "cs.IR", "authors": ["Huishi Luo", "Fuzhen Zhuang", "Ruobing Xie", "Hengshu Zhu", "Deqing Wang", "Zhulin An", "Yongjun Xu"]}, "12": {"id": "2212.00862v1", "title": "An introduction to optimization under uncertainty -- A short survey", "url": "http://arxiv.org/pdf/2212.00862v1", "date": "2022-12-01 20:48:06", "abs": "Optimization equips engineers and scientists in a variety of fields with the\nability to transcribe their problems into a generic formulation and receive\noptimal solutions with relative ease. Industries ranging from aerospace to\nrobotics continue to benefit from advancements in optimization theory and the\nassociated algorithmic developments. Nowadays, optimization is used in real\ntime on autonomous systems acting in safety critical situations, such as\nself-driving vehicles. It has become increasingly more important to produce\nrobust solutions by incorporating uncertainty into optimization programs. This\npaper provides a short survey about the state of the art in optimization under\nuncertainty. The paper begins with a brief overview of the main classes of\noptimization without uncertainty. The rest of the paper focuses on the\ndifferent methods for handling both aleatoric and epistemic uncertainty. Many\nof the applications discussed in this paper are within the domain of control.\nThe goal of this survey paper is to briefly touch upon the state of the art in\na variety of different methods and refer the reader to other literature for\nmore in-depth treatments of the topics discussed here.", "cat": "cs.AI", "authors": ["Keivan Shariatmadar", "Kaizheng Wang", "Calvin R. Hubbard", "Hans Hallez", "David Moens"]}, "13": {"id": "2111.00881v1", "title": "Artificial Intelligence in the Low-Level Realm -- A Survey", "url": "http://arxiv.org/pdf/2111.00881v1", "date": "2021-09-19 19:36:54", "abs": "Resource-aware machine learning has been a trending topic in recent years,\nfocusing on making ML computational aspects more exploitable by the edge\ndevices in the Internet of Things. This paper attempts to review a conceptually\nand practically related area concentrated on efforts and challenges for\napplying ML in the operating systems' main tasks in a low-resource environment.\nArtificial Intelligence has been integrated into the operating system with\napplications such as voice or image recognition. However, this integration is\nonly in user space. Here, we seek methods and efforts that exploit AI\napproaches, specifically machine learning, in the OSes' primary\nresponsibilities. We provide the improvements that ML can bring to OS to make\nthem more trustworthy. In other words, the main question to be answered is how\nAI has played/can play a role directly in improving the traditional OS kernel\nmain tasks. Also, the challenges and limitations in the way of this combination\nare provided.", "cat": "cs.LG", "authors": ["Vahid Mohammadi Safarzadeh", "Hamed Ghasr Loghmani"]}, "14": {"id": "1807.06016v1", "title": "The Dragonfly Nearby Galaxies Survey. V. HST/ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC1052, NGC1084, M96, and NGC4258", "url": "http://arxiv.org/pdf/1807.06016v1", "date": "2018-07-16 18:00:00", "abs": "We present HST/ACS imaging of twenty-three very low surface brightness\n($\\mu_{e,V}$=25-27.5) galaxies detected in the fields of four nearby galaxy\ngroups. These objects were selected from deep optical imaging obtained with the\nDragonfly Telephoto Array. Seven are new discoveries, while most of the others\nhad been identified previously in visual surveys of deep photographic plates\nand more recent surveys. Few have previously been studied in detail. From the\nACS images, we measure distances to the galaxies using both the tip of the red\ngiant branch method and the surface brightness fluctuations method. We\ndemonstrate that the two methods are consistent with each other in the regime\nwhere both can be applied. The distances to 15 out of 20 galaxies with stable\nmeasurements are consistent with that of the targeted group within errors. This\nsuggests that assuming group membership based solely on projected proximity is\n~75% successful in this regime. The galaxies are nearly round, with a median\naxis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The\nobjects have a range of sizes, from $R_e$=0.4 kpc to $R_e$=1.8 kpc, with a\nmedian of 1.0 kpc. They range in luminosity from $M_V$=-11.4 to $M_V$=-15.6,\nwith a median of -12.4. Galaxies with $R_e$~1 kpc and $M_V$~-12 are fairly rare\nin the Local Group but we find many of them in this relatively small sample.\nFour of the objects fall in the class of ultra diffuse galaxies (UDGs), with\n$R_e$>1.5 kpc and $\\mu_{0,V}$>24 mag/arcsec^2, including the recently\nidentified dark matter deficient galaxy NGC1052-DF2.", "cat": "astro-ph.GA", "authors": ["Yotam Cohen", "Pieter van Dokkum", "Shany Danieli", "Aaron J. Romanowsky", "Roberto Abraham", "Allison Merritt", "Jielai Zhang", "Lamiya Mowla", "J. M. Diederik Kruijssen", "Charlie Conroy", "Asher Wasserman"]}, "15": {"id": "0803.4032v2", "title": "The effects of stellar populations on galaxy scaling relations in the 6dF Galaxy Survey", "url": "http://arxiv.org/pdf/0803.4032v2", "date": "2008-04-08 03:43:13", "abs": "We present an analysis of the stellar populations in a sample of ~7000\ngalaxies from the 6dF Galaxy Survey (6dFGS). We derive ages and metallicities\nusing stellar population models. We also derive dynamical masses and dynamical\nmass-to-light ratios by combining central velocity dispersions with global\nphotometry in B, R and K bands. Together, these data allow to reduce the\ndegeneracies between age, metallicity and star formation burst-strength that\nhave limited previous studies. We find old galaxies exhibit a mass-metallicity\nrelation with slope d[Fe/H]/dlogM = 0.25, while young galaxies show slopes\nconsistent with zero. When we account for the effects of the mass-metallicity\nrelation, we obtain a single, consistent relation between mass-to-light ratio\nand mass for old galaxies in all passbands. As we have accounted for stellar\npopulation effects, this relation must have a dynamical origin. However, we\ndemonstrate that any simple trend between mass-to-light-ratio and mass or\nluminosity is inconsistent with the observations, and that a more complex\nrelationship must exist. We find the central regions of galaxies often exhibit\nyoung stellar populations. However it is only in the lowest-mass galaxies\n(~10^{10} M$_{\\odot}$) that these populations are evident in the global\nphotometry. In higher-mass galaxies, young central populations have decreasing\ninfluence on the global photometry, with there being no discernible impact in\ngalaxies more massive than ~2x10^{11} M$_{\\odot}$. We conclude that the young\nstellar populations detected in spectroscopic studies are generally centrally\nconcentrated, and that there is an upper limit on the mass of star-forming\nevents in massive galaxies. These results have ramifications for mass-to-light\nratios estimated from photometric observations.", "cat": "astro-ph", "authors": ["Robert N. Proctor", "Philip Lah", "Duncan A. Forbes", "Matthew Colless", "Warrick Couch"]}, "16": {"id": "2301.03694v2", "title": "Growth and Geometry Split in Light of the DES-Y3 Survey", "url": "http://arxiv.org/pdf/2301.03694v2", "date": "2023-06-02 19:32:22", "abs": "We test the smooth dark energy paradigm using Dark Energy Survey (DES) Year 1\nand Year 3 weak lensing and galaxy clustering data. Within the $\\Lambda$CDM and\n$w$CDM model we separate the expansion and structure growth history by\nsplitting $\\Omega_\\mathrm{m}$ (and $w$) into two meta-parameters that allow for\ndifferent evolution of growth and geometry in the Universe. We consider three\ndifferent combinations of priors on geometry from CMB, SNIa, BAO, BBN that\ndiffer in constraining power but have been designed such that the growth\ninformation comes solely from the DES weak lensing and galaxy clustering. For\nthe DES-Y1 data we find no detectable tension between growth and geometry\nmeta-parameters in both the $\\Lambda$CDM and $w$CDM parameter space. This\nstatement also holds for DES-Y3 cosmic shear and 3x2pt analyses. For the\ncombination of DES-Y3 galaxy-galaxy lensing and galaxy clustering (2x2pt) we\nmeasure a tension between our growth and geometry meta-parameters of\n2.6$\\sigma$ in the $\\Lambda$CDM and 4.48$\\sigma$ in the $w$CDM model space,\nrespectively. We attribute this tension to residual systematics in the DES-Y3\nRedMagic galaxy sample rather than to new physics. We plan to investigate our\nfindings further using alternative lens samples in DES-Y3 and future weak\nlensing and galaxy clustering datasets.", "cat": "astro-ph.CO", "authors": ["Kunhao Zhong", "Evan Saraivanov", "Vivian Miranda", "Jiachuan Xu", "Tim Eifler", "Elisabeth Krause"]}, "17": {"id": "2109.00014v1", "title": "Strong lens systems search in the Dark Energy Survey using Convolutional Neural Networks", "url": "http://arxiv.org/pdf/2109.00014v1", "date": "2021-08-31 18:00:06", "abs": "We performed a search for strong lens galaxy-scale systems in the first data\nrelease of the Dark Energy Survey (DES), from a color-selected parent sample of\n18~745~029 Luminous Red Galaxies (LRGs). Our search was based on a\nConvolutional Neural Network (CNN) to grade our LRG selection with values\nbetween 0 (non-lens) and 1 (lens). Our training set was data-driven, i.e. using\nlensed sources taken from HST COSMOS images and where the light distribution of\nthe lens plane was taken directly from DES images of our LRGs. A total of\n76~582 cutouts obtained a score above 0.9. These were visually inspected and\nresulted in two catalogs. The first one contains 405 lens candidates, where 90\npresent clear lensing features and counterparts, while the others 315 require\nmore evidence, such as higher resolution images or spectra to be conclusive. A\ntotal of 186 candidates were totally new identified in this search. The second\ncatalog includes 539 ring galaxy candidates that will be useful to train CNNs\nagainst this type of false positives. For the 90 best lens candidates we\ncarried out color-based deblending of the lens and source light without fitting\nany analytical profile to the data. The method turned out to be very efficient\nin the deblending, even for very compact objects and for objects with very\ncomplex morphology. Finally, from the 90 best lens candidates we selected 52\nsystems having one single deflector, to test an automated modeling pipeline\nwhich successfully modeled 79\\% of the sample within an acceptable amount of\ncomputing time.", "cat": "astro-ph.GA", "authors": ["K. Rojas", "E. Savary", "B. Cl\u00e9ment", "M. Maus", "F. Courbin", "C. Lemon", "J. H. H. Chan", "G. Vernardos", "R. Joseph", "R. Ca\u00f1ameras", "A. Galan"]}, "18": {"id": "1905.03279v1", "title": "Period Analysis of All-Sky Automated Survey for Supernovae (ASAS-SN) Data on Pulsating Red Giants", "url": "http://arxiv.org/pdf/1905.03279v1", "date": "2019-05-08 18:12:15", "abs": "The All-Sky Automated Survey for Supernovae (ASAS-SN) has recently used over\n2000 days of data to identify more than 50,000 variable stars, automatically\nclassify these, determine periods and amplitudes for those that are periodic --\npart of a remarkable project to classify 412,000 known variable stars, and\ndetermine their basic properties. This information about the newly-discovered\nvariables, along with the photometric data is freely available on-line. In this\npaper, we analyze ASAS-SN data on two small random samples of pulsating red\ngiants (PRGs) in detail, and compare our results with those found by ASAS-SN.\nFor the majority of a sample of 29 mostly semi-regular (SR) PRGs, the ASAS-SN\nresults are incorrect or incomplete: either the ASAS-SN periods are 2, 3, or 4\ntimes the actual period, or the ASAS-SN period is a \"long secondary period\"\nwith a shorter pulsation present, or the star is multi-periodic or otherwise\ncomplex, or the star's data are contaminated by instrumental effects. For\nalmost all of a sample of 20 of the longest-period Mira stars (period 640 days\nor more), the ASAS-SN period is actually 2 or more times the actual period. Our\nresults are not surprising, given the very complex behavior of PRGs.", "cat": "astro-ph.SR", "authors": ["John R. Percy", "Lucas Fenaux"]}, "19": {"id": "2110.07935v2", "title": "Star-Forming S0 Galaxies in SDSS-IV MaNGA Survey", "url": "http://arxiv.org/pdf/2110.07935v2", "date": "2021-11-16 00:48:45", "abs": "To investigate star-forming activities in early-type galaxies, we select a\nsample of 52 star-forming S0 galaxies (SFS0s) from the SDSS-IV MaNGA survey. We\nfind that SFS0s have smaller stellar mass compared to normal S0s in MaNGA.\nAfter matching the stellar mass to select the control sample, we find that the\nmean S\\'{e}rsic index of SFS0s' bulges (1.76$\\pm$0.21) is significantly smaller\nthan that of the control sample (2.57$\\pm$0.20), suggesting the existence of a\npseudo bulge in SFS0s. After introducing the environmental information, SFS0s\nshow smaller spin parameters in the field than in groups, while the control\nsample has no obvious difference in different environments, which may suggest\ndifferent dynamical processes in SFS0s. Furthermore, with derived N/O and O/H\nabundance ratios, SFS0s in the field show nitrogen enrichment, providing\nevidence for the accretion of metal-poor gas in the field environment. To study\nthe star formation relation, we show that the slope of the spatially resolved\nstar formation main sequence is nearly 1.0 with MaNGA IFU data, confirming the\nself-regulation of star formation activities at the kpc scales.", "cat": "astro-ph.GA", "authors": ["Ke Xu", "Qiusheng Gu", "Shiying Lu", "Xue Ge", "Mengyuan Xiao", "Emanuele Contini"]}, "20": {"id": "2311.07218v2", "title": "A Near-infrared Variability Survey of Young Planetary-mass Objects", "url": "http://arxiv.org/pdf/2311.07218v2", "date": "2023-11-28 21:46:35", "abs": "We present a photometric variability survey of young planetary-mass objects\nusing the New Technology Telescope in the Js and Ks bands. Surface gravity\nplays an important role in the atmospheric structure of brown dwarfs, as young\nlow gravity L dwarfs have a higher variability rate than field L dwarfs. In\nthis study, we extend variability studies to young T-type planetary-mass\nobjects and investigate the effects of surface gravity on the variability of L\nand T dwarfs across a large sample. We conduct continuous monitoring for 18\nobjects with spectral types from L5 to T8 and detect four new variables and two\nvariable candidates. Combining with previous variability surveys of field and\nyoung L and T objects, we find that young objects tend to be more variable than\nfield objects within peak-to-peak variability amplitude ranges of 0.5-10 per\ncent and period ranges of 1.5-20 hr. For the first time, we constrain the\nvariability rate of young T dwarfs to be 56 per cent compared to 25 per cent\nfor field T dwarfs. Both field and young samples have higher variability rates\nat the L/T transition than outside the L/T transition. The differences in the\nvariability rates between field and young samples are about 1 sigma and\ntherefore larger sample sizes are needed to confirm and refine the results.\nBesides the L/T transition, young L dwarfs with strong variability tend to\nassemble in a narrow spectral type range of L6-L7.5. This work supports the\ncritical role of surface gravity on the atmospheric structure from L to T\nspectral types.", "cat": "astro-ph.EP", "authors": ["Pengyu Liu", "Beth A. Biller", "Johanna M. Vos", "Niall Whiteford", "Zhoujian Zhang", "Michael C. Liu", "Clemence Fontanive", "Elena Manjavacas", "Thomas Henning", "Matthew A. Kenworthy", "Mariangela Bonavita", "Mickael Bonnefoy", "Emma Bubb", "Simon Petrus", "Joshua Schlieder"]}, "21": {"id": "2312.07275v2", "title": "The SARAO MeerKAT 1.3 GHz Galactic Plane Survey", "url": "http://arxiv.org/pdf/2312.07275v2", "date": "2024-05-02 10:14:44", "abs": "We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz\ncontinuum survey of almost half of the Galactic Plane (251\\deg $\\le l \\le$\n358\\deg and 2\\deg $\\le l \\le$ 61\\deg at $|b| \\le 1.5\\deg $). SMGPS is the\nlargest, most sensitive and highest angular resolution 1 GHz survey of the\nPlane yet carried out, with an angular resolution of 8\" and a broadband RMS\nsensitivity of $\\sim$10--20 $\\mu$ Jy/beam. Here we describe the first publicly\navailable data release from SMGPS which comprises data cubes of\nfrequency-resolved images over 908--1656 MHz, power law fits to the images, and\nbroadband zeroth moment integrated intensity images. A thorough assessment of\nthe data quality and guidance for future usage of the data products are given.\nFinally, we discuss the tremendous potential of SMGPS by showcasing highlights\nof the Galactic and extragalactic science that it permits. These highlights\ninclude the discovery of a new population of non-thermal radio filaments;\nidentification of new candidate supernova remnants, pulsar wind nebulae and\nplanetary nebulae; improved radio/mid-IR classification of rare Luminous Blue\nVariables and discovery of associated extended radio nebulae; new radio stars\nidentified by Bayesian cross-matching techniques; the realisation that many of\nthe largest radio-quiet WISE HII region candidates are not true HII regions;\nand a large sample of previously undiscovered background HI galaxies in the\nZone of Avoidance.", "cat": "astro-ph.GA", "authors": ["S. Goedhart", "W. D. Cotton", "F. Camilo", "M. A. Thompson", "G. Umana", "M. Bietenholz", "P. A. Woudt", "L. D. Anderson", "C. Bordiu", "D. A. H. Buckley", "C. S. Buemi", "F. Bufano", "F. Cavallaro", "H. Chen", "J. O. Chibueze", "D. Egbo", "B. S. Frank", "M. G. Hoare", "A. Ingallinera", "T. Irabor", "R. C. Kraan-Korteweg", "S. Kurapati", "P. Leto", "S. Loru", "M. Mutale", "W. O. Obonyo", "A. Plavin", "S. H. A. Rajohnson", "A. Rigby", "S. Riggi", "M. Seidu", "P. Serra", "B. M. Smart", "B. W. Stappers", "N. Steyn", "M. Surnis", "C. Trigilio", "G. M. Williams", "T. D. Abbott", "R. M. Adam", "K. M. B. Asad", "T. Baloyi", "E. F. Bauermeister", "T. G. H. Bennet", "H. Bester", "A. G. Botha", "L. R. S. Brederode", "S. Buchner", "J. P. Burger", "T. Cheetham", "K. Cloete", "M. S. de Villiers", "D. I. L. de Villiers", "L. J. du Toit", "S. W. P. Esterhuyse", "B. L. Fanaroff", "D. J. Fourie", "R. R. G. Gamatham", "T. G. Gatsi", "M. Geyer", "M. Gouws", "S. C. Gumede", "I. Heywood", "A. Hokwana", "S. W. Hoosen", "D. M. Horn", "L. M. G. Horrell", "B. V. Hugo", "A. I. Isaacson", "G. I. G. J\u00f3zsa", "J. L. Jonas", "J. D. B. L. Jordaan", "A. F. Joubert", "R. P. M. Julie", "F. B. Kapp", "N. Kriek", "H. Kriel", "V. K. Krishnan", "T. W. Kusel", "L. S. Legodi", "R. Lehmensiek", "R. T. Lord", "P. S. Macfarlane", "L. G. Magnus", "C. Magozore", "J. P. L. Main", "J. A. Malan", "J. R. Manley", "S. J. Marais", "M. D. J. Maree", "A. Martens", "P. Maruping", "K. McAlpine", "B. C. Merry", "M. Mgodeli", "R. P. Millenaar", "O. J. Mokone", "T. E. Monama", "W. S. New", "B. Ngcebetsha", "K. J. Ngoasheng", "G. D. Nicolson", "M. T. Ockards", "N. Oozeer", "S. S. Passmoor", "A. A. Patel", "A. Peens-Hough", "S. J. Perkins", "A. J. T. Ramaila", "S. M. Ratcliffe", "R. Renil", "L. L. Richter", "S. Salie", "N. Sambu", "C. T. G. Schollar", "L. C. Schwardt", "R. L. Schwartz", "M. Serylak", "R. Siebrits", "S. K. Sirothia", "M. J. Slabber", "O. M. Smirnov", "A. J. Tiplady", "T. J. van Balla", "A. van der Byl", "V. Van Tonder", "A. J. Venter", "M. Venter", "M. G. Welz", "L. P. Williams"]}, "22": {"id": "1308.2912v1", "title": "Service Discovery -- A Survey and Comparison", "url": "http://arxiv.org/pdf/1308.2912v1", "date": "2013-08-13 16:44:27", "abs": "With the increasing number of services in the internet, companies intranets,\nand home networks: service discovery becomes an integral part of modern\nnetworked system. This paper provides a comprehensive survey of major solutions\nfor service discovery. We cover techniques and features used in existing\nsystems. Although a few survey articles have been published on this object, our\ncontribution focuses on comparing and analyzing surveyed solutions according\neight prime criteria, which we have defined before. This comparison will be\nhelpful to determine limits of existing discovery protocols and identify future\nresearch opportunities in service discovery.", "cat": "cs.NI", "authors": ["Bendaoud Karim Talal", "Merzougui Rachid"]}, "23": {"id": "2105.03148v2", "title": "A State-of-the-art Survey of Object Detection Techniques in Microorganism Image Analysis: From Classical Methods to Deep Learning Approaches", "url": "http://arxiv.org/pdf/2105.03148v2", "date": "2022-04-11 07:44:04", "abs": "Microorganisms play a vital role in human life. Therefore, microorganism\ndetection is of great significance to human beings. However, the traditional\nmanual microscopic detection methods have the disadvantages of long detection\ncycle, low detection accuracy in large orders, and great difficulty in\ndetecting uncommon microorganisms. Therefore, it is meaningful to apply\ncomputer image analysis technology to the field of microorganism detection.\nComputer image analysis can realize high-precision and high-efficiency\ndetection of microorganisms. In this review, first,we analyse the existing\nmicroorganism detection methods in chronological order, from traditional image\nprocessing and traditional machine learning to deep learning methods. Then, we\nanalyze and summarize these existing methods and introduce some potential\nmethods, including visual transformers. In the end, the future development\ndirection and challenges of microorganism detection are discussed. In general,\nwe have summarized 142 related technical papers from 1985 to the present. This\nreview will help researchers have a more comprehensive understanding of the\ndevelopment process, research status, and future trends in the field of\nmicroorganism detection and provide a reference for researchers in other\nfields.", "cat": "cs.CV", "authors": ["Pingli Ma", "Chen Li", "Md Mamunur Rahaman", "Yudong Yao", "Jiawei Zhang", "Shuojia Zou", "Xin Zhao", "Marcin Grzegorzek"]}, "24": {"id": "2212.04702v2", "title": "Dark against luminous matter around isolated central galaxies: a comparative study between modern surveys and Illustris-TNG", "url": "http://arxiv.org/pdf/2212.04702v2", "date": "2023-03-06 05:50:30", "abs": "Based on independent shear measurements using the DECaLS/DR8 imaging data, we\nmeasure the weak lensing signals around isolated central galaxies (ICGs) from\nSDSS/DR7 at $z\\sim0.1$. The projected stellar mass density profiles of\nsurrounding satellite galaxies are further deduced, using photometric sources\nfrom the Hyper Suprime-Cam (HSC) survey (pDR3). The signals of ICGs $+$ their\nextended stellar halos are taken from Wang et al.(2021). All measurements are\ncompared with predictions by the Illustris-TNG300-1 simulation. We find,\noverall, a good agreement between observation and TNG300. In particular, a\ncorrection to the stellar mass of massive observed ICGs is applied based on the\ncalibration of He et al.(2013), which brings a much better agreement with\nTNG300 predicted lensing signals at $\\log_{10}M_\\ast/M_\\odot>11.1$. In real\nobservation, red ICGs are hosted by more massive dark matter halos, have more\nsatellites and more extended stellar halos than blue ICGs at fixed stellar\nmass. However, in TNG300 there are more satellites around blue ICGs at fixed\nstellar mass, and the outer stellar halos of red and blue ICGs are similar. The\nstellar halos of TNG galaxies are more extended compared with real observed\ngalaxies, especially for blue ICGs with $\\log_{10}M_\\ast/M_\\odot>10.8$. We find\nthe same trend for TNG100 galaxies and for true halo central galaxies. The\ntensions between TNG and real galaxies might indicate that satellite\ndisruptions are stronger in TNG. In both TNG300 and observation, satellites\napproximately trace the underlying dark matter distribution beyond\n$0.1R_{200}$, but the fraction of total stellar mass in TNG300 does not show\nthe same radial distribution as real galaxies.", "cat": "astro-ph.GA", "authors": ["Pedro Alonso", "Wenting Wang", "Jun Zhang", "Hekun Li", "Shi Shao", "Qi Guo", "Yanqin He", "Cai-Na Hao", "Rui Shi"]}, "25": {"id": "2212.08294v2", "title": "Understanding the early stages of galaxy formation using very metal-poor stars from the Hamburg/ESO survey", "url": "http://arxiv.org/pdf/2212.08294v2", "date": "2023-01-03 00:49:47", "abs": "We explore the chemo-dynamical properties of a sample of very metal-poor\n(VMP) stars selected from the Hamburg/ESO survey, matched with Gaia EDR3, in\nthe phase-space identified by the three integrals of motion ($L_z$, $E$,\n$I_3$). Disk and halo orbits are separated by using the criteria defined in\nCarollo et al. (2021). We found 26 stars with $[Fe/H] \\leq -2.5$ possessing\ndisk kinematics, of which 14 are extremely metal-poor. At these metallicities,\nthe number of stars with disk kinematics is three times its retrograde\ncounterpart. In the same range of metallicity we also identified 37 halo stars\nmost tightly bound to the gravitational potential of the progenitor halo. The\norigin of these stars are investigated by comparing the observational results\nwith simulated galaxies from the Aquarius Project and the IllustrisTNG\nsimulations. We found two mechanisms of formation of VMP stars with disk\nkinematics: accretion from early satellites (which is dominant), and {\\it\nin-situ} formation. These stars are very old, with ages > 12.5 Gyr ($z$ > 5),\nand they are $\\alpha$-enriched. Accretion and {\\it in-situ} formation are also\nfound for the retrograde counterparts with being accretion also the dominant\nmode. Contributing accreted satellites have stellar masses in the range\n$[10^{6}-10^9]$ M_sun, and are very gas-rich. The most bound halo stars are the\noldest detected with a median age of ~ 13.3 Gyr ($z$ ~ 11), and\n$\\alpha$-enriched. Our finding clearly show that very old, very metal-poor\nstars store important information on the first stages of assembly of our Galaxy\nand its halo.", "cat": "astro-ph.GA", "authors": ["Daniela Carollo", "Norbert Christlieb", "Patricia B. Tissera", "Emanuel Sillero"]}, "26": {"id": "2208.04601v2", "title": "The first catalogue of spectroscopically confirmed red nuggets at z~0.7 from the VIPERS survey. Linking high-z red nuggets and local relics", "url": "http://arxiv.org/pdf/2208.04601v2", "date": "2022-08-10 09:10:48", "abs": "'Red nuggets' are a rare population of passive compact massive galaxies\nthought to be the first massive galaxies that formed in the Universe. First\nfound at $z \\sim 3$, they are even less abundant at lower redshifts, and it is\nbelieved that with time they mostly transformed through mergers into today's\ngiant ellipticals. Those red nuggets which managed to escape this fate can\nserve as unique laboratories to study the early evolution of massive galaxies.\nIn this paper, we aim to make use of the VIMOS Public Extragalactic Redshift\nSurvey to build the largest up-to-date catalogue of spectroscopically confirmed\nred nuggets at the intermediate redshift $0.5 8\\times10^{10}$ $\\rm{M}_{\\odot}$ and effective radii\n$R_\\mathrm{e}<1.5$ kpc. Among them, we select red, passive galaxies with old\nstellar population based on colour--colour NUVrK diagram, star formation rate\nvalues, and verification of their optical spectra. Verifying the influence of\nthe limit of the source compactness on the selection, we found that the sample\nsize can vary even up to two orders of magnitude, depending on the chosen\ncriterion. Using one of the most restrictive criteria with additional checks on\ntheir spectra and passiveness, we spectroscopically identified only 77\npreviously unknown red nuggets. The resultant catalogue of 77 red nuggets is\nthe largest such catalogue built based on the uniform set of selection criteria\nabove the local Universe. Number density calculated on the final sample of 77\nVIPERS passive red nuggets per comoving Mpc$^3$ increases from\n4.7$\\times10^{-6}$ at $z \\sim 0.61$ to $9.8 \\times 10^{-6}$ at $z \\sim 0.95$,\nwhich is higher than values estimated in the local Universe, and lower than the\nones found at $z>2$. It fills the gap at intermediate redshift.", "cat": "astro-ph.GA", "authors": ["Krzysztof Lisiecki", "Katarzyna Ma\u0142ek", "Ma\u0142gorzata Siudek", "Agnieszka Pollo", "Janusz Krywult", "Agata Karska", "Junais"]}, "27": {"id": "2310.06726v1", "title": "Status Quo and Problems of Requirements Engineering for Machine Learning: Results from an International Survey", "url": "http://arxiv.org/pdf/2310.06726v1", "date": "2023-10-10 15:53:50", "abs": "Systems that use Machine Learning (ML) have become commonplace for companies\nthat want to improve their products and processes. Literature suggests that\nRequirements Engineering (RE) can help address many problems when engineering\nML-enabled systems. However, the state of empirical evidence on how RE is\napplied in practice in the context of ML-enabled systems is mainly dominated by\nisolated case studies with limited generalizability. We conducted an\ninternational survey to gather practitioner insights into the status quo and\nproblems of RE in ML-enabled systems. We gathered 188 complete responses from\n25 countries. We conducted quantitative statistical analyses on contemporary\npractices using bootstrapping with confidence intervals and qualitative\nanalyses on the reported problems involving open and axial coding procedures.\nWe found significant differences in RE practices within ML projects. For\ninstance, (i) RE-related activities are mostly conducted by project leaders and\ndata scientists, (ii) the prevalent requirements documentation format concerns\ninteractive Notebooks, (iii) the main focus of non-functional requirements\nincludes data quality, model reliability, and model explainability, and (iv)\nmain challenges include managing customer expectations and aligning\nrequirements with data. The qualitative analyses revealed that practitioners\nface problems related to lack of business domain understanding, unclear goals\nand requirements, low customer engagement, and communication issues. These\nresults help to provide a better understanding of the adopted practices and of\nwhich problems exist in practical environments. We put forward the need to\nadapt further and disseminate RE-related practices for engineering ML-enabled\nsystems.", "cat": "cs.SE", "authors": ["Antonio Pedro Santos Alves", "Marcos Kalinowski", "G\u00f6rkem Giray", "Daniel Mendez", "Niklas Lavesson", "Kelly Azevedo", "Hugo Villamizar", "Tatiana Escovedo", "Helio Lopes", "Stefan Biffl", "J\u00fcrgen Musil", "Michael Felderer", "Stefan Wagner", "Teresa Baldassarre", "Tony Gorschek"]}, "28": {"id": "2211.05640v1", "title": "UAV Traffic Management : A Survey On Communication Security", "url": "http://arxiv.org/pdf/2211.05640v1", "date": "2022-11-10 15:13:18", "abs": "Unmanned Aerial Systems (UAS) have a wide variety of applications, and their\ndevelopment in terms of capabilities is continuously evolving. Many missions\nperformed by an Unmanned Aerial Vehicle (UAV) require flying in public\nairspace. This requires very high safety standards, similar to those mandatory\nin commercial civil aviation. A safe UAV Traffic Management (UTM) requires\nseveral communication links between aircraft, their pilots and UTM systems. The\nintegrity of these communication links is critical for the safety of\noperations. Several security requirements also have to be met on each of these\nlinks. Unfortunately, current cryptographic standards used over the internet\nare most often not suitable to UAS due to their limited resources and dynamic\nnature. This survey discusses the security required for every communication\nlink in order to enable a safe traffic management. Research works focusing on\nthe security of communication links using cryptographic primitives are then\npresented and discussed. Authentication protocols developed for UAVs or other\nconstrained systems are compared and evaluated as solutions for UAS security.\nSymmetrical alternatives to the AES algorithm are also presented. Works to\nsecure current UTM protocols such as ADS-B and RemoteID are discussed. The\nanalysis reveals a need for the development of a complete secure architecture\nable to provide authentication and integrity to external systems (other\naircraft, UTM systems...).", "cat": "cs.CR", "authors": ["Ridwane Aissaoui", "Jean-Christophe Deneuville", "Christophe Guerber", "Alain Pirovano"]}, "29": {"id": "2405.01221v1", "title": "A Survey on Semantic Communication Networks: Architecture, Security, and Privacy", "url": "http://arxiv.org/pdf/2405.01221v1", "date": "2024-05-02 12:04:35", "abs": "Semantic communication, emerging as a breakthrough beyond the classical\nShannon paradigm, aims to convey the essential meaning of source data rather\nthan merely focusing on precise yet content-agnostic bit transmission. By\ninterconnecting diverse intelligent agents (e.g., autonomous vehicles and VR\ndevices) via semantic communications, the semantic communication networks\n(SemComNet) supports semantic-oriented transmission, efficient spectrum\nutilization, and flexible networking among collaborative agents. Consequently,\nSemComNet stands out for enabling ever-increasing intelligent applications,\nsuch as autonomous driving and Metaverse. However, being built on a variety of\ncutting-edge technologies including AI and knowledge graphs, SemComNet\nintroduces diverse brand-new and unexpected threats, which pose obstacles to\nits widespread development. Besides, due to the intrinsic characteristics of\nSemComNet in terms of heterogeneous components, autonomous intelligence, and\nlarge-scale structure, a series of critical challenges emerge in securing\nSemComNet. In this paper, we provide a comprehensive and up-to-date survey of\nSemComNet from its fundamentals, security, and privacy aspects. Specifically,\nwe first introduce a novel three-layer architecture of SemComNet for\nmulti-agent interaction, which comprises the control layer, semantic\ntransmission layer, and cognitive sensing layer. Then, we discuss its working\nmodes and enabling technologies. Afterward, based on the layered architecture\nof SemComNet, we outline a taxonomy of security and privacy threats, while\ndiscussing state-of-the-art defense approaches. Finally, we present future\nresearch directions, clarifying the path toward building intelligent, robust,\nand green SemComNet. To our knowledge, this survey is the first to\ncomprehensively cover the fundamentals of SemComNet, alongside a detailed\nanalysis of its security and privacy issues.", "cat": "cs.NI", "authors": ["Shaolong Guo", "Yuntao Wang", "Ning Zhang", "Zhou Su", "Tom H. Luan", "Zhiyi Tian", "Xuemin Shen"]}, "30": {"id": "2407.15855v1", "title": "Data Poisoning Attacks in Intelligent Transportation Systems: A Survey", "url": "http://arxiv.org/pdf/2407.15855v1", "date": "2024-07-06 01:02:22", "abs": "Emerging technologies drive the ongoing transformation of Intelligent\nTransportation Systems (ITS). This transformation has given rise to\ncybersecurity concerns, among which data poisoning attack emerges as a new\nthreat as ITS increasingly relies on data. In data poisoning attacks, attackers\ninject malicious perturbations into datasets, potentially leading to inaccurate\nresults in offline learning and real-time decision-making processes. This paper\nconcentrates on data poisoning attack models against ITS. We identify the main\nITS data sources vulnerable to poisoning attacks and application scenarios that\nenable staging such attacks. A general framework is developed following\nrigorous study process from cybersecurity but also considering specific ITS\napplication needs. Data poisoning attacks against ITS are reviewed and\ncategorized following the framework. We then discuss the current limitations of\nthese attack models and the future research directions. Our work can serve as a\nguideline to better understand the threat of data poisoning attacks against ITS\napplications, while also giving a perspective on the future development of\ntrustworthy ITS.", "cat": "cs.CR", "authors": ["Feilong Wang", "Xin Wang", "Xuegang Ban"]}, "31": {"id": "2402.06641v3", "title": "A Survey of a Random Matrix Model for a Family of Cusp Forms", "url": "http://arxiv.org/pdf/2402.06641v3", "date": "2024-04-17 14:42:11", "abs": "The Katz-Sarnak philosophy states that statistics of zeros of $L$-function\nfamilies near the central point as the conductors tend to infinity agree with\nthose of eigenvalues of random matrix ensembles as the matrix size tends to\ninfinity. While numerous results support this conjecture, S. J. Miller observed\nthat for finite conductors, very different behavior can occur for zeros near\nthe central point in elliptic curve families. This led to the excised model of\nDue\\~{n}ez, Huynh, Keating, Miller, and Snaith, whose predictions for quadratic\ntwists of a given elliptic curve are beautifully fit by the data. The key\ningredients are relating the discretization of central values of the\n$L$-functions to excising matrices based on the value of the characteristic\npolynomials at 1 and using lower order terms (in statistics such as the\none-level density and pair-correlation) to adjust the matrix size. We discuss\nrecent successes by the authors in extending this model to a family of\nquadratic twists of finite conductor of a given holomorphic cuspidal newform of\nlevel an odd prime level. In particular, we predict very little repulsion for\nforms with weight greater than 2.", "cat": "math.NT", "authors": ["Owen Barrett", "Zo\u00eb X. Batterman", "Aditya Jambhale", "Steven J. Miller", "Akash L. Narayanan", "Kishan Sharma", "Chris Yao"]}, "32": {"id": "1507.02737v1", "title": "The Next Generation Virgo Cluster Survey. IX. Estimating the Efficiency of Galaxy Formation on the Lowest-Mass Scales", "url": "http://arxiv.org/pdf/1507.02737v1", "date": "2015-07-09 23:01:20", "abs": "The Next Generation Virgo Cluster Survey has recently determined the\nluminosity function of galaxies in the core of the Virgo cluster down to\nunprecedented magnitude and surface brightness limits. Comparing simulations of\ncluster formation to the derived central stellar mass function, we attempt to\nestimate the stellar-to-halo-mass ratio (SHMR) for dwarf galaxies, as it would\nhave been before they fell into the cluster. This approach ignores several\ndetails and complications, e.g., the contribution of ongoing star formation to\nthe present-day stellar mass of cluster members, and the effects of adiabatic\ncontraction and/or violent feedback on the subhalo and cluster potentials. The\nfinal results are startlingly simple, however; we find that the trends in the\nSHMR determined previously for bright galaxies appear to extend down in a\nscale-invariant way to the faintest objects detected in the survey. These\nresults extend measurements of the formation efficiency of field galaxies by\ntwo decades in halo mass, or five decades in stellar mass, down to some of the\nleast massive dwarf galaxies known, with stellar masses of $\\sim 10^5 M_\\odot$.", "cat": "astro-ph.GA", "authors": ["Jonathan Grossauer", "James E. Taylor", "Laura Ferrarese", "Lauren A. MacArthur", "Patrick Cote", "Joel Roediger", "Stephane Courteau", "Jean-Charles Cuillandre", "Pierre-Alain Duc", "Patrick R. Durrell", "S. D. J. Gwyn", "Andres Jordan", "Simona Mei", "Eric W. Peng"]}, "33": {"id": "2403.19683v1", "title": "Corrigendum of \"Construction of Kuranishi structures on the moduli spaces of pseudo holomorphic disks I, Surveys in Differential Geometry XXII (2018), 133-190\"", "url": "http://arxiv.org/pdf/2403.19683v1", "date": "2024-02-28 01:11:07", "abs": "This is a corrigendum of Lemma 9.1 of the paper [FOOO3] in the title. This\nlemma is not correct as pointed out by A. Daemi and a referee of the paper\n[DF]. The corrigendum does not affect the applications of this lemma in [FOOO3]\nand other papers and exactly the same proofs as therein apply if one replaces\nthe statement of [FOOO3,Lemma 9.1] by Lemma 2 of the present note.", "cat": "math.SG", "authors": ["Kenji Fukaya", "Yong-Geun Oh", "Hiroshi Ohta", "Kaoru Ono"]}, "34": {"id": "1807.06346v1", "title": "A Survey on Essential Components of a Self-Sovereign Identity", "url": "http://arxiv.org/pdf/1807.06346v1", "date": "2018-07-17 11:13:38", "abs": "This paper provides an overview of the Self-Sovereign Identity (SSI) concept,\nfocusing on four different components that we identified as essential to the\narchitecture. Self-Sovereign Identity is enabled by the new development of\nblockchain technology. Through the trustless, decentralised database that is\nprovided by a blockchain, classic Identity Management registration processes\ncan be replaced. We start off by giving a simple overview of blockchain based\nSSI, introducing an architecture overview as well as relevant actors in such a\nsystem. We further distinguish two major approaches, namely the Identifier\nRegistry Model and its extension the Claim Registry Model. Subsequently we\ndiscuss identifiers in such a system, presenting past research in the area and\ncurrent approaches in SSI in the context of Zooko's Triangle. As the user of an\nSSI has to be linked with his digital identifier we also discuss authentication\nsolutions. Most central to the concept of an SSI are the verifiable claims that\nare presented to relying parties. Resources in the field are only losely\nconnected. We will provide a more coherent view of verifiable claims in regards\nto blockchain based SSI and clarify differences in the used terminology.\nStorage solutions for the verifiable claims, both on- and off-chain, are\npresented with their advantages and disadvantages.", "cat": "cs.CR", "authors": ["Alexander M\u00fchle", "Andreas Gr\u00fcner", "Tatiana Gayvoronskaya", "Christoph Meinel"]}, "35": {"id": "1710.10715v1", "title": "The VIMOS Ultra-Deep Survey: evidence for AGN feedback in galaxies with CIII]-$\u03bb$1908\u00c5~emission 10.8 to 12.5 Gyr ago", "url": "http://arxiv.org/pdf/1710.10715v1", "date": "2017-10-29 23:19:28", "abs": "We analyze the CIII]-1908\\AA emission properties in a sample of 3899\nstar-forming galaxies (SFGs) at 23\\AA, including 20% with 310\\AA. A significant fraction of 1.2% of SFGs presents\nstrong CIII] emission 2010^10 MSun at z~3 into the population\nof quiescent galaxies observed at redshift z~1-2.", "cat": "astro-ph.GA", "authors": ["O. Le F\u00e8vre", "B. C. Lemaux", "K. Nakajima", "D. Schaerer", "M. Talia", "G. Zamorani", "P. Cassata", "B. Garilli", "D. Maccagni", "L. Pentericci", "L. A. M. Tasca", "E. Zucca", "R. Amorin", "S. Bardelli", "A. Cimatti", "M. Giavalisco", "L. Guaita", "N. P. Hathi", "F. Marchi", "E. Vanzella", "D. Vergani", "J. Dunlop"]}, "36": {"id": "0806.3979v1", "title": "The NStED Exoplanet Transit Survey Service", "url": "http://arxiv.org/pdf/0806.3979v1", "date": "2008-06-24 20:20:58", "abs": "The NASA Star and Exoplanet Database (NStED) is a general purpose stellar\narchive with the aim of providing support for NASA's planet finding and\ncharacterization goals, stellar astrophysics, and the planning of NASA and\nother space missions. There are two principal components of NStED: a database\nof (currently) 140,000 nearby stars and exoplanet-hosting stars, and an archive\ndedicated to high-precision photometric surveys for transiting exoplanets. We\npresent a summary of the latter component: the NStED Exoplanet Transit Survey\nService (NStED-ETSS), along with its content, functionality, tools, and user\ninterface. NStED-ETSS currently serves data from the TrES Survey of the Kepler\nField as well as dedicated photometric surveys of four stellar clusters.\nNStED-ETSS aims to serve both the surveys and the broader astronomical\ncommunity by archiving these data and making them available in a homogeneous\nformat. Examples of usability of ETSS include investigation of any\ntime-variable phenomena in data sets not studied by the original survey team,\napplication of different techniques or algorithms for planet transit\ndetections, combination of data from different surveys for given objects,\nstatistical studies, etc. NStED-ETSS can be accessed at\n\\tt{http://nsted.ipac.caltech.edu}", "cat": "astro-ph", "authors": ["K. von Braun", "M. Abajian", "B. Ali", "R. Baker", "G. B. Berriman", "N-M. Chiu", "D. R. Ciardi", "J. Good", "S. R. Kane", "A. C. Laity", "D. L. McElroy", "S. Monkewitz", "A. N. Payne", "S. Ramirez", "M. Schmitz", "J. R. Stauffer", "P. L. Wyatt", "A. Zhang"]}, "37": {"id": "1305.6654v1", "title": "SZ observations with AMI of the hottest galaxy clusters detected in the XMM-Newton Cluster Survey", "url": "http://arxiv.org/pdf/1305.6654v1", "date": "2013-05-28 23:16:18", "abs": "We have obtained deep SZ observations towards 15 of the apparently hottest\nXMM Cluster Survey (XCS) clusters that can be observed with the Arcminute\nMicrokelvin Imager (AMI). We use a Bayesian analysis to quantify the\nsignificance of our SZ detections. We detect the SZ effect at high significance\ntowards three of the clusters and at lower significance for a further two\nclusters. Towards the remaining ten clusters, no clear SZ signal was measured.\nWe derive cluster parameters using the XCS mass estimates as a prior in our\nBayesian analysis. For all AMI-detected clusters, we calculate large-scale mass\nand temperature estimates while for all undetected clusters we determine upper\nlimits on these parameters. We find that the large- scale mean temperatures\nderived from our AMI SZ measurements (and the upper limits from null\ndetections) are substantially lower than the XCS-based core-temperature\nestimates. For clusters detected in the SZ, the mean temperature is, on\naverage, a factor of 1.4 lower than temperatures from the XCS. For clusters\nundetected in SZ, the average 68% upper limit on the mean temperature is a\nfactor of 1.9 below the XCS temperature.", "cat": "astro-ph.CO", "authors": ["AMI Consortium", ":", "Timothy W. Shimwell", "Carmen Rodriguez-Gonzalvez", "Farhan Feroz", "Thomas M. O. Franzen", "Keith J. B. Grainge", "Michael P. Hobson", "Natasha Hurley-Walker", "Anthony N. Lasenby", "E. J. Lloyd-Davies", "Malak Olamaie", "Yvette C. Perrott", "Guy G. Pooley", "Clare Rumsey", "A. Kathy Romer", "Richard D. E. Saunders", "Anna M. M. Scaife", "Michel P. Schammel", "Paul F. Scott", "David J. Titterington", "Elizabeth M. Waldram"]}, "38": {"id": "2304.10968v3", "title": "The role of stabilization in the virtual element method: a survey", "url": "http://arxiv.org/pdf/2304.10968v3", "date": "2023-07-26 13:58:27", "abs": "The virtual element method was introduced 10 years ago and it has generated a\nlarge number of theoretical results and applications ever since. Here, we\noverview the main mathematical results concerning the stabilization term of the\nmethod as an introduction for newcomers in the field. In particular, we\nsummarize the proofs of some results for two dimensional ``nodal'' conforming\nand nonconforming virtual element spaces to pinpoint the essential tools used\nin the stability analysis. We discuss their extensions to several other virtual\nelements. Finally, we show several ways to prove interpolation estimates,\nincluding a recent one that is based on employing the stability bounds.", "cat": "math.NA", "authors": ["L. Mascotto"]}, "39": {"id": "2103.14690v1", "title": "The NEWFIRM HETDEX Survey: Photometric Catalog and a Conservative Sample of Massive Quiescent Galaxies at z=3-5 over 17.5 deg^2 in the SHELA Field", "url": "http://arxiv.org/pdf/2103.14690v1", "date": "2021-03-26 18:55:28", "abs": "We present the results of a deep K_s-band (2.1 um) imaging survey of the\nSpitzer/HETDEX Exploratory Large Area (SHELA) field using the NEWFIRM\nnear-infrared (NIR) camera on the KPNO Mayall 4-m telescope. This NEWFIRM\nHETDEX Survey (NHS) reaches a 5-sigma depth of 22.4 AB mag (2\"-diameter\napertures corrected to total), is ~50% and 90% complete at K~22.65 and K~22.15,\nrespectively, and covers 22 deg^2 of the 24 deg^2 SHELA Spitzer/ IRAC footprint\n(within ``Stripe 82' of the Sloan Digital Sky Survey). We present a\nK_s-band-selected catalog which includes deep ugriz imaging from the Dark\nEnergy Camera and 3.6 and 4.5 um imaging from Spitzer/IRAC, with\nforced-photometry of 1.7 million sources across 17.5 deg^2. The large area and\nmoderate depth of this catalog enables the study of the most massive galaxies\nat high redshift, and minimizes uncertainties associated with counting\nstatistics and cosmic variance. As a demonstration, we derive stellar masses\n(M*) and star-formation rates (SFRs) for candidate galaxies at 3 < z < 5, and\nselect a conservative sample of nine candidate massive (M* > 10^11 Msol)\nquiescent galaxies, which have measured SFRs significantly below the\nmain-sequence at this redshift. Five are ultra-massive with M* > 10^12, though\nuncertainties in IRAC blending, gravitational lensing, or AGN emission could\nresult in true masses which are lower. Simulations predict that these galaxies\nshould be extremely rare, thus we discuss what physical processes in models\ncould be altered to allow the formation of such massive quiescent galaxies at\nsuch early times.", "cat": "astro-ph.GA", "authors": ["Matthew L. Stevans", "Steven L. Finkelstein", "Lalitwadee Kawinwanichakij", "Isak Wold", "Casey Papovich", "Rachel S. Somerville", "L. Y. Aaron Yung", "Sydney Sherman", "Robin Ciardullo", "Romeel Dave", "Jonathan Florez", "Caryl Gronwall", "Shardha Jogee"]}, "40": {"id": "2207.08993v4", "title": "Machine Learning in Orbit Estimation: a Survey", "url": "http://arxiv.org/pdf/2207.08993v4", "date": "2024-04-07 17:59:07", "abs": "Since the late 1950s, when the first artificial satellite was launched, the\nnumber of Resident Space Objects has steadily increased. It is estimated that\naround one million objects larger than one cm are currently orbiting the Earth,\nwith only thirty thousand larger than ten cm being tracked. To avert a chain\nreaction of collisions, known as Kessler Syndrome, it is essential to\naccurately track and predict debris and satellites' orbits. Current approximate\nphysics-based methods have errors in the order of kilometers for seven-day\npredictions, which is insufficient when considering space debris, typically\nwith less than one meter. This failure is usually due to uncertainty around the\nstate of the space object at the beginning of the trajectory, forecasting\nerrors in environmental conditions such as atmospheric drag, and unknown\ncharacteristics such as the mass or geometry of the space object. Operators can\nenhance Orbit Prediction accuracy by deriving unmeasured objects'\ncharacteristics and improving non-conservative forces' effects by leveraging\ndata-driven techniques, such as Machine Learning. In this survey, we provide an\noverview of the work in applying Machine Learning for Orbit Determination,\nOrbit Prediction, and atmospheric density modeling.", "cat": "astro-ph.EP", "authors": ["Francisco Caldas", "Cl\u00e1udia Soares"]}, "41": {"id": "2110.05989v12", "title": "Furstenberg's Times 2, Times 3 Conjecture (a Short Survey)", "url": "http://arxiv.org/pdf/2110.05989v12", "date": "2023-05-17 18:05:32", "abs": "The following is a concise exposition on the conjecture and three of its\nproofs for the case of positive entropy, by D. Rudolph [22] , by B. Host [14]\nand by W. Parry [21]. A simpler theorem of R. Lyons [19] - preceding them - is\nalso presented and proved. This is a survey, no new results are introduced.", "cat": "math.DS", "authors": ["Matan Tal"]}, "42": {"id": "1101.1559v2", "title": "The Eighth Data Release of the Sloan Digital Sky Survey: First Data from SDSS-III", "url": "http://arxiv.org/pdf/1101.1559v2", "date": "2011-02-25 13:45:07", "abs": "The Sloan Digital Sky Survey (SDSS) started a new phase in August 2008, with\nnew instrumentation and new surveys focused on Galactic structure and chemical\nevolution, measurements of the baryon oscillation feature in the clustering of\ngalaxies and the quasar Ly alpha forest, and a radial velocity search for\nplanets around ~8000 stars. This paper describes the first data release of\nSDSS-III (and the eighth counting from the beginning of the SDSS). The release\nincludes five-band imaging of roughly 5200 deg^2 in the Southern Galactic Cap,\nbringing the total footprint of the SDSS imaging to 14,555 deg^2, or over a\nthird of the Celestial Sphere. All the imaging data have been reprocessed with\nan improved sky-subtraction algorithm and a final, self-consistent photometric\nrecalibration and flat-field determination. This release also includes all data\nfrom the second phase of the Sloan Extension for Galactic Understanding and\nEvolution (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars\nat both high and low Galactic latitudes. All the more than half a million\nstellar spectra obtained with the SDSS spectrograph have been reprocessed\nthrough an improved stellar parameters pipeline, which has better determination\nof metallicity for high metallicity stars.", "cat": "astro-ph.IM", "authors": ["SDSS-III collaboration", ":", "Hiroaki Aihara", "Carlos Allende Prieto", "Deokkeun An", "Scott F. Anderson", "\u00c9ric Aubourg", "Eduardo Balbinot", "Timothy C. Beers", "Andreas A. Berlind", "Steven J. Bickerton", "Dmitry Bizyaev", "Michael R. Blanton", "John J. Bochanski", "Adam S. Bolton", "Jo Bovy", "W. N. Brandt", "J. Brinkmann", "Peter J. Brown", "Joel R. Brownstein", "Nicolas G. Busca", "Heather Campbell", "Michael A. Carr", "Yanmei Chen", "Cristina Chiappini", "Johan Comparat", "Natalia Connolly", "Marina Cortes", "Rupert A. C. Croft", "Antonio J. Cuesta", "Luiz N. da Costa", "James R. A. Davenport", "Kyle Dawson", "Saurav Dhital", "Anne Ealet", "Garrett L. Ebelke", "Edward M. Edmondson", "Daniel J. Eisenstein", "Stephanie Escoffier", "Massimiliano Esposito", "Michael L. Evans", "Xiaohui Fan", "Bruno Femen\u00ed a Castell\u00e1", "Andreu Font-Ribera", "Peter M. Frinchaboy", "Jian Ge", "Bruce A. Gillespie", "G. Gilmore", "Jonay I. Gonz\u00e1lez Hern\u00e1ndez", "J. Richard Gott", "Andrew Gould", "Eva K. Grebel", "James E. Gunn", "Jean-Christophe Hamilton", "Paul Harding", "David W. Harris", "Suzanne L. Hawley", "Frederick R. Hearty", "Shirley Ho", "David W. Hogg", "Jon A. Holtzman", "Klaus Honscheid", "Naohisa Inada", "Inese I. Ivans", "Linhua Jiang", "Jennifer A. Johnson", "Cathy Jordan", "Wendell P. Jordan", "Eyal A. Kazin", "David Kirkby", "Mark A. Klaene", "G. R. Knapp", "Jean-Paul Kneib", "C. S. Kochanek", "Lars Koesterke", "Juna A. Kollmeier", "Richard G. Kron", "Hubert Lampeitl", "Dustin Lang", "Jean-Marc Le Goff", "Young Sun Lee", "Yen-Ting Lin", "Daniel C. Long", "Craig P. Loomis", "Sara Lucatello", "Britt Lundgren", "Robert H. Lupton", "Zhibo Ma", "Nicholas MacDonald", "Suvrath Mahadevan", "Marcio A. G. Maia", "Martin Makler", "Elena Malanushenko", "Viktor Malanushenko", "Rachel Mandelbaum", "Claudia Maraston", "Daniel Margala", "Karen L. Masters", "Cameron K. McBride", "Peregrine M. McGehee", "Ian D. McGreer", "Brice M\u00e9nard", "Jordi Miralda-Escud\u00e9", "Heather L. Morrison", "F. Mullally", "Demitri Muna", "Jeffrey A. Munn", "Hitoshi Murayama", "Adam D. Myers", "Tracy Naugle", "Angelo Fausti Neto", "Duy Cuong Nguyen", "Robert C. Nichol", "Robert W. O'Connell", "Ricardo L. C. Ogando", "Matthew D. Olmstead", "Daniel J. Oravetz", "Nikhil Padmanabhan", "Nathalie Palanque-Delabrouille", "Kaike Pan", "Parul Pandey", "Isabelle P\u00e2ris", "Will J. Percival", "Patrick Petitjean", "Robert Pfaffenberger", "Janine Pforr", "Stefanie Phleps", "Christophe Pichon", "Matthew M. Pieri", "Francisco Prada", "Adrian M. Price-Whelan", "M. Jordan Raddick", "Beatriz H. F. Ramos", "C\u00e9line Reyl\u00e9", "James Rich", "Gordon T. Richards", "Hans-Walter Rix", "Annie C. Robin", "Helio J. Rocha-Pinto", "Constance M. Rockosi", "Natalie A. Roe", "Emmanuel Rollinde", "Ashley J. Ross", "Nicholas P. Ross", "Bruno M. Rossetto", "Ariel G. S\u00e1nchez", "Conor Sayres", "David J. Schlegel", "Katharine J. Schlesinger", "Sarah J. Schmidt", "Donald P. Schneider", "Erin Sheldon", "Yiping Shu", "Jennifer Simmerer", "Audrey E. Simmons", "Thirupathi Sivarani", "Stephanie A. Snedden", "Jennifer S. Sobeck", "Matthias Steinmetz", "Michael A. Strauss", "Alexander S. Szalay", "Masayuki Tanaka", "Aniruddha R. Thakar", "Daniel Thomas", "Jeremy L. Tinker", "Benjamin M. Tofflemire", "Rita Tojeiro", "Christy A. Tremonti", "Jan Vandenberg", "M. Vargas Maga\u00f1a", "Licia Verde", "Nicole P. Vogt", "David A. Wake", "Ji Wang", "Benjamin A. Weaver", "David H. Weinberg", "Martin White", "Simon D. M. White", "Brian Yanny", "Naoki Yasuda", "Christophe Yeche", "Idit Zehavi"]}, "43": {"id": "2011.04677v2", "title": "MAGNUM survey: Compact jets causing large turmoil in galaxies -- Enhanced line widths perpendicular to radio jets as tracers of jet-ISM interaction", "url": "http://arxiv.org/pdf/2011.04677v2", "date": "2021-02-25 19:00:08", "abs": "Outflows accelerated by AGN are commonly observed in the form of coherent,\nmildly collimated high-velocity gas directed along the AGN ionisation cones and\nkinetically powerful (>$10^{44-45}$ erg/s) jets. Recent works found that\noutflows can also be accelerated by low-power (<$10^{44}$ erg/s) jets, and the\nmost recent cosmological simulations indicate that these are the dominant\nsource of feedback on sub-kpc scales. We study the relation between radio jets\nand the distribution and kinematics of the ionised gas in IC 5063, NGC 5643,\nNGC 1068, and NGC 1386 as part of our MAGNUM survey of nearby Seyfert galaxies.\nAll these objects host a small-scale (<1 kpc) low-power (<$10^{44}$ erg/s)\nradio jet that has small inclinations (<45\\deg) with respect to the galaxy\ndisc. We employed seeing-limited optical integral field spectroscopic\nobservations from MUSE at VLT to obtain flux, kinematic, and excitation maps of\nthe extended ionised gas, that we compared with archival radio images and\nChandra X-ray observations. We detect a strong (up to >800-1000 km/s), extended\n(>1 kpc) and shock-excited emission-line velocity spread perpendicular to the\nAGN ionisation cones and jets in all four targets. These broad and symmetric\nline profiles are not associated with a single coherent velocity of the gas,\ndifferently from the 'classical' asymmetric-line outflow observed along the\nionisation cones and jets. We interpret the observed phenomenon as due to the\naction of the jets perturbing the gas in the galaxy disc. These intense and\nextended velocity spreads perpendicular to AGN jets and cones are indeed\ncurrently only observed in galaxies hosting a low-power jet whose inclination\nis sufficiently low with respect to the galaxy disc to impact on and strongly\naffect its material. In line with cosmological simulations, our results\ndemonstrate that low-power jets are indeed capable of affecting the host\ngalaxy.", "cat": "astro-ph.GA", "authors": ["G. Venturi", "G. Cresci", "A. Marconi", "M. Mingozzi", "E. Nardini", "S. Carniani", "F. Mannucci", "A. Marasco", "R. Maiolino", "M. Perna", "E. Treister", "J. Bland-Hawthorn", "J. Gallimore"]}, "44": {"id": "2210.07252v1", "title": "The McDonald Accelerating Stars Survey (MASS): Architecture of the Ancient Five-Planet Host System Kepler-444", "url": "http://arxiv.org/pdf/2210.07252v1", "date": "2022-10-13 18:00:01", "abs": "We present the latest and most precise characterization of the architecture\nfor the ancient ($\\approx 11$ Gyr) Kepler-444 system, which is composed of a K0\nprimary star (Kepler-444 A) hosting five transiting planets, and a tight M-type\nspectroscopic binary (Kepler-444 BC) with an A-BC projected separation of 66\nau. We have measured the system's relative astrometry using the adaptive optics\nimaging from Keck/NIRC2 and Kepler-444 A's radial velocities from the Hobby\nEberly Telescope, and re-analyzed relative radial velocities between BC and A\nfrom Keck/HIRES. We also include the Hipparcos-Gaia astrometric acceleration\nand all published astrometry and radial velocities into an updated orbit\nanalysis of BC's barycenter. These data greatly extend the time baseline of the\nmonitoring and lead to significant updates to BC's barycentric orbit compared\nto previous work, including a larger semi-major axis ($a = 52.2^{+3.3}_{-2.7}$\nau), a smaller eccentricity ($e = 0.55 \\pm 0.05$), and a more precise\ninclination ($i =85.4^{+0.3}_{-0.4}$ degrees). We have also derived the first\ndynamical masses of B and C components. Our results suggest Kepler-444~A's\nprotoplanetary disk was likely truncated by BC to a radius of $\\approx 8$ au,\nwhich resolves the previously noticed tension between Kepler-444 A's disk mass\nand planet masses. Kepler-444 BC's barycentric orbit is likely aligned with\nthose of A's five planets, which might be primordial or a consequence of\ndynamical evolution. The Kepler-444 system demonstrates that compact\nmulti-planet systems residing in hierarchical stellar triples can form at early\nepochs of the Universe and survive their secular evolution throughout cosmic\ntime.", "cat": "astro-ph.EP", "authors": ["Zhoujian Zhang", "Brendan P. Bowler", "Trent J. Dupuy", "Timothy D. Brandt", "G. Mirek Brandt", "William D. Cochran", "Michael Endl", "Phillip J. MacQueen", "Kaitlin M. Kratter", "Howard T. Isaacson", "Kyle Franson", "Adam L. Kraus", "Caroline V. Morley", "Yifan Zhou"]}, "45": {"id": "1307.2236v1", "title": "A Megacam Survey of Outer Halo Satellites. II. Blue Stragglers in the Lowest Stellar Density Systems", "url": "http://arxiv.org/pdf/1307.2236v1", "date": "2013-07-08 20:00:01", "abs": "We present a homogeneous study of blue straggler stars across ten outer halo\nglobular clusters, three classical dwarf spheroidal and nine ultra-faint\ngalaxies based on deep and wide-field photometric data taken with MegaCam on\nthe Canada-France-Hawaii Telescope. We find blue straggler stars to be\nubiquitous among these Milky Way satellites. Based on these data, we can test\nthe importance of primordial binaries or multiple systems on blue straggler\nstar formation in low density environments. For the outer halo globular\nclusters we find an anti-correlation between the specific frequency of blue\nstraggler and absolute magnitude, similar to that previously observed for inner\nhalo clusters. When plotted against density and encounter rate, the frequency\nof blue stragglers are well fitted by single trends with smooth transitions\nbetween dwarf galaxies and globular clusters, which points to a common origin\nfor their blue stragglers. The fraction of blue stragglers stays constant and\nhigh in the low encounter rate regime spanned by our dwarf galaxies, and\ndecreases with density and encounter rate in the range spanned by our globular\nclusters. We find that young stars can mimic blue stragglers in dwarf galaxies\nonly if their ages are 2.5+/-0.5 Gyr and they represent ~1-7% of the total\nnumber of stars, which we deem highly unlikely. These results point to\nmass-transfer or mergers of primordial binaries or multiple systems as the\ndominant blue straggler formation mechanism in low density systems.", "cat": "astro-ph.GA", "authors": ["Felipe A. Santana", "Ricardo R. Munoz", "Marla Geha", "Patrick Cote", "Peter Stetson", "Joshua D. Simon", "S. G. Djorgovski"]}, "46": {"id": "1712.09882v1", "title": "A survey of TiO\u03bb567 nm absorption in solar-type stars", "url": "http://arxiv.org/pdf/1712.09882v1", "date": "2017-12-28 14:57:59", "abs": "Molecular absorption bands are estimators of stellar activity and spot cycles\non magnetically active stars. We have previously introduced a new color index\nthat compare absorption strength of the titanium oxide (TiO) at 567 nm with\nnearby continuum. In this paper we implement this index to measure long-term\nactivity variations and the statistical properties of the index in a sample of\n302 solar-type stars from the HARPS planet search program. The results indicate\na pattern of change in star's activity, covers a range of periods from 2 years\nup to 17 years.", "cat": "astro-ph.SR", "authors": ["Fatemeh Azizi", "Mohammad Taghi Mirtorabi"]}, "47": {"id": "1912.09271v1", "title": "Survey of deformation in nuclei in order to estimate the enhancement of sensitivity to atomic EDM", "url": "http://arxiv.org/pdf/1912.09271v1", "date": "2019-12-19 15:16:59", "abs": "The observed baryon asymmetry of the universe (BAU) cannot be explained by\nthe known sources of charge-parity (CP)-violation in the Standard Model (SM). A\nnon-zero permanent electric-dipole-moment (EDM) for fundamental particles,\nnuclei or atoms, violates CP. Measuring a non-zero EDM allows us to gain a\nhandle on additional sources of CP-violation required to explain the observed\nBAU. The EDM of an atom with an octupole and quadrupole deformed nucleus is\nenhanced. Therefore, the search for such atoms has become important in the\nquest to measure an EDM. Viability of EDM searches in $^{225}$Ra atoms with a\ndeformed nucleus have already been demonstrated. We have performed a\ncomprehensive survey for possible EDM candidates from a list of octupole\ndeformed nuclei predicted by various theoretical models. Our search of\nlong-lived isotopes with nuclear deformations comparable to or better than\n$^{225}$Ra results in a handful of viable candidates for future atomic EDM\nexperiments based out of the Facility for Rare Isotope Beams (FRIB):\n$^{221}$Rn, $^{221,223,227}$Fr, $^{221,223,225}$Ra, $^{223,225,227}$Ac,\n$^{229}$Th, and particularly $^{229}$Pa. Furthermore, nuclei of $^{223,225}$Rn,\n$^{225}$Fr and $^{226}$Ac are also highly quadrupole and octupole deformed, but\ntheir ground state parity doublet energy difference has not yet been measured.", "cat": "nucl-ex", "authors": ["Prajwal Mohanmurthy", "Umesh Silwal", "Durga P. Siwakoti", "Jeff A. Winger"]}, "48": {"id": "1703.06716v1", "title": "The GTC exoplanet transit spectroscopy survey. VII. Detection of sodium in WASP-52b's cloudy atmosphere", "url": "http://arxiv.org/pdf/1703.06716v1", "date": "2017-03-20 12:47:31", "abs": "We report the first detection of sodium absorption in the atmosphere of the\nhot Jupiter WASP-52b. We observed one transit of WASP-52b with the\nlow-resolution Optical System for Imaging and low-Intermediate-Resolution\nIntegrated Spectroscopy (OSIRIS) at the 10.4 m Gran Telescopio Canarias (GTC).\nThe resulting transmission spectrum, covering the wavelength range from 522 nm\nto 903 nm, is flat and featureless, except for the significant narrow\nabsorption signature at the sodium doublet, which can be explained by an\natmosphere in solar composition with clouds at 1 mbar. A cloud-free atmosphere\nis stringently ruled out. By assessing the absorption depths of sodium in\nvarious bin widths, we find that temperature increases towards lower\natmospheric pressure levels, with a positive temperature gradient of 0.88 +/-\n0.65 K/km, possibly indicative of upper atmospheric heating and a temperature\ninversion.", "cat": "astro-ph.EP", "authors": ["G. Chen", "E. Palle", "L. Nortmann", "F. Murgas", "H. Parviainen", "G. Nowak"]}, "49": {"id": "2303.09737v2", "title": "Jackknife empirical likelihood with complex surveys", "url": "http://arxiv.org/pdf/2303.09737v2", "date": "2023-03-27 03:27:10", "abs": "We propose the so-called jackknife empirical likelihood approach for the\nsurvey data of general unequal probability sampling designs, and analyze\nparameters defined according to U-statistics. We prove theoretically that\njackknife pseudo-empirical likelihood ratio statistic is asymptotically\ndistributed as a chi-square random variable, and can be used to construct\nconfidence intervals for complex survey samples. In the process of research, we\nconsider with or without auxiliary information, utilizing design weights or\ncalibration weights. Simulation studies are included to examine that in terms\nof coverage probability and tail error rates, the jackknife pseudo-empirical\nlikelihood ratio confidence intervals are superior to those based on the normal\napproximation.", "cat": "stat.ME", "authors": ["Mengdong Shang", "Xia Chen"]}, "50": {"id": "2303.14320v2", "title": "A Survey on Model-based, Heuristic, and Machine Learning Optimization Approaches in RIS-aided Wireless Networks", "url": "http://arxiv.org/pdf/2303.14320v2", "date": "2023-11-29 02:11:14", "abs": "Reconfigurable intelligent surfaces (RISs) have received considerable\nattention as a key enabler for envisioned 6G networks, for the purpose of\nimproving the network capacity, coverage, efficiency, and security with low\nenergy consumption and low hardware cost. However, integrating RISs into the\nexisting infrastructure greatly increases the network management complexity,\nespecially for controlling a significant number of RIS elements. To unleash the\nfull potential of RISs, efficient optimization approaches are of great\nimportance. This work provides a comprehensive survey on optimization\ntechniques for RIS-aided wireless communications, including model-based,\nheuristic, and machine learning (ML) algorithms. In particular, we first\nsummarize the problem formulations in the literature with diverse objectives\nand constraints, e.g., sum-rate maximization, power minimization, and imperfect\nchannel state information constraints. Then, we introduce model-based\nalgorithms that have been used in the literature, such as alternating\noptimization, the majorization-minimization method, and successive convex\napproximation. Next, heuristic optimization is discussed, which applies\nheuristic rules for obtaining low-complexity solutions. Moreover, we present\nstate-of-the-art ML algorithms and applications towards RISs, i.e., supervised\nand unsupervised learning, reinforcement learning, federated learning, graph\nlearning, transfer learning, and hierarchical learning-based approaches.\nModel-based, heuristic, and ML approaches are compared in terms of stability,\nrobustness, optimality and so on, providing a systematic understanding of these\ntechniques. Finally, we highlight RIS-aided applications towards 6G networks\nand identify future challenges.", "cat": "eess.SP", "authors": ["Hao Zhou", "Melike Erol-Kantarci", "Yuanwei Liu", "H. Vincent Poor"]}, "51": {"id": "1004.5135v1", "title": "The ACS Nearby Galaxy Survey Treasury VI. The Ancient Star Forming disk of NGC 404", "url": "http://arxiv.org/pdf/1004.5135v1", "date": "2010-04-28 20:20:27", "abs": "We present HST/WFPC2 observations across the disk of the nearby isolated\ndwarf S0 galaxy NGC 404, which hosts an extended gas disk. Our deepest field\nreaches the red clump and main-sequence stars with ages <500 Myr. Although we\ndetect trace amounts of star formation at times more recent than 10 Gyr for all\nfields, the proportion of red giant stars to asymptotic giants and main\nsequence stars suggests that the disk is dominated by an ancient (>10 Gyr)\npopulation. Detailed modeling of the color-magnitude diagram suggests that ~70%\nof the stellar mass in the NGC 404 disk formed by z~2 (10 Gyr ago) and at least\n~90% formed prior to z~1 (8 Gyr ago). These results indicate that the stellar\npopulations of the NGC 404 disk are on average significantly older than those\nof other nearby disk galaxies, suggesting that early and late type disks may\nhave different long-term evolutionary histories, not simply differences in\ntheir recent star formation rates. Comparisons of the spatial distribution of\nthe young stellar mass and FUV emission in GALEX images show that the brightest\nFUV regions contain the youngest stars, but that some young stars (<160 Myr)\nlie outside of these regions. FUV luminosity appears to be strongly affected by\nboth age and stellar mass within individual regions. Finally, we use our\nmeasurements to infer the relationship between the star formation rate and the\ngas density of the disk at previous epochs. We find that most of the history of\nthe NGC 404 disk is consistent with star formation that has decreased with the\ngas density according to the Schmidt law. However, 0.5-1 Gyr ago, the star\nformation rate was unusually low for the inferred gas density, consistent with\nthe possibility that there was a gas accretion event that reignited star\nformation ~0.5 Gyr ago. Such an event could explain why this S0 galaxy hosts an\nextended gas disk.", "cat": "astro-ph.CO", "authors": ["Benjamin F. Williams", "Julianne J. Dalcanton", "Karoline M. Gilbert", "Adrienne Stilp", "Andrew Dolphin", "Anil C. Seth", "Daniel Weisz", "Evan Skillman"]}, "52": {"id": "1612.07021v1", "title": "Generalized Robertson-Walker space times, a survey", "url": "http://arxiv.org/pdf/1612.07021v1", "date": "2016-12-21 09:12:34", "abs": "Generalized Robertson-Walker spacetimes extend the notion of Robertson-Walker\nspacetimes, by allowing for spatial non-homogeneity. A survey is presented,\nwith main focus on Chen's characterization in terms of a timelike concircular\nvector. Together with their most important properties, some new results are\npresented.", "cat": "math-ph", "authors": ["Carlo Alberto Mantica", "Luca Guido Molinari"]}, "53": {"id": "2408.08628v1", "title": "A survey on secure decentralized optimization and learning", "url": "http://arxiv.org/pdf/2408.08628v1", "date": "2024-08-16 09:42:19", "abs": "Decentralized optimization has become a standard paradigm for solving\nlarge-scale decision-making problems and training large machine learning models\nwithout centralizing data. However, this paradigm introduces new privacy and\nsecurity risks, with malicious agents potentially able to infer private data or\nimpair the model accuracy. Over the past decade, significant advancements have\nbeen made in developing secure decentralized optimization and learning\nframeworks and algorithms. This survey provides a comprehensive tutorial on\nthese advancements. We begin with the fundamentals of decentralized\noptimization and learning, highlighting centralized aggregation and distributed\nconsensus as key modules exposed to security risks in federated and distributed\noptimization, respectively. Next, we focus on privacy-preserving algorithms,\ndetailing three cryptographic tools and their integration into decentralized\noptimization and learning systems. Additionally, we examine resilient\nalgorithms, exploring the design and analysis of resilient aggregation and\nconsensus protocols that support these systems. We conclude the survey by\ndiscussing current trends and potential future directions.", "cat": "cs.LG", "authors": ["Changxin Liu", "Nicola Bastianello", "Wei Huo", "Yang Shi", "Karl H. Johansson"]}, "54": {"id": "1707.01443v1", "title": "The VIMOS Ultra Deep Survey: The role of HI kinematics and HI column density on the escape of Lyalpha photons in star-forming galaxies at 2300km/sec. An ISM\nwith this value of NHI would favour a large amount of scattering events,\nespecially when the medium is static, so it can explain large values of\nExt(Lya-C) and small EW(Lya). On the contrary, an ISM with a lower NHI, but\nlarge velocity outflows would lead to a Lya spatial profile peaked at the\ngalaxy center (i.e. low values of Ext(Lya-C)) and to a large EW(Lya), as we see\nin our data. Our results and their interpretation via radiative-transfer models\ntell us that it is possible to use Lya to study the properties of the HI gas.", "cat": "astro-ph.GA", "authors": ["L. Guaita", "M. Talia", "L. Pentericci", "A. Verhamme", "P. Cassata", "B. C. Lemaux", "I. Orlitova", "B. Ribeiro", "D. Schaerer", "G. Zamorani", "B. Garilli", "V. Le Brun", "O. Le Fevre", "D. Maccagni", "L. A. M. Tasca", "R. Thomas", "E. Vanzella", "E. Zucca", "R. Amorin", "S. Bardelli", "M. Castellano", "A. Grazian", "N. P. Hathi", "A. Koekemoer", "F. Marchi"]}, "55": {"id": "0910.5666v1", "title": "Chandra ACIS Survey of M33 (ChASeM33): The enigmatic X-ray emission from IC131", "url": "http://arxiv.org/pdf/0910.5666v1", "date": "2009-10-29 15:49:32", "abs": "We present the first X-ray analysis of the diffuse hot ionized gas and the\npoint sources in IC131, after NGC604 the second most X-ray luminous giant HII\nregion in M33. The X-ray emission is detected only in the south eastern part of\nIC131 (named IC131-se) and is limited to an elliptical region of ~200pc in\nextent. This region appears to be confined towards the west by a hemispherical\nshell of warm ionized gas and only fills about half that volume. Although the\ncorresponding X-ray spectrum has 1215 counts, it cannot conclusively be told\nwhether the extended X-ray emission is thermal, non-thermal, or a combination\nof both. A thermal plasma model of kT_e=4.3keV or a single power law of\nGamma=2.1 fit the spectrum equally well. If the spectrum is purely thermal\n(non-thermal), the total unabsorbed X-ray luminosity in the 0.35-8keV energy\nband amounts to L_X = 6.8(8.7)x10^35erg/s. Among other known HII regions\nIC131-se seems to be extreme regarding the combination of its large extent of\nthe X-ray plasma, the lack of massive O stars, its unusually high electron\ntemperature (if thermal), and the large fraction of L_X emitted above 2keV\n(~40-53%). A thermal plasma of ~4keV poses serious challenges to theoretical\nmodels, as it is not clear how high electron temperatures can be produced in\nHII regions in view of mass-proportional and collisionless heating. If the gas\nis non-thermal or has non-thermal contributions, synchrotron emission would\nclearly dominate over inverse Compton emission. It is not clear if the same\nmechanisms which create non-thermal X-rays or accelerate CRs in SNRs can be\napplied to much larger scales of 200pc. In both cases the existing theoretical\nmodels for giant HII regions and superbubbles do not explain the hardness and\nextent of the X-ray emission in IC131-se.", "cat": "astro-ph.HE", "authors": ["R. Tuellmann", "K. S. Long", "T. G. Pannuti", "P. F. Winkler", "T. J. Gaetz", "P. P. Plucinsky", "B. F. Williams", "K. D. Kuntz", "W. Pietsch", "W. P. Blair", "F. Haberl", "R. K. Smith"]}, "56": {"id": "1808.00022v2", "title": "Analyzing Human-Human Interactions: A Survey", "url": "http://arxiv.org/pdf/1808.00022v2", "date": "2019-08-17 09:24:43", "abs": "Many videos depict people, and it is their interactions that inform us of\ntheir activities, relation to one another and the cultural and social setting.\nWith advances in human action recognition, researchers have begun to address\nthe automated recognition of these human-human interactions from video. The\nmain challenges stem from dealing with the considerable variation in recording\nsetting, the appearance of the people depicted and the coordinated performance\nof their interaction. This survey provides a summary of these challenges and\ndatasets to address these, followed by an in-depth discussion of relevant\nvision-based recognition and detection methods. We focus on recent, promising\nwork based on deep learning and convolutional neural networks (CNNs). Finally,\nwe outline directions to overcome the limitations of the current\nstate-of-the-art to analyze and, eventually, understand social human actions.", "cat": "cs.CV", "authors": ["Alexandros Stergiou", "Ronald Poppe"]}, "57": {"id": "2104.02778v2", "title": "The PAU survey: Estimating galaxy photometry with deep learning", "url": "http://arxiv.org/pdf/2104.02778v2", "date": "2023-06-07 10:33:42", "abs": "With the dramatic rise in high-quality galaxy data expected from Euclid and\nVera C. Rubin Observatory, there will be increasing demand for fast\nhigh-precision methods for measuring galaxy fluxes. These will be essential for\ninferring the redshifts of the galaxies. In this paper, we introduce Lumos, a\ndeep learning method to measure photometry from galaxy images. Lumos builds on\nBKGnet, an algorithm to predict the background and its associated error, and\npredicts the background-subtracted flux probability density function. We have\ndeveloped Lumos for data from the Physics of the Accelerating Universe Survey\n(PAUS), an imaging survey using a 40 narrow-band filter camera (PAUCam). PAUCam\nimages are affected by scattered light, displaying a background noise pattern\nthat can be predicted and corrected for. On average, Lumos increases the SNR of\nthe observations by a factor of 2 compared to an aperture photometry algorithm.\nIt also incorporates other advantages like robustness towards distorting\nartefacts, e.g. cosmic rays or scattered light, the ability of deblending and\nless sensitivity to uncertainties in the galaxy profile parameters used to\ninfer the photometry. Indeed, the number of flagged photometry outlier\nobservations is reduced from 10% to 2%, comparing to aperture photometry.\nFurthermore, with Lumos photometry, the photo-z scatter is reduced by ~10% with\nthe Deepz machine learning photo-z code and the photo-z outlier rate by 20%.\nThe photo-z improvement is lower than expected from the SNR increment, however\ncurrently the photometric calibration and outliers in the photometry seem to be\nits limiting factor.", "cat": "astro-ph.CO", "authors": ["Laura Cabayol", "Martin Eriksen", "Adam Amara", "Jorge Carretero", "Ricard Casas", "Francisco Javier Castander", "Juan De Vicente", "Enrique Fern\u00e1ndez", "Juan Garc\u00eda-Bellido", "Enrique Gaztanaga", "Hendrik Hildebrandt", "Ramon Miquel", "Cristobal Padilla", "Eusebio S\u00e1nchez", "Santiago Serrano", "Igancio Sevilla-Noarbe", "Pau Tallada-Cresp\u00ed"]}, "58": {"id": "1701.08887v2", "title": "A southern-sky total intensity source catalogue at 2.3 GHz from S-band Polarisation All-Sky Survey data", "url": "http://arxiv.org/pdf/1701.08887v2", "date": "2017-02-22 03:39:31", "abs": "The S-band Polarisation All-Sky Survey (S-PASS) has observed the entire\nsouthern sky using the 64-metre Parkes radio telescope at 2.3GHz with an\neffective bandwidth of 184MHz. The surveyed sky area covers all declinations\n$\\delta\\leq 0^\\circ$. To analyse compact sources the survey data have been\nre-processed to produce a set of 107 Stokes $I$ maps with 10.75arcmin\nresolution and the large scale emission contribution filtered out. In this\npaper we use these Stokes $I$ images to create a total intensity southern-sky\nextragalactic source catalogue at 2.3GHz. The source catalogue contains 23,389\nsources and covers a sky area of 16,600deg$^2$, excluding the Galactic plane\nfor latitudes $|b|<10^\\circ$. Approximately 8% of catalogued sources are\nresolved. S-PASS source positions are typically accurate to within 35arcsec. At\na flux density of 225mJy the S-PASS source catalogue is more than 95% complete,\nand $\\sim$94% of S-PASS sources brighter than 500mJy beam$^{-1}$ have a\ncounterpart at lower frequencies.", "cat": "astro-ph.GA", "authors": ["B. W. Meyers", "N. Hurley-Walker", "P. J. Hancock", "T. M. O. Franzen", "E. Carretti", "L. Staveley-Smith", "B. M. Gaensler", "M. Haverkorn", "S. Poppi"]}, "59": {"id": "2211.10215v2", "title": "CARMA-NRO Orion Survey: unbiased survey of dense cores and core mass functions in Orion A", "url": "http://arxiv.org/pdf/2211.10215v2", "date": "2022-11-21 10:20:31", "abs": "The mass distribution of dense cores is a potential key to understand the\nprocess of star formation. Applying dendrogram analysis to the CARMA-NRO Orion\nC$^{18}$O ($J$=1--0) data, we identify 2342 dense cores, about 22 \\% of which\nhave virial ratios smaller than 2, and can be classified as gravitationally\nbound cores. The derived core mass function (CMF) for bound starless cores\nwhich are not associate with protostars has a slope similar to Salpeter's\ninitial mass function (IMF) for the mass range above 1 $M_\\odot$, with a peak\nat $\\sim$ 0.1 $M_\\odot$. We divide the cloud into four parts based on the\ndeclination, OMC-1/2/3, OMC-4/5, L1641N/V380 Ori, and L1641C, and derive the\nCMFs in these regions. We find that starless cores with masses greater than 10\n$M_\\odot$ exist only in OMC-1/2/3, whereas the CMFs in OMC-4/5, L1641N, and\nL1641C are truncated at around 5--10 $M_\\odot$. From the number ratio of bound\nstarless cores and Class II objects in each subregion, the lifetime of bound\nstarless cores is estimated to be 5--30 free-fall times, consistent with\nprevious studies for other regions. In addition, we discuss core growth by mass\naccretion from the surrounding cloud material to explain the coincidence of\npeak masses between IMFs and CMFs. The mass accretion rate required for\ndoubling the core mass within a core lifetime is larger than that of\nBondi-Hoyle accretion by a factor of order 2. This implies that more dynamical\naccretion processes are required to grow cores.", "cat": "astro-ph.GA", "authors": ["Hideaki Takemura", "Fumitaka Nakamura", "H\u00e9ctor G. Arce", "Nicola Schneider", "Volker Ossenkopf-Okada", "Shuo Kong", "Shun Ishii", "Kazuhito Dobashi", "Tomomi Shimoikura", "Patricio Sanhueza", "Takashi Tsukagoshi", "Paolo Padoan", "Ralf S. Klessen", "Paul. F. Goldsmith", "Blakesley Burkhart", "Dariusz C. Lis \u00c1lvaro S\u00e1nchez-Monge", "Yoshito Shimajiri", "Ryohei Kawabe"]}, "60": {"id": "1208.6444v3", "title": "Survey of Multiscale and Multiphysics Applications and Communities", "url": "http://arxiv.org/pdf/1208.6444v3", "date": "2013-05-23 16:02:04", "abs": "Multiscale and multiphysics applications are now commonplace, and many\nresearchers focus on combining existing models to construct combined multiscale\nmodels. Here we present a concise review of multiscale applications and their\nsource communities. We investigate the prevalence of multiscale projects in the\nEU and the US, review a range of coupling toolkits they use to construct\nmultiscale models and identify areas where collaboration between disciplines\ncould be particularly beneficial. We conclude that multiscale computing has\nbecome increasingly popular in recent years, that different communities adopt\nvery different approaches to constructing multiscale simulations, and that\nsimulations on a length scale of a few metres and a time scale of a few hours\ncan be found in many of the multiscale research domains. Communities may\nreceive additional benefit from sharing methods that are geared towards these\nscales.", "cat": "cs.OH", "authors": ["Derek Groen", "Stefan J. Zasada", "Peter V. Coveney"]}, "61": {"id": "2003.03369v5", "title": "A Survey on Deep Hashing Methods", "url": "http://arxiv.org/pdf/2003.03369v5", "date": "2022-04-23 11:43:07", "abs": "Nearest neighbor search aims to obtain the samples in the database with the\nsmallest distances from them to the queries, which is a basic task in a range\nof fields, including computer vision and data mining. Hashing is one of the\nmost widely used methods for its computational and storage efficiency. With the\ndevelopment of deep learning, deep hashing methods show more advantages than\ntraditional methods. In this survey, we detailedly investigate current deep\nhashing algorithms including deep supervised hashing and deep unsupervised\nhashing. Specifically, we categorize deep supervised hashing methods into\npairwise methods, ranking-based methods, pointwise methods as well as\nquantization according to how measuring the similarities of the learned hash\ncodes. Moreover, deep unsupervised hashing is categorized into similarity\nreconstruction-based methods, pseudo-label-based methods and prediction-free\nself-supervised learning-based methods based on their semantic learning\nmanners. We also introduce three related important topics including\nsemi-supervised deep hashing, domain adaption deep hashing and multi-modal deep\nhashing. Meanwhile, we present some commonly used public datasets and the\nscheme to measure the performance of deep hashing algorithms. Finally, we\ndiscuss some potential research directions in conclusion.", "cat": "cs.CV", "authors": ["Xiao Luo", "Haixin Wang", "Daqing Wu", "Chong Chen", "Minghua Deng", "Jianqiang Huang", "Xian-Sheng Hua"]}, "62": {"id": "2405.02364v1", "title": "A Survey on Contribution Evaluation in Vertical Federated Learning", "url": "http://arxiv.org/pdf/2405.02364v1", "date": "2024-05-03 06:32:07", "abs": "Vertical Federated Learning (VFL) has emerged as a critical approach in\nmachine learning to address privacy concerns associated with centralized data\nstorage and processing. VFL facilitates collaboration among multiple entities\nwith distinct feature sets on the same user population, enabling the joint\ntraining of predictive models without direct data sharing. A key aspect of VFL\nis the fair and accurate evaluation of each entity's contribution to the\nlearning process. This is crucial for maintaining trust among participating\nentities, ensuring equitable resource sharing, and fostering a sustainable\ncollaboration framework. This paper provides a thorough review of contribution\nevaluation in VFL. We categorize the vast array of contribution evaluation\ntechniques along the VFL lifecycle, granularity of evaluation, privacy\nconsiderations, and core computational methods. We also explore various tasks\nin VFL that involving contribution evaluation and analyze their required\nevaluation properties and relation to the VFL lifecycle phases. Finally, we\npresent a vision for the future challenges of contribution evaluation in VFL.\nBy providing a structured analysis of the current landscape and potential\nadvancements, this paper aims to guide researchers and practitioners in the\ndesign and implementation of more effective, efficient, and privacy-centric VFL\nsolutions. Relevant literature and open-source resources have been compiled and\nare being continuously updated at the GitHub repository:\n\\url{https://github.com/cuiyuebing/VFL_CE}.", "cat": "cs.LG", "authors": ["Yue Cui", "Chung-ju Huang", "Yuzhu Zhang", "Leye Wang", "Lixin Fan", "Xiaofang Zhou", "Qiang Yang"]}, "63": {"id": "2402.00350v2", "title": "Large Language Models Based Fuzzing Techniques: A Survey", "url": "http://arxiv.org/pdf/2402.00350v2", "date": "2024-02-07 06:03:15", "abs": "In the modern era where software plays a pivotal role, software security and\nvulnerability analysis have become essential for software development. Fuzzing\ntest, as an efficient software testing method, are widely used in various\ndomains. Moreover, the rapid development of Large Language Models (LLMs) has\nfacilitated their application in the field of software testing, demonstrating\nremarkable performance. Considering that existing fuzzing test techniques are\nnot entirely automated and software vulnerabilities continue to evolve, there\nis a growing trend towards employing fuzzing test generated based on large\nlanguage models. This survey provides a systematic overview of the approaches\nthat fuse LLMs and fuzzing tests for software testing. In this paper, a\nstatistical analysis and discussion of the literature in three areas, namely\nLLMs, fuzzing test, and fuzzing test generated based on LLMs, are conducted by\nsummarising the state-of-the-art methods up until 2024. Our survey also\ninvestigates the potential for widespread deployment and application of fuzzing\ntest techniques generated by LLMs in the future.", "cat": "cs.SE", "authors": ["Linghan Huang", "Peizhou Zhao", "Huaming Chen", "Lei Ma"]}, "64": {"id": "1308.6070v2", "title": "The Synergy between Weak Lensing and Galaxy Redshift Surveys", "url": "http://arxiv.org/pdf/1308.6070v2", "date": "2013-08-29 06:06:37", "abs": "We study the complementarity of weak lensing (WL) and spectroscopic galaxy\nclustering (GC) surveys, by forecasting dark energy and modified gravity\nconstraints for three upcoming survey combinations: SuMIRe (Subaru Measurement\nof Images and Redshifts, the combination of the Hyper Suprime-Cam lensing\nsurvey and the Prime Focus Spectrograph redshift survey), EUCLID and WFIRST.\nFrom the WL surveys, we take into account both the shear and clustering of the\nsource galaxies and from the GC surveys, we use the three-dimensional\nclustering of spectroscopic galaxies, including redshift space distortions. A\nCMB prior is included in all cases. Focusing on the large-scale, two-point\nfunction information, we find strong synergy between the two probes. The dark\nenergy figure of merit from WL+GC is up to a factor ~2.5 larger than from\neither probe alone. Considering modified gravity, if the growth factor f(z) is\ntreated as a free function, it is very poorly constrained by WL or GC alone,\nbut can be measured at the few percent level by the combination of the two. On\nthe other hand, for cosmological constraints derived from (angular) power\nspectra and considering statistical errors only, it hardly matters whether the\nsurveys overlap on the sky or not. For instance, the dark energy figure of\nmerit for overlapping surveys is at most ~20 % better than in the disjoint\ncase. This modest gain can be traced to the fundamental fact that only a small\nfraction of the total number of modes sampled by the GC survey (or by the WL\nsurvey) contributes to the cross-correlations between WL and GC.", "cat": "astro-ph.CO", "authors": ["Roland de Putter", "Olivier Dor\u00e9", "Masahiro Takada"]}, "65": {"id": "2406.00240v1", "title": "Exploring Vulnerabilities and Protections in Large Language Models: A Survey", "url": "http://arxiv.org/pdf/2406.00240v1", "date": "2024-06-01 00:11:09", "abs": "As Large Language Models (LLMs) increasingly become key components in various\nAI applications, understanding their security vulnerabilities and the\neffectiveness of defense mechanisms is crucial. This survey examines the\nsecurity challenges of LLMs, focusing on two main areas: Prompt Hacking and\nAdversarial Attacks, each with specific types of threats. Under Prompt Hacking,\nwe explore Prompt Injection and Jailbreaking Attacks, discussing how they work,\ntheir potential impacts, and ways to mitigate them. Similarly, we analyze\nAdversarial Attacks, breaking them down into Data Poisoning Attacks and\nBackdoor Attacks. This structured examination helps us understand the\nrelationships between these vulnerabilities and the defense strategies that can\nbe implemented. The survey highlights these security challenges and discusses\nrobust defensive frameworks to protect LLMs against these threats. By detailing\nthese security issues, the survey contributes to the broader discussion on\ncreating resilient AI systems that can resist sophisticated attacks.", "cat": "cs.LG", "authors": ["Frank Weizhen Liu", "Chenhui Hu"]}, "66": {"id": "2408.14612v1", "title": "Detection of Radio Emission from Super-flaring Solar-Type Stars in the VLA Sky Survey", "url": "http://arxiv.org/pdf/2408.14612v1", "date": "2024-08-26 20:17:38", "abs": "Solar-type stars have been observed to flare at optical wavelengths to\nenergies much higher than observed for the Sun. To date, no counterparts have\nbeen observed at longer wavelengths. We have searched the the VLA Sky Survey\n(VLASS) for radio emission associated with a sample of 150 single, solar-type\nstars previously been observed to exhibit superflares in the Transiting\nExoplanet Survey Satellite (TESS). Counterparts to six of these stars were\npresent in VLASS as transient or highly variable radio sources. One of the\nstars is detected in all three epochs, exhibiting an unprecedented level of\napparently persistent radio emission. The engine for this radio emission is\nunclear, but may be related to accretion, a binary companion, or the presence\nof large-scale magnetic field. Two stars show radio emission with >50 circular\npolarization fraction, indicating a coherent emission process likely being\npresent. We find that the six VLASS-detected stars tend to have higher flare\nrates and higher flare energies of our TESS sample. This, in addition to the\nVLASS-detected stars adhering to the Gudel-Benz relation, suggest that the\nradio emission may be directly associated with superflares. These results\nconfirm that the superflare phenomenon on solar-type stars extends to radio\nwavelengths, in this instance tracing particle acceleration. These data provide\nthe first window on the luminosity function of radio superflares for solar-type\nstars and highlights the need for coordinated, multi-wavelength monitoring of\nsuch stars to fully illustrate the stellar flare-particle relation.", "cat": "astro-ph.SR", "authors": ["Ivey Davis", "Gregg Hallinan", "Carlos Ayala", "Dillon Dong", "Steven Myers"]}, "67": {"id": "0810.1050v1", "title": "The clustering of radio galaxies at z~0.55 from the 2SLAQ LRG survey", "url": "http://arxiv.org/pdf/0810.1050v1", "date": "2008-10-06 20:38:08", "abs": "We examine the clustering properties of low-power radio galaxies at redshift\n0.410.5$) we do not find any significant\nexcess of transition galaxies in clusters, relative to a comparison field\nsample at the same redshift. It is likely that such galaxies were quenched\nprior to their accretion in the cluster, in group, filament or protocluster\nenvironments. For lower stellar mass galaxies\n($9.5<\\log{M/\\mathrm{M}_\\odot}<10.5$) there is a small but significant excess\nof transition galaxies in clusters, accounting for an additional $\\sim 5-10$\nper cent of the population compared with the field. We show that our data are\nconsistent with a scenario in which 20--30 per cent of low-mass, star-forming\ngalaxies in clusters are environmentally quenched every Gyr, and that this rate\nslowly declines from $z=1$ to $z=0$. While environmental quenching of these\ngalaxies may include a long delay time during which star formation declines\nslowly, in most cases this must end with a rapid ($\\tau<1$ Gyr) decline in star\nformation rate.", "cat": "astro-ph.GA", "authors": ["Karen McNab", "Michael L. Balogh", "Remco F. J. van der Burg", "Anya Forestell", "Kristi Webb", "Benedetta Vulcani", "Gregory Rudnick", "Adam Muzzin", "M. C. Cooper", "Sean McGee", "Andrea Biviano", "Pierluigi Cerulo", "Jeffrey C. C. Chan", "Gabriella De Lucia", "Ricardo Demarco", "Alexis Finoguenov", "Ben Forrest", "Caelan Golledge", "Pascale Jablonka", "Chris Lidman", "Julie Nantais", "Lyndsay Old", "Irene Pintos-Castro", "Bianca Poggianti", "Andrew M. M. Reeves", "Gillian Wilson", "Howard K. C. Yee", "Dennis Zaritsky"]}, "74": {"id": "2208.04972v2", "title": "The MOSDEF Survey: Probing Resolved Stellar Populations at $z\\sim2$ Using a New Bayesian-defined Morphology Metric Called Patchiness", "url": "http://arxiv.org/pdf/2208.04972v2", "date": "2022-11-16 19:01:02", "abs": "We define a new morphology metric called \"patchiness\" ($P$) that is sensitive\nto deviations from the average of a resolved distribution, does not require the\ngalaxy center to be defined, and can be used on the spatially-resolved\ndistribution of any galaxy property. While the patchiness metric has a broad\nrange of applications, we demonstrate its utility by investigating the\ndistribution of dust in the interstellar medium of 310 star-forming galaxies at\nspectroscopic redshifts $1.360.6 AGN. We\npresent galaxy-integrated spectra of 89 X-ray AGN (Lx=10^42-10^45 erg/s), for\nwhich we observed [O III] (z=1.1-1.7) or Halpha emission (z=0.6-1.1). The\ntargets have X-ray luminosities representative of the parent AGN population and\nwe explore the emission-line luminosities as a function of X-ray luminosity.\nFor the [O III] targets, ~50 per cent have ionised gas velocities indicative of\ngas that is dominated by outflows and/or highly turbulent material (i.e.,\noverall line-widths >~600 km/s). The most luminous half (i.e., Lx>6x10^43\nerg/s) have a >~2 times higher incidence of such velocities. On the basis of\nour results, we find no evidence that X-ray obscured AGN are more likely to\nhost extreme kinematics than unobscured AGN. Our KASHz sample has a\ndistribution of gas velocities that is consistent with a luminosity-matched\nsample of z<0.4 AGN. This implies little evolution in the prevalence of ionised\noutflows, for a fixed AGN luminosity, despite an order-of-magnitude decrease in\naverage star-formation rates over this redshift range. Furthermore, we compare\nour Halpha targets to a redshift-matched sample of star-forming galaxies and\ndespite a similar distribution of Halpha luminosities and likely star-formation\nrates, we find extreme ionised gas velocities are up to ~10x more prevalent in\nthe AGN-host galaxies. Our results reveal a high prevalence of extreme ionised\ngas velocities in high-luminosity X-ray AGN and imply that the most powerful\nionised outflows in high-redshift galaxies are driven by AGN activity.", "cat": "astro-ph.GA", "authors": ["C. M. Harrison", "D. M. Alexander", "J. R. Mullaney", "J. P. Stott", "A. M. Swinbank", "V. Arumugam", "F. E. Bauer", "R. G. Bower", "A. J. Bunker", "R. M. Sharples"]}, "85": {"id": "2103.07853v4", "title": "Membership Inference Attacks on Machine Learning: A Survey", "url": "http://arxiv.org/pdf/2103.07853v4", "date": "2022-02-03 04:29:23", "abs": "Machine learning (ML) models have been widely applied to various\napplications, including image classification, text generation, audio\nrecognition, and graph data analysis. However, recent studies have shown that\nML models are vulnerable to membership inference attacks (MIAs), which aim to\ninfer whether a data record was used to train a target model or not. MIAs on ML\nmodels can directly lead to a privacy breach. For example, via identifying the\nfact that a clinical record that has been used to train a model associated with\na certain disease, an attacker can infer that the owner of the clinical record\nhas the disease with a high chance. In recent years, MIAs have been shown to be\neffective on various ML models, e.g., classification models and generative\nmodels. Meanwhile, many defense methods have been proposed to mitigate MIAs.\nAlthough MIAs on ML models form a newly emerging and rapidly growing research\narea, there has been no systematic survey on this topic yet. In this paper, we\nconduct the first comprehensive survey on membership inference attacks and\ndefenses. We provide the taxonomies for both attacks and defenses, based on\ntheir characterizations, and discuss their pros and cons. Based on the\nlimitations and gaps identified in this survey, we point out several promising\nfuture research directions to inspire the researchers who wish to follow this\narea. This survey not only serves as a reference for the research community but\nalso provides a clear description for researchers outside this research domain.\nTo further help the researchers, we have created an online resource repository,\nwhich we will keep updated with future relevant work. Interested readers can\nfind the repository at\nhttps://github.com/HongshengHu/membership-inference-machine-learning-literature.", "cat": "cs.LG", "authors": ["Hongsheng Hu", "Zoran Salcic", "Lichao Sun", "Gillian Dobbie", "Philip S. Yu", "Xuyun Zhang"]}, "86": {"id": "1604.05911v1", "title": "Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues. First data release for Inner Milky Way: +68\u00b0> l > -70\u00b0", "url": "http://arxiv.org/pdf/1604.05911v1", "date": "2016-04-20 12:12:48", "abs": "(Abridged) We present the first public release of high-quality data products\n(DR1) from Hi-GAL, the {\\em Herschel} infrared Galactic Plane Survey. Hi-GAL is\nthe keystone of a suite of continuum Galactic Plane surveys from the near-IR to\nthe radio, and covers five wavebands at 70, 160, 250, 350 and 500 micron,\nencompassing the peak of the spectral energy distribution of cold dust for 8 <\nT < 50K. This first Hi-GAL data release covers the inner Milky Way in the\nlongitude range 68{\\deg} > l > -70{\\deg} in a |b|<1{\\deg} latitude strip.\nPhotometric maps have been produced with the ROMAGAL pipeline, that optimally\ncapitalizes on the excellent sensitivity and stability of the bolometer arrays\nof the {\\em Herschel} PACS and SPIRE photometric cameras, to deliver images of\nexquisite quality and dynamical range, absolutely calibrated with {\\em Planck}\nand {\\em IRAS}, and recovering extended emission at all wavelengths and all\nspatial scales. The compact source catalogues have been generated with the\nCuTEx algorithm, specifically developed to optimize source detection and\nextraction in the extreme conditions of intense and spatially varying\nbackground that are found in the Galactic Plane in the thermal infrared. Hi-GAL\nDR1 images will be accessible via a dedicated web-based image cutout service.\nThe DR1 Compact Source Catalogues are delivered as single-band photometric\nlists containing, in addition to source position, peak and integrated flux and\nsource sizes, a variety of parameters useful to assess the quality and\nreliability of the extracted sources, caveats and hints to help this assessment\nare provided. Flux completeness limits in all bands are determined from\nextensive synthetic source experiments and depend on the specific line of sight\nalong the Galactic Plane. Hi-GAL DR1 catalogues contain 123210, 308509, 280685,\n160972 and 85460 compact sources in the five bands, respectively.", "cat": "astro-ph.GA", "authors": ["S. Molinari", "E. Schisano", "D. Elia", "M. Pestalozzi", "A. Traficante", "S. Pezzuto", "B. M. Swinyard", "A. Noriega-Crespo", "J. Bally", "T. J. T. Moore", "R. Plume", "A. Zavagno", "A. M. di Giorgio", "S. J. Liu", "G. L. Pilbratt", "J. C. Mottram", "D. Russeil", "L. Piazzo", "M. Veneziani", "M. Benedettini", "L. Calzoletti", "F. Faustini", "P. Natoli", "F. Piacentini", "M. Merello", "A. Palmese", "R. Del Grande", "D. Polychroni", "K. L. J. Rygl", "G. Polenta", "M. J. Barlow", "J. -P. Bernard", "P. G. Martin", "L. Testi", "B. Ali", "P. Andr\u00e8", "M. T. Beltr\u00e1n", "N. Billot", "C. Brunt", "S. Carey", "R. Cesaroni", "M. Compi\u00e8gne", "D. Eden", "Y. Fukui", "P. Garcia-Lario", "M. G. Hoare", "M. Huang", "G. Joncas", "T. L. Lim", "S. D. Lord", "S. Martinavarro-Armengol", "F. Motte", "R. Paladini", "D. Paradis", "N. Peretto", "T. Robitaille", "P. Schilke", "N. Schneider", "B. Schulz", "B. Sibthorpe", "F. Strafella", "M. A. Thompson", "G. Umana", "D. Ward-Thompson", "F. Wyrowski"]}, "87": {"id": "1409.5914v2", "title": "Nonparametric Bayes modeling with sample survey weights", "url": "http://arxiv.org/pdf/1409.5914v2", "date": "2014-09-25 20:36:36", "abs": "In population studies, it is standard to sample data via designs in which the\npopulation is divided into strata, with the different strata assigned different\nprobabilities of inclusion. Although there have been some proposals for\nincluding sample survey weights into Bayesian analyses, existing methods\nrequire complex models or ignore the stratified design underlying the survey\nweights. We propose a simple approach based on modeling the distribution of the\nselected sample as a mixture, with the mixture weights appropriately adjusted,\nwhile accounting for uncertainty in the adjustment. We focus for simplicity on\nDirichlet process mixtures but the proposed approach can be applied more\nbroadly. We sketch a simple Markov chain Monte Carlo algorithm for computation,\nand assess the approach via simulations and an application.", "cat": "stat.ME", "authors": ["T. Kunihama", "A. H. Herring", "C. T. Halpern", "D. B. Dunson"]}, "88": {"id": "1607.03154v2", "title": "The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in configuration space", "url": "http://arxiv.org/pdf/1607.03154v2", "date": "2017-03-22 03:42:25", "abs": "We perform a tomographic baryon acoustic oscillations analysis using the\ntwo-point galaxy correlation function measured from the combined sample of BOSS\nDR12, which covers the redshift range of $0.2~1", "url": "http://arxiv.org/pdf/1511.03032v1", "date": "2015-11-10 09:41:14", "abs": "In order to investigate the FIR properties of radio-active AGN, we have\nconsidered three different fields where both radio and FIR observations are the\ndeepest to-date: GOODS-South, GOODS-North and the Lockman Hole. Out of a total\nof 92 radio-selected AGN, ~64% are found to have a counterpart in Herschel\nmaps. The percentage is maximum in the GOODS-North (72%) and minimum (~50%) in\nthe Lockman Hole, where FIR observations are shallower. Our study shows that in\nall cases FIR emission is associated to star-forming activity within the host\ngalaxy. Such an activity can even be extremely intense, with star-forming rates\nas high as ~10^3-10^4 Msun/yr. AGN activity does not inhibit star formation in\nthe host galaxy, just as on-site star-formation does not seem to affect AGN\nproperties, at least those detected at radio wavelengths and for z>~1.\nFurthermore, physical properties such as the mass and age distributions of the\ngalaxies hosting a radio-active AGN do not seem to be affected by the presence\nof an ongoing star-forming event. Given the very high rate of FIR detections,\nwe stress that this refers to the majority of the sample: most radio-active AGN\nare associated with intense episodes of star-formation. However, the two\nprocesses proceed independently within the same galaxy, at all redshifts but in\nthe local universe, where powerful enough radio activity reaches the necessary\nstrength to switch off the on-site star formation. Our data also show that for\nz>~1 the hosts of radio-selected star-forming galaxies and AGN are\nindistinguishable from each other both in terms of mass and IR luminosity\ndistributions. The two populations only differentiate in the very local\nuniverse, whereby the few AGN which are still FIR-active are found in galaxies\nwith much higher masses and luminosities.", "cat": "astro-ph.GA", "authors": ["Manuela Magliocchetti", "Dieter Lutz", "Paola Santini", "Mara Salvato", "Paola Popesso", "Stefano Berta", "Francesca Pozzi"]}, "92": {"id": "2102.06717v1", "title": "An HST Survey of Protostellar Outflow Cavities: Does Feedback Clear Envelopes?", "url": "http://arxiv.org/pdf/2102.06717v1", "date": "2021-02-12 19:00:09", "abs": "We study protostellar envelope and outflow evolution using Hubble Space\nTelescope NICMOS or WFC3 images of 304 protostars in the Orion Molecular\nclouds. These near-IR images resolve structures in the envelopes delineated by\nthe scattered light of the central protostars with 80 AU resolution and they\ncomplement the 1.2-870 micron spectral energy distributions obtained with the\nHerschel Orion Protostar Survey program (HOPS). Based on their 1.60 micron\nmorphologies, we classify the protostars into five categories: non-detections,\npoint sources without nebulosity, bipolar cavity sources, unipolar cavity\nsources, and irregulars. We find point sources without associated nebulosity\nare the most numerous, and show through monochromatic Monte Carlo radiative\ntransfer modeling that this morphology occurs when protostars are observed at\nlow inclinations or have low envelope densities. We also find that the\nmorphology is correlated with the SED-determined evolutionary class with Class\n0 protostars more likely to be non-detections, Class I protostars to show\ncavities and flat-spectrum protostars to be point sources. Using an edge\ndetection algorithm to trace the projected edges of the cavities, we fit\npower-laws to the resulting cavity shapes, thereby measuring the cavity\nhalf-opening angles and power-law exponents. We find no evidence for the growth\nof outflow cavities as protostars evolve through the Class I protostar phase,\nin contradiction with previous studies of smaller samples. We conclude that the\ndecline of mass infall with time cannot be explained by the progressive\nclearing of envelopes by growing outflow cavities. Furthermore, the low star\nformation efficiency inferred for molecular cores cannot be explained by\nenvelope clearing alone.", "cat": "astro-ph.GA", "authors": ["Nolan M. Habel", "S. Thomas Megeath", "Joseph Jon Booker", "William J. Fischer", "Marina Kounkel", "Charles Poteet", "Elise Furlan", "Amelia Stutz", "P. Manoj", "John J. Tobin", "Zsofia Nagy", "Riwaj Pokhrel", "Dan Watson"]}, "93": {"id": "2305.12834v2", "title": "Surveying an Energy Landscape", "url": "http://arxiv.org/pdf/2305.12834v2", "date": "2023-08-07 08:30:58", "abs": "We derive a formula that expresses the density of states of a system with\ncontinuous degrees of freedom as a function of microcanonical averages of\nsquared gradient and Laplacian of the Hamiltonian. This result is then used to\npropose a novel flat-histogram Monte Carlo algorithm, which is tested on a\nthree-dimensional system of interacting Lennard-Jones particles, the O(n)\nvector spin model on hypercubic lattices in D = 1 to 5 dimensions, and the O(3)\nHeisenberg model on a triangular lattice featuring frustration effects.", "cat": "cond-mat.stat-mech", "authors": ["Stefan Schnabel", "Wolfhard Janke"]}, "94": {"id": "1004.3231v1", "title": "Constraint on the cosmological f(R) model from the multipole power spectrum of the SDSS luminous red galaxy sample and prospects for a future redshift survey", "url": "http://arxiv.org/pdf/1004.3231v1", "date": "2010-04-19 15:38:03", "abs": "A constraint on the viable f(R) model is investigated by confronting\ntheoretical predictions with the multipole power spectrum of the luminous red\ngalaxy sample of the Sloan Digital Sky survey data release 7. We obtain a\nconstraint on the Compton wavelength parameter of the f(R) model on the scales\nof cosmological large-scale structure. A prospect of constraining the Compton\nwavelength parameter with a future redshift survey is also investigated. The\nusefulness of the redshift-space distortion for testing the gravity theory on\ncosmological scales is demonstrated.", "cat": "astro-ph.CO", "authors": ["Kazuhiro Yamamoto", "Gen Nakamura", "Gert Huetsi", "Tatsuya Narikawa", "Takahiro Sato"]}, "95": {"id": "2401.11617v2", "title": "A Survey on African Computer Vision Datasets, Topics and Researchers", "url": "http://arxiv.org/pdf/2401.11617v2", "date": "2024-02-04 18:17:27", "abs": "Computer vision encompasses a range of tasks such as object detection,\nsemantic segmentation, and 3D reconstruction. Despite its relevance to African\ncommunities, research in this field within Africa represents only 0.06% of\ntop-tier publications over the past decade. This study undertakes a thorough\nanalysis of 63,000 Scopus-indexed computer vision publications from Africa,\nspanning from 2012 to 2022. The aim is to provide a survey of African computer\nvision topics, datasets and researchers. A key aspect of our study is the\nidentification and categorization of African Computer Vision datasets using\nlarge language models that automatically parse abstracts of these publications.\nWe also provide a compilation of unofficial African Computer Vision datasets\ndistributed through challenges or data hosting platforms, and provide a full\ntaxonomy of dataset categories. Our survey also pinpoints computer vision\ntopics trends specific to different African regions, indicating their unique\nfocus areas. Additionally, we carried out an extensive survey to capture the\nviews of African researchers on the current state of computer vision research\nin the continent and the structural barriers they believe need urgent\nattention. In conclusion, this study catalogs and categorizes Computer Vision\ndatasets and topics contributed or initiated by African institutions and\nidentifies barriers to publishing in top-tier Computer Vision venues. This\nsurvey underscores the importance of encouraging African researchers and\ninstitutions in advancing computer vision research in the continent. It also\nstresses on the need for research topics to be more aligned with the needs of\nAfrican communities.", "cat": "cs.CV", "authors": ["Abdul-Hakeem Omotayo", "Ashery Mbilinyi", "Lukman Ismaila", "Houcemeddine Turki", "Mahmoud Abdien", "Karim Gamal", "Idriss Tondji", "Yvan Pimi", "Naome A. Etori", "Marwa M. Matar", "Clifford Broni-Bediako", "Abigail Oppong", "Mai Gamal", "Eman Ehab", "Gbetondji Dovonon", "Zainab Akinjobi", "Daniel Ajisafe", "Oluwabukola G. Adegboro", "Mennatullah Siam"]}, "96": {"id": "1601.05792v1", "title": "A Survey on Security Metrics", "url": "http://arxiv.org/pdf/1601.05792v1", "date": "2016-01-20 23:20:38", "abs": "The importance of security metrics can hardly be overstated. Despite the\nattention that has been paid by the academia, government and industry in the\npast decades, this important problem stubbornly remains open. In this survey,\nwe present a survey of knowledge on security metrics. The survey is centered on\na novel taxonomy, which classifies security metrics into four categories:\nmetrics for measuring the system vulnerabilities, metrics for measuring the\ndefenses, metrics for measuring the threats, and metrics for measuring the\nsituations. The insight underlying the taxonomy is that situations (or outcomes\nof cyber attack-defense interactions) are caused by certain threats (or\nattacks) against systems that have certain vulnerabilities (including human\nfactors) and employ certain defenses. In addition to systematically reviewing\nthe security metrics that have been proposed in the literature, we discuss the\ngaps between the state of the art and the ultimate goals.", "cat": "cs.CR", "authors": ["Marcus Pendleton", "Richard Garcia-Lebron", "Shouhuai Xu"]}, "97": {"id": "1710.03232v1", "title": "An Ultraviolet Survey of Low-Redshift Partial Lyman-Limit Systems with the HST Cosmic Origins Spectrograph", "url": "http://arxiv.org/pdf/1710.03232v1", "date": "2017-10-09 18:00:03", "abs": "We present an ultraviolet spectroscopic survey of strong H I absorbers in the\nintergalactic medium, probing their evolution over the last 6-7 Gyr at\nredshifts $0.24 \\leq z \\leq 0.84$. We measure column densities $N_{\\rm HI} \\,(\n{\\rm cm}^{-2})$ from the pattern of Lyman-series absorption lines and flux\ndecrement at the Lyman limit (LL) when available. We analyzed 220 H I absorbers\nin ultraviolet spectra of 102 active galactic nuclei (AGN) taken by the Cosmic\nOrigins Spectrograph aboard the Hubble Space Telescope with G130M/G160M\ngratings (1134-1795 \\AA). For 158 absorbers with $\\log N_{\\rm HI} \\geq 15$, the\nmean frequency is $d {\\cal N}/dz = 4.95 \\pm 0.39$ over pathlength $\\Delta z =\n31.94$ ($0.24 \\leq z \\leq 0.84)$. We identify 8 Lyman Limit Systems (LLS, $\\log\nN_{\\rm HI} \\geq 17.2$) and 54 partial systems (pLLS) with $16.0 \\leq \\log\nN_{\\rm HI} < 17.2$. Toward 159 AGN between $0.01 < z_{\\rm abs} < 0.84$ with\n$\\Delta z \\approx 48$, we find four damped Ly$\\alpha$ absorbers (DLA) with $(d\n{\\cal N}/dz)_{\\rm DLA} = 0.083^{+0.066}_{-0.040}$ at $\\langle z \\rangle =\n0.18$. The mean LLS frequency between $z = 0.24-0.48$ is $(d {\\cal N}/dz)_{\\rm\nLLS} = 0.36^{+0.20}_{-0.13}$ fitted to $N(z) =\n(0.25^{+0.13}_{-0.09})(1+z)^{1.14}$. For 54 pLLS we find $(d {\\cal N}/dz)_{\\rm\npLLS} = 1.69\\pm0.23$ at $\\langle z \\rangle = 0.39$, a frequency consistent with\ngaseous halo sizes $R \\approx 100 h^{-1}~{\\rm kpc}$ for ($0.3-3L^*$) galaxies.\nA maximum-likelihood analysis yields a distribution $f(N,z) = C_0 N^{-\\beta}\n(1+z)^{\\gamma}$ with $\\beta = 1.48 \\pm 0.05$ and $\\gamma =\n1.14^{+0.88}_{-0.89}$ for $15 \\leq \\log N_{\\rm HI} \\leq 17.5$. The far-UV\nopacity gradient is $d \\tau_{\\rm eff} / dz \\approx (0.444)(1+z)^{1.14}$ over\nthe range $15 \\leq \\log N_{\\rm HI} \\leq 17$, implying mean LyC optical depth\n$\\tau_{\\rm eff} \\approx 0.3-0.5$ toward sources at $z = 1-2$.", "cat": "astro-ph.GA", "authors": ["J. Michael Shull", "Charles W. Danforth", "Evan M. Tilton", "Joshua Moloney", "Matthew L. Stevans"]}, "98": {"id": "2312.14647v2", "title": "Towards Message Brokers for Generative AI: Survey, Challenges, and Opportunities", "url": "http://arxiv.org/pdf/2312.14647v2", "date": "2024-02-21 07:41:10", "abs": "In today's digital world, Generative Artificial Intelligence (GenAI) such as\nLarge Language Models (LLMs) is becoming increasingly prevalent, extending its\nreach across diverse applications. This surge in adoption has sparked a\nsignificant increase in demand for data-centric GenAI models, highlighting the\nnecessity for robust data communication infrastructures. Central to this need\nare message brokers, which serve as essential channels for data transfer within\nvarious system components. This survey aims to delve into a comprehensive\nanalysis of traditional and modern message brokers, offering a comparative\nstudy of prevalent platforms. Our study considers numerous criteria including,\nbut not limited to, open-source availability, integrated monitoring tools,\nmessage prioritization mechanisms, capabilities for parallel processing,\nreliability, distribution and clustering functionalities, authentication\nprocesses, data persistence strategies, fault tolerance, and scalability.\nFurthermore, we explore the intrinsic constraints that the design and operation\nof each message broker might impose, recognizing that these limitations are\ncrucial in understanding their real-world applicability. Finally, this study\nexamines the enhancement of message broker mechanisms specifically for GenAI\ncontexts, emphasizing the criticality of developing a versatile message broker\nframework. Such a framework would be poised for quick adaptation, catering to\nthe dynamic and growing demands of GenAI in the foreseeable future. Through\nthis dual-pronged approach, we intend to contribute a foundational compendium\nthat can guide future innovations and infrastructural advancements in the realm\nof GenAI data communication.", "cat": "cs.DC", "authors": ["Alaa Saleh", "Roberto Morabito", "Sasu Tarkoma", "Susanna Pirttikangas", "Lauri Lov\u00e9n"]}, "99": {"id": "1807.10163v1", "title": "Dark Energy Survey Year 1 Results: Measurement of the Galaxy Angular Power Spectrum", "url": "http://arxiv.org/pdf/1807.10163v1", "date": "2018-07-26 14:21:49", "abs": "We use data from the first-year (Y1) observations of the DES collaboration to\nmeasure the galaxy angular power spectrum (APS), and search for its BAO feature\nusing a template-fitting method. We test our methodology in a sample of 1800\nDES Y1-like mock catalogs. The APS is measured with the pseudo-$C_\\ell$ method,\nusing pixelized maps constructed from the mock catalogs and the DES mask. The\ncovariance matrix of the $C_\\ell$'s in these tests are also obtained from the\nmock catalogs. We use templates to model the measured spectra and estimate\ntemplate parameters firstly from the $C_\\ell$'s of the mocks using two\ndifferent methods, a maximum likelihood estimator and a MCMC, finding\nconsistent results with a good reduced $\\chi^2$. Robustness tests are performed\nto estimate the impact of different choices of settings used in our analysis.\nAfter these tests on mocks, we apply our method to a galaxy sample constructed\nfrom DES Y1 data specifically for LSS studies. This catalog comprises galaxies\nwithin an effective area of 1318 deg$^2$ and $0.670$% of the X-ray sources in this subfield have either\nspectroscopic or high-quality photometric redshifts.", "cat": "astro-ph.GA", "authors": ["C. -T. J. Chen", "W. N. Brandt", "B. Luo", "P. Ranalli", "G. Yang", "D. M. Alexander", "F. E. Bauer", "D. D. Kelson", "M. Lacy", "K. Nyland", "P. Tozzi", "F. Vito", "M. Cirasuolo", "R. Gilli", "M. J. Jarvis", "B. D. Lehmer", "M. Paolillo", "D. P. Schneider", "O. Shemmer", "I. Smail", "M. Sun", "M. Tanaka", "M. Vaccari", "C. Vignali", "Y. Q. Xue", "M. Banerji", "K. E. Chow", "B. H\u00e4u\u00dfler", "R. P. Norris", "J. D. Silverman", "J. R. Trump"]}, "104": {"id": "1611.02634v1", "title": "Physical characterization of Galactic O-type stars targeted by the IACOB and OWN surveys", "url": "http://arxiv.org/pdf/1611.02634v1", "date": "2016-11-08 17:53:46", "abs": "We present first results from the quantitative spectroscopic analysis of 266\nGalactic O-type stars targeted by the IACOB and OWN surveys (implying the\nlargest sample of stars of this type analyzed homogeneously). We also evaluate\nwhat is the present situation regarding available information about distances,\nas provided by the Hipparcos and Gaia missions.", "cat": "astro-ph.SR", "authors": ["G. Holgado", "S. Sim\u00f3n-D\u00edaz", "R. H. Barb\u00e1"]}, "105": {"id": "2006.16709v3", "title": "A Survey on Recent Progress in the Theory of Evolutionary Algorithms for Discrete Optimization", "url": "http://arxiv.org/pdf/2006.16709v3", "date": "2021-07-08 06:15:26", "abs": "The theory of evolutionary computation for discrete search spaces has made\nsignificant progress in the last ten years. This survey summarizes some of the\nmost important recent results in this research area. It discusses fine-grained\nmodels of runtime analysis of evolutionary algorithms, highlights recent\ntheoretical insights on parameter tuning and parameter control, and summarizes\nthe latest advances for stochastic and dynamic problems. We regard how\nevolutionary algorithms optimize submodular functions and we give an overview\nover the large body of recent results on estimation of distribution algorithms.\nFinally, we present the state of the art of drift analysis, one of the most\npowerful analysis technique developed in this field.", "cat": "cs.NE", "authors": ["Benjamin Doerr", "Frank Neumann"]}, "106": {"id": "2207.09511v1", "title": "Approximation Power of Deep Neural Networks: an explanatory mathematical survey", "url": "http://arxiv.org/pdf/2207.09511v1", "date": "2022-07-19 18:47:44", "abs": "The goal of this survey is to present an explanatory review of the\napproximation properties of deep neural networks. Specifically, we aim at\nunderstanding how and why deep neural networks outperform other classical\nlinear and nonlinear approximation methods. This survey consists of three\nchapters. In Chapter 1 we review the key ideas and concepts underlying deep\nnetworks and their compositional nonlinear structure. We formalize the neural\nnetwork problem by formulating it as an optimization problem when solving\nregression and classification problems. We briefly discuss the stochastic\ngradient descent algorithm and the back-propagation formulas used in solving\nthe optimization problem and address a few issues related to the performance of\nneural networks, including the choice of activation functions, cost functions,\noverfitting issues, and regularization. In Chapter 2 we shift our focus to the\napproximation theory of neural networks. We start with an introduction to the\nconcept of density in polynomial approximation and in particular study the\nStone-Weierstrass theorem for real-valued continuous functions. Then, within\nthe framework of linear approximation, we review a few classical results on the\ndensity and convergence rate of feedforward networks, followed by more recent\ndevelopments on the complexity of deep networks in approximating Sobolev\nfunctions. In Chapter 3, utilizing nonlinear approximation theory, we further\nelaborate on the power of depth and approximation superiority of deep ReLU\nnetworks over other classical methods of nonlinear approximation.", "cat": "cs.LG", "authors": ["Mohammad Motamed"]}, "107": {"id": "1811.11676v1", "title": "The SAMI Galaxy Survey: Observing the environmental quenching of star formation in GAMA groups", "url": "http://arxiv.org/pdf/1811.11676v1", "date": "2018-11-28 16:57:45", "abs": "We explore the radial distribution of star formation in galaxies in the SAMI\nGalaxy Survey as a function of their local group environment. Using a sample of\ngalaxies in groups (with halo masses less than $ \\simeq 10^{14} \\,\n\\mathrm{M_{\\odot}}$) from the Galaxy And Mass Assembly Survey, we find\nsignatures of environmental quenching in high-mass groups ($M_{G} > 10^{12.5}\n\\, \\mathrm{M_{\\odot}}$). The mean integrated specific star formation rate of\nstar-forming galaxies in high-mass groups is lower than for galaxies in\nlow-mass groups or that are ungrouped, with $\\Delta \\log(sSFR/\\mathrm{yr^{-1}})\n= 0.45 \\pm 0.07$. This difference is seen at all galaxy stellar masses. In\nhigh-mass groups, star-forming galaxies more massive than $M_{*} \\sim 10^{10}\n\\, \\mathrm{M_{\\odot}}$ have centrally-concentrated star formation. These\ngalaxies also lie below the star-formation main sequence, suggesting they may\nbe undergoing outside-in quenching. Lower mass galaxies in high-mass groups do\nnot show evidence of concentrated star formation. In groups less massive than\n$M_{G} = 10^{12.5} \\, \\mathrm{M_{\\odot}}$ we do not observe these trends. In\nthis regime we find a modest correlation between centrally-concentrated star\nformation and an enhancement in total star formation rate, consistent with\ntriggered star formation in these galaxies.", "cat": "astro-ph.GA", "authors": ["A. L. Schaefer", "S. M. Croom", "N. Scott", "S. Brough", "J. T. Allen", "K. Bekki", "J. Bland-Hawthorn", "J. V. Bloom", "J. J. Bryant", "L. Cortese", "L. J. M. Davies", "C. Federrath", "L. M. R. Fogarty", "A. W. Green", "B. Groves", "A. M. Hopkins", "I. S. Konstantopoulos", "A. R. L\u00f3pez-S\u00e1nchez", "J. S. Lawrence", "R. E. McElroy", "A. M. Medling", "M. S. Owers", "M. B. Pracy", "S. N. Richards", "A. S. G. Robotham", "J. van de Sande", "C. Tonini", "S. K. Yi"]}, "108": {"id": "2404.00621v2", "title": "Multimodal Pretraining, Adaptation, and Generation for Recommendation: A Survey", "url": "http://arxiv.org/pdf/2404.00621v2", "date": "2024-07-03 09:53:45", "abs": "Personalized recommendation serves as a ubiquitous channel for users to\ndiscover information tailored to their interests. However, traditional\nrecommendation models primarily rely on unique IDs and categorical features for\nuser-item matching, potentially overlooking the nuanced essence of raw item\ncontents across multiple modalities such as text, image, audio, and video. This\nunderutilization of multimodal data poses a limitation to recommender systems,\nespecially in multimedia services like news, music, and short-video platforms.\nThe recent advancements in large multimodal models offer new opportunities and\nchallenges in developing content-aware recommender systems. This survey seeks\nto provide a comprehensive exploration of the latest advancements and future\ntrajectories in multimodal pretraining, adaptation, and generation techniques,\nas well as their applications in enhancing recommender systems. Furthermore, we\ndiscuss current open challenges and opportunities for future research in this\ndynamic domain. We believe that this survey, alongside the curated resources,\nwill provide valuable insights to inspire further advancements in this evolving\nlandscape.", "cat": "cs.IR", "authors": ["Qijiong Liu", "Jieming Zhu", "Yanting Yang", "Quanyu Dai", "Zhaocheng Du", "Xiao-Ming Wu", "Zhou Zhao", "Rui Zhang", "Zhenhua Dong"]}, "109": {"id": "1503.08619v1", "title": "Wide-field Variability Survey of the Globular Cluster M79 and a New Period -- Luminosity Relation for SX Phe Stars", "url": "http://arxiv.org/pdf/1503.08619v1", "date": "2015-03-30 09:53:16", "abs": "We present the results of a search for variable stars in a 26x39 arcmin^2\nfield around globular cluster M79 (NGC1904). The search was made by means of an\nextended version of image subtraction, which allows to analyze in a uniform\nmanner CCD frames obtained with different telescopes and cameras of different\nsizes and resolutions. The search resulted in finding 20 new variable stars,\namong which 13 are cluster members. The members include one new RR Lyr star of\nsubtype c, three SX Phe stars, and nine variable red giants. We also show that\nV7 is a W Vir star with a period of 13.985 d. Revised mean periods of RRab and\nRRc stars, =0.71 d and =0.34 d, respectively, and relative\npercentage of RRc stars, N_c/(N_ab+N_c)=45 % confirm that M79 belongs to the\nOosterhoff II group of globular clusters. The mean V magnitude of the\nhorizontal branch of M79 based on ten RR Lyr stars has been estimated to be\n$V_HB==16.11\\pm0.03$ mag. In one RRc star, V9, light changes with three\nclose frequencies were detected, indicating excitation of nonradial modes. An\nSX Phe star, V18, is a double-mode pulsator with two radial modes excited,\nfundamental and first overtone. Moreover, we have discovered two SX Phe or\ndelta Sct stars and one W UMa type system, all likely field objects. We also\nstudied the period -- luminosity relation for SX Phe stars. Using 62\nfundamental and fundamentalized periods of radial double-mode and\nhigh-amplitude SX Phe stars known in Galactic globular clusters, we have\nderived the slope and zero point of this relation to be, $-3.35\\pm0.24$ and\n$2.68\\pm0.03$ mag (at log(P/d)=-1.24), respectively.", "cat": "astro-ph.SR", "authors": ["Grzegorz Kopacki"]}, "110": {"id": "1110.4599v1", "title": "A single-dish survey of the HCO+, HCN, and CN emission toward the T Tauri disk population in Taurus", "url": "http://arxiv.org/pdf/1110.4599v1", "date": "2011-10-20 18:29:39", "abs": "(Abridged) As the stellar X-ray and UV light penetration of a protoplanetary\ndisk depends sensitively on the dust properties, trace molecular species like\nHCO+, HCN, and CN are expected to show marked differences from photoprocessing\neffects as the dust content in the disk evolves. We investigate the evolution\nof the UV irradiation of the molecular gas in a sample of classical T Tauri\nstars in Taurus that exhibit a wide range in grain growth and dust settling\nproperties. We obtained HCO+ (J=3-2), HCN (J=3-2), and CN (J=2-1) observations\nof 13 sources with the JCMT. Our sample has 1.3mm fluxes in excess of 75mJy,\nindicating the presence of significant dust reservoirs; a range of dust\nsettling as traced through their spectral slopes between 6, 13, and 25 microns;\nand varying degrees of grain growth as extrapolated from the strength of their\n10-micron silicate emission features. We compare the emission line strengths\nwith the sources' continuum flux and infrared features, and use detailed\nmodeling based on two different model prescriptions to compare typical disk\nabundances for HCO+, HCN, and CN with the gas-line observations for our sample.\nWe detected HCO+ (3-2) toward 6 disks, HCN (3-2) from 0 disks, and CN (2-1)\ntoward 4 disks. For the complete sample, there is no correlation between the\ngas-line strengths or their ratios and either the sources' dust continuum flux\nor infrared slopes.", "cat": "astro-ph.GA", "authors": ["D. M. Salter", "M. R. Hogerheijde", "R. F. J. van der Burg", "L. E. Kristensen", "C. Brinch"]}, "111": {"id": "2402.11015v2", "title": "A Survey for Radio Emission from White Dwarfs in the VLA Sky Survey", "url": "http://arxiv.org/pdf/2402.11015v2", "date": "2024-05-14 16:23:11", "abs": "Radio emission has been detected from tens of white dwarfs, in particular in\naccreting systems. Additionally, radio emission has been predicted as a\npossible outcome of a planetary system around a white dwarf. We searched for 3\nGHz radio continuum emission in 846,000 candidate white dwarfs previously\nidentified in Gaia using the Very Large Array Sky Survey (VLASS) Epoch 1 Quick\nLook Catalogue. We identified 13 candidate white dwarfs with a counterpart in\nVLASS within 2\". Five of those were found not to be white dwarfs in follow-up\nor archival spectroscopy, whereas seven others were found to be chance\nalignments with a background source in higher-resolution optical or radio\nimages. The remaining source, WDJ204259.71+152108.06, is found to be a white\ndwarf and M-dwarf binary with an orbital period of 4.1 days and long-term\nstochastic optical variability, as well as luminous radio and X-ray emission.\nFor this binary, we find no direct evidence of a background contaminant, and a\nchance alignment probability of only ~2 per cent. However, other evidence\npoints to the possibility of an unfortunate chance alignment with a background\nradio and X-ray emitting quasar, including an unusually poor Gaia DR3\nastrometric solution for this source. With at most one possible radio emitting\nwhite dwarf found, we conclude that strong (> 1-3 mJy) radio emission from\nwhite dwarfs in the 3 GHz band is virtually nonexistent outside of interacting\nbinaries.", "cat": "astro-ph.SR", "authors": ["Ingrid Pelisoli", "Laura Chomiuk", "Jay Strader", "T. R. Marsh", "Elias Aydi", "Kristen C. Dage", "Rebecca Kyer", "Isabella Molina", "Teresa Panurach", "Ryan Urquhart", "Thomas J. Maccarone", "R. Michael Rich", "Antonio C. Rodriguez", "E. Breedt", "A. J. Brown", "V. S. Dhillon", "M. J. Dyer", "Boris. T. Gaensicke", "J. A. Garbutt", "M. J. Green", "M. R. Kennedy", "P. Kerry", "S. P. Littlefair", "James Munday", "S. G. Parsons"]}, "112": {"id": "1810.07204v2", "title": "The MOSDEF Survey: Stellar Continuum Spectra and Star Formation Histories of Active, Transitional, and Quiescent Galaxies at 1.4$<$\\lowercase{z}$<$2.6", "url": "http://arxiv.org/pdf/1810.07204v2", "date": "2018-10-18 02:57:26", "abs": "Using the MOSDEF rest-frame optical spectroscopic survey, we investigate the\nstar-formation histories (SFHs) of different galaxy types, ranging from\nactively star forming to quiescent at $1.4\\leq~z\\leq2.6$. SFHs are constrained\nutilizing stellar continuum spectroscopy, specifically through a combination of\nBalmer absorption lines, the 4000$\\AA$ break, and the equivalent width of the\nH$\\alpha$ emission line. To attain a sufficiently high signal-to-noise ratio\n(S/N) to conduct these measurements we stack spectra of galaxies with similar\nspectral types, as determined from their rest-frame $U-V$ and $V-J$ colors. We\nbin the MOSDEF sample into five spectral types, subdividing the quiescent and\nstar-forming bins to better explore galaxies transitioning between the two. We\nconstrain the average SFHs for each type, finding that quiescent and\ntransitional galaxies in the MOSDEF sample are dominated by an SFH with an\naverage star-formation timescale of $\\tau\\sim0.1-0.2$~Gyr. These findings\ncontrast with measurements from the low-redshift Universe where, on average,\ngalaxies form their stars over a more extended time period ($\\tau>1$~Gyr).\nFurthermore, our spectral index measurements correlate with mass surface\ndensity for all spectral types. Finally, we compare the average properties of\nthe galaxies in our transitional bins to investigate possible paths to\nquiescence, and speculate on the viability of a dusty post-starburst phase.", "cat": "astro-ph.GA", "authors": ["Tom O. Zick", "Mariska Kriek", "Alice E. Shapley", "Naveen A. Reddy", "William R. Freeman", "Brian Siana", "Alison L. Coil", "Mojegan Azadi", "Guillermo Barro", "Tara Fetherolf", "Francesca M. Fornasini", "Laura de Groot", "Gene Leung", "Bahram Mobasher", "Sedona H. Price", "Ryan L. Sanders", "Irene Shivaei"]}, "113": {"id": "0812.1202v1", "title": "Superallowed 0+ to 0+ nuclear beta decays: A new survey with precision tests of the conserved vector current hypothesis and the standard model", "url": "http://arxiv.org/pdf/0812.1202v1", "date": "2008-12-05 19:31:04", "abs": "A new critical survey is presented of all half-life, decay-energy and\nbranching-ratio measurements related to 20 0+ to 0+ beta decays. Compared with\nour last review, there are numerous improvements: First, we have added 27\nrecently published measurements and eliminated 9 references; of particular\nimportance, the new data include a number of high-precision Penning-trap\nmeasurements of decay energies. Second, we have used the recently improved\nisospin symmetry-breaking corrections. Third, our calculation of the\nstatistical rate function now accounts for possible excitation in the daughter\natom. Finally, we have re-examined the systematic uncertainty associated with\nthe isospin symmetry-breaking corrections by evaluating the radial-overlap\ncorrection using Hartree-Fock radial wave functions and comparing the results\nwith our earlier calculations, which used Saxon-Woods wave functions; the\nprovision for systematic uncertainty has been changed as a consequence. The new\ncorrected Ft values are impressively constant and their average, when combined\nwith the muon liftime, yields the up-down quark-mixing element of the\nCabibbo-Kobayashi-Maskawa (CKM) matrix, V_{ud} = 0.97425(22). The unitarity\ntest on the top row of the matrix becomes |V_{ud}|^2 + |V_{us}|^2 + |V_{ub}|^2\n= 0.99995(61). Both V_{ud} and the unitarity sum have significantly reduced\nuncertainties compared with our previous survey, although the new value of\nV_{ud} is statistically consistent with the old one. From these data we also\nset limits on the possible existence of scalar interactions, right-hand\ncurrents and extra Z bosons. Finally, we discuss the priorities for future\ntheoretical and experimental work with the goal of making the CKM unitarity\ntest even more definitive.", "cat": "nucl-ex", "authors": ["J. C. Hardy", "I. S. Towner"]}, "114": {"id": "2007.13069v1", "title": "A Survey on Complex Question Answering over Knowledge Base: Recent Advances and Challenges", "url": "http://arxiv.org/pdf/2007.13069v1", "date": "2020-07-26 07:13:32", "abs": "Question Answering (QA) over Knowledge Base (KB) aims to automatically answer\nnatural language questions via well-structured relation information between\nentities stored in knowledge bases. In order to make KBQA more applicable in\nactual scenarios, researchers have shifted their attention from simple\nquestions to complex questions, which require more KB triples and constraint\ninference. In this paper, we introduce the recent advances in complex QA.\nBesides traditional methods relying on templates and rules, the research is\ncategorized into a taxonomy that contains two main branches, namely Information\nRetrieval-based and Neural Semantic Parsing-based. After describing the methods\nof these branches, we analyze directions for future research and introduce the\nmodels proposed by the Alime team.", "cat": "cs.CL", "authors": ["Bin Fu", "Yunqi Qiu", "Chengguang Tang", "Yang Li", "Haiyang Yu", "Jian Sun"]}, "115": {"id": "2102.06919v2", "title": "Asset Management in Machine Learning: A Survey", "url": "http://arxiv.org/pdf/2102.06919v2", "date": "2021-02-17 08:55:41", "abs": "Machine Learning (ML) techniques are becoming essential components of many\nsoftware systems today, causing an increasing need to adapt traditional\nsoftware engineering practices and tools to the development of ML-based\nsoftware systems. This need is especially pronounced due to the challenges\nassociated with the large-scale development and deployment of ML systems. Among\nthe most commonly reported challenges during the development, production, and\noperation of ML-based systems are experiment management, dependency management,\nmonitoring, and logging of ML assets. In recent years, we have seen several\nefforts to address these challenges as witnessed by an increasing number of\ntools for tracking and managing ML experiments and their assets. To facilitate\nresearch and practice on engineering intelligent systems, it is essential to\nunderstand the nature of the current tool support for managing ML assets. What\nkind of support is provided? What asset types are tracked? What operations are\noffered to users for managing those assets? We discuss and position ML asset\nmanagement as an important discipline that provides methods and tools for ML\nassets as structures and the ML development activities as their operations. We\npresent a feature-based survey of 17 tools with ML asset management support\nidentified in a systematic search. We overview these tools' features for\nmanaging the different types of assets used for engineering ML-based systems\nand performing experiments. We found that most of the asset management support\ndepends on traditional version control systems, while only a few tools support\nan asset granularity level that differentiates between important ML assets,\nsuch as datasets and models.", "cat": "cs.SE", "authors": ["Samuel Idowu", "Daniel Str\u00fcber", "Thorsten Berger"]}, "116": {"id": "2403.08091v1", "title": "Emergence of high-mass stars in complex fiber networks (EMERGE). I. Early ALMA Survey: observations and massive data reduction", "url": "http://arxiv.org/pdf/2403.08091v1", "date": "2024-03-12 22:01:27", "abs": "(Abridged) Recent molecular surveys have revealed a rich gas organization of\nsonic-like fibers in all kind of environments prior to the formation of low-\nand high-mass stars. This paper introduces the EMERGE project aiming to\ninvestigate whether complex fiber arrangements could explain the origin of\nhigh-mass stars and clusters. We analyzed the EMERGE Early ALMA Survey\nincluding 7 star-forming regions in Orion (OMC-1/2/3/4 South, L1641N, NGC2023,\nand Flame Nebula) homogeneously surveyed in both molecular lines (N$_2$H$^+$\nJ=1-0, HNC J=1-0, plus HC3N J=10-9) and 3mm-continuum using a combination of\ninterferometric ALMA mosaics and IRAM-30m single-dish (SD) maps. Based on our\nlow-resolution (SD) observations, we describe the global properties of our\nsample covering a wide range of physical conditions including low-,\nintermediate, and high-mass star-forming regions in different evolutionary\nstages. Their comparison with ancillary YSO catalogs denotes N$_2$H$^+$ as the\nbest proxy for the dense, star-forming gas in our targets showing a constant\nstar formation efficiency and a fast time evolution of <1 Myr. While apparently\nclumpy and filamentary in our SD data, all targets show a much more complex\nfibrous substructure at the enhanced resolution of our ALMA+IRAM-30m maps. A\nlarge number of filamentary features at sub-parsec scales are clearly\nrecognized in the high-density gas traced by N$_2$H$^+$ directly connected to\nthe formation of individual protostars. This complex gas organization appears\nto extend further into the more diffuse gas traced by HNC. This paper presents\nthe EMERGE Early ALMA survey including a first data release of continuum maps\nand spectral products for this project to be analysed in future papers of this\nseries. A first look at these results illustrates the need of advanced data\ncombination techniques to investigate the intrinsic multi-scale, gas structure\nof the ISM.", "cat": "astro-ph.GA", "authors": ["A. Hacar", "A. Socci", "F. Bonanomi", "D. Petry", "M. Tafalla", "D. Harsono", "J. Forbrich", "J. Alves", "J. Grossschedl", "J. R. Goicoechea", "J. Pety", "A. Burkert", "G. X. Li"]}, "117": {"id": "1109.4441v2", "title": "The cosmological analysis of X-ray cluster surveys: II- Application of the CR-HR method to the XMM archive", "url": "http://arxiv.org/pdf/1109.4441v2", "date": "2012-05-10 08:45:05", "abs": "We have processed 2774 high-galactic observations from the XMM archive (as of\nMay 2010) and extracted a serendipitous catalogue of some 850 clusters of\ngalaxies based on purely X-ray criteria, following the methodology developed\nfor the XMM-LSS survey. Restricting the sample to the highest signal-to-noise\nobjects (347 clusters), we perform a cosmological analysis using the X-ray\ninformation only. The analysis consists in the modelling of the observed\ncolour-magnitude (CR-HR) diagram constructed from cluster instrumental\ncount-rates measured in the [0.5-2], [1-2] and [0.5-1] keV bands. A MCMC\nprocedure simultaneously fits the cosmological parameters, the evolution of the\ncluster scaling laws and the selection effects. Our results are consistent with\nthe sigma_8 and Omega_m values obtained by WMAP-5 and point toward a negative\nevolution of the cluster scaling relations with respect to the self-similar\nexpectation. We are further able to constrain the cluster fractional radius\nxc0=r_c/r500c, to xc0=0.24 +/- 0.04. This study stresses again the critical\nrole of selection effects in deriving cluster scaling relations, even in the\nlocal universe. Finally, we show that CR-HR method applied to the eRosita\nall-sky survey - provided that cluster photometric redshifts are available -\nwill enable the determination of the equation of state of the dark energy at\nthe level of the DETF stage IV predictions; simultaneously, the evolution of\nthe cluster scaling-relations will be unambiguously determined. The XMM CLuster\nArchive Super Survey (XCLASS) serendipitous cluster catalogue is available\nonline at: http://xmm-lss.in2p3.fr:8080/l4sdb/.", "cat": "astro-ph.CO", "authors": ["Nicolas Clerc", "Tatyana Sadibekova", "Marguerite Pierre", "Florian Pacaud", "Jean-Paul Le F\u00e8vre", "Christophe Adami", "Bruno Altieri", "Ivan Valtchanov"]}, "118": {"id": "1411.5003v3", "title": "Survey of End-to-End Mobile Network Measurement Testbeds, Tools, and Services", "url": "http://arxiv.org/pdf/1411.5003v3", "date": "2015-05-19 02:47:16", "abs": "Mobile (cellular) networks enable innovation, but can also stifle it and lead\nto user frustration when network performance falls below expectations. As\nmobile networks become the predominant method of Internet access, developer,\nresearch, network operator, and regulatory communities have taken an increased\ninterest in measuring end-to-end mobile network performance to, among other\ngoals, minimize negative impact on application responsiveness. In this survey\nwe examine current approaches to end-to-end mobile network performance\nmeasurement, diagnosis, and application prototyping. We compare available tools\nand their shortcomings with respect to the needs of researchers, developers,\nregulators, and the public. We intend for this survey to provide a\ncomprehensive view of currently active efforts and some auspicious directions\nfor future work in mobile network measurement and mobile application\nperformance evaluation.", "cat": "cs.NI", "authors": ["Utkarsh Goel", "Mike P. Wittie", "Kimberly C. Claffy", "Andrew Le"]}, "119": {"id": "2209.03127v2", "title": "Multi-fidelity hydrodynamic analysis of an autonomous surface vehicle at surveying speed in deep water subject to variable payload", "url": "http://arxiv.org/pdf/2209.03127v2", "date": "2022-09-09 09:19:55", "abs": "Autonomous surface vehicles (ASV) allow the investigation of coastal areas,\nports and harbors as well as harsh and dangerous environments such as the\narctic regions. Despite receiving increasing attention, the hydrodynamic\nanalysis of ASV performance subject to variable operational parameters is\nlittle investigated. In this context, this paper presents a multi-fidelity (MF)\nhydrodynamic analysis of an ASV, namely the Shallow Water Autonomous\nMultipurpose Platform (SWAMP), at surveying speed in calm water and subject to\nvariable payload and location of the center of mass, accounting for the variety\nof equipment that the vehicle can carry. The analysis is conducted in deep\nwater, which is the condition mostly encountered by the ASV during surveys of\ncoastal and harbors areas. Quantities of interest are the resistance, the\nvehicle attitude, and the wave generated in the region between the catamaran\nhulls. These are assessed using a Reynolds Averaged Navier Stokes Equation\n(RANSE) code and a linear potential flow (PF) solver. The objective is to\naccurately assess the quantities of interest, along with identifying the\nlimitation of PF analysis in the current context. Finally, a multi-fidelity\nGaussian Process (MF-GP) model is obtained combining RANSE and PF solutions.\nThe latter also include variable grid refinement and coupling between\nhydrodynamic loads and rigid body equations of motion. The surrogate model is\niteratively refined using an active learning approach. Numerical results show\nthat the MF-GP is effective in producing response surfaces of the SWAMP\nperformance with a limited computational cost. It is highlighted how the SWAMP\nperformance is significantly affected not only by the payload, but also by the\nlocation of the center of mass. The latter can be therefore properly calibrated\nto minimize the resistance and allow for longer-range operations.", "cat": "physics.flu-dyn", "authors": ["Riccardo Pellegrini", "Simone Ficini", "Angelo Odetti", "Andrea Serani", "Massimo Caccia", "Matteo Diez"]}, "120": {"id": "2111.04731v2", "title": "Survey of Deep Learning Methods for Inverse Problems", "url": "http://arxiv.org/pdf/2111.04731v2", "date": "2021-11-13 14:38:23", "abs": "In this paper we investigate a variety of deep learning strategies for\nsolving inverse problems. We classify existing deep learning solutions for\ninverse problems into three categories of Direct Mapping, Data Consistency\nOptimizer, and Deep Regularizer. We choose a sample of each inverse problem\ntype, so as to compare the robustness of the three categories, and report a\nstatistical analysis of their differences. We perform extensive experiments on\nthe classic problem of linear regression and three well-known inverse problems\nin computer vision, namely image denoising, 3D human face inverse rendering,\nand object tracking, selected as representative prototypes for each class of\ninverse problems. The overall results and the statistical analyses show that\nthe solution categories have a robustness behaviour dependent on the type of\ninverse problem domain, and specifically dependent on whether or not the\nproblem includes measurement outliers. Based on our experimental results, we\nconclude by proposing the most robust solution category for each inverse\nproblem class.", "cat": "cs.CV", "authors": ["Shima Kamyab", "Zohreh Azimifar", "Rasool Sabzi", "Paul Fieguth"]}, "121": {"id": "1410.7464v1", "title": "HIGHz: A Survey of the Most HI-Massive Galaxies at z~0.2", "url": "http://arxiv.org/pdf/1410.7464v1", "date": "2014-10-28 00:34:05", "abs": "We present the results of the HIGHz Arecibo survey, which measured the HI\ncontent of 39 galaxies at redshift $z>0.16$ selected from the Sloan Digital Sky\nSurvey. These are all actively star-forming, disk-dominated systems in\nrelatively isolated environments, with stellar and HI masses larger than\n$10^{10}$ M$_\\odot$ and redshifts $0.17\\leq z\\leq 0.25$. Our sample includes\nnot only the highest-redshift detections of HI emission from individual\ngalaxies to date, but also some of the most HI-massive systems known. Despite\nbeing exceptionally large, the HI reservoirs of these galaxies are consistent\nwith what is expected from their ultraviolet and optical properties. This, and\nthe fact that the galaxies lie on the baryonic Tully-Fisher relation, suggests\nthat HIGHz systems are rare, scaled-up versions of local disk galaxies. We show\nthat the most HI-massive galaxies discovered in the Arecibo Legacy Fast ALFA\nsurvey are the local analogues of HIGHz, and discuss the possible connection\nbetween our sample and the turbulent, gas-rich disks identified at $z\\sim 1$.\nThe HIGHz sample provides a first glimpse into the properties of the massive,\nHI-rich galaxies that will be detected at higher redshifts by the\nnext-generation HI surveys with the Square Kilometer Array and its pathfinders.", "cat": "astro-ph.GA", "authors": ["Barbara Catinella", "Luca Cortese"]}, "122": {"id": "1504.00782v1", "title": "A comparative study of four significance measures for periodicity detection in astronomical surveys", "url": "http://arxiv.org/pdf/1504.00782v1", "date": "2015-04-03 08:47:43", "abs": "We study the problem of periodicity detection in massive data sets of\nphotometric or radial velocity time series, as presented by ESA's Gaia mission.\nPeriodicity detection hinges on the estimation of the false alarm probability\n(FAP) of the extremum of the periodogram of the time series. We consider the\nproblem of its estimation with two main issues in mind. First, for a given\nnumber of observations and signal-to-noise ratio, the rate of correct\nperiodicity detections should be constant for all realized cadences of\nobservations regardless of the observational time patterns, in order to avoid\nsky biases that are difficult to assess. Second, the computational loads should\nbe kept feasible even for millions of time series. Using the Gaia case, we\ncompare the $F^M$ method (Paltani 2004, Schwarzenberg-Czerny 2012), the Baluev\nmethod (Baluev 2008) and the GEV method (S\\\"uveges 2014), as well as a method\nfor the direct estimation of a threshold. Three methods involve some unknown\nparameters, which are obtained by fitting a regression-type predictive model\nusing easily obtainable covariates derived from observational time series. We\nconclude that the GEV and the Baluev methods both provide good solutions to the\nissues posed by a large-scale processing. The first of these yields the best\nscientific quality at the price of some moderately costly pre-processing. When\nthis pre-processing is impossible for some reason (e.g. the computational costs\nare prohibitive or good regression models cannot be constructed), the Baluev\nmethod provides a computationally inexpensive alternative with slight biases in\nregions where time samplings exhibit strong aliases.", "cat": "astro-ph.IM", "authors": ["Maria S\u00fcveges", "Leanne P. Guy", "Laurent Eyer", "Jan Cuypers", "Berry Holl", "Isabelle Lecoeur-Ta\u00efbi", "Nami Mowlavi", "Krzysztof Nienartowicz", "Diego Ord\u00f3\u00f1ez Blanco", "Lorenzo Rimoldini", "Idoia Ruiz"]}, "123": {"id": "1806.11126v1", "title": "Far-IR dust properties of highly dust obscured AGNs from the AKARI and WISE all-sky surveys", "url": "http://arxiv.org/pdf/1806.11126v1", "date": "2018-06-28 18:00:16", "abs": "The combination of the AKARI and WISE infrared all-sky surveys provides an\nunique opportunity to identify and characterize the most highly dust obscured\nAGNs in the universe. Dust-obscured AGNs are not easily detectable and\npotentially underrepresented in extragalactic surveys due to their high optical\nextinction, but are readily found in the WISE catalog due to their extremely\nred mid-IR colors. Combining these surveys with photometry from Pan-STARRS and\nHerschel, we use SED modeling to characterize the extinction and dust\nproperties of these AGNs. From mid-IR WISE colors, we are able to compute\nbolometric corrections to AGN luminosities. Using AKARI's far-IR wavelength\nphotometry and broadband AGN/galaxy spectral templates, we estimate AGN dust\nmass and temperature using simple analytic models with 3-4 parameters. Even\nwithout spectroscopic data, we can determine a number of AGN dust properties\nonly using SED analysis. These methods, combined with the abundance of archival\nphotometric data publically available, will be valuable for large-scale studies\nof dusty, IR-luminous AGNs.", "cat": "astro-ph.GA", "authors": ["Anson Lam", "Matthew A. Malkan", "Edward L. Wright"]}, "124": {"id": "1404.4935v1", "title": "Opinion Mining In Hindi Language: A Survey", "url": "http://arxiv.org/pdf/1404.4935v1", "date": "2014-04-19 08:14:39", "abs": "Opinions are very important in the life of human beings. These Opinions\nhelped the humans to carry out the decisions. As the impact of the Web is\nincreasing day by day, Web documents can be seen as a new source of opinion for\nhuman beings. Web contains a huge amount of information generated by the users\nthrough blogs, forum entries, and social networking websites and so on To\nanalyze this large amount of information it is required to develop a method\nthat automatically classifies the information available on the Web. This domain\nis called Sentiment Analysis and Opinion Mining. Opinion Mining or Sentiment\nAnalysis is a natural language processing task that mine information from\nvarious text forms such as reviews, news, and blogs and classify them on the\nbasis of their polarity as positive, negative or neutral. But, from the last\nfew years, enormous increase has been seen in Hindi language on the Web.\nResearch in opinion mining mostly carried out in English language but it is\nvery important to perform the opinion mining in Hindi language also as large\namount of information in Hindi is also available on the Web. This paper gives\nan overview of the work that has been done Hindi language.", "cat": "cs.IR", "authors": ["Richa Sharma", "Shweta Nigam", "Rekha Jain"]}, "125": {"id": "1807.09338v1", "title": "C-V2X Security Requirements and Procedures: Survey and Research Directions", "url": "http://arxiv.org/pdf/1807.09338v1", "date": "2018-07-24 20:31:03", "abs": "The 3rd Generation Partnership Project (3GPP) defines the first\nspecifications for cellular-based vehicle-to-everything (C-V2X) communications\nin Release 14. C-V2X extends LTE's device-to-device communication modes by\nadding two new modes of operation for vehicular systems in coverage and out of\ncoverage of an LTE base station, or eNB. The vehicle-to-vehicle (V2V)\ncommunication mode does not rely on the cellular infrastructure and the C-V2X\ndevices employ a distributed and sensing-based semi-persistent scheduling to\nschedule their packet transmissions. As a promising alternative to dedicated\nshort range communications, the security aspects of C-V2X need to be carefully\ndesigned and evaluated to ensure the availability and integrity of the service\nand data. This paper discusses possible threat scenarios, reviews the 3GPP\nspecifications and finds that, despite the safety-critical nature of C-V2X,\nonly few mechanisms and procedures have be specified to secure the system. We\ndiscuss emerging technologies and provide research directions to improve C-V2X\nsystem security and reliability and ensure their widespread adoption in\ncivilian and mission-critical communication contexts.", "cat": "eess.SP", "authors": ["Vuk Marojevic"]}, "126": {"id": "2406.09646v1", "title": "A Survey of Video Datasets for Grounded Event Understanding", "url": "http://arxiv.org/pdf/2406.09646v1", "date": "2024-06-14 00:36:55", "abs": "While existing video benchmarks largely consider specialized downstream tasks\nlike retrieval or question-answering (QA), contemporary multimodal AI systems\nmust be capable of well-rounded common-sense reasoning akin to human visual\nunderstanding. A critical component of human temporal-visual perception is our\nability to identify and cognitively model \"things happening\", or events.\nHistorically, video benchmark tasks have implicitly tested for this ability\n(e.g., video captioning, in which models describe visual events with natural\nlanguage), but they do not consider video event understanding as a task in\nitself. Recent work has begun to explore video analogues to textual event\nextraction but consists of competing task definitions and datasets limited to\nhighly specific event types. Therefore, while there is a rich domain of\nevent-centric video research spanning the past 10+ years, it is unclear how\nvideo event understanding should be framed and what resources we have to study\nit. In this paper, we survey 105 video datasets that require event\nunderstanding capability, consider how they contribute to the study of robust\nevent understanding in video, and assess proposed video event extraction tasks\nin the context of this body of research. We propose suggestions informed by\nthis survey for dataset curation and task framing, with an emphasis on the\nuniquely temporal nature of video events and ambiguity in visual content.", "cat": "cs.CV", "authors": ["Kate Sanders", "Benjamin Van Durme"]}, "127": {"id": "2205.05701v3", "title": "New Observational $H(z)$ Data from Full-Spectrum Fitting of Cosmic Chronometers in the LEGA-C Survey", "url": "http://arxiv.org/pdf/2205.05701v3", "date": "2023-04-07 14:42:08", "abs": "In this work, we perform a full-spectrum fitting of 350 massive and passive\ngalaxies selected as cosmic chronometers from the LEGA-C ESO public survey to\nderive their stellar ages, metallicities, and star-formation histories. We\nextensively test our results by assessing their dependence on the possible\ncontribution of dust, calibration of noise and signal, and the use of\nphotometric data in addition to spectral information; we as well identify\nindicators of the correct convergence of the results, including the shape of\nthe posterior distributions, the analysis of specific spectral features, and\nthe correct reproduction of the observed spectrum. We derive a clear\nage-redshift trend compatible with the aging in a standard cosmological model,\nshowing a clear downsizing pattern, with more massive galaxies being formed at\nhigher redshift ($z_f\\sim2.5$) with respect to lower massive ones ($z_f\\sim2$).\nFrom these data, we measure the differential aging of this population of cosmic\nchronometers to derive a new measurement of the Hubble parameter, obtaining\n$H(z=0.8) = 113.1 \\pm 15.1 (\\mathrm{stat.}) ^{+29.1}_{-11.3} (\\mathrm{syst.})\\\n\\mathrm{ km\\ s^{-1}\\ Mpc^{-1}}$. This analysis allows us for the first time to\ncompare the differential ages of cosmic chronometers measured on the same\nsample with two completely different methods, the full-spectrum fit (this work)\nand the analysis of Lick indices, known to correlate with the age and\nmetallicity of the stellar populations \\citep{Borghi2022a}. Albeit an\nunderstood offset in the absolute ages, the differential ages have proven to be\nextremely compatible between the two methods, despite the very different data,\nassumptions, and models considered, demonstrating the robustness of the method.", "cat": "astro-ph.CO", "authors": ["Kang Jiao", "Nicola Borghi", "Michele Moresco", "Tong-Jie Zhang"]}, "128": {"id": "1505.05347v1", "title": "The VIMOS Public Extragalactic Redshift Survey (VIPERS). Hierarchical scaling and biasing", "url": "http://arxiv.org/pdf/1505.05347v1", "date": "2015-05-20 12:47:30", "abs": "We investigate the higher-order correlation properties of the VIMOS Public\nExtragalactic Redshift Survey (VIPERS) to test the hierarchical scaling\nhypothesis at z~1 and the dependence on galaxy luminosity, stellar mass, and\nredshift. We also aim to assess deviations from the linearity of galaxy bias\nindependently from a previously performed analysis of our survey (Di Porto et\nal. 2014). We have measured the count probability distribution function in\ncells of radii 3 < R < 10 Mpc/h, deriving $\\sigma_{8g}$, the volume-averaged\ntwo-,three-,and four-point correlation functions and the normalized skewness\n$S_{3g}$ and kurtosis $S_{4g}$ for volume-limited subsamples covering the\nranges $-19.5 \\le M_B(z=1.1)-5log(h) \\le -21.0$, $9.0 < log(M*/M_{\\odot}\nh^{-2}) \\le 11.0$, $0.5 \\le z < 1.1$. We have thus performed the first\nmeasurement of high-order correlations at z~1 in a spectroscopic redshift\nsurvey. Our main results are the following. 1) The hierarchical scaling holds\nthroughout the whole range of scale and z. 2) We do not find a significant\ndependence of $S_{3g}$ on luminosity (below z=0.9 $S_{3g}$ decreases with\nluminosity but only at 1{\\sigma}-level). 3) We do not detect a significant\ndependence of $S_{3g}$ and $S_{4g}$ on scale, except beyond z~0.9, where the\ndependence can be explained as a consequence of sample variance. 4) We do not\ndetect an evolution of $S_{3g}$ and $S_{4g}$ with z. 5) The linear bias factor\n$b=\\sigma_{8g}/\\sigma_{8m}$ increases with z, in agreement with previous\nresults. 6) We quantify deviations from the linear bias by means of the Taylor\nexpansion parameter $b_2$. Our results are compatible with a null non-linear\nbias term, but taking into account other available data we argue that there is\nevidence for a small non-linear bias term.", "cat": "astro-ph.CO", "authors": ["A. Cappi", "F. Marulli", "J. Bel", "O. Cucciati", "E. Branchini", "S. de la Torre", "L. Moscardini", "M. Bolzonella", "L. Guzzo", "U. Abbas", "C. Adami", "S. Arnouts", "D. Bottini", "J. Coupon", "I. Davidzon", "G. De Lucia", "A. Fritz", "P. Franzetti", "M. Fumana", "B. Garilli", "B. R. Granett", "O. Ilbert", "A. Iovino", "J. Krywult", "V. Le Brun", "O. Le F\u00e8vre", "D. Maccagni", "K. Ma\u0142ek", "H. J. McCracken", "L. Paioro", "M. Polletta", "A. Pollo", "M. Scodeggio", "L. A. . M. Tasca", "R. Tojeiro", "D. Vergani", "A. Zanichelli", "A. Burden", "C. Di Porto", "A. Marchetti", "C. Marinoni", "Y. Mellier", "R. C. Nichol", "J. A. Peacock", "W. J. Percival", "S. Phleps", "C. Schimd", "H. Schlagenhaufer", "M. Wolk", "G. Zamorani"]}, "129": {"id": "2107.07927v1", "title": "A Survey on Deep Domain Adaptation and Tiny Object Detection Challenges, Techniques and Datasets", "url": "http://arxiv.org/pdf/2107.07927v1", "date": "2021-07-16 14:33:31", "abs": "This survey paper specially analyzed computer vision-based object detection\nchallenges and solutions by different techniques. We mainly highlighted object\ndetection by three different trending strategies, i.e., 1) domain adaptive deep\nlearning-based approaches (discrepancy-based, Adversarial-based,\nReconstruction-based, Hybrid). We examined general as well as tiny object\ndetection-related challenges and offered solutions by historical and\ncomparative analysis. In part 2) we mainly focused on tiny object detection\ntechniques (multi-scale feature learning, Data augmentation, Training strategy\n(TS), Context-based detection, GAN-based detection). In part 3), To obtain\nknowledge-able findings, we discussed different object detection methods, i.e.,\nconvolutions and convolutional neural networks (CNN), pooling operations with\ntrending types. Furthermore, we explained results with the help of some object\ndetection algorithms, i.e., R-CNN, Fast R-CNN, Faster R-CNN, YOLO, and SSD,\nwhich are generally considered the base bone of CV, CNN, and OD. We performed\ncomparative analysis on different datasets such as MS-COCO, PASCAL VOC07,12,\nand ImageNet to analyze results and present findings. At the end, we showed\nfuture directions with existing challenges of the field. In the future, OD\nmethods and models can be analyzed for real-time object detection, tracking\nstrategies.", "cat": "cs.CV", "authors": ["Muhammed Muzammul", "Xi Li"]}, "130": {"id": "2205.03558v1", "title": "From Fontaine-Mazur conjecture to analytic pro-p groups -- A survey", "url": "http://arxiv.org/pdf/2205.03558v1", "date": "2022-05-07 05:14:30", "abs": "Fontaine-Mazur Conjecture is one of the core statements in modern arithmetic\ngeometry. Several formulations were given since its original statement in 1993,\nand various angles have been adopted by numerous authors to try to tackle it.\nBoston's seminal paper in 1992 gave a range of purely group-theoretic methods\nrather than representation-theoretic ones to prove some special cases of this\nconjecture. Such methods have been later successfully carried on by Maire and\nhis co-authors, and brings different informations on the objects involved in\nthe conjecture. This survey article aims to review what is known in this\ndirection and to present some interesting related questions the authors work\non.", "cat": "math.NT", "authors": ["Ramla Abdellatif", "Supriya Pisolkar", "Marine Rougnant", "Lara Thomas"]}, "131": {"id": "2208.05348v2", "title": "First release of Apertif imaging survey data", "url": "http://arxiv.org/pdf/2208.05348v2", "date": "2022-11-22 08:22:51", "abs": "(Abridged) Apertif is a phased-array feed system for WSRT, providing forty\ninstantaneous beams over 300 MHz of bandwidth. A dedicated survey program\nstarted on 1 July 2019, with the last observations taken on 28 February 2022.\nWe describe the release of data products from the first year of survey\noperations, through 30 June 2020. We focus on defining quality control metrics\nfor the processed data products. The Apertif imaging pipeline, Apercal,\nautomatically produces non-primary beam corrected continuum images,\npolarization images and cubes, and uncleaned spectral line and dirty beam cubes\nfor each beam of an Apertif imaging observation. For this release, processed\ndata products are considered on a beam-by-beam basis within an observation. We\nvalidate the continuum images by using metrics that identify deviations from\nGaussian noise in the residual images. If the continuum image passes\nvalidation, we release all processed data products for a given beam. We apply\nfurther validation to the polarization and line data products. We release all\nraw observational data from the first year of survey observations, for a total\nof 221 observations of 160 independent target fields, covering approximately\none thousand square degrees of sky. Images and cubes are released on a per beam\nbasis, and 3374 beams are released. The median noise in the continuum images is\n41.4 uJy/bm, with a slightly lower median noise of 36.9 uJy/bm in the Stokes V\npolarization image. The median angular resolution is 11.6\"/sin(Dec). The median\nnoise for all line cubes, with a spectral resolution of 36.6 kHz, is 1.6\nmJy/bm, corresponding to a 3-sigma HI column density sensitivity of 1.8 x 10^20\natoms cm^-2 over 20 km/s (for a median angular resolution of 24\" x 15\"). We\nalso provide primary beam images for each individual Apertif compound beam. The\ndata are made accessible using a Virtual Observatory interface.", "cat": "astro-ph.IM", "authors": ["Elizabeth A. K. Adams", "B. Adebahr", "W. J. G. de Blok", "H. Denes", "K. M. Hess", "J. M. van der Hulst", "A. Kutkin", "D. M. Lucero", "R. Morganti", "V. A. Moss", "T. A. Oosterloo", "E. Orru", "R. Schulz", "A. S. van Amesfoort", "A. Berger", "O. M. Boersma", "M. Bouwhuis", "R. van den Brink", "W. A. van Cappellen", "L. Connor", "A. H. W. M. Coolen", "S. Damstra", "G. N. J. van Diepen", "T. J. Dijkema", "N. Ebbendorf", "Y. G. Grange", "R. de Goei", "A. W. Gunst", "H. A. Holties", "B. Hut", "M. V. Ivashina", "G. I. G. Jozsa", "G. M. Loose", "J. van Leeuwen", "Y. Maan", "M. Mancini", "A. Mika", "H. Mulder", "M. J. Norden", "A. R. Offringa", "L. C. Oostrum", "I. Pastor-Marazuela", "D. J. Pisano", "A. A. Ponomareva", "J. W. Romein", "M Ruiter", "A. P. Schoenmakers", "D. van der Schuur", "J. J. Sluman", "R. Smits", "K. J. C Stuurwold", "J. Verstappen", "N. P. E Vilchez", "D. Vohl", "K. J. Wierenga", "S. J. Wijnholds", "E. E. M. Woestenburg", "A. W. Zanting", "J. Ziemke"]}, "132": {"id": "2203.00483v4", "title": "A Survey on How Test Flakiness Affects Developers and What Support They Need To Address It", "url": "http://arxiv.org/pdf/2203.00483v4", "date": "2022-04-08 06:55:53", "abs": "Non-deterministically passing and failing test cases, so-called flaky tests,\nhave recently become a focus area of software engineering research. While this\nresearch focus has been met with some enthusiastic endorsement from industry,\nprior work nevertheless mostly studied flakiness using a code-centric approach\nby mining software repositories. What data extracted from software repositories\ncannot tell us, however, is how developers perceive flakiness: How prevalent is\ntest flakiness in developers' daily routine, how does it affect them, and most\nimportantly: What do they want us researchers to do about it? To answer these\nquestions, we surveyed 335 professional software developers and testers in\ndifferent domains. The survey respondents confirm that flaky tests are a common\nand serious problem, thus reinforcing ongoing research on flaky test detection.\nDevelopers are less worried about the computational costs caused by re-running\ntests and more about the loss of trust in the test outcomes. Therefore, they\nwould like to have IDE plugins to detect flaky code as well as better\nvisualizations of the problem, particularly dashboards showing test outcomes\nover time; they also wish for more training and information on flakiness. These\nimportant aspects will require the attention of researchers as well as tool\ndevelopers.", "cat": "cs.SE", "authors": ["Martin Gruber", "Gordon Fraser"]}, "133": {"id": "2106.15638v1", "title": "Rotation periods of TESS Objects of Interest from the Magellan-TESS Survey with multiband photometry from Evryscope and TESS", "url": "http://arxiv.org/pdf/2106.15638v1", "date": "2021-06-29 18:00:06", "abs": "Stellar RV jitter due to surface activity may bias the RV semi-amplitude and\nmass of rocky planets. The amplitude of the jitter may be estimated from the\nuncertainty in the rotation period, allowing the mass to be more accurately\nobtained. We find candidate rotation periods for 17 out of 35 TESS Objects of\nInterest (TOI) hosting <3 R_Earth planets as part of the Magellan-TESS Survey,\nwhich is the first-ever statistically robust study of exoplanet masses and\nradii across the photo-evaporation gap. Seven periods are 3+ sigma detections,\ntwo are 1.5+ sigma, and 8 show plausible variability but the periods remain\nunconfirmed. The other 18 TOIs are non-detections. Candidate rotators include\nthe host stars of the confirmed planets L 168-9 b, the HD 21749 system, LTT\n1445 A b, TOI 1062 b, and the L 98-59 system. 13 candidates have no counterpart\nin the 1000 TOI rotation catalog of Canto Martins et al. (2020). We find\nperiods for G3-M3 dwarfs using combined light curves from TESS and the\nEvryscope all-sky array of small telescopes, sometimes with longer periods than\nwould be possible with TESS alone. Secure periods range from 1.4 to 26 d with\nEvryscope-measured photometric amplitudes as small as 2.1 mmag in g'. We also\napply Monte Carlo sampling and a Gaussian Process stellar activity model from\nthe code exoplanet to the TESS light curves of 6 TOIs to confirm the Evryscope\nperiods.", "cat": "astro-ph.SR", "authors": ["Ward S. Howard", "Johanna Teske", "Hank Corbett", "Nicholas M. Law", "Sharon Xuesong Wang", "Jeffrey K. Ratzloff", "Nathan W. Galliher", "Ramses Gonzalez", "Alan Vasquez Soto", "Amy L. Glazier", "Joshua Haislip"]}, "134": {"id": "2304.07864v2", "title": "Radio AGN Selection and Characterization in Three Deep-Drilling Fields of the Vera C. Rubin Observatory Legacy Survey of Space and Time", "url": "http://arxiv.org/pdf/2304.07864v2", "date": "2023-04-18 16:27:16", "abs": "The Australia Telescope Large Area Survey (ATLAS) and the VLA survey in the\nXMM-LSS/VIDEO deep field provide deep ($\\approx 15$ ${\\mu}$Jybeam$^{-1}$) and\nhigh-resolution ($\\approx$ 4.5--8 arcsec) radio coverage of the three XMM-SERVS\nfields (W-CDF-S, ELAIS-S1, and XMM-LSS). These data cover a total sky area of\n11.3 deg$^2$ and contain $\\approx 11000$ radio components. Furthermore, about\n3~deg$^2$ of the XMM-LSS field also has deeper MIGHTEE data that achieve a\nmedian RMS of 5.6 ${\\mu}$Jy beam$^{-1}$ and detect more than 20000 radio\nsources. We analyze all these radio data and find source counterparts at other\nwavebands utilizing deep optical and IR surveys. The nature of these radio\nsources is studied using radio-band properties (spectral slope and morphology),\nand the IR-radio correlation. %and spectral energy distribution. Radio AGNs are\nselected and compared with those selected using other methods (e.g. X-ray). We\nfound 1656 new AGNs that were not selected using X-ray and/or MIR methods. We\nconstrain the FIR-to-UV SEDs of radio AGNs using {\\sc cigale} and investigate\nthe dependence of radio AGN fraction upon galaxy stellar mass and\nstar-formation rate.", "cat": "astro-ph.GA", "authors": ["Shifu Zhu", "William N. Brandt", "Fan Zou", "Bin Luo", "Qingling Ni", "Yongquan Xue", "Wei Yan"]}, "135": {"id": "2404.15593v1", "title": "A Survey of Deep Long-Tail Classification Advancements", "url": "http://arxiv.org/pdf/2404.15593v1", "date": "2024-04-24 01:59:02", "abs": "Many data distributions in the real world are hardly uniform. Instead, skewed\nand long-tailed distributions of various kinds are commonly observed. This\nposes an interesting problem for machine learning, where most algorithms assume\nor work well with uniformly distributed data. The problem is further\nexacerbated by current state-of-the-art deep learning models requiring large\nvolumes of training data. As such, learning from imbalanced data remains a\nchallenging research problem and a problem that must be solved as we move\ntowards more real-world applications of deep learning. In the context of class\nimbalance, state-of-the-art (SOTA) accuracies on standard benchmark datasets\nfor classification typically fall less than 75%, even for less challenging\ndatasets such as CIFAR100. Nonetheless, there has been progress in this niche\narea of deep learning. To this end, in this survey, we provide a taxonomy of\nvarious methods proposed for addressing the problem of long-tail\nclassification, focusing on works that happened in the last few years under a\nsingle mathematical framework. We also discuss standard performance metrics,\nconvergence studies, feature distribution and classifier analysis. We also\nprovide a quantitative comparison of the performance of different SOTA methods\nand conclude the survey by discussing the remaining challenges and future\nresearch direction.", "cat": "cs.LG", "authors": ["Charika de Alvis", "Suranga Seneviratne"]}, "136": {"id": "1910.11912v2", "title": "Caltech-NRAO Stripe 82 Survey (CNSS). III: The First Radio-discovered Tidal Disruption Event, CNSS J0019+00", "url": "http://arxiv.org/pdf/1910.11912v2", "date": "2020-10-21 21:07:14", "abs": "We present the discovery of a nuclear transient with the Caltech-NRAO Stripe\n82 Survey (CNSS), a dedicated radio transient survey carried out with the Karl\nG. Jansky Very Large Array (VLA). This transient, CNSS J001947.3+003527,\nexhibited a turn-on over a timescale of $\\lesssim$1 yr, increasing in flux\ndensity at 3 GHz from $<0.14$ mJy in 2014 February to $4.4\\pm0.1$ mJy in 2015\nMarch, reaching a peak luminosity of $5\\times10^{28} \\text{erg s}^{-1}\n\\text{Hz}^{-1}$ around 2015 October. The association of CNSS J0019+00 with the\nnucleus (Gaia and our VLBI positions are consistent to within 1 pc) of a nearby\nS0 Seyfert galaxy at 77 Mpc, together with the radio spectral evolution,\nimplies that this transient is most likely a tidal disruption event (TDE). Our\nequipartition analysis indicates the presence of a $\\sim$15,000 km s$^{-1}$\noutflow, having energy $\\sim$10$^{49}$ erg. We derive the radial density\nprofile for the circumnuclear material in the host galaxy to be proportional to\n$R^{-2.5}$. All of these properties suggest resemblance with radio-detected\nthermal TDEs like ASASSN-14li and XMMSL1 J0740-85. No significant X-ray or\noptical emission is detected from CNSS J0019+00, although this may simply be\ndue to the thermal emission being weak during our late-time follow-up\nobservations. From the CNSS survey we have obtained the first unbiased\nmeasurement of the rate of radio TDEs, $R(>500 \\mu{\\rm Jy})$ of about\n$2\\times10^{-3}$ deg$^{-2}$, or equivalently a volumetric rate of about 10\nGpc$^{-3}$ yr$^{-1}$. This rate implies that all-sky radio surveys such as the\nVLA Sky Survey and those planned with ASKAP, will find many tens of radio TDEs\nover the next few years.", "cat": "astro-ph.HE", "authors": ["M. M. Anderson", "K. P. Mooley", "G. Hallinan", "D. Dong", "E. S. Phinney", "A. Horesh", "S. Bourke", "S. B. Cenko", "D. Frail", "S. R. Kulkarni", "S. Myers"]}, "137": {"id": "1912.00715v2", "title": "Learning Bayesian networks from demographic and health survey data", "url": "http://arxiv.org/pdf/1912.00715v2", "date": "2020-04-29 12:27:51", "abs": "Child mortality from preventable diseases such as pneumonia and diarrhoea in\nlow and middle-income countries remains a serious global challenge. We combine\nknowledge with available Demographic and Health Survey (DHS) data from India,\nto construct Causal Bayesian Networks (CBNs) and investigate the factors\nassociated with childhood diarrhoea. We make use of freeware tools to learn the\ngraphical structure of the DHS data with score-based, constraint-based, and\nhybrid structure learning algorithms. We investigate the effect of missing\nvalues, sample size, and knowledge-based constraints on each of the structure\nlearning algorithms and assess their accuracy with multiple scoring functions.\nWeaknesses in the survey methodology and data available, as well as the\nvariability in the CBNs generated by the different algorithms, mean that it is\nnot possible to learn a definitive CBN from data. However, knowledge-based\nconstraints are found to be useful in reducing the variation in the graphs\nproduced by the different algorithms, and produce graphs which are more\nreflective of the likely influential relationships in the data. Furthermore,\nvaluable insights are gained into the performance and characteristics of the\nstructure learning algorithms. Two score-based algorithms in particular, TABU\nand FGES, demonstrate many desirable qualities; a) with sufficient data, they\nproduce a graph which is similar to the reference graph, b) they are relatively\ninsensitive to missing values, and c) behave well with knowledge-based\nconstraints. The results provide a basis for further investigation of the DHS\ndata and for a deeper understanding of the behaviour of the structure learning\nalgorithms when applied to real-world settings.", "cat": "cs.AI", "authors": ["Neville Kenneth Kitson", "Anthony C. Constantinou"]}, "138": {"id": "2309.17257v1", "title": "A Survey on Deep Learning Techniques for Action Anticipation", "url": "http://arxiv.org/pdf/2309.17257v1", "date": "2023-09-29 14:07:56", "abs": "The ability to anticipate possible future human actions is essential for a\nwide range of applications, including autonomous driving and human-robot\ninteraction. Consequently, numerous methods have been introduced for action\nanticipation in recent years, with deep learning-based approaches being\nparticularly popular. In this work, we review the recent advances of action\nanticipation algorithms with a particular focus on daily-living scenarios.\nAdditionally, we classify these methods according to their primary\ncontributions and summarize them in tabular form, allowing readers to grasp the\ndetails at a glance. Furthermore, we delve into the common evaluation metrics\nand datasets used for action anticipation and provide future directions with\nsystematical discussions.", "cat": "cs.CV", "authors": ["Zeyun Zhong", "Manuel Martin", "Michael Voit", "Juergen Gall", "J\u00fcrgen Beyerer"]}, "139": {"id": "1302.0939v1", "title": "Security and Privacy Issues in Wireless Mesh Networks: A Survey", "url": "http://arxiv.org/pdf/1302.0939v1", "date": "2013-02-05 05:20:50", "abs": "This book chapter identifies various security threats in wireless mesh\nnetwork (WMN). Keeping in mind the critical requirement of security and user\nprivacy in WMNs, this chapter provides a comprehensive overview of various\npossible attacks on different layers of the communication protocol stack for\nWMNs and their corresponding defense mechanisms. First, it identifies the\nsecurity vulnerabilities in the physical, link, network, transport, application\nlayers. Furthermore, various possible attacks on the key management protocols,\nuser authentication and access control protocols, and user privacy preservation\nprotocols are presented. After enumerating various possible attacks, the\nchapter provides a detailed discussion on various existing security mechanisms\nand protocols to defend against and wherever possible prevent the possible\nattacks. Comparative analyses are also presented on the security schemes with\nregards to the cryptographic schemes used, key management strategies deployed,\nuse of any trusted third party, computation and communication overhead involved\netc. The chapter then presents a brief discussion on various trust management\napproaches for WMNs since trust and reputation-based schemes are increasingly\nbecoming popular for enforcing security in wireless networks. A number of open\nproblems in security and privacy issues for WMNs are subsequently discussed\nbefore the chapter is finally concluded.", "cat": "cs.CR", "authors": ["Jaydip Sen"]}, "140": {"id": "0710.5163v1", "title": "Newly Discovered Cataclysmic Variables from the INT/WFC Photometric H alpha Survey of the Northern Galactic Plane", "url": "http://arxiv.org/pdf/0710.5163v1", "date": "2007-10-26 19:22:10", "abs": "We report the discovery of 11 new cataclysmic variable (CV) candidates by the\nIsaac Newton Telescope (INT) Photometric H alpha Survey of the northern\nGalactic plane (IPHAS). Three of the systems have been the subject of further\nfollow-up observations. For the CV candidates IPHAS J013031.90+622132.4 and\nIPHAS J051814.34+294113.2, time-resolved optical spectroscopy has been obtained\nand radial-velocity measurements of the H alpha emission-line have been used to\nestimate their orbital periods. A third CV candidate (IPHAS J062746.41+\n014811.3) was observed photometrically and found to be eclipsing. All three\nsystems have orbital periods above the CV period-gap of 2-3 h. We also\nhighlight one other system, IPHAS J025827.88+635234.9, whose spectrum\ndistinguishes it as a likely high luminosity object with unusual C and N\nabundances.", "cat": "astro-ph", "authors": ["A. R. Witham", "C. Knigge", "A. Aungwerojwit", "J. E. Drew", "B. T. Gaensicke", "R. Greimel", "P. J. Groot", "G. H. A. Roelofs", "D. Steeghs", "P. A. Woudt"]}, "141": {"id": "0806.4936v1", "title": "A near-infrared interferometric survey of debris disc stars. II. CHARA/FLUOR observations of six early-type dwarfs", "url": "http://arxiv.org/pdf/0806.4936v1", "date": "2008-06-30 16:24:04", "abs": "High-precision interferometric observations of six early-type main sequence\nstars known to harbour cold debris discs have been obtained in the\nnear-infrared K band with the FLUOR instrument at the CHARA Array. The measured\nsquared visibilities are compared to the expected visibility of the stellar\nphotospheres based on theoretical photospheric models taking into account\nrotational distortion, searching for potential visibility reduction at short\nbaselines due to circumstellar emission. Our observations bring to light the\npresence of resolved circumstellar emission around one of the six target stars\n(zeta Aql) at the 5 sigma level. The morphology of the emission source cannot\nbe directly constrained because of the sparse spatial frequency sampling of our\ninterferometric data. Using complementary adaptive optics observations and\nradial velocity measurements, we find that the presence of a low-mass companion\nis a likely origin for the excess emission. The potential companion has a\nK-band contrast of four magnitudes, a most probable mass of about 0.6 Msun, and\nis expected to orbit between about 5.5 AU and 8 AU from its host star assuming\na purely circular orbit. Nevertheless, by adjusting a physical debris disc\nmodel to the observed Spectral Energy Distribution of the zeta Aql system, we\nalso show that the presence of hot dust within 10 AU from zeta Aql, producing a\ntotal thermal emission equal to 1.69 +- 0.31% of the photospheric flux in the K\nband, is another viable explanation for the observed near-infrared excess. Our\nre-interpretation of archival near- to far-infrared photometric measurements\nshows however that cold dust is not present around zeta Aql at the sensitivity\nlimit of the IRS and MIPS instruments onboard Spitzer, and urges us to remove\nzeta Aql from the category of bona fide debris disc stars.", "cat": "astro-ph", "authors": ["O. Absil", "E. Di Folco", "A. Merand", "J. -C. Augereau", "V. Coude du Foresto", "D. Defrere", "P. Kervella", "J. P. Aufdenberg", "M. Desort", "D. Ehrenreich", "A. -M. Lagrange", "G. Montagnier", "J. Olofsson", "T. A. ten Brummelaar", "H. A. McAlister", "J. Sturmann", "L. Sturmann", "N. H. Turner"]}, "142": {"id": "1511.04183v2", "title": "The NuSTAR Extragalactic Surveys: The Number Counts of Active Galactic Nuclei and the Resolved Fraction of the Cosmic X-ray Background", "url": "http://arxiv.org/pdf/1511.04183v2", "date": "2016-09-10 14:33:56", "abs": "We present the 3-8 keV and 8-24 keV number counts of active galactic nuclei\n(AGN) identified in the NuSTAR extragalactic surveys. NuSTAR has now resolved\n33-39% of the X-ray background in the 8-24 keV band, directly identifying AGN\nwith obscuring columns up to approximately 1e25 /cm2. In the softer 3-8 keV\nband the number counts are in general agreement with those measured by\nXMM-Newton and Chandra over the flux range 5e-15 < S(3 - 8 keV)/(erg/cm2/s) <\n1e-12 probed by NuSTAR. In the hard 8-24 keV band NuSTAR probes fluxes over the\nrange 2e-14 < S(8-24 keV)/(erg/cm2/s) < 1e-12, a factor of approximately 100\nfainter than previous measurements. The 8-24 keV number counts match\npredictions from AGN population synthesis models, directly confirming the\nexistence of a population of obscured and/or hard X-ray sources inferred from\nthe shape of the integrated cosmic X-ray background. The measured NuSTAR counts\nlie significantly above simple extrapolation with a Euclidian slope to low flux\nof the Swift/BAT 15-55 keV number counts measured at higher fluxes S(15-55 keV)\n> 1e-11 erg/cm2/s, reflecting the evolution of the AGN population between the\nSwift/BAT local (z<0.1) sample and NuSTAR's z~1 sample. CXB synthesis models,\nwhich account for AGN evolution, lie above the Swift/BAT measurements,\nsuggesting that they do not fully capture the evolution of obscured AGN at low\nredshifts.", "cat": "astro-ph.HE", "authors": ["F. A. Harrison", "J. Aird", "F. Civano", "G. Lansbury", "J. R. Mullaney", "D. R. Ballantyne", "D. M. Alexander", "D. Stern", "M. Ajello", "D. Barret", "F. E. Bauer", "M. Balokovic", "W. N. Brandt", "M. Brightman", "S. E. Boggs", "F. E. Christensen", "A. Comastri", "W. W. Craig", "A. Del Moro", "K. Forster", "P. Gandhi", "P. Giommi", "B. W. Grefenstette", "C. J. Hailey", "R. C. Hickox", "A. Hornstrup", "T. Kitaguchi", "J. Koglin", "B. Luo", "K. K. Madsen", "P. H. Mao", "H. Miyasaka", "K. Mori", "M. Perri", "M. Pivovaroff", "S. Puccetti", "V. Rana", "E. Treister", "D. Walton", "N. J. Westergaard", "D. Wik", "L. Zappacosta", "W. W. Zhang", "A. Zoglauer"]}, "143": {"id": "2002.02980v1", "title": "The role of galaxy mass on AGN emission: a view from the VANDELS survey", "url": "http://arxiv.org/pdf/2002.02980v1", "date": "2020-02-07 19:02:02", "abs": "We present a comparative analysis of the properties of AGN emitting at radio\nand X-ray wavelengths. The study is performed on 907 X-ray AGN and 100 radio\nAGN selected on the CDFS and UDS fields and makes use of new and ancillary data\navailable to the VANDELS collaboration. Our results indicate that the mass of\nthe host galaxy is a fundamental quantity which determines the level of AGN\nactivity at the various wavelengths. Indeed large stellar masses are found to\nbe connected with AGN radio emission, as virtually all radio-active AGN reside\nwithin galaxies of M*>10^{10} Msun. Large stellar masses also seem to favour\nAGN activity in the X-ray, even though X-ray AGN present a mass distribution\nwhich is more spread out and with a non-negligible tail at M*<10^{9} Msun.\nStellar mass alone is also observed to play a fundamental role in simultaneous\nradio and X-ray emission: the percentage of AGN active at both wavelengths\nincreases from around 1% of all X-ray AGN residing within hosts of M*<10^{11}\nMsun to about 13% in more massive galaxies. In the case of radio-selected AGN,\nsuch a percentage moves from about 15% to about 45% (but up to 80% in the\ndeepest fields). Neither cosmic epoch, nor radio luminosity, X-ray luminosity,\nEddington ratio or star-formation rate of the hosts are found to be connected\nto an enhanced probability for joint radio+X-ray emission of AGN origin.\nFurthermore, only a loose relation is observed between X-ray and radio\nluminosity in those AGN which are simultaneously active at both frequencies.", "cat": "astro-ph.GA", "authors": ["M. Magliocchetti", "L. Pentericci", "M. Cirasuolo", "G. Zamorani", "R. Amorin", "A. Bongiorno", "A. Cimatti", "A. Fontana", "B. Garilli", "A. Gargiulo", "N. P. Hathi", "D. J. McLeod", "R. J. McLure", "M. Brusa", "A. Saxena", "M. Talia"]}, "144": {"id": "1002.1776v2", "title": "The Westerbork SINGS survey III. Global magnetic field topology", "url": "http://arxiv.org/pdf/1002.1776v2", "date": "2010-02-26 00:07:28", "abs": "A sample of large northern Spitzer Infrared Nearby Galaxies Survey (SINGS)\ngalaxies was recently observed with the Westerbork Synthesis Radio Telescope\n(WSRT) at 1300-1760 MHz. In Paper II of this series, we described sensitive\nobservations of the linearly polarized radio continuum emission in this\nWSRT-SINGS galaxy sample. Here we explore the systematic patterns of azimuthal\nmodulation of both the Faraday depth and the polarized intensity and their\nvariation with galaxy inclination. A self-consistent and fully general model\nfor both the locations of net polarized emissivity at 1-2 GHz frequencies and\nthe global magnetic field topology of nearby galaxies emerges. Net polarized\nemissivity is concentrated into two zones located above and below the galaxy\nmid-plane, with the back-side zone suffering substantial depolarization (by a\nfactor of 4-5) relative to the front-side zone in its propagation through the\nturbulent mid-plane. The field topology, which characterizes the thick-disk\nemission zone is in all cases an axisymmetric spiral with a quadrupole\ndependence on height above the mid-plane. The front-side emission is affected\nby only mild dispersion (10's of rad/m2) from the thermal plasma in the galaxy\nhalo, while the back-side emission is affected by additional strong dispersion\n(100's of rad/m2) from an axisymmetric spiral field in the galaxy mid-plane.\nThe field topology in the upper halo of galaxies is a mix of two distinct\ntypes: a simple extension of the axisymmetric spiral quadrupole field of the\nthick disk and a radially directed dipole field. The dipole component might be\na manifestation of (1) a circumnuclear, bipolar outflow, (2) an in situ\ngenerated dipole field, or (3) evidence of a non-stationary global halo.", "cat": "astro-ph.CO", "authors": ["Robert Braun", "George Heald", "Rainer Beck"]}, "145": {"id": "2108.12392v1", "title": "Pairing for Greenhorn: Survey and Future Perspective", "url": "http://arxiv.org/pdf/2108.12392v1", "date": "2021-08-27 16:59:56", "abs": "Pairing is the most powerful tool in cryptography that maps two points on the\nelliptic curve to the group over the finite field. Mostly cryptographers\nconsider pairing as a black box and use it for implementing pairing-based\ncryptographic protocols. This paper aims to give the overview of pairing as\nsimple as possible for greenhorn and those who are working and wish to work in\nthe pairing. The paper gives the concrete background of pairing and recommends\nan appropriate pairing among different choices for constructing pairing-based\ncryptographic protocols. We also analyze the bandwidth and computational\nefficiency of pairing and submitting those pairing suitable for implementing a\ncryptographic protocol for lightweight devices. Additionally, we discuss the\nextension of bilinear pairing to tri-linear and multilinear pairing and discuss\na few assumptions to check their feasibility to implement multilinear pairing.", "cat": "cs.CR", "authors": ["Mahender Kumar", "Satish Chand"]}, "146": {"id": "2302.06712v1", "title": "The SAMI Survey: Evidence for dynamical coupling of ionised gas and young stellar populations", "url": "http://arxiv.org/pdf/2302.06712v1", "date": "2023-02-13 21:54:42", "abs": "We explore local and global dynamical differences between the kinematics of\nionised gas and stars in a sample of galaxies from Data Release 3 of the SAMI\nGalaxy Survey. We find better agreement between local (i.e., comparing on a\nspaxel-to-spaxel basis) velocities and dispersion of gas and stars in younger\nsystems as with previous work on the asymmetric drift in galaxies, suggesting\nthat the dynamics of stars and ionised gas are initially coupled. The intrinsic\nscatter around the velocity and dispersion relations increases with increasing\nstellar age and mass, suggesting that subsequent mechanisms such as internal\nprocesses, divergent star formation and assembly histories also play a role in\nsetting and altering the dynamics of galaxies. The global (flux-weighted)\ndynamical support of older galaxies is hotter than in younger systems. We find\nthat the ionised gas in galaxies is almost always dynamically colder than the\nstars with a steeper velocity gradient. In absolute terms, the local difference\nin velocity dispersion is more pronounced than the local difference in\nvelocity, possibly reflecting inherent differences in the impact of turbulence,\ninflow and/or feedback on gas compared to stars. We suggest how these findings\nmay be taken into account when comparing high and low redshift galaxy samples\nto infer dynamical evolution.", "cat": "astro-ph.GA", "authors": ["Caroline Foster", "Sam Vaughan", "Amelia Fraser-McKelvie", "Sarah Brough", "Julia J. Bryant", "Scott M. Croom", "Francesco D'Eugenio", "Brent Groves", "Iraklis S. Konstantopoulos", "\u00c1ngel R. L\u00f3pez-S\u00e1nchez", "Sree Oh", "Matt S. Owers", "Sarah M. Sweet", "Jesse van de Sande", "Emily Wisnioski", "Sukyoung K. Yi", "Henry R. M. Zovaro"]}, "147": {"id": "1008.2428v2", "title": "A Spitzer c2d Legacy Survey to Identify and Characterize Disks with Inner Dust Holes", "url": "http://arxiv.org/pdf/1008.2428v2", "date": "2010-08-18 09:59:33", "abs": "Understanding how disks dissipate is essential to studies of planet\nformation. However, identifying exactly how dust and gas dissipates is\ncomplicated due to difficulty in finding objects clearly in the transition of\nlosing their surrounding material. We use Spitzer IRS spectra to examine 35\nphotometrically-selected candidate cold disks (disks with large inner dust\nholes). The infrared spectra are supplemented with optical spectra to determine\nstellar and accretion properties and 1.3mm photometry to measure disk masses.\nBased on detailed SED modeling, we identify 15 new cold disks. The remaining 20\nobjects have IRS spectra that are consistent with disks without holes, disks\nthat are observed close to edge-on, or stars with background emission. Based on\nthese results, we determine reliable criteria for identifying disks with inner\nholes from Spitzer photometry and examine criteria already in the literature.\nApplying these criteria to the c2d surveyed star-forming regions gives a\nfrequency of such objects of at least 4% and most likely of order 12% of the\nYSO population identified by Spitzer.\n We also examine the properties of these new cold disks in combination with\ncold disks from the literature. Hole sizes in this sample are generally smaller\nthan for previously discovered disks and reflect a distribution in better\nagreement with exoplanet orbit radii. We find correlations between hole size\nand both disk and stellar masses. Silicate features, including crystalline\nfeatures, are present in the overwhelming majority of the sample although 10\nmicron feature strength above the continuum declines for holes with radii\nlarger than ~7 AU. In contrast, PAHs are only detected in 2 out of 15 sources.\nOnly a quarter of the cold disk sample shows no signs of accretion, making it\nunlikely that photoevaporation is the dominant hole forming process in most\ncases.", "cat": "astro-ph.SR", "authors": ["Bruno Mer\u00edn", "Joanna M. Brown", "Isa Oliveira", "Gregory J. Herczeg", "Ewine F. van Dishoeck", "Sandrine Bottinelli", "Neal J. Evans II", "Lucas Cieza", "Loredana Spezzi", "Juan M. Alcal\u00e1", "Paul M. Harvey", "Geoffrey A. Blake", "Amelia Bayo", "Vincent G. Geers", "Fred Lahuis", "Timo Prusti", "Jean-Charles Augereau", "Johan Olofsson", "Frederick M. Walter", "Kuenley Chiu"]}, "148": {"id": "2209.15370v1", "title": "Automatic Context-Driven Inference of Engagement in HMI: A Survey", "url": "http://arxiv.org/pdf/2209.15370v1", "date": "2022-09-30 10:46:13", "abs": "An integral part of seamless human-human communication is engagement, the\nprocess by which two or more participants establish, maintain, and end their\nperceived connection. Therefore, to develop successful human-centered\nhuman-machine interaction applications, automatic engagement inference is one\nof the tasks required to achieve engaging interactions between humans and\nmachines, and to make machines attuned to their users, hence enhancing user\nsatisfaction and technology acceptance. Several factors contribute to\nengagement state inference, which include the interaction context and\ninteractants' behaviours and identity. Indeed, engagement is a multi-faceted\nand multi-modal construct that requires high accuracy in the analysis and\ninterpretation of contextual, verbal and non-verbal cues. Thus, the development\nof an automated and intelligent system that accomplishes this task has been\nproven to be challenging so far. This paper presents a comprehensive survey on\nprevious work in engagement inference for human-machine interaction, entailing\ninterdisciplinary definition, engagement components and factors, publicly\navailable datasets, ground truth assessment, and most commonly used features\nand methods, serving as a guide for the development of future human-machine\ninteraction interfaces with reliable context-aware engagement inference\ncapability. An in-depth review across embodied and disembodied interaction\nmodes, and an emphasis on the interaction context of which engagement\nperception modules are integrated sets apart the presented survey from existing\nsurveys.", "cat": "cs.HC", "authors": ["Hanan Salam", "Oya Celiktutan", "Hatice Gunes", "Mohamed Chetouani"]}, "149": {"id": "1112.0327v2", "title": "Probing dark energy with the next generation X-ray surveys of galaxy clusters", "url": "http://arxiv.org/pdf/1112.0327v2", "date": "2012-07-09 13:02:29", "abs": "We present forecasts on the capability of future wide-area high-sensitivity\nX-ray surveys of galaxy clusters to yield constraints on the parameters\ndefining the Dark Energy (DE) equation of state (EoS). Our analysis is carried\nout for future X-ray surveys which have enough sensitivity to provide accurate\nmeasurements of X-ray mass proxies and Fe-line based redshifts for about 2x10^4\nclusters. We base our analysis on the Fisher Matrix formalism, by combining\ninformation on the cluster number counts and power spectrum, also including,\nfor the first time in the analysis of the large scale cluster distribution, the\neffect of linear redshift-space distortions (RSDs). This study is performed\nwith the main purpose of dissecting the cosmological information provided by\ngeometrical and growth tests, which are both included in the analysis of number\ncounts and clustering of galaxy clusters. We compare cosmological constraints\nobtained by assuming different levels of prior knowledge of the parameters\nwhich define the observable-mass X-ray relation. This comparison further\ndemonstrates the fundamental importance of having a well calibrated\nobservable-mass relation and, most importantly, its redshift evolution. Such a\ncalibration can be achieved only by having at least $\\sim 10^3$ net photon\ncounts for each cluster included in the survey. We show that RSDs in the power\nspectrum analysis carry important cosmological information also when traced\nwith galaxy clusters and the DE FoM increases by a factor of 8. Besides\nconfirming the potential that large cluster surveys have in constraining the\nnature of DE, our analysis emphasizes that a full exploitation of the\ncosmological information carried by such surveys requires not only a large\nstatistic but also a robust measurement of the mass proxies and redshifts for a\nsignificant fraction of the cluster sample, derived from the same X-ray survey\ndata.", "cat": "astro-ph.CO", "authors": ["B. Sartoris", "S. Borgani", "P. Rosati", "J. Weller"]}, "150": {"id": "1001.0027v1", "title": "New candidate Planetary Nebulae in the IPHAS survey: the case of PNe with ISM interaction", "url": "http://arxiv.org/pdf/1001.0027v1", "date": "2009-12-30 21:25:44", "abs": "We present the results of the search for candidate Planetary Nebulae\ninteracting with the interstellar medium (PN-ISM) in the framework of the INT\nPhotometric H$\\alpha$ Survey (IPHAS) and located in the right ascension range\n18h-20h. The detection capability of this new Northern survey, in terms of\ndepth and imaging resolution, has allowed us to overcome the detection problem\ngenerally associated to the low surface brightness inherent to PNe-ISM. We\ndiscuss the detection of 21 IPHAS PN-ISM candidates. Thus, different stages of\ninteraction were observed, implying various morphologies i.e. from the\nunaffected to totally disrupted shapes. The majority of the sources belong to\nthe so-called WZO2 stage which main characteristic is a brightening of the\nnebula's shell in the direction of motion. The new findings are encouraging as\nthey would be a first step into the reduction of the scarcity of observational\ndata and they would provide new insights into the physical processes occurring\nin the rather evolved PNe.", "cat": "astro-ph.GA", "authors": ["Laurence Sabin", "Albert A. Zijlstra", "Christopher Wareing", "Romano L. M. Corradi", "Antonio Mampaso", "Kerttu Viironen", "Nicholas J. Wright", "Quentin A. Parker"]}, "151": {"id": "2203.16584v2", "title": "The GMRT archive atomic gas survey -- I. Survey definition, methodology, and initial results from the pilot sample", "url": "http://arxiv.org/pdf/2203.16584v2", "date": "2022-06-01 18:00:25", "abs": "Interferometric observations of HI in galaxies played a pivotal role in\nstudies of nearby galaxies. Compared to single-dish observation, it provides\nresolved distribution of gas in galaxies with unprecedented resolution. Several\nextensive HI surveys of nearby galaxies have been performed in the past;\nhowever, most of them consist of less than 100 galaxies due to individual\nefforts. On the other hand, present-day archives of the radio telescopes\ninclude data for at least several hundred galaxies. To utilize these data sets\nto their full potential, we construct a sample including all galaxies observed\nby the Giant Meter wave Radio Telescope (GMRT) in HI. This results in a total\nof 515 galaxies, the largest sample to date. We intend to analyze all the data\nuniformly and carry out different exciting science. As a pilot project, we\nanalyze data from 11 galaxies and present the data products in this paper. We\nfurther investigate the neutral ISM in these galaxies and extract cold and warm\nphases using a multi-Gaussian decomposition method. This pilot project assures\nthe quality of the data, which will enable us to perform critical science\ninvestigations using the full sample.", "cat": "astro-ph.GA", "authors": ["Prerana Biswas", "Narendra Nath Patra", "Nirupam Roy", "Md. Rashid"]}, "152": {"id": "1311.5087v1", "title": "A High Angular Resolution Survey of Massive Stars in Cygnus OB2: Results from the Hubble Space Telescope Fine Guidance Sensors", "url": "http://arxiv.org/pdf/1311.5087v1", "date": "2013-11-20 15:06:06", "abs": "We present results of a high angular resolution survey of massive OB stars in\nthe Cygnus OB2 association that we conducted with the Fine Guidance Sensor 1R\n(FGS1r) on the Hubble Space Telescope. FGS1r is able to resolve binary systems\nwith a magnitude difference delta-V < 4 down to separations as small as 0.01\narcsec. The sample includes 58 of the brighter members of Cyg OB2, one of the\nclosest examples of an environment containing a large number of very young and\nmassive stars. We resolved binary companions for 12 targets and confirmed the\ntriple nature of one other target, and we offer evidence of marginally resolved\ncompanions for two additional stars. We confirm the binary nature of 11 of\nthese systems from complementary adaptive optics imaging observations. The\noverall binary frequency in our study is 22% to 26% corresponding to orbital\nperiods ranging from 20 - 20,000 years. When combined with the known\nshort-period spectroscopic binaries, the results supports the hypothesis that\nthe binary fraction among massive stars is > 60%. One of the new discoveries is\na companion to the hypergiant star MT 304 = Cyg OB2-12, and future measurements\nof orbital motion should provide mass estimates for this very luminous star.", "cat": "astro-ph.SR", "authors": ["Saida M. Caballero-Nieves", "Edmund P. Nelan", "Douglas R. Gies", "Debra J. Wallace", "Katherine DeGioia-Eastwood", "Artemio Herrero", "Wei-Chun Jao", "Brian D. Mason", "Philip Massey", "Anthony F. J. Moffat", "Nolan R. Walborn"]}, "153": {"id": "2304.09206v1", "title": "The ALMA REBELS Survey: Discovery of a massive, highly star-forming and morphologically complex ULIRG at $z =7.31$", "url": "http://arxiv.org/pdf/2304.09206v1", "date": "2023-04-18 18:00:41", "abs": "We present Atacama Large Millimeter/Submillimeter Array (ALMA) [CII] and\n$\\sim158$ $\\rm\\mu m$ continuum observations of REBELS-25, a massive,\nmorphologically complex ultra-luminous infrared galaxy (ULIRG; $L_{\\rm\nIR}=1.5^{+0.8}_{-0.5}\\times10^{12}$ L$_\\odot$) at $z=7.31$, spectroscopically\nconfirmed by the Reionization Era Bright Emission Line Survey (REBELS) ALMA\nLarge Programme. REBELS-25 has a significant stellar mass of\n$M_{*}=8^{+4}_{-2}\\times10^{9}$ M$_\\odot$. From dust-continuum and ultraviolet\nobservations, we determine a total obscured + unobscured star formation rate of\nSFR $=199^{+101}_{-63}$ M$_\\odot$ yr$^{-1}$. This is about four times the SFR\nestimated from an extrapolated main-sequence. We also infer a [CII]-based\nmolecular gas mass of $M_{\\rm H_2}=5.1^{+5.1}_{-2.6}\\times10^{10}$ $M_\\odot$,\nimplying a molecular gas depletion time of $ t_{\\rm depl,\nH_2}=0.3^{+0.3}_{-0.2}$ Gyr. We observe a [CII] velocity gradient consistent\nwith disc rotation, but given the current resolution we cannot rule out a more\ncomplex velocity structure such as a merger. The spectrum exhibits excess [CII]\nemission at large positive velocities ($\\sim500$ km s$^{-1}$), which we\ninterpret as either a merging companion or an outflow. In the outflow scenario,\nwe derive a lower limit of the mass outflow rate of 200 M$_\\odot$ yr$^{-1}$,\nwhich is consistent with expectations for a star formation-driven outflow.\nGiven its large stellar mass, SFR and molecular gas reservoir $\\sim700$ Myr\nafter the Big Bang, we explore the future evolution of REBELS-25. Considering a\nsimple, conservative model assuming an exponentially declining star formation\nhistory, constant star formation efficiency, and no additional gas inflow, we\nfind that REBELS-25 has the potential to evolve into a galaxy consistent with\nthe properties of high-mass quiescent galaxies recently observed at $z\\sim4$.", "cat": "astro-ph.GA", "authors": ["A. P. S. Hygate", "J. A. Hodge", "E. da Cunha", "M. Rybak", "S. Schouws", "H. Inami", "M. Stefanon", "L. Graziani", "R. Schneider", "P. Dayal", "R. J. Bouwens", "R. Smit", "R. A. A. Bowler", "R. Endsley", "V. Gonzalez", "P. A. Oesch", "D. P. Stark", "H. S. B. Algera", "M. Aravena", "L. Barrufet", "A. Ferrara", "Y. Fudamoto", "J. H. A", "I. De Looze", "T. Nanayakkara", "A. Pallottin", "D. A. Riechers", "L. Sommovigo", "M. W. Topping", "P. van der Werf"]}, "154": {"id": "2312.17253v1", "title": "Deep Learning-based Sentiment Classification: A Comparative Survey", "url": "http://arxiv.org/pdf/2312.17253v1", "date": "2023-12-12 15:57:44", "abs": "Recently, Deep Learning (DL) approaches have been applied to solve the\nSentiment Classification (SC) problem, which is a core task in reviews mining\nor Sentiment Analysis (SA). The performances of these approaches are affected\nby different factors. This paper addresses these factors and classifies them\ninto three categories: data preparation based factors, feature representation\nbased factors and the classification techniques based factors. The paper is a\ncomprehensive literature-based survey that compares the performance of more\nthan 100 DL-based SC approaches by using 21 public datasets of reviews given by\ncustomers within three specific application domains (products, movies and\nrestaurants). These 21 datasets have different characteristics\n(balanced/imbalanced, size, etc.) to give a global vision for our study. The\ncomparison explains how the proposed factors quantitatively affect the\nperformance of the studied DL-based SC approaches.", "cat": "cs.CL", "authors": ["Mohamed Kayed", "Rebeca P. D\u00edaz-Redondo", "Alhassan Mabrouk"]}, "155": {"id": "2111.12173v2", "title": "The VLT-FLAMES survey of massive stars. NGC2004#115: A triple system hosting a possible short period B+BH binary", "url": "http://arxiv.org/pdf/2111.12173v2", "date": "2021-11-30 22:36:23", "abs": "The star NGC2004#115 in the LMC, originally classified as an (SB1) Be\nspectroscopic binary, bears some morphological resemblance to the Galactic\nsystems LB-1 and HR 6819, both of which are proposed as either Be+black hole\n(BH) or Be+stripped He-star systems. Two data-sets (ESO/VLT and SALT) of\nmulti-epoch optical spectra of NGC 2004#115, separated by baseline of $\\sim$20\nyears, lead us conclude it is a triple system hosting an inner binary with a\nperiod of 2.92 d, eccentricity $\\sim$0.0 and mass function $\\sim$0.07\n$M_\\odot$. The inner binary harbours a B-type star (the primary) with projected\nrotational velocity of 10km/s, and luminosity $\\log L/L_\\odot$=3.87,\ncontributing $\\sim$60% of the V-band light to the system. The secondary is not\ndetected, while the tertiary, which contributes 40% of the light, is\ntentatively identified as a less luminous B-type star with high projected\nrotational velocity. No ellipsoidal light variability is detected, with\nstringent limits being set by MACHO and Gaia data. Assuming the primary to be a\nmain sequence star yields a mass of 8.6$ M_\\odot$, while the additional\nassumption of synchronous rotation constrains the inclination to be almost\npole-on with i~9 degrees, implying the secondary is a BH with a mass of\n$\\sim$25 $M_\\odot$. A low mass stripped star with similar luminosity is ruled\nout as a potential solution as its mass implies a Roche radius that is\nsubstantially smaller than the stellar radius. The outer period likely exceeds\n120 days and, while the disk-like emission is variable (it is almost absent in\nthe SALT dataset), it may be associated with the inner binary rather than the\nrapidly rotating tertiary. XMM-Newton provides an upper limit of 5x$10^{33}$\nergs/s on the X-ray flux, consistent with, though not constraining of, the\nsystem hosting a quiescent B+BH binary. A number of caveats to this scenario\nare discussed in the paper.", "cat": "astro-ph.SR", "authors": ["D. J. Lennon", "P. L. Dufton", "J. I. Villase\u00f1or", "C. J. Evans", "N. Langer", "R. Saxton", "I. M. Monageng", "S. Toonen"]}, "156": {"id": "2205.01040v1", "title": "A Survey on Uncertainty Toolkits for Deep Learning", "url": "http://arxiv.org/pdf/2205.01040v1", "date": "2022-05-02 17:23:06", "abs": "The success of deep learning (DL) fostered the creation of unifying\nframeworks such as tensorflow or pytorch as much as it was driven by their\ncreation in return. Having common building blocks facilitates the exchange of,\ne.g., models or concepts and makes developments easier replicable. Nonetheless,\nrobust and reliable evaluation and assessment of DL models has often proven\nchallenging. This is at odds with their increasing safety relevance, which\nrecently culminated in the field of \"trustworthy ML\". We believe that, among\nothers, further unification of evaluation and safeguarding methodologies in\nterms of toolkits, i.e., small and specialized framework derivatives, might\npositively impact problems of trustworthiness as well as reproducibility. To\nthis end, we present the first survey on toolkits for uncertainty estimation\n(UE) in DL, as UE forms a cornerstone in assessing model reliability. We\ninvestigate 11 toolkits with respect to modeling and evaluation capabilities,\nproviding an in-depth comparison for the three most promising ones, namely\nPyro, Tensorflow Probability, and Uncertainty Quantification 360. While the\nfirst two provide a large degree of flexibility and seamless integration into\ntheir respective framework, the last one has the larger methodological scope.", "cat": "cs.LG", "authors": ["Maximilian Pintz", "Joachim Sicking", "Maximilian Poretschkin", "Maram Akila"]}, "157": {"id": "1105.2395v3", "title": "Population III.1 and III.2 gamma-Ray Bursts: Constraints on the event rate for future radio and X-ray surveys", "url": "http://arxiv.org/pdf/1105.2395v3", "date": "2011-08-12 16:07:38", "abs": "We calculate the theoretical event rate of gamma-ray bursts (GRBs) from the\ncollapse of massive first-generation (Population III; Pop III) stars. The Pop\nIII GRBs could be super-energetic with the isotropic energy up to $E_{\\rm iso}\n\\gtrsim 10^{55-57}$ ergs, providing a unique probe of the high-redshift\nUniverse. We consider both the so-called Pop III.1 stars (primordial) and Pop\nIII.2 stars (primordial but affected by radiation from other stars). We employ\na semi-analytical approach that considers inhomogeneous hydrogen reionization\nand chemical evolution of the intergalactic medium. We show that Pop III.2 GRBs\noccur more than 100 times more frequently than Pop III.1 GRBs, and thus should\nbe suitable targets for future GRB missions. Interestingly, our optimistic\nmodel predicts an event rate that is already constrained by the current radio\ntransient searches. We expect $\\sim10-10^4$ radio afterglows above $\\sim$ 0.3\nmJy on the sky with $\\sim 1$ year variability and mostly without GRBs\n(orphans), which are detectable by ALMA, EVLA, LOFAR, and SKA, while we expect\nto observe maximum of $N < 20$ GRBs per year integrated over at $z>6$ for Pop\nIII.2 and $N < 0.08$ per year integrated over at $z>10$ for Pop III.1 with\nEXIST, and $N < 0.2$ for Pop III.2 GRBs per year integrated over at $z > 6$\nwith \\textit{Swift}.", "cat": "astro-ph.CO", "authors": ["Rafael S de Souza", "Naoki Yoshida", "Kunihito Ioka"]}, "158": {"id": "1512.03565v1", "title": "A Survey of multimedia streaming in wireless sensor networks: progress, issues and design challenges", "url": "http://arxiv.org/pdf/1512.03565v1", "date": "2015-12-11 09:51:58", "abs": "Advancements in Complementary Metal Oxide Semiconductor (CMOS) technology\nhave enabled Wireless Sensor Networks (WSN) to gather, process and transport\nmultimedia (MM) data as well and not just limited to handling ordinary scalar\ndata anymore. This new generation of WSN type is called Wireless Multimedia\nSensor Networks (WMSNs). Better and yet relatively cheaper sensors that are\nable to sense both scalar data and multimedia data with more advanced\nfunctionalities such as being able to handle rather intense computations easily\nhave sprung up. In this paper, the applications, architectures, challenges and\nissues faced in the design of WMSNs are explored. Security and privacy issues,\nover all requirements, proposed and implemented solutions so far, some of the\nsuccessful achievements and other related works in the field are also\nhighlighted. Open research areas are pointed out and a few solution suggestions\nto the still persistent problems are made, which, to the best of my knowledge,\nso far have not been explored yet.", "cat": "cs.NI", "authors": ["Taner Cevik", "Alex Gunagwera", "Nazife Cevik"]}, "159": {"id": "2204.11866v1", "title": "Red supergiant stars in binary systems. I. Identification and characterisation in the Small Magellanic Cloud from the UVIT ultraviolet imaging survey", "url": "http://arxiv.org/pdf/2204.11866v1", "date": "2022-04-25 18:00:01", "abs": "We aim to identify and characterise binary systems containing red supergiant\n(RSG) stars in the Small Magellanic Cloud (SMC) using a newly available\nultraviolet (UV) point source catalogue obtained using the Ultraviolet Imaging\nTelescope (UVIT) on board AstroSat. We select a sample of 560 SMC RSGs based on\nphotometric and spectroscopic observations at optical wavelengths and\ncross-match this with the far-UV point source catalogue using the UVIT F172M\nfilter, finding 88 matches down to m$_{F172M}$=20.3 ABmag, which we interpret\nas hot companions to the RSGs. Stellar parameters (luminosities, effective\ntemperatures and masses) for both components in all 88 binary systems are\ndetermined and we find mass distributions in the ranges 6.1 to 22.3 Solar\nmasses for RSGs and 3.7 to 15.6 Solar masses for their companions. The most\nmassive RSG binary system in the SMC has a combined mass of 32 $\\pm$4\nM$_\\odot$, with a mass ratio (q) of 0.92. By simulating observing biases, we\nfind an intrinsic multipliciy fraction of 18.8 $\\pm$ 1.5% for mass ratios in\nthe range 0.3 < q < 1.0 and orbital periods approximately in the range 3 < log\nP [days] < 8. By comparing our results with those of a similar mass on the\nmain-sequence, we determine the fraction of single stars to be ~20% and argue\nthat the orbital period distribution declines rapidly beyond log P ~ 3.5. We\nstudy the mass-ratio distribution of RSG binary systems and find that a uniform\ndistribution best describes the data below 14 M$_\\odot$. Above 15 M$_\\odot$, we\nfind a lack of high mass-ratio systems.", "cat": "astro-ph.SR", "authors": ["L. R. Patrick", "D. Thilker", "D. J. Lennon", "L. Bianchi", "A. Schootemeijer", "R. Dorda", "N. Langer", "I. Negueruela"]}, "160": {"id": "2302.05927v1", "title": "Transfer Learning for Bayesian Optimization: A Survey", "url": "http://arxiv.org/pdf/2302.05927v1", "date": "2023-02-12 14:37:25", "abs": "A wide spectrum of design and decision problems, including parameter tuning,\nA/B testing and drug design, intrinsically are instances of black-box\noptimization. Bayesian optimization (BO) is a powerful tool that models and\noptimizes such expensive \"black-box\" functions. However, at the beginning of\noptimization, vanilla Bayesian optimization methods often suffer from slow\nconvergence issue due to inaccurate modeling based on few trials. To address\nthis issue, researchers in the BO community propose to incorporate the spirit\nof transfer learning to accelerate optimization process, which could borrow\nstrength from the past tasks (source tasks) to accelerate the current\noptimization problem (target task). This survey paper first summarizes transfer\nlearning methods for Bayesian optimization from four perspectives: initial\npoints design, search space design, surrogate model, and acquisition function.\nThen it highlights its methodological aspects and technical details for each\napproach. Finally, it showcases a wide range of applications and proposes\npromising future directions.", "cat": "cs.LG", "authors": ["Tianyi Bai", "Yang Li", "Yu Shen", "Xinyi Zhang", "Wentao Zhang", "Bin Cui"]}, "161": {"id": "1801.00649v1", "title": "Validation of Hardware Security and Trust: A Survey", "url": "http://arxiv.org/pdf/1801.00649v1", "date": "2018-01-02 17:47:07", "abs": "With ever advancing in digital system, security has been emerged as a major\nconcern. Many researchers all around the world come up with solutions to\naddress various challenges that are crucial for industry and market. The aim of\nthis survey is a brief review of challenges of security validation as well as\ndefine and classify Hardware Trojans. Then, we provide more details about\nvarious validation techniques for hardware security and trust.", "cat": "cs.CR", "authors": ["Payman Behnam"]}, "162": {"id": "2211.15224v1", "title": "The Pristine Inner Galaxy Survey (PIGS) VI: Different vertical distributions between two DIBs at 442.8 nm and 862.1 nm", "url": "http://arxiv.org/pdf/2211.15224v1", "date": "2022-11-28 11:21:33", "abs": "Although diffuse interstellar bands (DIBs) were discovered over 100 years\nago, for most of them, their origins are still unknown. Investigation on the\ncorrelations between different DIBs is an important way to study the behavior\nand distributions of their carriers. Based on stacking thousands of spectra\nfrom the Pristine Inner Galaxy Survey, we study the correlations between two\nDIBs at 442.8 nm ($\\lambda$442.8) and 862.1 nm ($\\lambda$862.1), as well as the\ndust grains, in a range of latitude spanning ${\\sim}22^{\\circ}$\n($4^{\\circ}\\,{<}\\,|b|\\,{<}\\,15^{\\circ}$) toward the Galactic center\n($|\\ell|\\,{<}\\,11^{\\circ}$). Tight linear intensity correlations can be found\nbetween $\\lambda$442.8, $\\lambda$862.1, and dust grains for\n$|b|\\,{<}\\,12^{\\circ}$ or $E(B-V)\\,{>}\\,0.3$ mag. For $|b|\\,{>}\\,12^{\\circ}$,\n$\\lambda$442.8 and $\\lambda$862.1 present larger relative strength with respect\nto the dust grains. A systematic variation of the relative strength between\n$\\lambda$442.8 and $\\lambda$862.1 with $|b|$ and $E(B-V)$ concludes that the\ntwo DIBs do not share a common carrier. Furthermore, the carrier of\n$\\lambda$862.1 is more abundant at high latitudes than that of $\\lambda$442.8.\nThis work can be treated as an example showing the significance and potentials\nto the DIB research covering a large latitude range.", "cat": "astro-ph.GA", "authors": ["He Zhao", "Mathias Schultheis", "Anke Arentsen", "Georges Kordopatis", "Morgan Fouesneau", "Else Starkenburg", "Federico Sestito", "Vanessa Hill", "Nicolas F. Martin", "S\u00e9bastien Fabbro", "A. B. A. Queiroz"]}, "163": {"id": "1706.00411v2", "title": "Persistent topology for natural data analysis - A survey", "url": "http://arxiv.org/pdf/1706.00411v2", "date": "2017-08-18 09:51:17", "abs": "Natural data offer a hard challenge to data analysis. One set of tools is\nbeing developed by several teams to face this difficult task: Persistent\ntopology. After a brief introduction to this theory, some applications to the\nanalysis and classification of cells, lesions, music pieces, gait, oil and gas\nreservoirs, cyclones, galaxies, bones, brain connections, languages,\nhandwritten and gestured letters are shown.", "cat": "math.AT", "authors": ["Massimo Ferri"]}, "164": {"id": "2404.14942v1", "title": "Manipulating Recommender Systems: A Survey of Poisoning Attacks and Countermeasures", "url": "http://arxiv.org/pdf/2404.14942v1", "date": "2024-04-23 11:36:36", "abs": "Recommender systems have become an integral part of online services to help\nusers locate specific information in a sea of data. However, existing studies\nshow that some recommender systems are vulnerable to poisoning attacks,\nparticularly those that involve learning schemes. A poisoning attack is where\nan adversary injects carefully crafted data into the process of training a\nmodel, with the goal of manipulating the system's final recommendations. Based\non recent advancements in artificial intelligence, such attacks have gained\nimportance recently. While numerous countermeasures to poisoning attacks have\nbeen developed, they have not yet been systematically linked to the properties\nof the attacks. Consequently, assessing the respective risks and potential\nsuccess of mitigation strategies is difficult, if not impossible. This survey\naims to fill this gap by primarily focusing on poisoning attacks and their\ncountermeasures. This is in contrast to prior surveys that mainly focus on\nattacks and their detection methods. Through an exhaustive literature review,\nwe provide a novel taxonomy for poisoning attacks, formalise its dimensions,\nand accordingly organise 30+ attacks described in the literature. Further, we\nreview 40+ countermeasures to detect and/or prevent poisoning attacks,\nevaluating their effectiveness against specific types of attacks. This\ncomprehensive survey should serve as a point of reference for protecting\nrecommender systems against poisoning attacks. The article concludes with a\ndiscussion on open issues in the field and impactful directions for future\nresearch. A rich repository of resources associated with poisoning attacks is\navailable at https://github.com/tamlhp/awesome-recsys-poisoning.", "cat": "cs.CR", "authors": ["Thanh Toan Nguyen", "Quoc Viet Hung Nguyen", "Thanh Tam Nguyen", "Thanh Trung Huynh", "Thanh Thi Nguyen", "Matthias Weidlich", "Hongzhi Yin"]}, "165": {"id": "2002.11545v2", "title": "Towards Utilizing Unlabeled Data in Federated Learning: A Survey and Prospective", "url": "http://arxiv.org/pdf/2002.11545v2", "date": "2020-05-11 11:44:11", "abs": "Federated Learning (FL) proposed in recent years has received significant\nattention from researchers in that it can bring separate data sources together\nand build machine learning models in a collaborative but private manner. Yet,\nin most applications of FL, such as keyboard prediction, labeling data requires\nvirtually no additional efforts, which is not generally the case. In reality,\nacquiring large-scale labeled datasets can be extremely costly, which motivates\nresearch works that exploit unlabeled data to help build machine learning\nmodels. However, to the best of our knowledge, few existing works aim to\nutilize unlabeled data to enhance federated learning, which leaves a\npotentially promising research topic. In this paper, we identify the need to\nexploit unlabeled data in FL, and survey possible research fields that can\ncontribute to the goal.", "cat": "cs.LG", "authors": ["Yilun Jin", "Xiguang Wei", "Yang Liu", "Qiang Yang"]}, "166": {"id": "2405.10630v1", "title": "Medical Dialogue: A Survey of Categories, Methods, Evaluation and Challenges", "url": "http://arxiv.org/pdf/2405.10630v1", "date": "2024-05-17 08:46:15", "abs": "This paper surveys and organizes research works on medical dialog systems,\nwhich is an important yet challenging task. Although these systems have been\nsurveyed in the medical community from an application perspective, a systematic\nreview from a rigorous technical perspective has to date remained noticeably\nabsent. As a result, an overview of the categories, methods, and evaluation of\nmedical dialogue systems remain limited and underspecified, hindering the\nfurther improvement of this area. To fill this gap, we investigate an initial\npool of 325 papers from well-known computer science, and natural language\nprocessing conferences and journals, and make an overview. Recently, large\nlanguage models have shown strong model capacity on downstream tasks, which\nalso reshaped medical dialog systems' foundation. Despite the alluring\npractical application value, current medical dialogue systems still suffer from\nproblems. To this end, this paper lists the grand challenges of medical dialog\nsystems, especially of large language models.", "cat": "cs.CL", "authors": ["Xiaoming Shi", "Zeming Liu", "Li Du", "Yuxuan Wang", "Hongru Wang", "Yuhang Guo", "Tong Ruan", "Jie Xu", "Shaoting Zhang"]}, "167": {"id": "1807.10655v2", "title": "Pristine Dwarf-Galaxy Survey I: A detailed photometric and spectroscopic study of the very metal-poor Draco II satellite", "url": "http://arxiv.org/pdf/1807.10655v2", "date": "2018-08-06 12:18:46", "abs": "We present a detailed study of the faint Milky Way satellite Draco II (Dra\nII) from deep CFHT/MegaCam broadband $g$ and $i$ photometry and narrow-band\nmetallicity-sensitive CaHK observations, along with follow-up Keck II/DEIMOS\nmulti-object spectroscopy. Forward modeling of the deep photometry allows us to\nrefine the structural and photometric properties of Dra II: the distribution of\nstars in colour-magnitude space implies Dra II is old (13.5 $ \\pm 0.5 $ Gyr),\nvery metal poor, very faint ($ L_V = 180 ^{+124}_{-72} L_\\odot $), and at a\ndistance $d = 21.5 \\pm 0.4$ kpc. The narrow-band, metallicity-sensitive CaHK\nPristine photometry confirms this very low metallicity ([Fe/H]$ = -2.7 \\pm 0.1$\ndex). Even though our study benefits from a doubling of the spectroscopic\nsample size compared to previous investigations, the velocity dispersion of the\nsystem is still only marginally resolved ($\\sigma_{vr}<5.9$ km s$^{-1}$ at the\n95 per cent confidence level) and confirms that Dra II is a dynamically cold\nstellar system with a large recessional velocity ($\\langle v_{r}\\rangle =\n-342.5^{+1.1}_{-1.2} $ km s$^{-1}$). We further show that the spectroscopically\nconfirmed members of Dra~II have a mean proper motion of\n$(\\mu_\\alpha^*,\\mu_\\delta)=(1.26 \\pm 0.27,0.94 \\pm 0.28) $ mas yr$^{-1}$ in the\nGaia DR2 data, which translates to an orbit with a pericenter and an apocenter\nof $21.3 ^{+0.7}_{-1.0}$ and $153.8 ^{+56.7}_{-34.7}$ kpc, respectively. Taken\naltogether, these properties favour the scenario of Dra~II being a potentially\ndisrupting dwarf galaxy. The low-significance extra-tidal features we map\naround the satellite tentatively support this scenario.", "cat": "astro-ph.GA", "authors": ["Nicolas Longeard", "Nicolas Martin", "Else Starkenburg", "Rodrigo A. Ibata", "Michelle L. M. Collins", "Marla Geha", "Benjamin P. M. Laevens", "R. Michael Rich", "David S. Aguado", "Anke Arentsen", "Raymond G. Carlberg", "Patrick C\u00f4t\u00e9", "Vanessa Hill", "Pascale Jablonka", "Jonay I. Gonz\u00e1lez Hern\u00e1ndez", "Julio F. Navarro", "Rub\u00e9n S\u00e1nchez-Janssen", "Eline Tolstoy", "Kim A. Venn", "Kris Youakim"]}, "168": {"id": "2206.11308v1", "title": "Super-resolution trends in the ALMA Taurus survey: Structured inner discs and compact discs", "url": "http://arxiv.org/pdf/2206.11308v1", "date": "2022-06-22 18:18:47", "abs": "The 1.33 mm survey of protoplanetary discs in the Taurus molecular cloud\nfound annular gaps and rings to be common in extended sources (>~55 au), when\ntheir 1D visibility distributions were fit parametrically. We first demonstrate\nthe advantages and limitations of nonparametric visibility fits for data at the\nsurvey's 0.12\" resolution. Then we use the nonparametric model in Frankenstein\n('frank') to identify new substructure in three compact and seven extended\nsources. Among the new features we identify three trends: a higher occurrence\nrate of substructure in the survey's compact discs than previously seen,\nunderresolved (potentially azimuthally asymmetric) substructure in the\ninnermost disc of extended sources, and a 'shoulder' on the trailing edge of a\nring in discs with strong depletion at small radii. Noting the shoulder\nmorphology is present in multiple discs observed at higher resolution, we\npostulate it is tracing a common physical mechanism. We further demonstrate how\na super-resolution frank brightness profile is useful in motivating an accurate\nparametric model, using the highly structured source DL Tau in which frank\nfinds two new rings. Finally we show that sparse (u, v) plane sampling may be\nmasking the presence of substructure in several additional compact survey\nsources.", "cat": "astro-ph.EP", "authors": ["Jeff Jennings", "Marco Tazzari", "Cathie J. Clarke", "Richard A. Booth", "Giovanni P. Rosotti"]}, "169": {"id": "2210.09621v1", "title": "Dust extinction map of the Galactic plane based on the VVV survey data", "url": "http://arxiv.org/pdf/2210.09621v1", "date": "2022-10-18 06:29:46", "abs": "Dust extinction is one of the most reliable tracers of the gas distribution\nin the Milky Way. The near-infrared (NIR) Vista Variables in the Via Lactea\n(VVV) survey enables extinction mapping based on stellar photometry over a\nlarge area in the Galactic plane. We devise a novel extinction mapping\napproach, XPNICER, by bringing together VVV photometric catalogs, stellar\nparameter data from StarHorse catalogs, and previously published Xpercentile\nand PNICER extinction mapping techniques. We apply the approach to the VVV\nsurvey area, resulting in an extinction map that covers the Galactic disk\nbetween 295 and 350 degrees at longitude and -2 to 2 degrees at latitude, and\nthe Galactic bulge between -10 and 5 degrees at latitude. The map has 30\narcseconds spatial resolution and it traces extinctions typically up to about\n10-20 mag of visual extinction and maximally up to Av~30 mag. We compare our\nmap to previous dust based maps, concluding that it provides a high-fidelity\nextinction-based map, especially in its ability to recover both the diffuse\ndust component of the Galaxy and moderately extincted giant molecular cloud\nregions. The map is especially useful as independent, extinction-based data on\nthe Galactic dust distribution and applicable for a wide range of studies from\nindividual molecular clouds to the studies of the Galactic stellar populations.", "cat": "astro-ph.GA", "authors": ["Miaomiao Zhang", "Jouni Kainulainen"]}, "170": {"id": "1210.1020v1", "title": "Radio Halos in future surveys in the radio continuum", "url": "http://arxiv.org/pdf/1210.1020v1", "date": "2012-10-03 08:24:10", "abs": "Giant radio halos (RH) are Mpc-scale synchrotron sources detected in a\nsignificant fraction of massive and merging galaxy clusters.Their statistical\nproperties can be used to discriminate among various models for their origin.\nTheoretical predictions are important as new radio telescopes are about to\nbegin to survey the sky at low and high frequencies with unprecedented\nsensitivity. We carry out Monte Carlo simulations to model the formation and\nevolution of RH in a cosmological framework by assuming that RH are either\ngenerated in turbulent merging clusters, or are purely hadronic sources\ngenerated in more relaxed clusters, \"off-state\" halos. The models predict that\nthe luminosity function of RH at high radio luminosities is dominated by the\ncontribution of RH generated in turbulent clusters. The generation of these RH\nbecomes less efficient in less massive systems causing a flattening of the\nluminosity function at lower luminosities. This flattening is compensated by\nthe contribution of \"off-state\" RH that dominate at lower luminosities. By\nrestricting to clusters at z<0.6, we show that the planned EMU+WODAN surveys at\n1.4 GHz have the potential to detect up to ~200 RH, increasing their number by\none order of magnitude. A fraction of these sources will be \"off-state\" RH that\nshould be found at flux level < 10 mJy, presently accessible only to deep\npointed observations. We also explore the synergy between the Tier 1 LOFAR\nsurvey at 150 MHz and the EMU+WODAN surveys at 1.4 GHz. We predict a larger\nnumber of RH in the LOFAR survey due to the high LOFAR sensitivity, but also\ndue to the existence of RH with very steep spectrum that glow up preferentially\nat lower frequencies. These RH are only predicted in the framework of turbulent\nre-acceleration models and should not have counterparts in the EMU+WODAN\nsurveys, thus the combination of the two surveys will test theoretical models.", "cat": "astro-ph.CO", "authors": ["R. Cassano", "G. Brunetti", "Ray P. Norris", "H. J. A. Roettgering", "M. Johnston-Hollitt", "M. Trasatti"]}, "171": {"id": "2306.08158v5", "title": "Sociodemographic Bias in Language Models: A Survey and Forward Path", "url": "http://arxiv.org/pdf/2306.08158v5", "date": "2024-08-13 19:51:48", "abs": "Sociodemographic bias in language models (LMs) has the potential for harm\nwhen deployed in real-world settings. This paper presents a comprehensive\nsurvey of the past decade of research on sociodemographic bias in LMs,\norganized into a typology that facilitates examining the different aims: types\nof bias, quantifying bias, and debiasing techniques. We track the evolution of\nthe latter two questions, then identify current trends and their limitations,\nas well as emerging techniques. To guide future research towards more effective\nand reliable solutions, and to help authors situate their work within this\nbroad landscape, we conclude with a checklist of open questions.", "cat": "cs.CL", "authors": ["Vipul Gupta", "Pranav Narayanan Venkit", "Shomir Wilson", "Rebecca J. Passonneau"]}, "172": {"id": "1409.5605v1", "title": "A Far-Infrared Spectroscopic Survey of Intermediate Redshift (Ultra) Luminous Infrared Galaxies", "url": "http://arxiv.org/pdf/1409.5605v1", "date": "2014-09-19 11:23:54", "abs": "We present Herschel far-IR photometry and spectroscopy as well as ground\nbased CO observations of an intermediate redshift (0.21 < z < 0.88) sample of\nHerschel-selected (ultra)-luminous infrared galaxies (L_IR > 10^11.5L_sun).\nWith these measurements we trace the dust continuum, far-IR atomic line\nemission, in particular [CII]\\,157.7microns, as well as the molecular gas of\nz~0.3 (U)LIRGs and perform a detailed investigation of the interstellar medium\nof the population. We find that the majority of Herschel-selected intermediate\nredshift (U)LIRGs have L_CII/L_FIR ratios that are a factor of about 10 higher\nthan that of local ULIRGs and comparable to that of local normal and high-$z$\nstar forming galaxies. Using our sample to bridge local and high-z [CII]\nobservations, we find that the majority of galaxies at all redshifts and all\nluminosities follow a L_CII-L_FIR relation with a slope of unity, from which\nlocal ULIRGs and high-z AGN dominated sources are clear outliers. We also\nconfirm that the strong anti-correlation between the L_CII/L_FIR ratio and the\nfar-IR color L_60/L_100 observed in the local Universe holds over a broad range\nof redshifts and luminosities, in the sense that warmer sources exhibit lower\nL_CII/L_FIR at any epoch. Intermediate redshift ULIRGs are also characterised\nby large molecular gas reservoirs and by lower star formation efficiencies\ncompared to that of local ULIRGs. The high L_CII/L_FIR ratios, the moderate\nstar formation efficiencies (L_LIR/L_CO or L_IR/M_gas) and the relatively low\ndust temperatures of our sample (which are also common characteristics of\nhigh-z star forming galaxies with ULIRG-like luminosities) indicate that the\nevolution of the physical properties of (U)LIRGs between the present day and z\n> 1 is already significant by z ~ 0.3.", "cat": "astro-ph.GA", "authors": ["Georgios E. Magdis", "D. Rigopoulou", "R. Hopwood", "J. -S Huang", "D. Farrah", "C. Pearson", "A. Alonso-Herrero", "J. J. Bock", "D. Clements", "A. Cooray", "M. J. Griffin", "S. Oliver", ". Perez Fournon", "D. Riechers", "B. M. Swinyard", "D. Scott", "N. Thatte", "I. Valtchanov", "M. Vaccari"]}, "173": {"id": "2109.03999v3", "title": "Towards Efficient Synchronous Federated Training: A Survey on System Optimization Strategies", "url": "http://arxiv.org/pdf/2109.03999v3", "date": "2022-05-30 13:44:21", "abs": "The increasing demand for privacy-preserving collaborative learning has given\nrise to a new computing paradigm called federated learning (FL), in which\nclients collaboratively train a machine learning (ML) model without revealing\ntheir private training data. Given an acceptable level of privacy guarantee,\nthe goal of FL is to minimize the time-to-accuracy of model training. Compared\nwith distributed ML in data centers, there are four distinct challenges to\nachieving short time-to-accuracy in FL training, namely the lack of information\nfor optimization, the tradeoff between statistical and system utility, client\nheterogeneity, and large configuration space. In this paper, we survey recent\nworks in addressing these challenges and present them following a typical\ntraining workflow through three phases: client selection, configuration, and\nreporting. We also review system works including measurement studies and\nbenchmarking tools that aim to support FL developers.", "cat": "cs.DC", "authors": ["Zhifeng Jiang", "Wei Wang", "Bo Li", "Qiang Yang"]}, "174": {"id": "2405.14221v1", "title": "Survey on Visual Signal Coding and Processing with Generative Models: Technologies, Standards and Optimization", "url": "http://arxiv.org/pdf/2405.14221v1", "date": "2024-05-23 06:32:27", "abs": "This paper provides a survey of the latest developments in visual signal\ncoding and processing with generative models. Specifically, our focus is on\npresenting the advancement of generative models and their influence on research\nin the domain of visual signal coding and processing. This survey study begins\nwith a brief introduction of well-established generative models, including the\nVariational Autoencoder (VAE) models, Generative Adversarial Network (GAN)\nmodels, Autoregressive (AR) models, Normalizing Flows and Diffusion models. The\nsubsequent section of the paper explores the advancements in visual signal\ncoding based on generative models, as well as the ongoing international\nstandardization activities. In the realm of visual signal processing, our focus\nlies on the application and development of various generative models in the\nresearch of visual signal restoration. We also present the latest developments\nin generative visual signal synthesis and editing, along with visual signal\nquality assessment using generative models and quality assessment for\ngenerative models. The practical implementation of these studies is closely\nlinked to the investigation of fast optimization. This paper additionally\npresents the latest advancements in fast optimization on visual signal coding\nand processing with generative models. We hope to advance this field by\nproviding researchers and practitioners a comprehensive literature review on\nthe topic of visual signal coding and processing with generative models.", "cat": "eess.IV", "authors": ["Zhibo Chen", "Heming Sun", "Li Zhang", "Fan Zhang"]}, "175": {"id": "1811.07949v1", "title": "The environments of radio-loud AGN from the LOFAR Two-Metre Sky Survey (LoTSS)", "url": "http://arxiv.org/pdf/1811.07949v1", "date": "2018-11-19 19:41:42", "abs": "An understanding of the relationship between radio-loud active galaxies and\ntheir large-scale environments is essential for realistic modelling of\nradio-galaxy evolution and environmental impact, for understanding AGN\ntriggering and life cycles, and for calibrating galaxy feedback in cosmological\nmodels. We use the LOFAR Two-Metre Sky Survey (LoTSS) Data Release 1 catalogues\nto investigate this relationship. We cross-matched 8,745 radio-loud AGN with\n0.08 10^7.5-8 M_sun. 156/187 (83%) sources are identified with optical\ngalaxies from the Virgo Cluster Catalogue (Binggeli et al. 1985), all but 8\nwith late-type galaxies. Ten sources are not associated with optical galaxies\nand were found to correspond to tidally-disrupted systems (see Kent et al. 2007\nand Haynes, Giovanelli and Kent 2007). The remaining 21 (11%) are associated\nwith galaxies that are not listed in the Virgo Cluster Catalogue. For all\nsources with an optical counterpart in the Sloan Digital Sky Survey, we\nanalyzed i-band SDSS plates to measure optical structural parameters. We find\nthat in the Virgo cluster: i) HI inhabits galaxies that are structurally\nsimilar to ordinary late-type galaxies; ii) their HI content can be predicted\nfrom their optical luminosity; iii) low surface brightness galaxies have low\noptical luminosity and contain small quantities of neutral hydrogen; iv) low\nsurface brightness, massive Malin1 type galaxies are comfortably rare objects\n(less than 0.5%); v) there are no \"dark-galaxies\" with HI masses M_HI >\n10^7.5-8 M_sun; vi) less than 1% of early-type galaxies contain neutral\nhydrogen with M_HI>10^7.5-8 M_sun (di Serego Alighieri et al. 2007).", "cat": "astro-ph", "authors": ["Giuseppe Gavazzi", "Riccardo Giovanelli", "Martha P. Haynes", "Silvia Fabello", "Michele Fumagalli", "Brian R. Kent", "Rebecca A. Koopmann", "Noah Brosch", "G. Lyle Hoffman", "John J. Salzer", "Alessandro Boselli"]}, "186": {"id": "1903.11081v2", "title": "The VANDELS survey: the stellar metallicities of star-forming galaxies at 2.5 < z < 5.0", "url": "http://arxiv.org/pdf/1903.11081v2", "date": "2019-05-22 11:07:36", "abs": "We present the results of a study utilising ultra-deep, rest-frame UV,\nspectroscopy to quantify the relationship between stellar mass and stellar\nmetallicity for 681 star-forming galaxies at $2.550) photometry for main sequence stars with mass down to\n~0.5 M_SUN in a large sample of clusters using both archival and proprietary U,\nB, V, and I data from ground-based telescopes. In this paper, we focus on the\noccurrence of multiple stellar populations in twenty three clusters. We have\ndefined a new photometric index cubi= (U-B)-(B-I), that turns out to be very\neffective for identifying multiple sequences along the red giant branch (RGB).\nWe found that in the V-cubi diagram all clusters presented in this paper show\nbroadened or multimodal RGBs, with the presence of two or more components. We\nfound a direct connection with the chemical properties of different sequences,\nthat display different abundances of light elements (O, Na, C, N, and Al). The\ncubi index is also a powerful tool to identify distinct sequences of stars\nalong the horizontal branch and, for the first time in the case of NGC104 (47\nTuc), along the asymptotic giant branch. Our results demonstrate that i) the\npresence of more than two stellar populations is a common feature among\nglobular clusters, as already highlighted in previous work; ii) multiple\nsequences with different chemical contents can be easily identified by using\nstandard Johnson photometry obtained with ground-based facilities; iii) in the\nstudy of GC multiple stellar populations the cubi index is alternative to\nspectroscopy, and has the advantage of larger statistics.", "cat": "astro-ph.SR", "authors": ["M. Monelli", "A. P. Milone", "P. B. Stetson", "A. F. Marino", "S. Cassisi", "A. Del Pino Molina", "M. Salaris", "A. Aparicio", "M. Asplund", "F. Grundahl", "G. Piotto", "A. Weiss", "R. Carrera", "M. Cebrian", "S. Murabito", "A. Pietrinferni", "L. Sbordone"]}, "190": {"id": "0802.1424v1", "title": "The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds.X. The Chamaeleon II Pre-Main Sequence Population as Observed With IRAC and MIPS", "url": "http://arxiv.org/pdf/0802.1424v1", "date": "2008-02-11 11:59:44", "abs": "We discuss the results from the combined IRAC and MIPS c2d Spitzer Legacy\nsurvey observations and complementary optical and near infrared data of the\nChamaeleon II (Cha II) dark cloud. We perform a census of the young population\nof Cha II, in a mapped area of ~1.75 square degrees, and study the spatial\ndistribution and properties of the cloud members and candidate pre-main\nsequence (PMS) objects and their circumstellar matter. From the analysis of the\nvolume density of the PMS objects and candidates we find two tight groups of\nobjects with volume densities higher than 25 solar masses per cubic parsec and\n5-10 members each. These groups correlate well in space with the regions of\nhigh extinction. A multiplicity fraction of about 13% is observed for objects\nwith separations between 0.8\" and 6.0\". Using the results of masses and ages\nfrom a companion paper, we estimate the star formation efficiency to be 1-4%\nsignificantly lower than for Cha I. This might mean that different\nstar-formation activities in the Chamaeleon clouds reflect a different history\nof star formation. We also find that the Cha II cloud is turning some 6-7 solar\nmasses into stars every Myr, which is low in comparison with the star formation\nrate in other c2d clouds. On the other hand, the disk fraction of 70-80% that\nwe estimate in Cha II is much higher than in other star forming regions and\nindicates that the population in this cloud is dominated by objects with active\naccretion. Finally, the Cha II outflows are discussed, with particular regard\nto the discovery of a new Herbig-Haro outflow, HH 939, driven by the classical\nT Tauri star Sz 50.", "cat": "astro-ph", "authors": ["Juan M. Alcala'", "Loredana Spezzi", "Nicholas Chapman", "Neal J. Evans II", "Tracy L. Huard", "Jes K. Jorgens", "Bruno Merin", "Karl R. Stapelfel", "Elvira Covino", "Antonio Frasca", "Davide Gandolfi", "Isa Oliveira"]}, "191": {"id": "2306.14956v1", "title": "The continuous cadence Roman Galactic Bulge survey", "url": "http://arxiv.org/pdf/2306.14956v1", "date": "2023-06-26 18:00:03", "abs": "Galactic binaries with orbital periods less than 1 hour are strong\ngravitational wave sources in the mHz regime, ideal for the Laser\nInterferometer Space Antenna (LISA). At least several hundred, maybe up to a\nthousand of those binaries are predicted to be sufficiently bright in\nelectromagnetic wavebands to allow detection in both the electromagnetic and\nthe gravitational bands allowing us to perform multi-messenger studies on a\nstatistically significant sample. Theory predicts that a large number of these\nsources will be located in the Galactic Plane and in particular towards the\nGalactic Bulge region. Some of these tight binaries may host sub-stellar\ntertiaries. In this white paper we propose an observing strategy for the\nGalactic Bulge Time Domain Survey which would use the unique observing\ncapabilities of the Nancy Grace Roman Space telescope to discover and study\nseveral 10s of new strong LISA gravitational sources as well as exoplanet\ncandidates around compact white dwarf binaries and other short period variables\nsuch as flaring stars, compact pulsators and rotators.", "cat": "astro-ph.IM", "authors": ["Thomas Kupfer", "Camilla Danielski", "Poshak Gandhi", "Thomas J. Maccarone", "Gijs Nelemans", "Valeriya Korol", "Liliana Rivera Sandoval"]}, "192": {"id": "1909.10946v3", "title": "Forecast for FAST: from Galaxies Survey to Intensity Mapping", "url": "http://arxiv.org/pdf/1909.10946v3", "date": "2020-03-27 15:20:41", "abs": "The Five-Hundred-Meter Aperture Spherical Radio Telescope(FAST) is the\nlargest single-dish radio telescope in the world. In this paper, we make\nforecast on the FAST HI large scale structure survey by mock observations. We\nconsider a drift scan survey with the L-band 19 beam receiver, which may be\ncommensal with the pulsar search and Galactic HI survey. We also consider\nsurveys at lower frequency, either using the current single feed wide band\nreceiver, or a future multi-beam phased array feed (PAF) in the UHF band. We\nestimate the number density of detected HI galaxies and the measurement error\nin positions, the precision of the surveys are evaluated using both Fisher\nmatrix and simulated observations. The measurement error in the HI galaxy power\nspectrum is estimated, and we find that the error is relatively large even at\nmoderate redshifts, as the number of positively detected galaxies drops\ndrastically with increasing redshift. However, good cosmological measurement\ncould be obtained with the intensity mapping technique where the large scale HI\ndistribution is measured without resolving individual galaxies. The figure of\nmerit (FoM) for the dark energy equation of state with different observation\ntimes are estimated, we find that with the existing L-band multi-beam receiver,\na good measurement of low redshift large scale structure can be obtained, which\ncomplements the existing optical surveys. With a PAF in the UHF band, the\nconstraint can be much stronger, reaching the level of a dark energy task force\n(DETF) stage IV experiment.", "cat": "astro-ph.CO", "authors": ["Wenkai Hu", "Xin Wang", "Fengquan Wu", "Yougang Wang", "Pengjie Zhang", "Xuelei Chen"]}, "193": {"id": "2009.14116v1", "title": "A Survey on Semantic Parsing from the perspective of Compositionality", "url": "http://arxiv.org/pdf/2009.14116v1", "date": "2020-09-29 16:03:13", "abs": "Different from previous surveys in semantic parsing (Kamath and Das, 2018)\nand knowledge base question answering(KBQA)(Chakraborty et al., 2019; Zhu et\nal., 2019; Hoffner et al., 2017) we try to takes a different perspective on the\nstudy of semantic parsing. Specifically, we will focus on (a)meaning\ncomposition from syntactical structure(Partee, 1975), and (b) the ability of\nsemantic parsers to handle lexical variation given the context of a knowledge\nbase (KB). In the following section after an introduction of the field of\nsemantic parsing and its uses in KBQA, we will describe meaning representation\nusing grammar formalism CCG (Steedman, 1996). We will discuss semantic\ncomposition using formal languages in Section 2. In section 3 we will consider\nsystems that uses formal languages e.g. $\\lambda$-calculus (Steedman, 1996),\n$\\lambda$-DCS (Liang, 2013). Section 4 and 5 consider semantic parser using\nstructured-language for logical form. Section 6 is on different benchmark\ndatasets ComplexQuestions (Bao et al.,2016) and GraphQuestions (Su et al.,\n2016) that can be used to evaluate semantic parser on their ability to answer\ncomplex questions that are highly compositional in nature.", "cat": "cs.CL", "authors": ["Pawan Kumar", "Srikanta Bedathur"]}, "194": {"id": "1206.0403v1", "title": "The IRAM-30m line survey of the Horsehead PDR: I. CF+ as a tracer of C+ and a measure of the Fluorine abundance", "url": "http://arxiv.org/pdf/1206.0403v1", "date": "2012-06-02 21:18:33", "abs": "C+ is a key species in the interstellar medium but its 158 {\\mu}m fine\nstructure line cannot be observed from ground-based telescopes. Current models\nof fluorine chemistry predict that CF+ is the second most important fluorine\nreservoir, in regions where C+ is abundant. We detected the J = 1-0 and J = 2-1\nrotational lines of CF+ with high signal-to-noise ratio towards the PDR and\ndense core positions in the Horsehead. Using a rotational diagram analysis, we\nderive a column density of N(CF+) = (1.5 - 2.0) \\times 10^12 cm^-2. Because of\nthe simple fluorine chemistry, the CF+ column density is proportional to the\nfluorine abundance. We thus infer the fluorine gas-phase abundance to be F/H =\n(0.6 - 1.5) \\times 10^-8. Photochemical models indicate that CF+ is found in\nthe layers where C+ is abundant. The emission arises in the UV illuminated skin\nof the nebula, tracing the outermost cloud layers. Indeed, CF+ and C+ are the\nonly species observed to date in the Horsehead with a double peaked line\nprofile caused by kinematics. We therefore propose that CF+, which is\ndetectable from the ground, can be used as a proxy of the C+ layers.", "cat": "astro-ph.GA", "authors": ["V. Guzm\u00e1n", "J. Pety", "P. Gratier", "J. R. Goicoechea", "M. Gerin", "E. Roueff", "D. Teyssier"]}, "195": {"id": "1612.01453v1", "title": "A note and a short survey on supporting lines of compact convex sets in the plane", "url": "http://arxiv.org/pdf/1612.01453v1", "date": "2016-12-05 17:49:43", "abs": "After surveying some known properties of compact convex sets in the plane, we\ngive a two rigorous proofs of the general feeling that supporting lines can be\nslide-turned slowly and continuously. Targeting a wide readership, our\ntreatment is elementary on purpose.", "cat": "math.CO", "authors": ["G\u00e1bor Cz\u00e9dli", "L\u00e1szl\u00f3 L. Stach\u00f3"]}, "196": {"id": "1811.02518v1", "title": "Luminous red galaxies in the Kilo Degree Survey: selection with broad-band photometry and weak lensing measurements", "url": "http://arxiv.org/pdf/1811.02518v1", "date": "2018-11-06 17:39:05", "abs": "We use the overlap between multiband photometry of the Kilo-Degree Survey\n(KiDS) and spectroscopic data based on the Sloan Digital Sky Survey (SDSS) and\nGalaxy And Mass Assembly (GAMA) to infer the colour-magnitude relation of\nred-sequence galaxies. We then use this inferred relation to select luminous\nred galaxies (LRGs) in the redshift range of $0.1 4).", "cat": "astro-ph", "authors": ["Timothy Garn", "Paul Alexander"]}, "207": {"id": "2002.00207v2", "title": "Web Table Extraction, Retrieval and Augmentation: A Survey", "url": "http://arxiv.org/pdf/2002.00207v2", "date": "2020-02-05 18:46:58", "abs": "Tables are a powerful and popular tool for organizing and manipulating data.\nA vast number of tables can be found on the Web, which represents a valuable\nknowledge resource. The objective of this survey is to synthesize and present\ntwo decades of research on web tables. In particular, we organize existing\nliterature into six main categories of information access tasks: table\nextraction, table interpretation, table search, question answering, knowledge\nbase augmentation, and table augmentation. For each of these tasks, we identify\nand describe seminal approaches, present relevant resources, and point out\ninterdependencies among the different tasks.", "cat": "cs.IR", "authors": ["Shuo Zhang", "Krisztian Balog"]}, "208": {"id": "2001.06070v1", "title": "The Deepest Radio Observations of Nearby Type IA Supernovae: Constraining Progenitor Types and Optimizing Future Surveys", "url": "http://arxiv.org/pdf/2001.06070v1", "date": "2020-01-16 21:04:25", "abs": "We report deep radio observations of nearby Type Ia Supernovae (SNe Ia) with\nthe electronic Multi-Element Radio Linked Interferometer Net-work (e-MERLIN),\nand the Australia Telescope Compact Array (ATCA). No detections were made. With\nstandard assumptions for the energy densities of relativistic electrons going\ninto a power-law energy distribution, and the magnetic field strength\n(epsilon_e = epsilon_B = 0.1), we arrive at the upper limits on mass-loss rate\nfor the progenitor system of SN 2013dy (2016coj, 2018gv, 2018pv, 2019np), to be\nless than 12 (2.8,1.3, 2.1, 1.7)EE(-8) solar masses per year (for a wind speed\nof 100 km/s). To SNe 2016coj, 2018gv, 2018pv and 2019np we add radio data for\n17 other nearby SNe Ia, and model their non-detections. With the same model as\ndescribed, all 21 SNe Ia have mass-loss rates less than 4EE(-8) solar masses\nper year (for a wind speed of 100 km/s). We compare those limits with the\nexpected mass loss rates in different single-degenerate progenitor scenarios.\nWe also discuss how information on epsilon_e and epsilon_B can be obtained from\nlate observations of SNe Ia and the youngest SN Ia remnant detected in radio,\nG1.9+0.3, as well as stripped-envelope core-collapse SNe. We highlight SN\n2011dh, and argue for epsilon_e approximately equal to 0.1 and epsilon_B\napproximately equal to 0.0033. Finally, we discuss strategies to observe at\nradio frequencies to maximize the chance of detection, given the time since\nexplosion, the distance to the supernova and the telescope sensitivity.", "cat": "astro-ph.HE", "authors": ["Peter Lundqvist", "Esha Kundu", "Miguel A. Perez-Torres", "Stuart D. Ryder", "Claes-Ingvar Bjornsson", "Javier Moldon", "Megan K. Argo", "Robert J. Beswick", "Antxon Alberdi", "Erik C. Kool"]}, "209": {"id": "2401.03722v1", "title": "From Data to Insights: A Comprehensive Survey on Advanced Applications in Thyroid Cancer Research", "url": "http://arxiv.org/pdf/2401.03722v1", "date": "2024-01-08 08:10:37", "abs": "Thyroid cancer, the most prevalent endocrine cancer, has gained significant\nglobal attention due to its impact on public health. Extensive research efforts\nhave been dedicated to leveraging artificial intelligence (AI) methods for the\nearly detection of this disease, aiming to reduce its morbidity rates. However,\na comprehensive understanding of the structured organization of research\napplications in this particular field remains elusive. To address this\nknowledge gap, we conducted a systematic review and developed a comprehensive\ntaxonomy of machine learning-based applications in thyroid cancer pathogenesis,\ndiagnosis, and prognosis. Our primary objective was to facilitate the research\ncommunity's ability to stay abreast of technological advancements and\npotentially lead the emerging trends in this field. This survey presents a\ncoherent literature review framework for interpreting the advanced techniques\nused in thyroid cancer research. A total of 758 related studies were identified\nand scrutinized. To the best of our knowledge, this is the first review that\nprovides an in-depth analysis of the various aspects of AI applications\nemployed in the context of thyroid cancer. Furthermore, we highlight key\nchallenges encountered in this domain and propose future research opportunities\nfor those interested in studying the latest trends or exploring\nless-investigated aspects of thyroid cancer research. By presenting this\ncomprehensive review and taxonomy, we contribute to the existing knowledge in\nthe field, while providing valuable insights for researchers, clinicians, and\nstakeholders in advancing the understanding and management of this disease.", "cat": "cs.LG", "authors": ["Xinyu Zhang", "Vincent CS Lee", "Feng Liu"]}, "210": {"id": "1706.00636v1", "title": "WiFi based trajectory alignment, calibration and easy site survey using smart phones and foot-mounted IMUs", "url": "http://arxiv.org/pdf/1706.00636v1", "date": "2017-06-02 11:34:01", "abs": "Foot-mounted inertial positioning (FMIP) can face problems of inertial drifts\nand unknown initial states in real applications, which renders the estimated\ntrajectories inaccurate and not obtained in a well defined coordinate system\nfor matching trajectories of different users. In this paper, an approach\nadopting received signal strength (RSS) measurements for Wifi access points\n(APs) are proposed to align and calibrate the trajectories estimated from foot\nmounted inertial measurement units (IMUs). A crowd-sourced radio map (RM) can\nbe built subsequently and can be used for fingerprinting based Wifi indoor\npositioning (FWIP). The foundation of the proposed approach is graph based\nsimultaneously localization and mapping (SLAM). The nodes in the graph denote\nusers poses and the edges denote the pairwise constrains between the nodes. The\nconstrains are derived from: (1) inertial estimated trajectories; (2) vicinity\nin the RSS space. With these constrains, an error functions is defined. By\nminimizing the error function, the graph is optimized and the\naligned/calibrated trajectories along with the RM are acquired. The\nexperimental results have corroborated the effectiveness of the approach for\ntrajectory alignment, calibration as well as RM construction.", "cat": "stat.ML", "authors": ["Yang Gu", "Caifa Zhou", "Andreas Wieser", "Zhimin Zhou"]}, "211": {"id": "2106.05818v3", "title": "Unrepresentative Big Surveys Significantly Overestimate US Vaccine Uptake", "url": "http://arxiv.org/pdf/2106.05818v3", "date": "2021-11-01 17:58:06", "abs": "Surveys are a crucial tool for understanding public opinion and behavior, and\ntheir accuracy depends on maintaining statistical representativeness of their\ntarget populations by minimizing biases from all sources. Increasing data size\nshrinks confidence intervals but magnifies the impact of survey bias, an\ninstance of the Big Data Paradox (Meng 2018). Here we demonstrate this paradox\nin estimates of first-dose COVID-19 vaccine uptake in US adults:\nDelphi-Facebook (about 250,000 responses per week) and Census Household Pulse\n(about 75,000 per week). By May 2021, Delphi-Facebook overestimated uptake by\n17 percentage points and Census Household Pulse by 14, compared to a benchmark\nfrom the Centers for Disease Control and Prevention (CDC). Moreover, their\nlarge data sizes led to minuscule margins of error on the incorrect estimates.\nIn contrast, an Axios-Ipsos online panel with about 1,000 responses following\nsurvey research best practices (AAPOR) provided reliable estimates and\nuncertainty. We decompose observed error using a recent analytic framework to\nexplain the inaccuracy in the three surveys. We then analyze the implications\nfor vaccine hesitancy and willingness. We show how a survey of 250,000\nrespondents can produce an estimate of the population mean that is no more\naccurate than an estimate from a simple random sample of size 10. Our central\nmessage is that data quality matters far more than data quantity, and\ncompensating the former with the latter is a mathematically provable losing\nproposition.", "cat": "stat.AP", "authors": ["Valerie C. Bradley", "Shiro Kuriwaki", "Michael Isakov", "Dino Sejdinovic", "Xiao-Li Meng", "Seth Flaxman"]}, "212": {"id": "1205.5573v2", "title": "Using Multipoles of the Correlation Function to Measure H(z), D_A(z), and \u03b2(z) from Sloan Digital Sky Survey Luminous Red Galaxies", "url": "http://arxiv.org/pdf/1205.5573v2", "date": "2013-06-24 08:57:24", "abs": "Galaxy clustering data can be used to measure the cosmic expansion history\nH(z), the angular-diameter distance D_A(z), and the linear redshift-space\ndistortion parameter beta(z). Here we present a method for using effective\nmultipoles of the galaxy two-point correlation function (\\xi_0(s), \\xi_2(s),\n\\xi}_4(s), and \\xi_6(s), with s denoting the comoving separation) to measure\nH(z), D_A(z)$, and beta(z), and validate it using LasDamas mock galaxy\ncatalogs. Our definition of effective multipoles explicitly incorporates the\ndiscreteness of measurements, and treats the measured correlation function and\nits theoretical model on the same footing. We find that for the mock data,\n\\xi_0+\\xi_2+\\xi_4 captures nearly all the information, and gives significantly\nstronger constraints on H(z), D_A(z), and beta(z), compared to using only\n\\xi_0+\\xi_2.\n We apply our method to the sample of luminous red galaxies (LRGs) from the\nSloan Digital Sky Survey (SDSS) Data Release 7 (DR7) without assuming a dark\nenergy model or a flat Universe. We find that \\xi}_4(s) deviates on scales of\ns<60Mpc/h from the measurement from mock data (in contrast to \\xi_0(s),\n\\xi_2(s), and \\xi_6(s)), thus we only use \\xi_0+\\xi_2 for our fiducial\nconstraints. We obtain {H(0.35), D_A(0.35), Omega_mh^2, beta(z)} =\n{79.6_{-8.7}^{+8.3} km/s/Mpc, 1057_{-87}^{+88}Mpc, 0.103\\pm0.015, 0.44\\pm0.15}\nusing \\xi_0+\\xi_2. We find that H(0.35)r_s(z_d)/c and D_A(0.35)/r_s(z_d) (where\nr_s(z_d) is the sound horizon at the drag epoch) are more tightly constrained:\n{H(0.35)r_s(z_d)/c, D_A(0.35)/r_s(z_d)} = {0.0437_{-0.0043}^{+0.0041},\n6.48_{-0.43}^{+0.44}\\} using \\xi_0+\\xi_2.", "cat": "astro-ph.CO", "authors": ["Chia-Hsun Chuang", "Yun Wang"]}, "213": {"id": "2311.12351v2", "title": "Advancing Transformer Architecture in Long-Context Large Language Models: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2311.12351v2", "date": "2024-02-23 19:22:58", "abs": "Transformer-based Large Language Models (LLMs) have been applied in diverse\nareas such as knowledge bases, human interfaces, and dynamic agents, and\nmarking a stride towards achieving Artificial General Intelligence (AGI).\nHowever, current LLMs are predominantly pretrained on short text snippets,\nwhich compromises their effectiveness in processing the long-context prompts\nthat are frequently encountered in practical scenarios. This article offers a\ncomprehensive survey of the recent advancement in Transformer-based LLM\narchitectures aimed at enhancing the long-context capabilities of LLMs\nthroughout the entire model lifecycle, from pre-training through to inference.\nWe first delineate and analyze the problems of handling long-context input and\noutput with the current Transformer-based models. We then provide a taxonomy\nand the landscape of upgrades on Transformer architecture to solve these\nproblems. Afterwards, we provide an investigation on wildly used evaluation\nnecessities tailored for long-context LLMs, including datasets, metrics, and\nbaseline models, as well as optimization toolkits such as libraries,\nframeworks, and compilers to boost the efficacy of LLMs across different stages\nin runtime. Finally, we discuss the challenges and potential avenues for future\nresearch. A curated repository of relevant literature, continuously updated, is\navailable at https://github.com/Strivin0311/long-llms-learning.", "cat": "cs.CL", "authors": ["Yunpeng Huang", "Jingwei Xu", "Junyu Lai", "Zixu Jiang", "Taolue Chen", "Zenan Li", "Yuan Yao", "Xiaoxing Ma", "Lijuan Yang", "Hao Chen", "Shupeng Li", "Penghao Zhao"]}, "214": {"id": "1810.00305v1", "title": "Resource Management in Fog/Edge Computing: A Survey", "url": "http://arxiv.org/pdf/1810.00305v1", "date": "2018-09-30 03:14:59", "abs": "Contrary to using distant and centralized cloud data center resources,\nemploying decentralized resources at the edge of a network for processing data\ncloser to user devices, such as smartphones and tablets, is an upcoming\ncomputing paradigm, referred to as fog/edge computing. Fog/edge resources are\ntypically resource-constrained, heterogeneous, and dynamic compared to the\ncloud, thereby making resource management an important challenge that needs to\nbe addressed. This article reviews publications as early as 1991, with 85% of\nthe publications between 2013-2018, to identify and classify the architectures,\ninfrastructure, and underlying algorithms for managing resources in fog/edge\ncomputing.", "cat": "cs.DC", "authors": ["Cheol-Ho Hong", "Blesson Varghese"]}, "215": {"id": "1808.03010v2", "title": "The California-Kepler Survey. VI: Kepler Multis and Singles Have Similar Planet and Stellar Properties Indicating a Common Origin", "url": "http://arxiv.org/pdf/1808.03010v2", "date": "2018-10-09 22:54:54", "abs": "The California-Kepler Survey (CKS) catalog contains precise stellar and\nplanetary properties for the \\Kepler\\ planet candidates, including systems with\nmultiple detected transiting planets (\"multis\") and systems with just one\ndetected transiting planet (\"singles,\" although additional planets could\nexist). We compared the stellar and planetary properties of the multis and\nsingles in a homogenous subset of the full CKS-Gaia catalog. We found that\nsub-Neptune sized singles and multis do not differ in their stellar properties\nor planet radii. In particular: (1.) The distributions of stellar properties\n$M_\\star$, [Fe/H], and $v\\mathrm{sin}i$ for the Kepler sub Neptune-sized\nsingles and multis are statistically indistinguishable. (2.) The radius\ndistributions of the sub-Neptune sized singles and multis with $P > 3$ days are\nindistinguishable, and both have a valley at $\\sim1.8~R_\\oplus$. However, there\nare significantly more detected short-period ($P < 3$ days), sub-Neptune sized\nsingles than multis. The similarity of the host star properties, planet radii,\nand radius valley for singles and multis suggests a common origin. The similar\nradius valley, which is likely sculpted by photo-evaporation from the host star\nwithin the first 100 Myr, suggests that planets in both singles and multis\nspend much of the first 100 Myr near their present, close-in locations. One\nexplanation that is consistent with the similar fundamental properties of\nsingles and multis is that many of the singles are members of multi-planet\nsystems that underwent planet-planet scattering.", "cat": "astro-ph.EP", "authors": ["Lauren M. Weiss", "Howard T. Isaacson", "Geoffrey W. Marcy", "Andrew W. Howard", "Erik A. Petigura", "Benjamin J. Fulton", "Joshua N. Winn", "Lea Hirsch", "Evan Sinukoff", "Jason F. Rowe"]}, "216": {"id": "2401.14464v1", "title": "Spectroscopic confirmation of high-amplitude eruptive YSOs and dipping giants from the VVV survey", "url": "http://arxiv.org/pdf/2401.14464v1", "date": "2024-01-25 19:01:19", "abs": "During the pre-main-sequence (pre-MS) evolution stage of a star, significant\namounts of stellar mass are accreted during episodic accretion events, such as\nmulti-decade FUor-type outbursts. Here, we present a near-infrared\nspectroscopic follow-up study of 33 high-amplitude (most with $\\Delta K_s$ > 4\nmag) variable sources discovered by the Vista Variables in the Via Lactea (VVV)\nsurvey. Based on the spectral features, 25 sources are classified as eruptive\nyoung stellar objects (YSOs), including 15 newly identified FUors, six with\nlong-lasting but EXor-like bursts of magnetospheric accretion and four\ndisplaying outflow-dominated spectra. By examining the photometric behaviours\nof eruptive YSOs, we found most FUor-type outbursts have higher amplitudes\n($\\Delta K_s$ and $\\Delta W2$), faster eruptive timescales and bluer infrared\ncolours than the other outburst types. In addition, we identified seven\npost-main sequence variables apparently associated with deep dipping events and\nan eruptive star with deep AlO absorption bands resembling those seen in the\nV838 Mon stellar merger.", "cat": "astro-ph.SR", "authors": ["Zhen Guo", "P. W. Lucas", "R. Kurtev", "J. Borissova", "C. Contreras Pe\u00f1a", "S. N. Yurchenko", "L. C. Smith", "D. Minniti", "R. K. Saito", "A. Bayo", "M. Catelan", "J. Alonso-Garc\u00eda", "A. Caratti o Garatti", "C. Morris", "D. Froebrich", "J. Tennyson", "K. Mauc\u00f3", "A. Aguayo", "N. Miller", "H. D. S. Muthu"]}, "217": {"id": "0909.0014v2", "title": "Highly Variable Objects in the Palomar-QUEST Survey: A Blazar Search using Optical Variability", "url": "http://arxiv.org/pdf/0909.0014v2", "date": "2009-09-02 10:39:03", "abs": "We identify 3,113 highly variable objects in 7,200 square degrees of the\nPalomar-QUEST Survey, which each varied by more than 0.4 magnitudes\nsimultaneously in two broadband optical filters on timescales from hours to\nroughly 3.5 years. The primary goal of the selection is to find blazars by\ntheir well-known violent optical variability. Because most known blazars have\nbeen found in radio and/or X-ray wavelengths, a sample discovered through\noptical variability may have very different selection effects, elucidating the\nrange of behavior possible in these systems. A set of blazars selected in this\nunusual manner will improve our understanding of the physics behind this\nextremely variable and diverse class of AGN. The object positions, variability\nstatistics, and color information are available using the Palomar-QUEST CasJobs\nserver. The time domain is just beginning to be explored over large sky areas;\nwe do not know exactly what a violently variable sample will hold. About 20% of\nthe sample has been classified in the literature; over 70% of those objects are\nknown or likely AGN. The remainder largely consists of a variety of variable\nstars, including a number of RR Lyrae and cataclysmic variables.", "cat": "astro-ph.CO", "authors": ["Anne Bauer", "Charles Baltay", "Paolo Coppi", "Ciro Donalek", "Andrew Drake", "S. G. Djorgovski", "Nancy Ellman", "Eilat Glikman", "Matthew Graham", "Jonathan Jerke", "Ashish Mahabal", "David Rabinowitz", "Richard Scalzo", "Roy Williams"]}, "218": {"id": "1705.09510v1", "title": "A new method for finding and characterizing galaxy groups via low-frequency radio surveys", "url": "http://arxiv.org/pdf/1705.09510v1", "date": "2017-05-26 10:06:46", "abs": "We describe a new method for identifying and characterizing the thermodynamic\nstate of large samples of evolved galaxy groups at high redshifts using\nhigh-resolution, low-frequency radio surveys, such as those that will be\ncarried out with LOFAR and the Square Kilometre Array (SKA). We identify a\nsub-population of morphologically regular powerful (FRII) radio galaxies and\ndemonstrate that, for this sub-population, the internal pressure of the radio\nlobes is a reliable tracer of the external intragroup/intracluster medium (ICM)\npressure, and that the assumption of a universal pressure profile for relaxed\ngroups enables the total mass and X-ray luminosity to be estimated. Using a\nsample of well-studied FRII radio galaxies, we demonstrate that our method\nenables the estimation of group/cluster X-ray luminosities over three orders of\nmagnitude in luminosity to within a factor of ~2 from low-frequency radio\nproperties alone. Our method could provide a powerful new tool for building\nsamples of thousands of evolved galaxy groups at z>1 and characterizing their\nICM.", "cat": "astro-ph.GA", "authors": ["J. H. Croston", "J. Ineson", "M. J. Hardcastle", "B. Mingo"]}, "219": {"id": "1109.1886v1", "title": "The Australia Telescope 20GHz Survey: Hardware, Observing Strategy, and Scanning Survey Catalog", "url": "http://arxiv.org/pdf/1109.1886v1", "date": "2011-09-09 03:38:26", "abs": "The Australia Telescope 20GHz (AT20G) survey is a large area (2{\\pi} sr),\nsensitive (40mJy), high frequency (20GHz) survey of the southern sky. The\nsurvey was conducted in two parts: an initial fast scanning survey, and a\nseries of more accurate follow-up observations. The follow-up survey catalog\nhas been presented by Murphy et al. 2010. In this paper we discuss the hardware\nsetup and scanning survey strategy as well as the production of the scanning\nsurvey catalog.", "cat": "astro-ph.IM", "authors": ["Paul J. Hancock", "Paul Roberts", "Michael J. Kesteven", "Ronald D. Ekers", "Elaine M. Sadler", "Tara Murphy", "Marcella Massardi", "Roberto Ricci", "Mark Calabretta", "Gianfranco de Zotti", "Philip G. Edwards", "Jennifer A. Ekers", "Carole A. Jackson", "Mark Leach", "Chris Phillips", "Robert J. Sault", "Lister Staveley-Smith", "Ravi Subrahmanyan", "Mark A. Walker", "Warwick E. Wilson"]}, "220": {"id": "2009.10521v1", "title": "A survey on Kornia: an Open Source Differentiable Computer Vision Library for PyTorch", "url": "http://arxiv.org/pdf/2009.10521v1", "date": "2020-09-21 08:48:28", "abs": "This work presents Kornia, an open source computer vision library built upon\na set of differentiable routines and modules that aims to solve generic\ncomputer vision problems. The package uses PyTorch as its main backend, not\nonly for efficiency but also to take advantage of the reverse\nauto-differentiation engine to define and compute the gradient of complex\nfunctions. Inspired by OpenCV, Kornia is composed of a set of modules\ncontaining operators that can be integrated into neural networks to train\nmodels to perform a wide range of operations including image\ntransformations,camera calibration, epipolar geometry, and low level image\nprocessing techniques, such as filtering and edge detection that operate\ndirectly on high dimensional tensor representations on graphical processing\nunits, generating faster systems. Examples of classical vision problems\nimplemented using our framework are provided including a benchmark comparing to\nexisting vision libraries.", "cat": "cs.CV", "authors": ["E. Riba", "D. Mishkin", "J. Shi", "D. Ponsa", "F. Moreno-Noguer", "G. Bradski"]}, "221": {"id": "1108.6010v1", "title": "A State-of-the-art Survey on IDS for Mobile Ad-Hoc Networks and Wireless Mesh Networks", "url": "http://arxiv.org/pdf/1108.6010v1", "date": "2011-08-30 16:50:55", "abs": "An Intrusion Detection System (IDS) detects malicious and selfish nodes in a\nnetwork. Ad hoc networks are often secured by using either intrusion detection\nor by secure routing. Designing efficient IDS for wireless ad-hoc networks that\nwould not affect the performance of the network significantly is indeed a\nchallenging task. Arguably, the most common thing in a review paper in the\ndomain of wireless networks is to compare the performances of different\nsolutions using simulation results. However, variance in multiple configuration\naspects including that due to different underlying routing protocols, makes the\ntask of simulation based comparative evaluation of IDS solutions somewhat\nunrealistic. In stead, the authors have followed an analytic approach to\nidentify the gaps in the existing IDS solutions for MANETs and wireless mesh\nnetworks. The paper aims to ease the job of a new researcher by exposing him to\nthe state of the art research issues on IDS. Nearly 80% of the works cited in\nthis paper are published with in last 3 to 4 years.", "cat": "cs.CR", "authors": ["Novarun Deb", "Manali Chakraborty", "Nabendu Chaki"]}, "222": {"id": "1103.4651v2", "title": "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", "url": "http://arxiv.org/pdf/1103.4651v2", "date": "2011-06-01 15:48:10", "abs": "We present a re-analysis of the Geneva-Copenhagen survey, which benefits from\nthe infrared flux method to improve the accuracy of the derived stellar\neffective temperatures and uses the latter to build a consistent and improved\nmetallicity scale. Metallicities are calibrated on high-resolution spectroscopy\nand checked against four open clusters and a moving group, showing excellent\nconsistency. The new temperature and metallicity scales provide a better match\nto theoretical isochrones, which are used for a Bayesian analysis of stellar\nages. With respect to previous analyses, our stars are on average 100 K hotter\nand 0.1 dex more metal rich, which shift the peak of the metallicity\ndistribution function around the solar value. From Stromgren photometry we are\nable to derive for the first time a proxy for alpha elements, which enables us\nto perform a tentative dissection of the chemical thin and thick disc. We find\nevidence for the latter being composed of an old, mildly but systematically\nalpha-enhanced population that extends to super solar metallicities, in\nagreement with spectroscopic studies. Our revision offers the largest existing\nkinematically unbiased sample of the solar neighbourhood that contains full\ninformation on kinematics, metallicities, and ages and thus provides better\nconstraints on the physical processes relevant in the build-up of the Milky Way\ndisc, enabling a better understanding of the Sun in a Galactic context.", "cat": "astro-ph.GA", "authors": ["Luca Casagrande", "Ralph Schoenrich", "Martin Asplund", "Santi Cassisi", "Ivan Ramirez", "Jorge Melendez", "Thomas Bensby", "Sofia Feltzing"]}, "223": {"id": "0806.4778v2", "title": "The XMM-Newton survey of the ELAIS-S1 field II: optical identifications and multiwavelength catalogue of X-ray sources", "url": "http://arxiv.org/pdf/0806.4778v2", "date": "2008-07-03 21:15:55", "abs": "We present optical identifications and a multi-band catalogue of a sample of\n478 X-ray sources in the XMM and Chandra surveys of the central 0.6 deg^2 of\nthe ELAIS-S1 field. The optical/infrared counterpart of each X-ray source was\nidentified using R and IRAC 3.6 um bands. This method was complemented by the\nprecise positions obtained through Chandra observations. Approximately 94% of\nthe counterparts are detected in the R band, while the remaining are blank\nfields in the optical down to R~24.5, but have a near-infrared counterpart\ndetected by IRAC within 6 arcsec from the XMM centroid. The multi-band\ncatalogue contains photometry in ten photometric bands (B to the MIPS 24 um).\nWe determined redshift and classification for 237 sources (~50% of the sample)\nbrighter than R=24. We classified 47% of the sources with spectroscopic\nredshift as broad-line active galactic nuclei (BL AGNs) with z=0.1-3.5, while\nsources without broad-lines are about 46% of the spectroscopic sample and are\nfound up to z=2.6. We identified 11 type 2 QSOs among the sources with X/O>8,\nwith z=0.9-2.6, high 2-10 keV luminosity (log(L2-10keV)>=43.8 erg/s) and hard\nX-ray colors suggesting large absorbing columns at the rest frame (logN_H up to\n23.6 cm^-2). BL AGNs show on average blue optical-to-near-infrared colors,\nsofter X-ray colors and X-ray-to-optical colors typical of optically selected\nAGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray\nflux ratio and span a wider range of X-ray-to-optical colors. On average the\nSEDs of high-luminosity BL AGNs resemble the power-law typical of unobscured\nAGNs. The SEDs of NOT BL AGNs are dominated by the galaxy emission in the\noptical/near-infrared, and show a rise in the mid-infrared which suggests the\npresence of an obscured active nucleus.", "cat": "astro-ph", "authors": ["C. Feruglio", "F. Fiore", "F. La Franca", "N. Sacchi", "S. Puccetti", "A. Comastri", "S. Berta", "M. Brusa", "A. Franceschini", "C. Gruppioni", "S. Mathur", "I. Matute", "M. Mignoli", "F. Pozzi", "C. Vignali", "G. Zamorani"]}, "224": {"id": "2102.09519v1", "title": "WALOP-South: A wide-field one-shot linear optical polarimeter for PASIPHAE survey", "url": "http://arxiv.org/pdf/2102.09519v1", "date": "2021-02-18 18:02:59", "abs": "WALOP (Wide-Area Linear Optical Polarimeter)-South, to be mounted on the 1m\nSAAO telescope in South Africa, is first of the two WALOP instruments currently\nunder development for carrying out the PASIPHAE survey. Scheduled for\ncommissioning in the year 2021, the WALOP instruments will be used to measure\nthe linear polarization of around $10^{6}$ stars in the SDSS-r broadband with\n$0.1~\\%$ polarimetric accuracy, covering 4000 square degrees in the Galactic\npolar regions. The combined capabilities of one-shot linear polarimetry, high\npolarimetric accuracy ($< 0.1~\\%$) and polarimetric sensitivity ($< 0.05~\\%$),\nand a large field of view (FOV) of $35\\times35~arcminutes$ make WALOP-South a\nunique astronomical instrument. In a single exposure, it is designed to measure\nthe Stokes parameters $I$, $q$ and $u$ in the SDSS-r broadband and narrowband\nfilters between $500-700~nm$. During each measurement, four images of the full\nfield corresponding to the polarization angles of $0^{\\circ}$, $45^{\\circ}$,\n$90^{\\circ}$ and $135^{\\circ}$ will be imaged on four detectors and carrying\nout differential photometry on these images will yield the Stokes parameters.\nMajor challenges in designing WALOP-South instrument include- (a) in the\noptical design, correcting for the spectral dispersion introduced by large\nsplit angle Wollaston Prisms used as polarization analyzers as well as\naberrations from the wide field, and (b) making an optomechanical design\nadherent to the tolerances required to obtain good imaging and polarimetric\nperformance under all temperature conditions as well as telescope pointing\npositions. We present the optical and optomechanical design for WALOP-South\nwhich overcomes these challenges.", "cat": "astro-ph.IM", "authors": ["Siddharth Maharana", "John A. Kypriotakis", "A. N. Ramaprakash", "Pravin Khodade", "Chaitanya Rajarshi", "Bhushan S. Joshi", "Pravin Chordia", "Ramya M. Anche", "Shrish Mishra", "Dmitry Blinov", "Hans Kristian Eriksen", "Tuhin Ghosh", "Eirik Gjerl\u00f8w", "Nikolaos Mandarakas", "Georgia V. Panopoulou", "Vasiliki Pavlidou", "Timothy J. Pearson", "Vincent Pelgrims", "Stephen B. Potter", "Anthony C. S. Readhead", "Raphail Skalidis", "Konstantinos Tassis", "Ingunn K. Wehus"]}, "225": {"id": "1008.3149v3", "title": "The RMS Survey: Distribution and properties of a sample of massive young stars", "url": "http://arxiv.org/pdf/1008.3149v3", "date": "2010-09-10 04:27:50", "abs": "The Red MSX Source (RMS) survey has identified a large sample of massive\nyoung stellar objects (MYSOs) and ultra compact (UC) HII regions from a sample\nof ~2000 MSX and 2MASS colour selected sources. Using a recent catalogue of\nmolecular clouds derived from the Boston University-Five College Radio\nAstronomy Observatory Galactic Ring Survey (GRS), and by applying a Galactic\nscaleheight cut off of 120 pc, we solve the distance ambiguity for RMS sources\nlocated within 18\\degr < |l| > 54\\degr. These two steps yield kinematic\ndistances to 291 sources out of a possible 326 located within the GRS longitude\nrange. Combining distances and integrated fluxes derived from spectral energy\ndistributions, we estimate luminosities to these sources and find that > 90%\nare indicative of the presence of a massive star. We find the completeness\nlimit of our sample is ~10^4 Lsun, which corresponds to a zero age main\nsequence (ZAMS) star with a mass of ~12 Msun. Selecting only these sources, we\nconstruct a complete sample of 196 sources. Comparing the properties of the\nsample of young massive stars with the general population, we find the\nRMS-clouds are generally larger, more massive, and more turbulent. We examine\nthe distribution of this sub-sample with respect to the location of the spiral\narms and the Galactic bar and find them to be spatially correlated. We identify\nthree significant peaks in the source surface density at Galactocentric radii\nof approximately 4, 6 and 8 kpc, which correspond to the proposed positions of\nthe Scutum, Sagittarius and Perseus spiral arms, respectively. Fitting a scale\nheight to the data we obtain an average value of ~29+-0.5 pc, which agrees well\nwith other reported values in the literature, however, we note a dependence of\nthe scale height on galactocentric radius with it increases from 30 pc to 45 pc\nbetween 2.5 and 8.5 kpc.", "cat": "astro-ph.GA", "authors": ["J. S. Urquhart", "T. J. T. Moore", "M. G. Hoare", "S. L. Lumsden", "R. D. Oudmaijer", "J. M. Rathborne", "J. C. Mottram", "B. Davies", "J. J. Stead"]}, "226": {"id": "2311.11383v3", "title": "A Survey of Emerging Applications of Diffusion Probabilistic Models in MRI", "url": "http://arxiv.org/pdf/2311.11383v3", "date": "2024-05-07 20:02:43", "abs": "Diffusion probabilistic models (DPMs) which employ explicit likelihood\ncharacterization and a gradual sampling process to synthesize data, have gained\nincreasing research interest. Despite their huge computational burdens due to\nthe large number of steps involved during sampling, DPMs are widely appreciated\nin various medical imaging tasks for their high-quality and diversity of\ngeneration. Magnetic resonance imaging (MRI) is an important medical imaging\nmodality with excellent soft tissue contrast and superb spatial resolution,\nwhich possesses unique opportunities for DPMs. Although there is a recent surge\nof studies exploring DPMs in MRI, a survey paper of DPMs specifically designed\nfor MRI applications is still lacking. This review article aims to help\nresearchers in the MRI community to grasp the advances of DPMs in different\napplications. We first introduce the theory of two dominant kinds of DPMs,\ncategorized according to whether the diffusion time step is discrete or\ncontinuous, and then provide a comprehensive review of emerging DPMs in MRI,\nincluding reconstruction, image generation, image translation, segmentation,\nanomaly detection, and further research topics. Finally, we discuss the general\nlimitations as well as limitations specific to the MRI tasks of DPMs and point\nout potential areas that are worth further exploration.", "cat": "cs.CV", "authors": ["Yuheng Fan", "Hanxi Liao", "Shiqi Huang", "Yimin Luo", "Huazhu Fu", "Haikun Qi"]}, "227": {"id": "2309.14637v1", "title": "SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines", "url": "http://arxiv.org/pdf/2309.14637v1", "date": "2023-09-26 03:34:35", "abs": "We investigate the physical structure and conditions of photodissociation\nregions (PDRs) and molecular gas within the Pillars of Creation in the Eagle\nNebula using SOFIA FEEDBACK observations of the [C II] 158 micron line. These\nobservations are velocity resolved to 0.5 km s$^{-1}$ and are analyzed\nalongside a collection of complimentary data with similar spatial and spectral\nresolution: the [O I] 63 micron line, also observed with SOFIA, and rotational\nlines of CO, HCN, HCO$^{+}$, CS, and N$_2$H$^{+}$. Using the superb spectral\nresolution of SOFIA, APEX, CARMA, and BIMA, we reveal the relationships between\nthe warm PDR and cool molecular gas layers in context of the Pillars' kinematic\nstructure. We assemble a geometric picture of the Pillars and their\nsurroundings informed by illumination patterns and kinematic relationships and\nderive physical conditions in the PDRs associated with the Pillars. We estimate\nan average molecular gas density $n_{{\\rm H}_2} \\sim 1.3 \\times 10^5$ cm$^{-3}$\nand an average atomic gas density $n_{\\rm H} \\sim 1.8 \\times 10^4$ cm$^{-3}$\nand infer that the ionized, atomic, and molecular phases are in pressure\nequilibrium if the atomic gas is magnetically supported. We find pillar masses\nof 103, 78, 103, and 18 solar masses for P1a, P1b, P2, and P3 respectively, and\nevaporation times of $\\sim$1-2 Myr. The dense clumps at the tops of the pillars\nare currently supported by the magnetic field. Our analysis suggests that\nambipolar diffusion is rapid and these clumps are likely to collapse within\ntheir photoevaporation timescales.", "cat": "astro-ph.GA", "authors": ["Ramsey L. Karim", "Marc W. Pound", "Alexander G. G. M. Tielens", "Maitraiyee Tiwari", "Lars Bonne", "Mark G. Wolfire", "Nicola Schneider", "\u00dcmit Kavak", "Lee G. Mundy", "Robert Simon", "Rolf G\u00fcsten", "J\u00fcrgen Stutzki", "Friedrich Wyrowski", "Netty Honingh"]}, "228": {"id": "1606.03114v2", "title": "The Alcock Paczynski test with Baryon Acoustic Oscillations: systematic effects for future surveys", "url": "http://arxiv.org/pdf/1606.03114v2", "date": "2017-02-24 12:45:19", "abs": "We investigate the Alcock Paczynski (AP) test applied to the Baryon Acoustic\nOscillation (BAO) feature in the galaxy correlation function. By using a\ngeneral formalism that includes relativistic effects, we quantify the\nimportance of the linear redshift space distortions and gravitational lensing\ncorrections to the galaxy number density fluctuation. We show that redshift\nspace distortions significantly affect the shape of the correlation function,\nboth in radial and transverse directions, causing different values of galaxy\nbias to induce offsets up to 1% in the AP test. On the other hand, we find that\nthe lensing correction around the BAO scale modifies the amplitude but not the\nshape of the correlation function and therefore does not introduce any\nsystematic effect. Furthermore, we investigate in details how the AP test is\nsensitive to redshift binning: a window function in transverse direction\nsuppresses correlations and shifts the peak position toward smaller angular\nscales. We determine the correction that should be applied in order to account\nfor this effect, when performing the test with data from three future planned\ngalaxy redshift surveys: Euclid, the Dark Energy Spectroscopic Instrument\n(DESI) and the Square Kilometer Array (SKA).", "cat": "astro-ph.CO", "authors": ["Francesca Lepori", "Enea Di Dio", "Matteo Viel", "Carlo Baccigalupi", "Ruth Durrer"]}, "229": {"id": "1706.02401v1", "title": "A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M-dwarfs", "url": "http://arxiv.org/pdf/1706.02401v1", "date": "2017-06-07 22:30:58", "abs": "We report the discovery of KELT J041621-620046, a moderately bright\n(J$\\sim$10.2) M dwarf eclipsing binary system at a distance of 39$\\pm$3 pc.\nKELT J041621-620046 was first identified as an eclipsing binary using\nobservations from the Kilodegree Extremely Little Telescope (KELT) survey. The\nsystem has a short orbital period of $\\sim$1.11 days and consists of components\nwith M$_1$ = $0.447^{-0.047}_{+0.052}\\,M_\\odot$ and M$_2$ =\n$0.399^{-0.042}_{+0.046}\\,M_\\odot$ in nearly circular orbits. The radii of the\ntwo stars are R$_1$ = $0.540^{-0.032}_{+0.034}\\,R_\\odot$ and R$_2$ =\n$0.453\\pm0.017\\,R_\\odot$. Full system and orbital properties were determined\n(to $\\sim$10% error) by conducting an EBOP global modeling of the high\nprecision photometric and spectroscopic observations obtained by the KELT\nFollow-up Network. Each star is larger by 17-28% and cooler by 4-10% than\npredicted by standard (non-magnetic) stellar models. Strong H$\\alpha$ emission\nindicates chromospheric activity in both stars. The observed radii and\ntemperature discrepancies for both components are more consistent with those\npredicted by empirical relations that account for convective suppression due to\nmagnetic activity.", "cat": "astro-ph.SR", "authors": ["Jack B. Lubin", "Joseph E. Rodriguez", "George Zhou", "Kyle E. Conroy", "Keivan G. Stassun", "Karen Collins", "Daniel J. Stevens", "Jonathan Labadie-Bartz", "Christopher Stockdale", "Gordon Myers", "Knicole D. Col\u00f3n", "Joao Bento", "Petri Kehusmaa", "Romina Petrucci", "Emiliano Jofr\u00e9", "Samuel N. Quinn", "Michael B. Lund", "Rudolf B. Kuhn", "Robert J. Siverd", "Thomas G. Beatty", "Caisey Harlingten", "Joshua Pepper", "B. Scott Gaudi", "David James", "Eric L. N. Jensen", "Daniel Reichart", "Lucyna Kedziora-Chudczer", "Jeremy Bailey", "Graeme Melville"]}, "230": {"id": "2303.09136v1", "title": "A Short Survey of Viewing Large Language Models in Legal Aspect", "url": "http://arxiv.org/pdf/2303.09136v1", "date": "2023-03-16 08:01:22", "abs": "Large language models (LLMs) have transformed many fields, including natural\nlanguage processing, computer vision, and reinforcement learning. These models\nhave also made a significant impact in the field of law, where they are being\nincreasingly utilized to automate various legal tasks, such as legal judgement\nprediction, legal document analysis, and legal document writing. However, the\nintegration of LLMs into the legal field has also raised several legal\nproblems, including privacy concerns, bias, and explainability. In this survey,\nwe explore the integration of LLMs into the field of law. We discuss the\nvarious applications of LLMs in legal tasks, examine the legal challenges that\narise from their use, and explore the data resources that can be used to\nspecialize LLMs in the legal domain. Finally, we discuss several promising\ndirections and conclude this paper. By doing so, we hope to provide an overview\nof the current state of LLMs in law and highlight the potential benefits and\nchallenges of their integration.", "cat": "cs.CL", "authors": ["Zhongxiang Sun"]}, "231": {"id": "2312.04997v1", "title": "Beyond Transduction: A Survey on Inductive, Few Shot, and Zero Shot Link Prediction in Knowledge Graphs", "url": "http://arxiv.org/pdf/2312.04997v1", "date": "2023-12-08 12:13:40", "abs": "Knowledge graphs (KGs) comprise entities interconnected by relations of\ndifferent semantic meanings. KGs are being used in a wide range of\napplications. However, they inherently suffer from incompleteness, i.e.\nentities or facts about entities are missing. Consequently, a larger body of\nworks focuses on the completion of missing information in KGs, which is\ncommonly referred to as link prediction (LP). This task has traditionally and\nextensively been studied in the transductive setting, where all entities and\nrelations in the testing set are observed during training. Recently, several\nworks have tackled the LP task under more challenging settings, where entities\nand relations in the test set may be unobserved during training, or appear in\nonly a few facts. These works are known as inductive, few-shot, and zero-shot\nlink prediction. In this work, we conduct a systematic review of existing works\nin this area. A thorough analysis leads us to point out the undesirable\nexistence of diverging terminologies and task definitions for the\naforementioned settings, which further limits the possibility of comparison\nbetween recent works. We consequently aim at dissecting each setting\nthoroughly, attempting to reveal its intrinsic characteristics. A unifying\nnomenclature is ultimately proposed to refer to each of them in a simple and\nconsistent manner.", "cat": "cs.AI", "authors": ["Nicolas Hubert", "Pierre Monnin", "Heiko Paulheim"]}, "232": {"id": "2102.01924v1", "title": "Eclipsing Binary Populations across the Northern Galactic Plane from the KISOGP survey", "url": "http://arxiv.org/pdf/2102.01924v1", "date": "2021-02-03 07:54:59", "abs": "We present a catalog of eclipsing binaries in the northern Galactic Plane\nfrom the Kiso Wide-Field Camera Intensive Survey of the Galactic Plane\n(KISOGP). We visually identified 7055 eclipsing binaries spread across\n$\\sim$330 square degrees, including 4197 W Ursa Majoris/EW-, 1458 $\\beta$\nLyrae/EB-, and 1400 Algol/EA-type eclipsing binaries. For all systems, $I$-band\nlight curves were used to obtain accurate system parameters. We derived the\ndistances and extinction values for the EW-type objects from their\nperiod--luminosity relation. We also obtained the structure of the thin disk\nfrom the distribution of our sample of eclipsing binary systems, combined with\nthose of high-mass star-forming regions and Cepheid tracers. We found that the\nthin disk is inhomogeneous in number density as a function of Galactic\nlongitude. Using this new set of distance tracers, we constrain the detailed\nstructure of the thin disk. Finally, we report a global parallax zero-point\noffset of $ \\Delta \\pi=-42.1\\pm1.9\\mbox{(stat.)}\\pm12.9\\mbox{(syst.)}$ $\\mu$as\nbetween our carefully calibrated EW-type eclipsing binary positions and those\nprovided by Gaia Early Data Release 3. Implementation of the officially\nrecommended parallax zero-point correction results in a significantly reduced\noffset. Additionally, we provide a photometric characterization of our EW-type\neclipsing binaries that can be applied to further analyses.", "cat": "astro-ph.SR", "authors": ["Fangzhou Ren", "Richard de Grijs", "Huawei Zhang", "Licai Deng", "Xiaodian Chen", "Noriyuki Matsunaga", "Chao Liu", "Weijia Sun", "Hiroyuki Maehara", "Nobuharu Ukita", "Naoto Kobayashi"]}, "233": {"id": "2407.20181v1", "title": "Blockchain for Large Language Model Security and Safety: A Holistic Survey", "url": "http://arxiv.org/pdf/2407.20181v1", "date": "2024-07-26 15:24:01", "abs": "With the advent of accessible interfaces for interacting with large language\nmodels, there has been an associated explosion in both their commercial and\nacademic interest. Consequently, there has also been an sudden burst of novel\nattacks associated with large language models, jeopardizing user data on a\nmassive scale. Situated at a comparable crossroads in its development, and\nequally prolific to LLMs in its rampant growth, blockchain has emerged in\nrecent years as a disruptive technology with the potential to redefine how we\napproach data handling. In particular, and due to its strong guarantees about\ndata immutability and irrefutability as well as inherent data provenance\nassurances, blockchain has attracted significant attention as a means to better\ndefend against the array of attacks affecting LLMs and further improve the\nquality of their responses. In this survey, we holistically evaluate current\nresearch on how blockchains are being used to help protect against LLM\nvulnerabilities, as well as analyze how they may further be used in novel\napplications. To better serve these ends, we introduce a taxonomy of blockchain\nfor large language models (BC4LLM) and also develop various definitions to\nprecisely capture the nature of different bodies of research in these areas.\nMoreover, throughout the paper, we present frameworks to contextualize broader\nresearch efforts, and in order to motivate the field further, we identify\nfuture research goals as well as challenges present in the blockchain for large\nlanguage model (BC4LLM) space.", "cat": "cs.CR", "authors": ["Caleb Geren", "Amanda Board", "Gaby G. Dagher", "Tim Andersen", "Jun Zhuang"]}, "234": {"id": "1805.11499v1", "title": "The Arecibo Legacy Fast ALFA Survey: The ALFALFA Extragalactic HI Source Catalog", "url": "http://arxiv.org/pdf/1805.11499v1", "date": "2018-05-29 14:28:46", "abs": "We present the catalog of ~31500 extragalactic HI line sources detected by\nthe completed ALFALFA survey out to z < 0.06 including both high\nsignal-to-noise ratio (> 6.5) detections and ones of lower quality which\ncoincide in both position and recessional velocity with galaxies of known\nredshift. We review the observing technique, data reduction pipeline, and\ncatalog construction process, focusing on details of particular relevance to\nunderstanding the catalog's compiled parameters. We further describe and make\navailable the digital HI line spectra associated with the catalogued sources.\nIn addition to the extragalactic HI line detections, we report nine confirmed\nOH megamasers and ten OH megamaser candidates at 0.16 < z < 0.22 whose OH line\nsignals are redshifted into the ALFALFA frequency band. Because of complexities\nin data collection and processing associated with the use of a feed-horn array\non a complex single-dish antenna in the terrestrial radio frequency\ninterference environment, we also present a list of suggestions and caveats for\nconsideration by users of the ALFALFA extragalactic catalog for future\nscientific investigations.", "cat": "astro-ph.GA", "authors": ["Martha P. Haynes", "Riccardo Giovanelli", "Brian R. Kent", "Elizabeth A. K. Adams", "Thomas J. Balonek", "David W. Craig", "Derek Fertig", "Rose Finn", "Carlo Giovanardi", "Gregory Hallenbeck", "Kelley M. Hess", "G. Lyle Hoffman", "Shan Huang", "Michael G. Jones", "Rebecca A. Koopmann", "David A. Kornreich", "Lukas Leisman", "Jeffrey R. Miller", "Crystal Moorman", "Jessica O'Connor", "Aileen O'Donoghue", "Emmanouil Papastergis", "Parker Troischt", "David Stark", "Li Xiao"]}, "235": {"id": "2311.05632v1", "title": "The Impact of Performance Expectancy, Workload, Risk, and Satisfaction on Trust in ChatGPT: Cross-sectional Survey Analysis", "url": "http://arxiv.org/pdf/2311.05632v1", "date": "2023-10-20 16:06:11", "abs": "This study investigated how perceived workload, satisfaction, performance\nexpectancy, and risk-benefit perception influenced users' trust in Chat\nGenerative Pre-Trained Transformer (ChatGPT). We aimed to understand the\nnuances of user engagement and provide insights to improve future design and\nadoption strategies for similar technologies. A semi-structured, web-based\nsurvey was conducted among adults in the United States who actively use ChatGPT\nat least once a month. The survey was conducted from 22nd February 2023 through\n24th March 2023. We used structural equation modeling to understand the\nrelationships among the constructs of perceived workload, satisfaction,\nperformance expectancy, risk-benefit, and trust. The analysis of 607 survey\nresponses revealed a significant negative relationship between perceived\nworkload and user satisfaction, a negative but insignificant relationship\nbetween perceived workload and trust, and a positive relationship between user\nsatisfaction and trust. Trust was also found to increase with performance\nexpectancy. In contrast, the relationship between the benefit-to-risk ratio of\nusing ChatGPT and trust was insignificant. The findings underscore the\nimportance of ensuring user-friendly design and functionality in AI-based\napplications to reduce workload and enhance user satisfaction, thereby\nincreasing user trust. Future research should further explore the relationship\nbetween the benefit-to-risk ratio and trust in the context of AI chatbots.", "cat": "cs.CY", "authors": ["Hamid Shamszare", "Avishek Choudhury"]}, "236": {"id": "2405.10047v2", "title": "Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey: II. the bolometric and photospheric calibration", "url": "http://arxiv.org/pdf/2405.10047v2", "date": "2024-05-22 13:38:00", "abs": "The dependence of stellar magnetic activity on stellar parameters would be\ninspired by the chromospheric activity studies based on the large-scale\nspectroscopic surveys. The Ca II H and K lines are employed to construct\nindicators for assessing and studying the chromospheric activity of solar-like\nstars. We investigate the widely used bolometric and photospheric calibrated\nchromospheric activity index $R'_{\\rm HK}$, derived from the method in the\nclassic literature ($R'_{\\rm HK,classic}$) and the method based on the PHOENIX\nmodel ($R'_{\\rm HK,PHOENIX}$). Since the detailed stellar atmospheric\nparameters, effective temperature ($T_{\\rm eff}$), surface gravity ($\\log\\,g$),\nand metallicity ([Fe/H]), are available for LAMOST, we estimate the\nchromospheric activity index $R'_{\\rm HK,PHOENIX}$, along with the\ncorresponding bolometric calibrated index $R_{\\rm HK,PHOENIX}$, taking these\nparameters into account. We provide the database of the derived chromospheric\nactivity parameters for 1,122,495 LAMOST LRS spectra of solar-like stars. Our\ncalculations show that $\\log\\,R'_{\\rm HK,PHOENIX}$ is approximately linearly\ncorrelated with $\\log\\,R'_{\\rm HK,classic}$. The results based on our extensive\narchive support the view that the dynamo mechanism of solar-like stars is\ngenerally consistent with the Sun; and the value of solar chromospheric\nactivity index is located at the midpoint of the solar-like star sample. We\nfurther investigate the proportions of solar-like stars with different\nchromospheric activity levels (very active, active, inactive and very\ninactive). The investigation indicates that the occurrence rate of high levels\nof chromospheric activity is lower among the stars with effective temperatures\nbetween $5600$ and $5900 \\,{\\rm K}$.", "cat": "astro-ph.SR", "authors": ["Weitao Zhang", "Jun Zhang", "Han He", "Ali Luo", "Haotong Zhang"]}, "237": {"id": "2303.10559v2", "title": "Deep Learning for Camera Calibration and Beyond: A Survey", "url": "http://arxiv.org/pdf/2303.10559v2", "date": "2024-06-04 08:57:38", "abs": "Camera calibration involves estimating camera parameters to infer geometric\nfeatures from captured sequences, which is crucial for computer vision and\nrobotics. However, conventional calibration is laborious and requires dedicated\ncollection. Recent efforts show that learning-based solutions have the\npotential to be used in place of the repeatability works of manual\ncalibrations. Among these solutions, various learning strategies, networks,\ngeometric priors, and datasets have been investigated. In this paper, we\nprovide a comprehensive survey of learning-based camera calibration techniques,\nby analyzing their strengths and limitations. Our main calibration categories\ninclude the standard pinhole camera model, distortion camera model, cross-view\nmodel, and cross-sensor model, following the research trend and extended\napplications. As there is no benchmark in this community, we collect a holistic\ncalibration dataset that can serve as a public platform to evaluate the\ngeneralization of existing methods. It comprises both synthetic and real-world\ndata, with images and videos captured by different cameras in diverse scenes.\nToward the end of this paper, we discuss the challenges and provide further\nresearch directions. To our knowledge, this is the first survey for the\nlearning-based camera calibration (spanned 8 years). The summarized methods,\ndatasets, and benchmarks are available and will be regularly updated at\nhttps://github.com/KangLiao929/Awesome-Deep-Camera-Calibration.", "cat": "cs.CV", "authors": ["Kang Liao", "Lang Nie", "Shujuan Huang", "Chunyu Lin", "Jing Zhang", "Yao Zhao", "Moncef Gabbouj", "Dacheng Tao"]}, "238": {"id": "2112.09138v1", "title": "The DESI $N$-body Simulation Project I: Testing the Robustness of Simulations for the DESI Dark Time Survey", "url": "http://arxiv.org/pdf/2112.09138v1", "date": "2021-12-16 19:00:00", "abs": "Analysis of large galaxy surveys requires confidence in the robustness of\nnumerical simulation methods. The simulations are used to construct mock galaxy\ncatalogs to validate data analysis pipelines and identify potential\nsystematics. We compare three $N$-body simulation codes, ABACUS, GADGET, and\nSWIFT, to investigate the regimes in which their results agree. We run $N$-body\nsimulations at three different mass resolutions, $6.25\\times10^{8}$,\n$2.11\\times10^{9}$, and $5.00\\times10^{9}~h^{-1}$M$_{\\odot}$, matching phases\nto reduce the noise within the comparisons. We find systematic errors in the\nhalo clustering between different codes are smaller than the DESI statistical\nerror for $s > 20\\, h^{-1}$Mpc in the correlation function in redshift space.\nThrough the resolution comparison we find that simulations run with a mass\nresolution of $2.1\\times10^{9}~h^{-1}$M$_{\\odot}$ are sufficiently converged\nfor systematic effects in the halo clustering to be smaller than the DESI\nstatistical error at scales larger than $20 \\, h^{-1}$Mpc. These findings show\nthat the simulations are robust for extracting cosmological information from\nlarge scales which is the key goal of the DESI survey. Comparing matter power\nspectra, we find the codes agree to within 1% for $k \\leq 10~h$Mpc$^{-1}$. We\nalso run a comparison of three initial condition generation codes and find good\nagreement. In addition, we include a quasi-$N$-body code, FastPM, since we plan\nuse it for certain DESI analyses. The impact of the halo definition and\ngalaxy-halo relation will be presented in a follow up study.", "cat": "astro-ph.CO", "authors": ["Cameron Grove", "Chia-Hsun Chuang", "Ningombam Chandrachani Devi", "Lehman Garrison", "Benjamin L'Huillier", "Yu Feng", "John Helly", "C\u00e9sar Hern\u00e1ndez-Aguayo", "Shadab Alam", "Hanyu Zhang", "Yu Yu", "Shaun Cole", "Daniel Eisenstein", "Peder Norberg", "Risa Wechsler", "David Brooks", "Kyle Dawson", "Martin Landriau", "Aaron Meisner", "Claire Poppett", "Gregory Tarl\u00e9", "Octavio Valenzuela"]}, "239": {"id": "2204.08610v2", "title": "Image Data Augmentation for Deep Learning: A Survey", "url": "http://arxiv.org/pdf/2204.08610v2", "date": "2023-11-05 11:00:23", "abs": "Deep learning has achieved remarkable results in many computer vision tasks.\nDeep neural networks typically rely on large amounts of training data to avoid\noverfitting. However, labeled data for real-world applications may be limited.\nBy improving the quantity and diversity of training data, data augmentation has\nbecome an inevitable part of deep learning model training with image data.\n As an effective way to improve the sufficiency and diversity of training\ndata, data augmentation has become a necessary part of successful application\nof deep learning models on image data. In this paper, we systematically review\ndifferent image data augmentation methods. We propose a taxonomy of reviewed\nmethods and present the strengths and limitations of these methods. We also\nconduct extensive experiments with various data augmentation methods on three\ntypical computer vision tasks, including semantic segmentation, image\nclassification and object detection. Finally, we discuss current challenges\nfaced by data augmentation and future research directions to put forward some\nuseful research guidance.", "cat": "cs.CV", "authors": ["Suorong Yang", "Weikang Xiao", "Mengchen Zhang", "Suhan Guo", "Jian Zhao", "Furao Shen"]}, "240": {"id": "1906.10809v1", "title": "Compact Disks in a High Resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud", "url": "http://arxiv.org/pdf/1906.10809v1", "date": "2019-06-26 02:00:19", "abs": "We present a high-resolution ($\\sim0.''12$, $\\sim16$ au, mean sensitivity of\n$50~\\mu$Jy~beam$^{-1}$ at 225 GHz) snapshot survey of 32 protoplanetary disks\naround young stars with spectral type earlier than M3 in the Taurus\nstar-forming region using Atacama Large Millimeter Array (ALMA). This sample\nincludes most mid-infrared excess members that were not previously imaged at\nhigh spatial resolution, excluding close binaries and highly extincted objects,\nthereby providing a more representative look at disk properties at 1--2 Myr.\nOur 1.3 mm continuum maps reveal 12 disks with prominent dust gaps and rings, 2\nof which are around primary stars in wide binaries, and 20 disks with no\nresolved features at the observed resolution (hereafter smooth disks), 8 of\nwhich are around the primary star in wide binaries. The smooth disks were\nclassified based on their lack of resolved substructures, but their most\nprominent property is that they are all compact with small effective emission\nradii ($R_{\\rm eff,95\\%} \\lesssim 50$ au). In contrast, all disks with $R_{\\rm\neff,95\\%}$ of at least 55 au in our sample show detectable substructures.\nNevertheless, their inner emission cores (inside the resolved gaps) have\nsimilar peak brightness, power law profiles, and transition radii to the\ncompact smooth disks, so the primary difference between these two categories is\nthe lack of outer substructures in the latter. These compact disks may lose\ntheir outer disk through fast radial drift without dust trapping, or they might\nbe born with small sizes. The compact dust disks, as well as the inner disk\ncores of extended ring disks, that look smooth at the current resolution will\nlikely show small-scale or low-contrast substructures at higher resolution. The\ncorrelation between disk size and disk luminosity correlation demonstrates that\nsome of the compact disks are optically thick at millimeter wavelengths.", "cat": "astro-ph.SR", "authors": ["Feng Long", "Gregory J. Herczeg", "Daniel Harsono", "Paola Pinilla", "Marco Tazzari", "Carlo F. Manara", "Ilaria Pascucci", "Sylvie Cabrit", "Brunella Nisini", "Doug Johnstone", "Suzan Edwards", "Colette Salyk", "Francois Menard", "Giuseppe Lodato", "Yann Boehler", "Gregory N. Mace", "Yao Liu", "Gijs D. Mulders", "Nathanial Hendler", "Enrico Ragusa", "William J. Fischer", "Andrea Banzatti", "Elisabetta Rigliaco", "Gerrit van der Plas", "Giovanni Dipierro", "Michael Gully-Santiago", "Ricardo Lopez-Valdivia"]}, "241": {"id": "2209.15255v1", "title": "Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey", "url": "http://arxiv.org/pdf/2209.15255v1", "date": "2022-09-30 06:31:48", "abs": "$\\require{mediawiki-texvc}$A stellar chromospheric activity database of\nsolar-like stars is constructed based on the Large Sky Area Multi-Object Fiber\nSpectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The\ndatabase contains spectral bandpass fluxes and indexes of Ca II H&K lines\nderived from 1,330,654 high-quality LRS spectra of solar-like stars. We measure\nthe mean fluxes at line cores of the Ca II H&K lines using a 1 ${\\AA}$\nrectangular bandpass as well as a 1.09 ${\\AA}$ full width at half maximum\n(FWHM) triangular bandpass, and the mean fluxes of two 20 ${\\AA}$\npseudo-continuum bands on the two sides of the lines. Three activity indexes,\n$S_{\\rm rec}$ based on the 1 ${\\AA}$ rectangular bandpass, and $S_{\\rm tri}$\nand $S_L$ based on the 1.09 ${\\AA}$ FWHM triangular bandpass, are evaluated\nfrom the measured fluxes to quantitatively indicate the chromospheric activity\nlevel. The uncertainties of all the obtained parameters are estimated. We also\nproduce spectrum diagrams of Ca II H&K lines for all the spectra in the\ndatabase. The entity of the database is composed of a catalog of spectral\nsample and activity parameters, and a library of spectrum diagrams. Statistics\nreveal that the solar-like stars with high level of chromospheric activity\n($S_{\\rm rec}>0.6$) tend to appear in the parameter range of $T_{\\rm eff}\\text{\n(effective temperature)}<5500\\,{\\rm K}$, $4.3<\\log\\,g\\text{ (surface\ngravity)}<4.6$, and $-0.2<[{\\rm Fe/H}]\\text{ (metallicity)}<0.3$. This database\nwith more than one million high-quality LAMOST LRS spectra of Ca II H&K lines\nand basal chromospheric activity parameters can be further used for\ninvestigating activity characteristics of solar-like stars and solar-stellar\nconnection.", "cat": "astro-ph.SR", "authors": ["Weitao Zhang", "Jun Zhang", "Han He", "Zhiping Song", "Ali Luo", "Haotong Zhang"]}, "242": {"id": "0810.4520v1", "title": "Detecting the Cosmic Dipole Anisotropy in Large-Scale Radio Surveys", "url": "http://arxiv.org/pdf/0810.4520v1", "date": "2008-10-24 18:43:52", "abs": "The detection of a dipole anisotropy in the sky distribution of sources in\nlarge-scale radio surveys can be used to constrain the magnitude and direction\nof our local motion with respect to an isotropically distributed extragalactic\nradio source population. Such a population is predicted to be present at\ncosmological redshifts in an isotropically expanding universe. The\nextragalactic radio source population is observed to have a median redshift of\nz ~ 1, a much later epoch than the cosmic microwave background (z ~ 1100). I\nconsider the detectability of a velocity dipole anisotropy in radio surveys\nhaving a finite number of source counts. The statistical significance of a\nvelocity dipole detection from radio source counts is also discussed in detail.\nI find that existing large-scale radio survey catalogs do not have a sufficient\nnumber of sources to detect the expected velocity dipole with statistical\nsignificance, even if survey masking and flux calibration complications can be\ncompletely eliminated (i.e., if both the surveys and observing instruments are\nperfect). However, a dipole anisotropy should be easily detectable in future\nradio surveys planned with next-generation radio facilities, such as the Low\nFrequency Array and the Square Kilometer Array; tight constraints on the dipole\nmagnitude and direction should be possible if flux calibration problems can be\nsufficiently minimized or corrected and contamination from local sources\neliminated.", "cat": "astro-ph", "authors": ["Fronefield Crawford"]}, "243": {"id": "0705.4037v1", "title": "An updated survey of globular clusters in M31. II Newly discovered bright and remote clusters", "url": "http://arxiv.org/pdf/0705.4037v1", "date": "2007-05-28 12:30:01", "abs": "We present the first results of a large spectroscopic survey of candidate\nglobular clusters located in the extreme outskirts of the nearby M31 galaxy. We\nobtained low resolution spectra of 48 targets selected from the XSC of 2MASS,\nas in Galleti et al. (2005). The observed candidates have been robustly\nclassified according to their radial velocity and by verifying their\nextended/point-source nature from ground-based optical images. Among the 48\nobserved candidates clusters we found 5 genuine remote globular clusters. One\nof them has been already identified independently by Mackey et al. (2007),\ntheir GC1; the other four are completely new discoveries: B516, B517, B518,\nB519. The newly discovered clusters lie at projected distance 40 kpc<~R_p<~100\nkpc from the center of M31, and have absolute integrated magnitude\n-9.5 40 kpc. At\nodds with the Milky Way, M31 appears to have a significant population of very\nbright globular clusters in its extreme outskirts.", "cat": "astro-ph", "authors": ["S. Galleti", "M. Bellazzini", "L. Federici", "A. Buzzoni", "F. Fusi Pecci"]}, "244": {"id": "2409.02501v1", "title": "Impact of survey spatial variability on galaxy redshift distributions and the cosmological $3\\times2$-point statistics for the Rubin Legacy Survey of Space and Time (LSST)", "url": "http://arxiv.org/pdf/2409.02501v1", "date": "2024-09-04 07:57:20", "abs": "We investigate the impact of spatial survey non-uniformity on the galaxy\nredshift distributions for forthcoming data releases of the Rubin Observatory\nLegacy Survey of Space and Time (LSST). Specifically, we construct a mock\nphotometry dataset degraded by the Rubin OpSim observing conditions, and\nestimate photometric redshifts of the sample using a template-fitting photo-$z$\nestimator, BPZ, and a machine learning method, FlexZBoost. We select the Gold\nsample, defined as $i<25.3$ for 10 year LSST data, with an adjusted magnitude\ncut for each year and divide it into five tomographic redshift bins for the\nweak lensing lens and source samples. We quantify the change in the number of\nobjects, mean redshift, and width of each tomographic bin as a function of the\ncoadd $i$-band depth for 1-year (Y1), 3-year (Y3), and 5-year (Y5) data. In\nparticular, Y3 and Y5 have large non-uniformity due to the rolling cadence of\nLSST, hence provide a worst-case scenario of the impact from non-uniformity. We\nfind that these quantities typically increase with depth, and the variation can\nbe $10-40\\%$ at extreme depth values. Based on these results and using Y3 as an\nexample, we propagate the variable depth effect to the weak lensing\n$3\\times2$pt data vector in harmonic space. We find that galaxy clustering is\nmost susceptible to variable depth, causing significant deviations at large\nscales if not corrected for, due to the depth-dependent number density\nvariations. For galaxy-shear and shear-shear power spectra, we find little\nimpact given the expected LSST Y3 noise.", "cat": "astro-ph.CO", "authors": ["Qianjun Hang", "Benjamin Joachimi", "Eric Charles", "John Franklin Crenshaw", "Patricia Larsen", "Alex I. Malz", "Sam Schmidt", "Ziang Yan", "Tianqing Zhang", "the LSST Dark Energy Science Collaboration"]}, "245": {"id": "1101.5271v1", "title": "Infrared Survey of Pulsating Giant Stars in the Spiral Galaxy M33: Dust Production, Star Formation History, and Galactic Structure", "url": "http://arxiv.org/pdf/1101.5271v1", "date": "2011-01-27 12:48:06", "abs": "We introduce a near-IR monitoring campaign of the Local Group spiral galaxy\nM33, carried out with the UK IR Telescope (UKIRT). The pulsating giant stars\nare identified and their distributions are used to derive the star formation\nrate as a function of age. We here present the star formation history for the\ncentral square kiloparsec. These stars are also important dust factories; we\nmeasure their dust production rates from a combination of our data with Spitzer\nSpace Telescope mid-IR photometry.", "cat": "astro-ph.GA", "authors": ["Atefeh Javadi", "Jacco Th. van Loon", "Mohammad Taghi Mirtorabi"]}, "246": {"id": "0810.3459v1", "title": "The Rise of Massive Red Galaxies: the color-magnitude and color-stellar mass diagrams for z < ~2 from the MUltiwavelength Survey by Yale-Chile (MUSYC)", "url": "http://arxiv.org/pdf/0810.3459v1", "date": "2008-10-20 03:59:38", "abs": "We present the color-magnitude and color-stellar mass diagrams for galaxies\nwith z_phot < ~2, based on a K < 22 (AB) catalog of the Extended Chandra Deep\nField South (ECDFS) from the MUltiwavelength Survey by Yale-Chile (MUSYC). Our\nmain sample of 7840 galaxies contains 1297 M_* > 10^11 M_Sol galaxies in the\nrange 0.2 < z_phot < 1.8. We show empirically that this catalog is\napproximately complete for M_* > 10^11 M_Sol galaxies for z_phot < 1.8. For\nthis mass-limited sample, we show that the locus of the red sequence\ncolor-stellar mass relation evolves as Del(u-r) ~ (-0.44+/-0.02) z_phot for\nz_phot < ~1.2. For z_phot > ~1.3, however, we are no longer able to reliably\ndistinguish red and blue subpopulations from the observed color distribution;\nwe show that this would require much deeper near infrared data. At 1.5 < z_phot\n<1.8, the comoving number density of M_* > 10^11 M_Sol galaxies is ~50% of the\nlocal value, with a red fraction of ~33%. Making a parametric fit to the\nobserved evolution, we find n_tot(z) ~ (1+z_phot)^(-0.52+/-0.12(+/-0.20)). We\nfind stronger evolution in the red fraction: f_red(z) ~\n(1+z_phot)^(-1.17+/-0.18(+/-0.21)). Through a series of sensitivity analyses,\nwe show that the most important sources of systematic error are: 1. systematic\ndifferences in the analysis of the z~0 and z>>0 samples; 2. systematic effects\nassociated with details of the photometric redshift calculation; and 3.\nuncertainties in the photometric calibration. With this in mind, we show that\nour results based on photometric redshifts are consistent with a completely\nindependent analysis which does not require redshift information for individual\ngalaxies. Our results suggest that, at most, 1/5 of local red sequence galaxies\nwith M_* >10^11 M_Sol were already in place at z ~ 2.", "cat": "astro-ph", "authors": ["Edward N Taylor", "Marijn Franx", "Pieter G van Dokkum", "Eric F Bell", "Gabriel B Brammer", "Gregory Rudnick", "Stijn Wuyts", "Eric Gawiser", "Paulina Lira", "C Megan Urry", "Hans-Walter Rix"]}, "247": {"id": "2306.09414v1", "title": "Optimizing Roman's High Latitude Wide Area Survey for Low Surface Brightness Astronomy", "url": "http://arxiv.org/pdf/2306.09414v1", "date": "2023-06-15 18:00:10", "abs": "One of the last remaining frontiers in optical/near-infrared observational\nastronomy is the low surface brightness regime (LSB, V-band surface brightness,\n$\\mu_V>$ 27 AB mag/arcsec$^2$). These are the structures at very low stellar\nsurface densities, largely unseen by even current wide-field surveys such as\nthe Legacy Survey. Studying this domain promises to be transformative for our\nunderstanding of star formation in low-mass galaxies, the hierarchical assembly\nof galaxies and galaxy clusters, and the nature of dark matter. It is thus\nessential to reach depths beyond $\\mu_V$ = 30 AB mag/arcsec$^2$ to detect the\nfaintest extragalactic sources, such as dwarf galaxies and the stellar halos\naround galaxies and within galaxy clusters. The High Latitude Wide Area Survey\noffers a unique opportunity to statistically study the LSB universe at\nunprecedented depths in the IR over an area of $\\sim$2000 square degrees. The\nhigh spatial resolution will minimize source confusion, allowing an unbiased\ncharacterization of LSB structures, including the identification of stars in\nnearby LSB galaxies and globular clusters. In addition, the combination of\nRoman with other upcoming deep imaging observatories (such as Rubin) will\nprovide multi-wavelength coverage to derive photometric redshifts and infer the\nstellar populations of LSB objects.", "cat": "astro-ph.GA", "authors": ["Mireia Montes", "Francesca Annibali", "Michele Bellazzini", "Alejandro S. Borlaff", "Sarah Brough", "Fernando Buitrago", "Nushkia Chamba", "Chris Collins", "Ian Dell'Antonio", "Ivanna Escala", "Anthony H. Gonzalez", "Benne Holwerda", "Sugata Kaviraj", "Johan Knapen", "Anton Koekemoer", "Seppo Laine", "Pamela Marcum", "Garreth Martin", "David Martinez-Delgado", "Chris Mihos", "Massimo Ricotti", "Ignacio Trujillo", "Aaron E. Watkins"]}, "248": {"id": "1607.08612v1", "title": "A Low Frequency Survey of Giant Pulses from the Crab Pulsar", "url": "http://arxiv.org/pdf/1607.08612v1", "date": "2016-07-28 20:00:00", "abs": "We present a large survey of giant pulses from the Crab Pulsar as observed\nwith the first station of the Long Wavelength Array. Automated methods for\ndetecting giant pulses at low frequencies where scattering becomes prevalent\nare also explored. More than 1400 pulses were detected across four frequency\nbands between 20 - 84 MHz over a seven month period beginning in 2013, with\nadditional followup observations in late 2014 and early 2015. A handful of\nthese pulses were detected simultaneously across all four frequency bands. We\nexamine pulse characteristics, including pulse broadening and power law indices\nfor amplitude distributions. We find that the flux density increases toward\nshorter wavelengths, consistent with a spectral turnover at 100 MHz. Our\nobservations uniquely span multiple scattering epochs, manifesting as a notable\ntrend in the number of detections per observation. These results are\ncharacteristic of the variable interface between the synchrotron nebula and the\nsurrounding interstellar medium.", "cat": "astro-ph.SR", "authors": ["T. Eftekhari", "K. Stovall", "J. Dowell", "F. K. Schinzel", "G. B. Taylor"]}, "249": {"id": "1507.08018v2", "title": "Photometry of Variable Stars from THU-NAOC Transient Survey I: The First 2 Years", "url": "http://arxiv.org/pdf/1507.08018v2", "date": "2015-09-12 15:33:48", "abs": "In this paper, we report the detections of stellar variabilities from the\nfirst 2-year observations of sky area of about 1300 square degrees from the\nTsinghua University-NAOC Transient Survey (TNTS). A total of 1237 variable\nstars (including 299 new ones) were detected with brightness < 18.0 mag and\nmagnitude variation >= 0.1 mag on a timescale from a few hours to few hundred\ndays. Among such detections, we tentatively identified 661 RR Lyrae stars, 431\nbinaries, 72 Semiregular pulsators, 29 Mira stars, 11 slow irregular variables,\n11 RS Canum Venaticorum stars, 7 Gamma Doradus stars, 5 long period variables,\n3 W Virginis stars, 3 Delta Scuti stars, 2 Anomalous Cepheids, 1 Cepheid, and 1\nnove-like star based on their time-series variability index Js and their phased\ndiagrams. Moreover, we found that 14 RR Lyrae stars show the Blazhko effect and\n67 contact eclipsing binaries exhibit the O'Connell effect. Since the period\nand amplitude of light variations of RR Lyrae variables depend on their\nchemical compositions, their photometric observations can be used to\ninvestigate distribution of metallicity along the direction perpendicular to\nthe Galactic disk. We find that the metallicity of RR Lyrae stars shows large\nscatter at regions closer to the Galactic plane (e.g., -3.0 < [Fe/H] < 0) but\ntends to converge at [Fe/H]~ -1.7 at larger Galactic latitudes. This variation\nmay be related to that the RRAB Lyrae stars in the Galactic halo come from\nglobular clusters with different metallicity and vertical distances, i.e. OoI\nand OoII populations, favoring for the dual-halo model.", "cat": "astro-ph.SR", "authors": ["Xinyu Yao", "Lingzhi Wang", "Xiaofeng Wang", "Tianmeng Zhang", "Juncheng Chen", "Wenlong Yuan", "Jun Mo", "Wenxiong Li", "Zhiping Jin", "Xuefeng Wu", "JunDan Nie", "Xu Zhou"]}, "250": {"id": "1110.0468v2", "title": "Overdensities of Y-dropout Galaxies from the Brightest-of-Reionizing Galaxies Survey: A Candidate Protocluster at Redshift z~8", "url": "http://arxiv.org/pdf/1110.0468v2", "date": "2011-11-21 10:40:08", "abs": "Theoretical and numerical modeling of dark-matter halo assembly predicts that\nthe most luminous galaxies at high redshift are surrounded by overdensities of\nfainter companions. We test this prediction with HST observations acquired by\nour Brightest of Reionizing Galaxies (BoRG) survey, which identified four very\nbright z~8 candidates as Y-dropout sources in four of the 23 non-contiguous\nWFC3 fields observed. We extend here the search for Y-dropouts to fainter\nluminosities (M_* galaxies with M_AB\\sim-20), with detections at >5sigma\nconfidence (compared to >8sigma confidence adopted earlier) identifying 17 new\ncandidates. We demonstrate that there is a correlation between number counts of\nfaint and bright Y-dropouts at >99.84% confidence. Field BoRG58, which contains\nthe best bright z\\sim8 candidate (M_AB=-21.3), has the most significant\noverdensity of faint Y-dropouts. Four new sources are located within 70arcsec\n(corresponding to 3.1 comoving Mpc at z=8) from the previously known brighter\nz\\sim8 candidate. The overdensity of Y-dropouts in this field has a physical\norigin to high confidence (p>99.975%), independent of completeness and\ncontamination rate of the Y-dropout selection. We modeled the overdensity by\nmeans of cosmological simulations and estimate that the principal dark matter\nhalo has mass M_h\\sim(4-7)x10^11Msun (\\sim5sigma density peak) and is\nsurrounded by several M_h\\sim10^11Msun halos which could host the fainter\ndropouts. In this scenario, we predict that all halos will eventually merge\ninto a M_h>2x10^14Msun galaxy cluster by z=0. Follow-up observations with\nground and space based telescopes are required to secure the z\\sim8 nature of\nthe overdensity, discover new members, and measure their precise redshift.", "cat": "astro-ph.CO", "authors": ["M. Trenti", "L. D. Bradley", "M. Stiavelli", "J. M. Shull", "P. Oesch", "R. J. Bouwens", "J. A. Munoz", "E. Romano-Diaz", "T. Treu", "I. Shlosman", "C. M. Carollo"]}, "251": {"id": "2111.04545v2", "title": "GASKAP Pilot Survey Science II: ASKAP Zoom Observations of Galactic 21-cm Absorption", "url": "http://arxiv.org/pdf/2111.04545v2", "date": "2022-02-26 22:58:07", "abs": "Using the Australian Square Kilometre Array Pathfinder to measure 21-cm\nabsorption spectra toward continuum background sources, we study the cool phase\nof the neutral atomic gas in the far outer disk, and in the inner Galaxy near\nthe end of the Galactic bar at longitude 340 degrees. In the inner Galaxy the\ncool atomic gas has a smaller scale height than in the solar neighborhood,\nsimilar to the molecular gas and the superthin stellar population in the bar.\nIn the outer Galaxy the cool atomic gas is mixed with the warm, neutral medium,\nwith the cool fraction staying roughly constant with Galactic radius. The mean\nspin temperature, i.e. the ratio of the emission brightness temperature to the\nabsorption, is roughly constant for velocities corresponding to Galactic radius\ngreater than about twice the solar circle radius. The ratio has a value of\nabout 300 K, but this does not correspond to a physical temperature in the gas.\nIf the gas causing the absorption has kinetic temperature of about 100 K, as in\nthe solar neighborhood, then the value 300 K indicates that the fraction of the\ngas mass in this phase is one-third of the total HI mass.", "cat": "astro-ph.GA", "authors": ["J. M. Dickey", "J. M. Dempsey", "N. M. Pingel", "N. M. McClure-Griffiths", "K. Jameson", "J. R. Dawson", "H. D\u00e9nes", "S. E. Clark", "G. Joncas", "D. Leahy", "Min-Young Lee", "M. -A. Miville-Desch\u00eanes", "S. Stanimirovi\u0107", "C. D. Tremblay", "J. Th. van Loon"]}, "252": {"id": "2305.16754v3", "title": "The FAST Galactic Plane Pulsar Snapshot Survey: III. Timing results of 30 FAST-GPPS discovered pulsars", "url": "http://arxiv.org/pdf/2305.16754v3", "date": "2023-10-11 08:12:47", "abs": "Timing observations are crucial for determining the basic parameters of newly\ndiscovered pulsars. Using the Five-hundred-meter Aperture Spherical radio\nTelescope (FAST) with the L-band 19-beam receiver covering the frequency range\nof 1.0--1.5 GHz, the FAST Galactic Plane Pulsar Snapshot (GPPS) Survey has\ndiscovered more than 600 faint pulsars with flux densities of only a few or a\nfew tens of $\\mu$Jy at 1.25 GHz. To obtain accurate position, spin parameters\nand dispersion measure of a pulsar, and to calculate derived parameters such as\nthe characteristic age and surface magnetic field, we collect available FAST\npulsar data obtained either through targeted follow-up observations or through\ncoincidental survey observations with one of the 19 beams of the receiver. From\nthese data we obtain time of arrival (TOA) measurements for 30 newly discovered\npulsars as well as for 13 known pulsars. We demonstrate that the TOA\nmeasurements acquired by the FAST from any beams of the receiver in any\nobservation mode (e.g. the tracking mode or the snapshot mode) can be combined\nto get timing solutions. We update the ephemerides of 13 previously known\npulsars and obtain the first phase-coherent timing results for 30 isolated\npulsars discovered in the FAST GPPS Survey. Notably, PSR J1904+0853 is an\nisolated millisecond pulsar, PSR J1906+0757 is a disrupted recycled pulsar, and\nPSR J1856+0211 has a long period of 9.89 s that can constrain pulsar death\nlines. Based on these timing solutions, all available FAST data have been added\ntogether to obtain the best pulse profiles for these pulsars.", "cat": "astro-ph.HE", "authors": ["W. Q. Su", "J. L. Han", "P. F. Wang", "J. P. Yuan", "Chen Wang", "D. J. Zhou", "Tao Wang", "Yi Yan", "W. C. Jing", "Z. L. Yang", "N. N. Cai", "Xue Chen", "Jun Xu", "Lang Xie", "H. G. Wang", "R. X. Xu", "X. P. You"]}, "253": {"id": "2301.12724v1", "title": "The LOFAR LBA Sky Survey II. First data release", "url": "http://arxiv.org/pdf/2301.12724v1", "date": "2023-01-30 08:45:11", "abs": "The Low Frequency Array (LOFAR) is the only existing radio interferometer\nable to observe at ultra-low frequencies (<100 MHz) with high resolution (<15\")\nand high sensitivity (<1 mJy/beam). To exploit these capabilities, the LOFAR\nSurveys Key Science Project is using the LOFAR Low Band Antenna (LBA) to carry\nout a sensitive wide-area survey at 41-66 MHz named the LOFAR LBA Sky Survey\n(LoLSS). LoLSS is covering the whole northern sky above declination 24 deg with\na resolution of 15\" and a sensitivity of 1-2 mJy/beam (1 sigma) depending on\ndeclination, field properties, and observing conditions. Here we present the\nfirst data release. An automated pipeline was used to reduce the 95 fields\nincluded in this data release. The data reduction procedures developed for this\nproject have general application and are currently being used to process LOFAR\nLBA interferometric observations. Compared to the preliminary release,\ndirection-dependent errors have been corrected for during the calibration\nprocess. This results in a typical sensitivity of 1.55 mJy/beam at the target\nresolution of 15\". The first data release of the LOFAR LBA Sky Survey covers\n650 sqdeg in the HETDEX spring field. The resultant data products released to\nthe community include mosaic images (I and V Stokes) of the region, and a\ncatalogue of 42463 detected sources and related Gaussian components used to\ndescribe sources' morphologies. Separate catalogues for 6 in-band frequencies\nare also released. The first data release of LoLSS shows that, despite the\ninfluences of the ionosphere, LOFAR can conduct large-scale surveys in the\nfrequency window 42-66 MHz with unprecedentedly high sensitivity and\nresolution. The data can be used to derive unique information on the\nlow-frequency spectral properties of many thousands of sources with a wide\nrange of applications in extragalactic and galactic astronomy.", "cat": "astro-ph.IM", "authors": ["F. de Gasperin", "H. W. Edler", "W. L. Williams", "J. R. Callingham", "B. Asabere", "M. Bruggen", "G. Brunetti", "T. J. Dijkema", "M. J. Hardcastle", "M. Iacobelli", "A. Offringa", "M. J. Norden", "H. J. A. Rottgering", "T. Shimwell", "R. J. van Weeren", "C. Tasse", "D. J. Bomans", "A. Bonafede", "A. Botteon", "R. Cassano", "K. T. Chyzy", "V. Cuciti", "K. L. Emig", "M. Kadler", "G. Miley", "B. Mingo", "M. S. S. L. Oei", "I. Prandoni", "D. J. Schwarz", "P. Zarka"]}, "254": {"id": "1803.02368v2", "title": "Likelihood for Detection of Sub-parsec Supermassive Black Hole Binaries in Spectroscopic Surveys", "url": "http://arxiv.org/pdf/1803.02368v2", "date": "2018-06-07 20:32:13", "abs": "Motivated by observational searches for sub-parsec supermassive black hole\nbinaries (SBHBs) we develop a modular analytic model to determine the\nlikelihood for detection of SBHBs by ongoing spectroscopic surveys. The model\ncombines the parametrized rate of orbital evolution of SBHBs in circumbinary\ndisks with the selection effects of spectroscopic surveys and returns a\nmultivariate likelihood for SBHB detection. Based on this model we find that in\norder to evolve into the detection window of the spectroscopic searches from\nlarger separations in less than a Hubble time, $10^8M_\\odot$ SBHBs must, on\naverage, experience angular momentum transport faster than that provided by a\ndisk with accretion rate $0.06\\,\\dot{M}_E$. Spectroscopic searches with yearly\ncadence of observations are in principle sensitive to binaries with orbital\nseparations $< {\\rm few}\\times 10^4\\, r_g$ ($r_g = GM/c^2$ and $M$ is the\nbinary mass), and for every one SBHB in this range there should be over 200\nmore gravitationally bound systems with similar properties, at larger\nseparations. Furthermore, if spectra of all SBHBs in this separation range\nexhibit the AGN-like emission lines utilized by spectroscopic searches, the\nprojection factors imply five undetected binaries for each observed\n$10^8M_\\odot$ SBHB with mass ratio $0.3$ and orbital separation $10^4\\,r_g$\n(and more if some fraction of SBHBs is inactive). This model can be used to\ninfer the most likely orbital parameters for observed SBHB candidates and to\nprovide constraints on the rate of orbital evolution of SBHBs, if observed\ncandidates are shown to be genuine binaries.", "cat": "astro-ph.HE", "authors": ["Bryan J. Pflueger", "Khai Nguyen", "Tamara Bogdanovic", "Michael Eracleous", "Jessie C. Runnoe", "Steinn Sigurdsson", "Todd Boroson"]}, "255": {"id": "2307.14737v2", "title": "SRG/eROSITA Survey in the Lockman Hole: Classification of X-ray Sources", "url": "http://arxiv.org/pdf/2307.14737v2", "date": "2023-09-29 08:12:22", "abs": "We have classified the point-like X-ray sources detected by the SRG/eROSITA\ntelescope in the deep Lockman Hole survey. The goal was to separate the sources\ninto Galactic and extragalactic objects. In this work have used the results of\nour previous cross-match of X-ray sources with optical catalogs. To classify\nSRG/eROSITA sources we have used the flux ratio $F_{x}/F_{o}$ and information\nabout the source optical extent. As a result, of the 6885 X-ray sources in the\neROSITA catalog 357 sources have been classified as Galactic and 5929 and as\nextragalactic. 539 out of 6885 have been treated as hostless, i.e., having no\noptical counterparts in the optical catalogs under consideration. 60 have\nremained unclassified due to the insufficient reliability of optical\nphotometry. Recall and precision for the extragalactic sources are 99.9 and\n98.9% (respectively) and 91.6 and 99.7% for the Galactic sources. Using this\nclassification, we have constructed the curves of cumulative number counts for\nthe Galactic and extragalactic sources in the Lockman Hole field. The code that\naccompanies this paper is available at\nhttps://github.com/mbelveder/ero-lh-class.git.", "cat": "astro-ph.HE", "authors": ["M. I. Belvedersky", "S. D. Bykov", "M. R. Gilfanov"]}, "256": {"id": "0704.1743v1", "title": "A Catalogue of Morphologically Classified Galaxies from the Sloan Digital Sky Survey: North Equatorial Region", "url": "http://arxiv.org/pdf/0704.1743v1", "date": "2007-04-13 12:45:55", "abs": "We present a catalogue of morphologically classified bright galaxies in the\nnorth equatorial stripe (230 deg$^2$) derived from the Third Data Release of\nthe Sloan Digital Sky Survey (SDSS). Morphological classification is performed\nby visual inspection of images in the $g$ band. The catalogue contains 2253\ngalaxies complete to a magnitude limit of $r=16$ after Galactic extinction\ncorrection, selected from 2658 objects that are judged as extended in the\nphotometric catalogue in the same magnitude limit. 1866 galaxies in our\ncatalogue have spectroscopic information. A brief statistical analysis is\npresented for the frequency of morphological types and mean colours in the\ncatalogue. A visual inspection of the images reveals that the rate of\ninteracting galaxies in the local Universe is approximately 1.5% in the\n$r\\le16$ sample. A verification is made for the photometric catalogue generated\nby the SDSS, especially as to its bright end completeness.", "cat": "astro-ph", "authors": ["Masataka Fukugita", "Osamu Nakamura", "Sadanori Okamura", "Naoki Yasuda", "John C. Barentine", "Jon Brinkmann", "James E. Gunn", "Mike Harvanek", "Takashi Ichikawa", "Robert H. Lupton", "Donald P. Schneider", "Michael A. Strauss", "Donald G. York"]}, "257": {"id": "1702.03571v1", "title": "The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey", "url": "http://arxiv.org/pdf/1702.03571v1", "date": "2017-02-12 20:42:25", "abs": "We describe a 20-year survey carried out by the Lick-Carnegie Exoplanet\nSurvey Team (LCES), using precision radial velocities from HIRES on the Keck-I\ntelescope to find and characterize extrasolar planetary systems orbiting nearby\nF, G, K, and M dwarf stars. We provide here 60,949 precision radial velocities\nfor 1,624 stars contained in that survey. We tabulate a list of 357 significant\nperiodic signals that are of constant period and phase, and not coincident in\nperiod and/or phase with stellar activity indices. These signals are thus\nstrongly suggestive of barycentric reflex motion of the star induced by one or\nmore candidate exoplanets in Keplerian motion about the host star. Of these\nsignals, 225 have already been published as planet claims, 60 are classified as\nsignificant unpublished planet candidates that await photometric follow-up to\nrule out activity-related causes, and 54 are also unpublished, but are\nclassified as \"significant\" signals that require confirmation by additional\ndata before rising to classification as planet candidates. Of particular\ninterest is our detection of a candidate planet with a minimum mass of 3.9\nEarth masses and an orbital period of 9.9 days orbiting Lalande 21185, the\nfourth-closest main sequence star to the Sun. For each of our exoplanetary\ncandidate signals, we provide the period and semi-amplitude of the Keplerian\norbital fit, and a likelihood ratio estimate of its statistical significance.\nWe also tabulate 18 Keplerian-like signals that we classify as likely arising\nfrom stellar activity.", "cat": "astro-ph.EP", "authors": ["R. Paul Butler", "Steven S. Vogt", "Gregory Laughlin", "Jennifer A. Burt", "Eugenio J. Rivera", "Mikko Tuomi", "Johanna Teske", "Pamela Arriagada", "Matias Diaz", "Brad Holden", "Sandy Keiser"]}, "258": {"id": "2102.08909v2", "title": "Surveying the Landscape of Ethics-Focused Design Methods", "url": "http://arxiv.org/pdf/2102.08909v2", "date": "2022-08-26 11:00:37", "abs": "Over the past decade, HCI researchers, design researchers, and practitioners\nhave increasingly addressed ethics-focused issues through a range of\ntheoretical, methodological and pragmatic contributions to the field. While\nmany forms of design knowledge have been proposed and described, we focus\nexplicitly on knowledge that has been codified as \"methods,\" which we define as\nany supports for everyday work practices of designers. In this paper, we\nidentify, analyze, and map a collection of 63 existing ethics-focused methods\nintentionally designed for ethical impact. We present a content analysis,\nproviding a descriptive record of how they operationalize ethics, their\nintended audience or context of use, their \"core\" or \"script,\" and the means by\nwhich these methods are formulated, articulated, and languaged. Building on\nthese results, we provide an initial definition of ethics-focused methods,\nidentifying potential opportunities for the development of future methods to\nsupport design practice and research.", "cat": "cs.HC", "authors": ["Shruthi Sai Chivukula", "Ziqing Li", "Anne C. Pivonka", "Jingning Chen", "Colin M. Gray"]}, "259": {"id": "1712.01415v1", "title": "From Clumps to Cores to Protostars: The JCMT Gould Belt Survey's \"First-Look\" analysis of Southern Orion A using SCUBA-2", "url": "http://arxiv.org/pdf/1712.01415v1", "date": "2017-12-04 23:41:08", "abs": "We present a subset of the James Clerk Maxwell Telescope Gould Belt Survey's\n\"first-look\" results of the southern extent of the Orion A molecular cloud.\nEmploying a two-step structure identification process, we constructed\nindividual catalogues for large-scale regions of significant emission labeled\nas \"islands\" and smaller-scale subregions called \"fragments\" using the 850\n$\\mu$m continuum maps obtained using the Submillimetre Common-User Bolometer\nArray 2 (SCUBA-2). We highlight the relationship between the concentration and\nJeans stability for regions of significant emission and present the results of\nan investigation into the spatial distribution of Young Stellar Objects\ndetected using the Spitzer Space Telescope and the Herschel Space Observatory.\nWe find an apparent evolution in the velocity dispersion from Class 0 to Class\nII objects which we derive from comparing our observations to a simple model.", "cat": "astro-ph.GA", "authors": ["Steve Mairs", "Doug Johnstone", "Helen Kirk"]}, "260": {"id": "2407.13485v1", "title": "Slope-semistability and moduli of coherent sheaves: a survey", "url": "http://arxiv.org/pdf/2407.13485v1", "date": "2024-07-18 13:04:12", "abs": "We survey old and new results on the existence of moduli spaces of semistable\ncoherent sheaves both in algebraic and in complex geometry.", "cat": "math.AG", "authors": ["Mihai Pavel", "Matei Toma"]}, "261": {"id": "1807.03505v1", "title": "Automatic Rumor Detection on Microblogs: A Survey", "url": "http://arxiv.org/pdf/1807.03505v1", "date": "2018-07-10 07:48:33", "abs": "The ever-increasing amount of multimedia content on modern social media\nplatforms are valuable in many applications. While the openness and convenience\nfeatures of social media also foster many rumors online. Without verification,\nthese rumors would reach thousands of users immediately and cause serious\ndamages. Many efforts have been taken to defeat online rumors automatically by\nmining the rich content provided on the open network with machine learning\ntechniques. Most rumor detection methods can be categorized in three paradigms:\nthe hand-crafted features based classification approaches, the\npropagation-based approaches and the neural networks approaches. In this\nsurvey, we introduce a formal definition of rumor in comparison with other\ndefinitions used in literatures. We summary the studies of automatic rumor\ndetection so far and present details in three paradigms of rumor detection. We\nalso give an introduction on existing datasets for rumor detection which would\nbenefit following researches in this area. We give our suggestions for future\nrumors detection on microblogs as a conclusion.", "cat": "cs.SI", "authors": ["Juan Cao", "Junbo Guo", "Xirong Li", "Zhiwei Jin", "Han Guo", "Jintao Li"]}, "262": {"id": "1711.04516v1", "title": "Source Finding in Linear Polarization for LOFAR, and SKA Predecessor Surveys, using Faraday Moments", "url": "http://arxiv.org/pdf/1711.04516v1", "date": "2017-11-13 10:56:47", "abs": "The optimal source-finding strategy for linear polarization data is an\nunsolved problem, with many inhibitive factors imposed by the\ntechnically-challenging nature of polarization observations. Such an algorithm\nis essential for Square Kilometre Array (SKA) pathfinder surveys, such as the\nMultifrequency Snapshot Sky Survey (MSSS) with the LOw Frequency ARray (LOFAR),\nas data volumes are significant enough to prohibit manual inspection. We\npresent a new strategy of `Faraday Moments' for source-finding in linear\npolarization with LOFAR, using the moments of the frequency-dependent\nfull-Stokes data (i.e. the mean, standard deviation, skewness, and excess\nkurtosis). Through simulations of the sky, we find that moments can identify\npolarized sources with a high completeness: 98.5% at a signal-to-noise of 5.\nWhile the method has low reliability, Rotation Measure (RM) Synthesis can be\napplied per candidate source to filter out instrumental and spurious\ndetections. This combined strategy will result in a complete and reliable\ncatalogue of polarized sources that includes the full sensitivity of the\nobservational bandwidth. We find that the technique can reduce the number of\npixels on which RM Synthesis needs to be performed by a factor of\n$\\approx1\\times10^{5}$ for source distributions anticipated with modern radio\ntelescopes. Through tests on LOFAR data, we find that the technique works\neffectively in the presence of diffuse emission. Extensions of this method are\ndirectly applicable to other upcoming radio surveys such as the POlarization\nSky Survey of the Universe's Magnetism (POSSUM) with the Australia Square\nKilometre Array Pathfinder (ASKAP), and the SKA itself.", "cat": "astro-ph.IM", "authors": ["J. S. Farnes", "G. Heald", "H. Junklewitz", "D. D. Mulcahy", "M. Haverkorn", "C. L. Van Eck", "C. J. Riseley", "M. Brentjens", "C. Horellou", "V. Vacca", "D. I. Jones", "A. Horneffer", "R. Paladino"]}, "263": {"id": "2211.05617v1", "title": "Debiasing Methods for Fairer Neural Models in Vision and Language Research: A Survey", "url": "http://arxiv.org/pdf/2211.05617v1", "date": "2022-11-10 14:42:46", "abs": "Despite being responsible for state-of-the-art results in several computer\nvision and natural language processing tasks, neural networks have faced harsh\ncriticism due to some of their current shortcomings. One of them is that neural\nnetworks are correlation machines prone to model biases within the data instead\nof focusing on actual useful causal relationships. This problem is particularly\nserious in application domains affected by aspects such as race, gender, and\nage. To prevent models from incurring on unfair decision-making, the AI\ncommunity has concentrated efforts in correcting algorithmic biases, giving\nrise to the research area now widely known as fairness in AI. In this survey\npaper, we provide an in-depth overview of the main debiasing methods for\nfairness-aware neural networks in the context of vision and language research.\nWe propose a novel taxonomy to better organize the literature on debiasing\nmethods for fairness, and we discuss the current challenges, trends, and\nimportant future work directions for the interested researcher and\npractitioner.", "cat": "cs.LG", "authors": ["Ot\u00e1vio Parraga", "Martin D. More", "Christian M. Oliveira", "Nathan S. Gavenski", "Lucas S. Kupssinsk\u00fc", "Adilson Medronha", "Luis V. Moura", "Gabriel S. Sim\u00f5es", "Rodrigo C. Barros"]}, "264": {"id": "2301.00640v3", "title": "Joint reconstructions of growth and expansion histories from stage-IV surveys with minimal assumptions. II. Modified gravity and massive neutrinos", "url": "http://arxiv.org/pdf/2301.00640v3", "date": "2023-06-28 05:53:53", "abs": "Based on a formalism introduced in our previous work, we reconstruct the\nphenomenological function $G_{\\rm eff}(z)$ describing deviations from General\nRelativity (GR) in a model-independent manner. In this alternative approach, we\nmodel $\\mu\\equiv G_\\mathrm{eff}/G$ as a Gaussian process and use forecasted\ngrowth-rate measurements from a stage-IV survey to reconstruct its shape for\ntwo different toy models. We follow a two-step procedure: (i) we first\nreconstruct the background expansion history from Supernovae (SNe) and Baryon\nAcoustic Oscillation (BAO) measurements; (ii) we then use it to obtain the\ngrowth history $f\\sigma_8$, that we fit to redshift-space distortions (RSD)\nmeasurements to reconstruct $G_\\mathrm{eff}$. We find that upcoming surveys\nsuch as the Dark Energy Spectroscopic Instrument (DESI) might be capable of\ndetecting deviations from GR, provided the dark energy behavior is accurately\ndetermined. We might even be able to constrain the transition redshift from\n$G\\to G_\\mathrm{eff}$ for some particular models. We further assess the impact\nof massive neutrinos on the reconstructions of $G_\\mathrm{eff}$ (or $\\mu$)\nassuming the expansion history is given, and only the neutrino mass is free to\nvary. Given the tight constraints on the neutrino mass, and for the profiles we\nconsidered in this work, we recover numerically that the effect of such massive\nneutrinos does not alter our conclusions. Finally, we stress that incorrectly\nassuming a $\\Lambda$CDM expansion history leads to a degraded reconstruction of\n$\\mu$, and/or a non-negligible bias in the\n($\\Omega_\\mathrm{m,0}$,$\\sigma_{8,0}$)-plane.", "cat": "astro-ph.CO", "authors": ["Rodrigo Calder\u00f3n", "Benjamin L'Huillier", "David Polarski", "Arman Shafieloo", "Alexei A. Starobinsky"]}, "265": {"id": "1803.04869v2", "title": "Rapidly evolving transients in the Dark Energy Survey", "url": "http://arxiv.org/pdf/1803.04869v2", "date": "2018-08-22 14:12:50", "abs": "We present the results of a search for rapidly evolving transients in the\nDark Energy Survey Supernova Programme. These events are characterized by fast\nlight curve evolution (rise to peak in $\\lesssim 10$ d and exponential decline\nin $\\lesssim30$ d after peak). We discovered 72 events, including 37 transients\nwith a spectroscopic redshift from host galaxy spectral features. The 37 events\nincrease the total number of rapid optical transients by more than factor of\ntwo. They are found at a wide range of redshifts ($0.05M_\\mathrm{g}>-22.25$). The multiband photometry is well\nfit by a blackbody up to few weeks after peak. The events appear to be hot\n($T\\approx10000-30000$ K) and large ($R\\approx 10^{14}-2\\cdot10^{15}$ cm) at\npeak, and generally expand and cool in time, though some events show evidence\nfor a receding photosphere with roughly constant temperature. Spectra taken\naround peak are dominated by a blue featureless continuum consistent with hot,\noptically thick ejecta. We compare our events with a previously suggested\nphysical scenario involving shock breakout in an optically thick wind\nsurrounding a core-collapse supernova (CCSNe), we conclude that current models\nfor such a scenario might need an additional power source to describe the\nexponential decline. We find these transients tend to favor star-forming host\ngalaxies, which could be consistent with a core-collapse origin. However, more\ndetailed modeling of the light curves is necessary to determine their physical\norigin.", "cat": "astro-ph.HE", "authors": ["M. Pursiainen", "M. Childress", "M. Smith", "S. Prajs", "M. Sullivan", "T. M. Davis", "R. J. Foley", "J. Asorey", "J. Calcino", "D. Carollo", "C. Curtin", "C. B. D'Andrea", "K. Glazebrook", "C. Gutierrez", "S. R. Hinton", "J. K. Hoormann", "C. Inserra", "R. Kessler", "A. King", "K. Kuehn", "G. F. Lewis", "C. Lidman", "E. Macaulay", "A. M\u00f6ller", "R. C. Nichol", "M. Sako", "N. E. Sommer", "E. Swann", "B. E. Tucker", "S. A. Uddin", "P. Wiseman", "B. Zhang", "T. M. C. Abbott", "F. B. Abdalla", "S. Allam", "J. Annis", "S. Avila", "D. Brooks", "E. Buckley-Geer", "D. L. Burke", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "F. J. Castander", "C. E. Cunha", "C. Davis", "J. De Vicente", "H. T. Diehl", "P. Doel", "T. F. Eifler", "B. Flaugher", "P. Fosalba", "J. Frieman", "J. Garc\u00eda-Bellido", "D. Gruen", "R. A. Gruendl", "G. Gutierrez", "W. G. Hartley", "D. L. Hollowood", "K. Honscheid", "D. J. James", "T. Jeltema", "N. Kuropatkin", "T. S. Li", "M. Lima", "M. A. G. Maia", "P. Martini", "F. Menanteau", "R. L. C. Ogando", "A. A. Plazas", "A. Roodman", "E. Sanchez", "V. Scarpine", "R. Schindler", "R. C. Smith", "M. Soares-Santos", "F. Sobreira", "E. Suchyta", "M. E. C. Swanson", "G. Tarle", "D. L. Tucker", "A. R. Walker"]}, "266": {"id": "1210.2727v1", "title": "A blind HI survey in the Ursa Major region", "url": "http://arxiv.org/pdf/1210.2727v1", "date": "2012-10-09 20:00:05", "abs": "We have conducted the first blind HI survey covering 480 deg^2 and a\nheliocentric velocity range from 300-1900 km/s to investigate the HI content of\nthe nearby spiral-rich Ursa Major region and to look for previously\nuncatalogued gas-rich objects. Here we present the catalog of HI sources. The\nHI data were obtained with the 4-beam receiver mounted on the 76.2-m Lovell\ntelescope (FWHM 12 arcmin) at the Jodrell Bank Observatory (UK) as part of the\nHI Jodrell All Sky Survey (HIJASS). We use the automated source finder DUCHAMP\nand identify 166 HI sources in the data cubes with HI masses in the range of\n10^7 - 10^{10.5} M_sun. Our Ursa Major HI catalogue includes 10 first time\ndetections in the 21-cm emission line.\n We identify optical counterparts for 165 HI sources (99 per cent). For 54 HI\nsources (33 per cent) we find numerous optical counterparts in the HIJASS beam,\nindicating a high density of galaxies and likely tidal interactions. Four of\nthese HI systems are discussed in detail.\n We find only one HI source (1 per cent) without a visible optical counterpart\nout of the 166 HI detections. Green Bank Telescope (FWHM 9 arcmin) follow-up\nobservations confirmed this HI source and its HI properties. The nature of this\ndetection is discussed and compared to similar sources in other HI surveys.", "cat": "astro-ph.CO", "authors": ["K. Wolfinger", "V. A. Kilborn", "B. S. Koribalski", "R. F. Minchin", "P. J. Boyce", "M. J. Disney", "R. H. Lang", "C. A. Jordan"]}, "267": {"id": "1202.5614v1", "title": "Survey on fusible numbers", "url": "http://arxiv.org/pdf/1202.5614v1", "date": "2012-02-25 05:55:40", "abs": "We point out that the recursive formula that appears in Erickson's\npresentation \"Fusible Numbers\" is incorrect, and pose an alternate conjecture\nabout the structure of fusible numbers. Although we are unable to solve the\nconjecture, we succeed in establishing some basic properties of fusible\nnumbers. We suggest some possible approaches to the conjecture, and list\nfurther problems in the final chapter.", "cat": "math.CO", "authors": ["Junyan Xu"]}, "268": {"id": "2204.01855v2", "title": "A Survey on Graph Representation Learning Methods", "url": "http://arxiv.org/pdf/2204.01855v2", "date": "2022-06-15 17:26:31", "abs": "Graphs representation learning has been a very active research area in recent\nyears. The goal of graph representation learning is to generate graph\nrepresentation vectors that capture the structure and features of large graphs\naccurately. This is especially important because the quality of the graph\nrepresentation vectors will affect the performance of these vectors in\ndownstream tasks such as node classification, link prediction and anomaly\ndetection. Many techniques are proposed for generating effective graph\nrepresentation vectors. Two of the most prevalent categories of graph\nrepresentation learning are graph embedding methods without using graph neural\nnets (GNN), which we denote as non-GNN based graph embedding methods, and graph\nneural nets (GNN) based methods. Non-GNN graph embedding methods are based on\ntechniques such as random walks, temporal point processes and neural network\nlearning methods. GNN-based methods, on the other hand, are the application of\ndeep learning on graph data. In this survey, we provide an overview of these\ntwo categories and cover the current state-of-the-art methods for both static\nand dynamic graphs. Finally, we explore some open and ongoing research\ndirections for future work.", "cat": "cs.LG", "authors": ["Shima Khoshraftar", "Aijun An"]}, "269": {"id": "2307.09990v2", "title": "Fluctuation-induced Interactions in Micro- and Nano-systems: Survey of Some Basic Results", "url": "http://arxiv.org/pdf/2307.09990v2", "date": "2023-07-27 21:11:00", "abs": "On the examples of the quantum-electrodynamical Casimir force, as well as\ncritical Casimir and Helmholtz forces, we present a review of some results\navailable for the class of fluctuation induced forces. In addition, we also\nconcisely present examples of other such fluctuation-induced forces. On the\ninstance of the Ising model we discuss the connection between the Casimir and\nHelmholtz forces. We discuss the importance of the presented results for the\nnanotechnology, and especially for devising micro- or nano-systems, and for\ntheir assembly. Some important problems for the nanotechnology, following from\nthe currently available experimental findings, are spelled out and possible\nstrategies for their overcoming are outlined.", "cat": "cond-mat.stat-mech", "authors": ["Daniel Dantchev"]}, "270": {"id": "1908.03669v1", "title": "A Survey of Tuning Parameter Selection for High-dimensional Regression", "url": "http://arxiv.org/pdf/1908.03669v1", "date": "2019-08-10 02:22:42", "abs": "Penalized (or regularized) regression, as represented by Lasso and its\nvariants, has become a standard technique for analyzing high-dimensional data\nwhen the number of variables substantially exceeds the sample size. The\nperformance of penalized regression relies crucially on the choice of the\ntuning parameter, which determines the amount of regularization and hence the\nsparsity level of the fitted model. The optimal choice of tuning parameter\ndepends on both the structure of the design matrix and the unknown random error\ndistribution (variance, tail behavior, etc). This article reviews the current\nliterature of tuning parameter selection for high-dimensional regression from\nboth theoretical and practical perspectives. We discuss various strategies that\nchoose the tuning parameter to achieve prediction accuracy or support recovery.\nWe also review several recently proposed methods for tuning-free\nhigh-dimensional regression.", "cat": "stat.ME", "authors": ["Yunan Wu", "Lan Wang"]}, "271": {"id": "2007.06197v1", "title": "The Betti side of the double shuffle theory: a survey", "url": "http://arxiv.org/pdf/2007.06197v1", "date": "2020-07-13 05:28:28", "abs": "This is a survey of arXiv:1803.10151v4, arXiv:1807.07786v2 and\narXiv:1908.00444v2 by H. Furusho and the author. The purpose of this series of\npapers is: (1) to give a proof that associator relations imply double shuffle\nrelations, alternative to Furusho's paper arXiv:0808.0319v3; (2) to make\nexplicit the bitorsor structure on Racinet's torsor of double shuffle\nrelations. The main tool is the interpretation of the harmonic coproduct in\nterms of the topology of the moduli spaces $\\mathfrak M_{0,4}$ and $\\mathfrak\nM_{0,5}$, introduced in Deligne and Terasoma's 2005 preprint, and its extension\nto the Betti setup.", "cat": "math.AG", "authors": ["Benjamin Enriquez"]}, "272": {"id": "1309.0781v1", "title": "An Exploratory Data Survey of Drug Name Incidence and Prevalence From the FDA's Adverse Event Reporting System, 2004 to 2012Q2", "url": "http://arxiv.org/pdf/1309.0781v1", "date": "2013-08-31 01:09:23", "abs": "Drug Names, Population Level Surveillance and the FDA's Adverse Event\nReporting System: An Exploratory Data Survey of Drug Name Incidence and\nPrevalence, 2004-2012Q2 Purpose: To count and monitor the drug names reported\nin the publicly available version of the Federal Adverse Event Reporting System\n(FAERS) from 2004 to 2012Q2 in a maximized sensitivity relational model.\nMethods: Data mining and data modeling was conducted and event based summary\nstatistics with plots were created from over nine continuous years of\ncontinuous FAERS data. Results: This FAERS model contains 344,452 individual\ndrug names and 432,541,994 count references which occurred across 4,148,761\nhuman subjects in the 34 quarter study period. Plots for the top 100 scoring\ndrug name references are reported by year and quarter; the top 100 drug names\ncontain 143,384,240 references or 33% of all drug name references over 34\nquarters of continuous FAERS data. Conclusions: While FAERS contains many drugs\nand adverse event reports, its data pertains to very few of them. Drug name\nincidence lends timely and effective surveillance of large populations of\nAverse Event Reports and does not require the cause of the AE, nor its validity\nto be known to detect a mass poisoning.", "cat": "cs.CE", "authors": ["Nick Williams"]}, "273": {"id": "2401.12025v3", "title": "A Survey of Recent Advances in Optimization Methods for Wireless Communications", "url": "http://arxiv.org/pdf/2401.12025v3", "date": "2024-06-07 08:41:19", "abs": "Mathematical optimization is now widely regarded as an indispensable modeling\nand solution tool for the design of wireless communications systems. While\noptimization has played a significant role in the revolutionary progress in\nwireless communication and networking technologies from 1G to 5G and onto the\nfuture 6G, the innovations in wireless technologies have also substantially\ntransformed the nature of the underlying mathematical optimization problems\nupon which the system designs are based and have sparked significant\ninnovations in the development of methodologies to understand, to analyze, and\nto solve those problems. In this paper, we provide a comprehensive survey of\nrecent advances in mathematical optimization theory and algorithms for wireless\ncommunication system design. We begin by illustrating common features of\nmathematical optimization problems arising in wireless communication system\ndesign. We discuss various scenarios and use cases and their associated\nmathematical structures from an optimization perspective. We then provide an\noverview of recently developed optimization techniques in areas ranging from\nnonconvex optimization, global optimization, and integer programming, to\ndistributed optimization and learning-based optimization. The key to successful\nsolution of mathematical optimization problems is in carefully choosing or\ndeveloping suitable algorithms (or neural network architectures) that can\nexploit the underlying problem structure. We conclude the paper by identifying\nseveral open research challenges and outlining future research directions.", "cat": "cs.IT", "authors": ["Ya-Feng Liu", "Tsung-Hui Chang", "Mingyi Hong", "Zheyu Wu", "Anthony Man-Cho So", "Eduard A. Jorswieck", "Wei Yu"]}, "274": {"id": "1602.03894v2", "title": "The Sloan Digital Sky Survey Reverberation Mapping Project: Velocity Shifts of Quasar Emission Lines", "url": "http://arxiv.org/pdf/1602.03894v2", "date": "2016-12-06 20:30:39", "abs": "Quasar emission lines are often shifted from the systemic velocity due to\nvarious dynamical and radiative processes in the line-emitting region. The\nlevel of these velocity shifts depends both on the line species and on quasar\nproperties. We study velocity shifts for the line peaks of various narrow and\nbroad quasar emission lines relative to systemic using a sample of 849 quasars\nfrom the Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project. The\ncoadded (from 32 epochs) spectra of individual quasars have sufficient\nsignal-to-noise ratio (SNR) to measure stellar absorption lines to provide\nreliable systemic velocity estimates, as well as weak narrow emission lines.\nThe sample also covers a large dynamic range in quasar luminosity (~2 dex),\nallowing us to explore potential luminosity dependence of the velocity shifts.\nWe derive average line peak velocity shifts as a function of quasar luminosity\nfor different lines, and quantify their intrinsic scatter. We further quantify\nhow well the peak velocity can be measured for various lines as a function of\ncontinuum SNR, and demonstrate there is no systematic bias in the line peak\nmeasurements when the spectral quality is degraded to as low as SNR~3 per SDSS\npixel. Based on the observed line shifts, we provide empirical guidelines on\nredshift estimation from [OII]3728, [OIII]5008, [NeV]3426, MgII, CIII],\nHeII1640, broad Hbeta, CIV, and SiIV, which are calibrated to provide unbiased\nsystemic redshifts in the mean, but with increasing intrinsic uncertainties of\n46, 56, 119, 205, 233, 242, 400, 415, and 477 km/s, in addition to the\nmeasurement uncertainties. These more realistic redshift uncertainties are\ngenerally much larger than the formal uncertainties reported by the redshift\npipelines for spectroscopic quasar surveys, and demonstrate the infeasibility\nof measuring quasar redshifts to better than ~200 km/s with only broad lines.", "cat": "astro-ph.GA", "authors": ["Yue Shen", "W. N. Brandt", "Gordon T. Richards", "Kelly D. Denney", "Jenny E. Greene", "C. J. Grier", "Luis C. Ho", "Bradley M. Peterson", "Patrick Petitjean", "Donald P. Schneider", "Charling Tao", "Jonathan R. Trump"]}, "275": {"id": "1906.02989v2", "title": "Learning Representations of Graph Data -- A Survey", "url": "http://arxiv.org/pdf/1906.02989v2", "date": "2019-07-01 16:26:01", "abs": "Deep Neural Networks have shown tremendous success in the area of object\nrecognition, image classification and natural language processing. However,\ndesigning optimal Neural Network architectures that can learn and output\narbitrary graphs is an ongoing research problem. The objective of this survey\nis to summarize and discuss the latest advances in methods to Learn\nRepresentations of Graph Data. We start by identifying commonly used types of\ngraph data and review basics of graph theory. This is followed by a discussion\nof the relationships between graph kernel methods and neural networks. Next we\nidentify the major approaches used for learning representations of graph data\nnamely: Kernel approaches, Convolutional approaches, Graph neural networks\napproaches, Graph embedding approaches and Probabilistic approaches. A variety\nof methods under each of the approaches are discussed and the survey is\nconcluded with a brief discussion of the future of learning representation of\ngraph data.", "cat": "cs.LG", "authors": ["Mital Kinderkhedia"]}, "276": {"id": "1004.2790v2", "title": "The XMM-Newton Wide-Field Survey in the COSMOS field (XMM-COSMOS): demography and multiwavelength properties of obscured and unobscured luminous AGN", "url": "http://arxiv.org/pdf/1004.2790v2", "date": "2010-04-20 12:50:10", "abs": "We report the final optical identifications of the medium-depth (~60 ksec),\ncontiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has\ndetected ~800 X-ray sources down to limiting fluxes of ~5x10^{-16},\n~3x10^{-15}, and ~7x10^{-15} erg/cm2/s in the 0.5-2 keV, 2-10 keV and 5-10 keV\nbands, respectively. The work is complemented by an extensive collection of\nmulti-wavelength data from 24 micron to UV, available from the COSMOS survey,\nfor each of the X-ray sources, including spectroscopic redshifts for ~50% of\nthe sample, and high-quality photometric redshifts for the rest. The XMM and\nmultiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources\nhave optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%)\nhave MIPS 24micron detections. Thanks to the redshift completeness (almost\n100%) we were able to constrain the high-luminosity tail of the X-ray\nluminosity function confirming that the peak of the number density of\nlogL_X>44.5 AGN is at z~2. Spectroscopically-identified obscured and unobscured\nAGN, as well as normal and starforming galaxies, present well-defined optical\nand infrared properties. We devised a robust method to identify a sample of\n~150 high redshift (z>1), obscured AGN candidates for which optical\nspectroscopy is not available. We were able to determine that the fraction of\nthe obscured AGN population at the highest (L_X>10^{44} erg s^{-1}) X-ray\nluminosity is ~15-30% when selection effects are taken into account, providing\nan important observational constraint for X-ray background synthesis. We\nstudied in detail the optical spectrum and the overall spectral energy\ndistribution of a prototypical Type 2 QSO, caught in a stage transitioning from\nbeing starburst dominated to AGN dominated, which was possible to isolate only\nthanks to the combination of X-ray and infrared observations.", "cat": "astro-ph.CO", "authors": ["M. Brusa", "F. Civano", "A. Comastri", "T. Miyaji", "M. Salvato", "G. Zamorani", "N. Cappelluti", "F. Fiore", "G. Hasinger", "V. Mainieri", "A. Merloni", "A. Bongiorno", "P. Capak", "M. Elvis", "R. Gilli", "H. Hao", "K. Jahnke", "A. M. Koekemoer", "O. Ilbert", "E. Le Floc'h", "E. Lusso", "M. Mignoli", "E. Schinnerer", "J. D. Silverman", "E. Treister", "J. D. Trump", "C. Vignali", "M. Zamojski", "T. Aldcroft", "H. Aussel", "S. Bardelli", "M. Bolzonella", "A. Cappi", "K. Caputi", "T. Contini", "A. Finoguenov", "A. Fruscione", "B. Garilli", "C. D. Impey", "A. Iovino", "K. Iwasawa", "P. Kampczyk", "J. Kartaltepe", "J. P. Kneib", "C. Knobel", "K. Kovac", "F. Lamareille", "J-F. Leborgne", "V. Le Brun", "O. Le Fevre", "S. J. Lilly", "C. Maier", "H. J. McCracken", "R. Pello", "Y-J Peng", "E. Perez-Montero", "L. de Ravel", "D. Sanders", "M. Scodeggio", "N. Z. Scoville", "M. Tanaka", "Y. Taniguchi", "L. Tasca", "S. de la Torre", "L. Tresse", "D. Vergani", "E. Zucca"]}, "277": {"id": "1812.09449v3", "title": "A Survey on Deep Learning for Named Entity Recognition", "url": "http://arxiv.org/pdf/1812.09449v3", "date": "2020-03-18 15:57:10", "abs": "Named entity recognition (NER) is the task to identify mentions of rigid\ndesignators from text belonging to predefined semantic types such as person,\nlocation, organization etc. NER always serves as the foundation for many\nnatural language applications such as question answering, text summarization,\nand machine translation. Early NER systems got a huge success in achieving good\nperformance with the cost of human engineering in designing domain-specific\nfeatures and rules. In recent years, deep learning, empowered by continuous\nreal-valued vector representations and semantic composition through nonlinear\nprocessing, has been employed in NER systems, yielding stat-of-the-art\nperformance. In this paper, we provide a comprehensive review on existing deep\nlearning techniques for NER. We first introduce NER resources, including tagged\nNER corpora and off-the-shelf NER tools. Then, we systematically categorize\nexisting works based on a taxonomy along three axes: distributed\nrepresentations for input, context encoder, and tag decoder. Next, we survey\nthe most representative methods for recent applied techniques of deep learning\nin new NER problem settings and applications. Finally, we present readers with\nthe challenges faced by NER systems and outline future directions in this area.", "cat": "cs.CL", "authors": ["Jing Li", "Aixin Sun", "Jianglei Han", "Chenliang Li"]}, "278": {"id": "2201.06953v1", "title": "Knowledge Tracing: A Survey", "url": "http://arxiv.org/pdf/2201.06953v1", "date": "2022-01-08 13:59:48", "abs": "Humans ability to transfer knowledge through teaching is one of the essential\naspects for human intelligence. A human teacher can track the knowledge of\nstudents to customize the teaching on students needs. With the rise of online\neducation platforms, there is a similar need for machines to track the\nknowledge of students and tailor their learning experience. This is known as\nthe Knowledge Tracing (KT) problem in the literature. Effectively solving the\nKT problem would unlock the potential of computer-aided education applications\nsuch as intelligent tutoring systems, curriculum learning, and learning\nmaterials' recommendation. Moreover, from a more general viewpoint, a student\nmay represent any kind of intelligent agents including both human and\nartificial agents. Thus, the potential of KT can be extended to any machine\nteaching application scenarios which seek for customizing the learning\nexperience for a student agent (i.e., a machine learning model). In this paper,\nwe provide a comprehensive and systematic review for the KT literature. We\ncover a broad range of methods starting from the early attempts to the recent\nstate-of-the-art methods using deep learning, while highlighting the\ntheoretical aspects of models and the characteristics of benchmark datasets.\nBesides these, we shed light on key modelling differences between closely\nrelated methods and summarize them in an easy-to-understand format. Finally, we\ndiscuss current research gaps in the KT literature and possible future research\nand application directions.", "cat": "cs.CY", "authors": ["Ghodai Abdelrahman", "Qing Wang", "Bernardo Pereira Nunes"]}, "279": {"id": "1411.6724v2", "title": "Dust Content, Galaxy Orientations, and Shape Noise in Imaging Surveys", "url": "http://arxiv.org/pdf/1411.6724v2", "date": "2015-06-10 07:09:00", "abs": "We show that dust absorption in disk galaxies leads to a color- and\norientation-dependent centroid shift which is expected to be observable in\nmulti-band imaging surveys. This centroid shift is an interesting new probe\nwhich contains astrophysically and cosmologically relevant information: it can\nbe used to probe the dust content of a large sample of galaxies, and to reduce\nthe shape noise due to inclination of disk galaxies for weak lensing shear.\nSpecifically, we find that data sets comparable to CFHTLenS, the Dark Energy\nSurvey (DES) or the Hyper Suprime-Cam (HSC) survey should provide a dust\nmeasurement for several hundred galaxies per square degree. Conversely, given\nknowledge of the dust optical depth, this technique will significantly lower\nthe shape noise for the brightest galaxies in the sample (signal-to-noise\ngreater than a few hundred), thereby increasing their relative importance for\nthe weak lensing shear measurement.", "cat": "astro-ph.CO", "authors": ["Petchara Pattarakijwanich", "Fabian Schmidt"]}, "280": {"id": "1707.08123v1", "title": "BAT AGN Spectroscopic Survey I: Spectral Measurements, Derived Quantities, and AGN Demographics", "url": "http://arxiv.org/pdf/1707.08123v1", "date": "2017-07-25 18:00:02", "abs": "We present the first catalog and data release of the Swift-BAT AGN\nSpectroscopic Survey (BASS). We analyze optical spectra of the majority of AGN\n(77%, 641/836) detected based on their 14-195 keV emission in the 70-month\nSwift BAT all-sky catalog. This includes redshift determination, absorption and\nemission line measurements, and black hole mass and accretion rate estimates\nfor the majority of obscured and un-obscured AGN (74%, 473/641) with 340\nmeasured for the first time. With ~90% of sources at z<0.2, the survey\nrepresents a significant census of hard-X-ray selected AGN in the local\nuniverse. In this first catalog paper, we describe the spectroscopic\nobservations and datasets, and our initial spectral analysis. The FWHM of the\nemission lines show broad agreement with the X-ray obscuration (~94%), such\nthat Sy 1-1.8 have NH<10^21.9 cm^-2, and Seyfert 2, have NH>10^21.9 cm^-2.\nSeyfert 1.9 show a range of column densities. Compared to narrow line AGN in\nthe SDSS, the X-ray selected AGN have a larger fraction of dusty host galaxies\nsuggesting these types of AGN are missed in optical surveys. Using the most\nsensitive [OIII]/Hbeta and [NII]/Halpha emission line diagnostic, about half of\nthe sources are classified as Seyferts, ~15% reside in dusty galaxies that lack\nan Hbeta detection, but for which the line upper limits imply either a Seyfert\nor LINER, ~15% are in galaxies with weak or no emission lines despite high\nquality spectra, and a few percent each are LINERS, composite galaxies, HII\nregions, or in known beamed AGN.", "cat": "astro-ph.HE", "authors": ["Michael Koss", "Benny Trakhtenbrot", "Claudio Ricci", "Isabella Lamperti", "Kyuseok Oh", "Simon Berney", "Kevin Schawinski", "Mislav Balokovic", "Linda Baronchelli", "D. Michael Crenshaw", "Travis Fischer", "Neil Gehrels", "Fiona Harrison", "Yasuhiro Hashimoto", "Drew Hogg", "Kohei Ichikawa", "Nicola Masetti", "Richard Mushotzky", "Daniel Stern", "Ezequiel Treister", "Yoshihiro Ueda", "Sylvain Veilleux", "Lisa Winter"]}, "281": {"id": "1108.4011v1", "title": "The ALFALFA HI Absorption Pilot Survey: A Wide-Area Blind Damped Lyman Alpha System Survey of the Local Universe", "url": "http://arxiv.org/pdf/1108.4011v1", "date": "2011-08-19 17:18:32", "abs": "We present the results of a pilot survey for neutral hydrogen (HI) 21 cm\nabsorption in the Arecibo Legacy Fast Arecibo L-Band Feed Array (ALFALFA)\nSurvey. This project is a wide-area \"blind\" search for HI absorption in the\nlocal universe, spanning -650 km/s < cz < 17,500 km/s and covering 517.0 square\ndegrees (7% of the full ALFALFA survey). The survey is sensitive to HI\nabsorption lines stronger than 7.7 mJy (8983 radio sources) and is 90% complete\nfor lines stronger than 11.0 mJy (7296 sources). The total redshift interval\nsensitive to all damped Lyman alpha (DLA) systems (N_HI >= 2x10^20 cm^-2) is\nDelta z = 7.0 (129 objects, assuming T_s = 100 K and covering fraction unity);\nfor super-DLAs (N_HI >= 2x10^21 cm^-2) it is Delta z= 128.2 (2353 objects). We\nre-detect the intrinsic HI absorption line in UGC 6081 but detect no\nintervening absorption line systems. We compute a 95% confidence upper limit on\nthe column density frequency distribution function f(N_HI,X) spanning four\norders of magnitude in column density, 10^19 (T_s/100 K)(1/f) cm^-2 < N_HI <\n10^23 (T_s/100 K)(1/f) cm^-2, that is consistent with previous redshifted\noptical damped Ly alpha surveys and the aggregate HI 21 cm emission in the\nlocal universe. The detection rate is in agreement with extant observations.\nThis pilot survey suggests that an absorption line search of the complete\nALFALFA survey --- or any higher redshift, larger bandwidth, or more sensitive\nsurvey, such as those planned for Square Kilometer Array pathfinders or a low\nfrequency lunar array --- will either make numerous detections or will set a\nstrong statistical lower limit on the typical spin temperature of neutral\nhydrogen gas.", "cat": "astro-ph.CO", "authors": ["Jeremy Darling", "Erin P. Macdonald", "Martha P. Haynes", "Riccardo Giovanelli"]}, "282": {"id": "1903.12099v1", "title": "Recommendation Systems for Tourism Based on Social Networks: A Survey", "url": "http://arxiv.org/pdf/1903.12099v1", "date": "2019-03-28 16:33:18", "abs": "Nowadays, recommender systems are present in many daily activities such as\nonline shopping, browsing social networks, etc. Given the rising demand for\nreinvigoration of the tourist industry through information technology,\nrecommenders have been included into tourism websites such as Expedia, Booking\nor Tripadvisor, among others. Furthermore, the amount of scientific papers\nrelated to recommender systems for tourism is on solid and continuous growth\nsince 2004. Much of this growth is due to social networks that, besides to\noffer researchers the possibility of using a great mass of available and\nconstantly updated data, they also enable the recommendation systems to become\nmore personalised, effective and natural. This paper reviews and analyses many\nresearch publications focusing on tourism recommender systems that use social\nnetworks in their projects. We detail their main characteristics, like which\nsocial networks are exploited, which data is extracted, the applied\nrecommendation techniques, the methods of evaluation, etc. Through a\ncomprehensive literature review, we aim to collaborate with the future\nrecommender systems, by giving some clear classifications and descriptions of\nthe current tourism recommender systems.", "cat": "cs.IR", "authors": ["Alan Menk", "Laura Sebastia", "Rebeca Ferreira"]}, "283": {"id": "1104.2000v2", "title": "A survey of test ideals", "url": "http://arxiv.org/pdf/1104.2000v2", "date": "2011-07-30 19:33:10", "abs": "Test ideals were first introduced by Mel Hochster and Craig Huneke in their\ncelebrated theory of tight closure, and since their invention have been closely\ntied to the theory of Frobenius splittings. Subsequently, test ideals have also\nfound application far beyond their original scope to questions arising in\ncomplex analytic geometry. In this paper we give a contemporary survey of test\nideals and their wide-ranging applications.", "cat": "math.AG", "authors": ["Karl Schwede", "Kevin Tucker"]}, "284": {"id": "1104.3244v1", "title": "The Physical Nature of Five-Dimensional Solutions: A Survey", "url": "http://arxiv.org/pdf/1104.3244v1", "date": "2011-04-16 14:50:38", "abs": "The basic quasi-Schwarzschild 5D objects known as solitons have a long\nhistory, which is reviewed. Then some material is added, leading to the\ninference that a soliton is a singularity in the geometry which represents a\nbivalent source of gravitational and scalar mass.", "cat": "gr-qc", "authors": ["Paul S. Wesson"]}, "285": {"id": "1706.06204v3", "title": "The California-Kepler Survey V. Peas in a Pod: Planets in a Kepler Multi-planet System are Similar in Size and Regularly Spaced", "url": "http://arxiv.org/pdf/1706.06204v3", "date": "2018-02-07 15:26:12", "abs": "We have established precise planet radii, semimajor axes, incident stellar\nfluxes, and stellar masses for 909 planets in 355 multi-planet systems\ndiscovered by Kepler. In this sample, we find that planets within a single\nmulti-planet system have correlated sizes: each planet is more likely to be the\nsize of its neighbor than a size drawn at random from the distribution of\nobserved planet sizes. In systems with three or more planets, the planets tend\nto have a regular spacing: the orbital period ratios of adjacent pairs of\nplanets are correlated. Furthermore, the orbital period ratios are smaller in\nsystems with smaller planets, suggesting that the patterns in planet sizes and\nspacing are linked through formation and/or subsequent orbital dynamics. Yet,\nwe find that essentially no planets have orbital period ratios smaller than\n$1.2$, regardless of planet size. Using empirical mass-radius relationships, we\nestimate the mutual Hill separations of planet pairs. We find that $93\\%$ of\nthe planet pairs are at least 10 mutual Hill radii apart, and that a spacing of\n$\\sim20$ mutual Hill radii is most common. We also find that when comparing\nplanet sizes, the outer planet is larger in $65 \\pm 0.4\\%$ of cases, and the\ntypical ratio of the outer to inner planet size is positively correlated with\nthe temperature difference between the planets. This could be the result of\nphoto-evaporation.", "cat": "astro-ph.EP", "authors": ["Lauren M. Weiss", "Geoffrey W. Marcy", "Erik A. Petigura", "Benjamin J. Fulton", "Andrew W. Howard", "Joshua N. Winn", "Howard T. Isaacson", "Timothy D. Morton", "Lea A. Hirsch", "Evan J. Sinukoff", "Andrew Cumming", "Leslie Hebb", "Phillip A. Cargile"]}, "286": {"id": "1708.05866v2", "title": "A Brief Survey of Deep Reinforcement Learning", "url": "http://arxiv.org/pdf/1708.05866v2", "date": "2017-09-28 21:51:43", "abs": "Deep reinforcement learning is poised to revolutionise the field of AI and\nrepresents a step towards building autonomous systems with a higher level\nunderstanding of the visual world. Currently, deep learning is enabling\nreinforcement learning to scale to problems that were previously intractable,\nsuch as learning to play video games directly from pixels. Deep reinforcement\nlearning algorithms are also applied to robotics, allowing control policies for\nrobots to be learned directly from camera inputs in the real world. In this\nsurvey, we begin with an introduction to the general field of reinforcement\nlearning, then progress to the main streams of value-based and policy-based\nmethods. Our survey will cover central algorithms in deep reinforcement\nlearning, including the deep $Q$-network, trust region policy optimisation, and\nasynchronous advantage actor-critic. In parallel, we highlight the unique\nadvantages of deep neural networks, focusing on visual understanding via\nreinforcement learning. To conclude, we describe several current areas of\nresearch within the field.", "cat": "cs.LG", "authors": ["Kai Arulkumaran", "Marc Peter Deisenroth", "Miles Brundage", "Anil Anthony Bharath"]}, "287": {"id": "1612.04748v3", "title": "Linear feature detection algorithm for astronomical surveys - I. Algorithm description", "url": "http://arxiv.org/pdf/1612.04748v3", "date": "2017-06-18 10:08:45", "abs": "Computer vision algorithms are powerful tools in astronomical image analyses,\nespecially when automation of object detection and extraction is required.\nModern object detection algorithms in astronomy are oriented towards detection\nof stars and galaxies, ignoring completely detection of existing linear\nfeatures. With the emergence of wide-field sky surveys, linear features attract\nscientific interest as possible trails of fast flybys of near-Earth asteroids\nand meteors. In this work we describe a new linear feature detection algorithm\ndesigned specifically for implementation in Big Data astronomy. The algorithm\ncombines a series of algorithmic steps that first remove other objects (stars,\ngalaxies) from the image and then enhance the line to enable more efficient\nline detection with the Hough algorithm. The rate of false positives is greatly\nreduced thanks to a step that replaces possible line segments with rectangles\nand then compares lines fitted to the rectangles with the lines obtained\ndirectly from the image. The speed of the algorithm and its applicability in\nastronomical surveys are also discussed.", "cat": "astro-ph.IM", "authors": ["Dino Bekte\u0161evi\u0107", "Dejan Vinkovi\u0107"]}, "288": {"id": "1703.02985v3", "title": "First Results from the Lyman Alpha Galaxies in the Epoch of Reionization (LAGER) Survey: Cosmological Reionization at z ~ 7", "url": "http://arxiv.org/pdf/1703.02985v3", "date": "2017-06-14 13:39:12", "abs": "We present the first results from the ongoing LAGER project (Lyman Alpha\nGalaxies in the Epoch of Reionization), which is the largest narrowband survey\nfor $z \\sim$ 7 galaxies to date. Using a specially built narrowband filter\nNB964 for the superb large-area Dark-Energy Camera (DECam) on the NOAO/CTIO 4m\nBlanco telescope, LAGER has collected 34 hours NB964 narrowband imaging data in\nthe 3 deg$^2$ COSMOS field. We have identified 23 Lyman Alpha Emitter (LAE)\ncandidates at $z$ = 6.9 in the central 2-deg$^2$ region, where DECam and public\nCOSMOS multi-band images exist. The resulting luminosity function can be\ndescribed as a Schechter function modified by a significant excess at the\nbright end (4 galaxies with $L_{Ly\\alpha} \\sim $ 10$^{43.4\\pm0.2}$ erg\ns$^{-1}$). The number density at $L_{Ly\\alpha}\\sim$ 10$^{43.4\\pm0.2}$ erg\ns$^{-1}$ is little changed from z= 6.6, while at fainter $L_{Ly\\alpha}$ it is\nsubstantially reduced. Overall, we see a fourfold reduction in Ly$\\alpha$\nluminosity density from $z$ = 5.7 to 6.9. Combined with a more modest evolution\nof the continuum UV luminosity density, this suggests a factor of $\\sim 3$\nsuppression of Ly$\\alpha$ by radiative transfer through the $z \\sim$ 7\nintergalactic medium (IGM). It indicates an IGM neutral fraction $x_{HI}$\n$\\sim$ 0.4--0.6 (assuming Ly$\\alpha$ velocity offsets of 100-200 km s$^{-1}$).\nThe changing shape of the Ly$\\alpha$ luminosity function between $z\\lesssim\n6.6$ and $z=6.9$ supports the hypothesis of ionized bubbles in a patchy\nreionization at $z\\sim$ 7.", "cat": "astro-ph.GA", "authors": ["Zhen-Ya Zheng", "Junxian Wang", "James Rhoads", "Leopoldo Infante", "Sangeeta Malhotra", "Weida Hu", "Alistair R. Walker", "Linhua Jiang", "Chunyan Jiang", "Pascale Hibon", "Alicia Gonzalez", "Xu Kong", "Xianzhong Zheng", "Gaspar Galaz", "L. Felipe Barrientos"]}, "289": {"id": "2101.09371v1", "title": "The TESS-Keck Survey IV: A Retrograde, Polar Orbit for the Ultra-Low-Density, Hot Super-Neptune WASP-107b", "url": "http://arxiv.org/pdf/2101.09371v1", "date": "2021-01-22 22:44:43", "abs": "We measured the Rossiter-McLaughlin effect of WASP-107b during a single\ntransit with Keck/HIRES. We found the sky-projected inclination of WASP-107b's\norbit, relative to its host star's rotation axis, to be $|\\lambda| =\n{118}^{+38}_{-19}$ degrees. This confirms the misaligned/polar orbit that was\npreviously suggested from spot-crossing events and adds WASP-107b to the\ngrowing population of hot Neptunes in polar orbits around cool stars. WASP-107b\nis also the fourth such planet to have a known distant planetary companion. We\nexamined several dynamical pathways by which this companion could have induced\nsuch an obliquity in WASP-107b. We find that nodal precession and disk\ndispersal-driven tilting can both explain the current orbital geometry while\nKozai-Lidov cycles are suppressed by general relativity. While each hypothesis\nrequires a mutual inclination between the two planets, nodal precession\nrequires a much larger angle which for WASP-107 is on the threshold of\ndetectability with future Gaia astrometric data. As nodal precession has no\nstellar type dependence, but disk dispersal-driven tilting does, distinguishing\nbetween these two models is best done on the population level. Finding and\ncharacterizing more extrasolar systems like WASP-107 will additionally help\ndistinguish whether the distribution of hot-Neptune obliquities is a dichotomy\nof aligned and polar orbits or if we are uniformly sampling obliquities during\nnodal precession cycles.", "cat": "astro-ph.EP", "authors": ["Ryan A. Rubenzahl", "Fei Dai", "Andrew W. Howard", "Ashley Chontos", "Steven Giacalone", "Jack Lubin", "Lee J. Rosenthal", "Howard Isaacson", "Natalie M. Batalha", "Ian J. M. Crossfield", "Courtney Dressing", "Benjamin Fulton", "Daniel Huber", "Stephen R. Kane", "Erik A Petigura", "Paul Robertson", "Arpita Roy", "Lauren M. Weiss", "Corey Beard", "Michelle L. Hill", "Andrew Mayo", "Teo Mo\u010dnik", "Joseph M. Akana Murphy", "Nicholas Scarsdale"]}, "290": {"id": "2207.06792v2", "title": "The Quasar Candidates Catalogs of DESI Legacy Imaging Survey Data Release 9", "url": "http://arxiv.org/pdf/2207.06792v2", "date": "2022-07-16 02:00:34", "abs": "Quasars can be used to measure baryon acoustic oscillations at high redshift,\nwhich are considered as direct tracers of the most distant large-scale\nstructures in the Universe. It is fundamental to select quasars from\nobservations before implementing the above research. This work focuses on\ncreating a catalog of quasar candidates based on photometric data to provide\nprimary priors for further object classification with spectroscopic data in the\nfuture, such as The Dark Energy Spectroscopic Instrument (DESI) Survey. We\nadopt a machine learning algorithm (Random Forest, RF) for quasar\nidentification. The training set includes $651,073$ positives and $1,227,172$\nnegatives, in which the photometric information are from DESI Legacy Imaging\nSurveys (DESI-LIS) \\& Wide-field Infrared Survey Explore (WISE), and the labels\nare from a database of spectroscopically confirmed quasars based on Sloan\nDigital Sky Survey (SDSS) and the Set of Identifications \\& Measurements and\nBibliography for Astronomical Data (SIMBAD). The trained RF model is applied to\npoint-like sources in DESI-LIS Data Release 9. To quantify the classifier's\nperformance, we also inject a testing set into the to-be-applied data.\nEventually, we obtained $1,953,932$ Grade-A quasar candidates and $22,486, 884$\nGrade-B quasar candidates out of $425,540,269$ sources ($\\sim 5.7\\%$). The\ncatalog covers $\\sim 99\\%$ of quasars in the to-be-applied data by evaluating\nthe completeness of the classification on the testing set. The statistical\nproperties of the candidates agree with that given by the method of color-cut\nselection. Our catalog can intensely decrease the workload for confirming\nquasars with the upcoming DESI data by eliminating enormous non-quasars but\nremaining high completeness. All data in this paper is publicly available\nonline.", "cat": "astro-ph.CO", "authors": ["Zizhao He", "Nan Li"]}, "291": {"id": "1205.4764v1", "title": "A new infrared color criterion for the selection of 0~2.5-3. However, when the\nsource redshift is unknown, these colors should be combined. We thus develop an\nimproved IR criterion (using Ks and IRAC bands, KI) as a new alternative at\nz<~2.5. KI does not show improved completeness (50-60% overall) in comparison\nto commonly used IRAC-based AGN criteria, but is less affected by non-AGN\ncontamination (revealing a >50-90% level of successful AGN selection). We also\npropose KIM (using Ks, IRAC, and MIPS-24um bands, KIM), which aims to select\nAGN hosts from local distances to as far back as the end of reionization\n(070-90% level of successful AGN selection. KI and KIM are built to be\nreliable against a ~10-20% error in flux, are based on existing filters, and\nare suitable for immediate use.", "cat": "astro-ph.CO", "authors": ["Hugo Messias", "Jose M. Afonso", "Mara Salvato", "Bahram Mobasher", "Andrew M. Hopkins"]}, "292": {"id": "1206.2643v2", "title": "A Spectroscopic Study of Type Ibc Supernova Host Galaxies from Untargeted Surveys", "url": "http://arxiv.org/pdf/1206.2643v2", "date": "2012-09-16 20:00:34", "abs": "We present the largest spectroscopic study of the host environments of Type\nIbc supernovae (SN Ibc) discovered exclusively by untargeted SN searches. Past\nstudies of SN Ibc host environments have been biased towards high-mass,\nhigh-metallicity galaxies by focusing on SNe discovered in galaxy-targeted SN\nsearches. Our new observations more than double the total number of\nspectroscopic stellar population age and metallicity measurements published for\nuntargeted SN Ibc host environments, and extend to a median redshift about\ntwice as large as previous statistical studies (z = 0.04). For the 12 SNe Ib\nand 21 SNe Ic in our metallicity sample, we find median metallicities of\nlog(O/H)+12 = 8.48 and 8.61, respectively, but determine that the discrepancy\nin the full distribution of metallicities is not statistically significant.\nThis median difference would correspond to only a small difference in the mass\nloss via metal-line driven winds (<30%), suggesting this does not play the\ndominant role in distinguishing SN Ib and Ic progenitors. However, the median\nmetallicity of the 7 broad-lined SN Ic (SN Ic-BL) in our sample is\nsignificantly lower, log(O/H)+12 = 8.34. The age of the young stellar\npopulation of SN Ic-BL host environments also seems to be lower than for SN Ib\nand Ic, but our age sample is small. A synthesis of SN Ibc host environment\nspectroscopy to date does not reveal a significant difference in SN Ib and Ic\nmetallicities, but reinforces the significance of the lower metallicities for\nSN Ic-BL. This combined sample demonstrates that galaxy-targeted SN searches\nintroduce a significant bias for studies seeking to infer the metallicity\ndistribution of SN progenitors, and we identify and discuss other systematic\neffects that play smaller roles. We discuss the path forward for making\nprogress on SN Ibc progenitor studies in the LSST era.", "cat": "astro-ph.HE", "authors": ["Nathan E. Sanders", "Alicia M. Soderberg", "Emily M. Levesque", "Ryan J. Foley", "Ryan Chornock", "Dan Milisavljevic", "Raffaella Margutti", "Edo Berger", "Maria R. Drout", "Ian Czekala", "Jason A. Dittmann"]}, "293": {"id": "2309.00102v1", "title": "The LOFAR Two-Metre Sky Survey (LoTSS): VI. Optical identifications for the second data release", "url": "http://arxiv.org/pdf/2309.00102v1", "date": "2023-08-31 19:42:01", "abs": "The second data release of the LOFAR Two-Metre Sky Survey (LoTSS) covers 27%\nof the northern sky, with a total area of $\\sim 5,700$ deg$^2$. The high\nangular resolution of LOFAR with Dutch baselines (6 arcsec) allows us to carry\nout optical identifications of a large fraction of the detected radio sources\nwithout further radio followup; however, the process is made more challenging\nby the many extended radio sources found in LOFAR images as a result of its\nexcellent sensitivity to extended structure. In this paper we present source\nassociations and identifications for sources in the second data release based\non optical and near-infrared data, using a combination of a likelihood-ratio\ncross-match method developed for our first data release, our citizen science\nproject Radio Galaxy Zoo: LOFAR, and new approaches to algorithmic optical\nidentification, together with extensive visual inspection by astronomers. We\nalso present spectroscopic or photometric redshifts for a large fraction of the\noptical identifications. In total 4,116,934 radio sources lie in the area with\ngood optical data, of which 85% have an optical or infrared identification and\n58% have a good redshift estimate. We demonstrate the quality of the dataset by\ncomparing it with earlier optically identified radio surveys. This is by far\nthe largest ever optically identified radio catalogue, and will permit robust\nstatistical studies of star-forming and radio-loud active galaxies.", "cat": "astro-ph.GA", "authors": ["M. J. Hardcastle", "M. A. Horton", "W. L. Williams", "K. J. Duncan", "L. Alegre", "B. Barkus", "J. H. Croston", "H. Dickinson", "E. Osinga", "H. J. A. R\u00f6ttgering", "J. Sabater", "T. W. Shimwell", "D. J. B. Smith", "P. N. Best", "A. Botteon", "M. Br\u00fcggen", "A. Drabent", "F. de Gasperin", "G. G\u00fcrkan", "M. Hajduk", "C. L. Hale", "M. Hoeft", "M. Jamrozy", "M. Kunert-Bajraszewska", "R. Kondapally", "M. Magliocchetti", "V. H. Mahatma", "R. I. J. Mostert", "S. P. O'Sullivan", "U. Pajdosz-\u015amierciak", "J. Petley", "J. C. S. Pierce", "I. Prandoni", "D. J. Schwarz", "A. Shulewski", "T. M. Siewert", "J. P. Stott", "H. Tang", "M. Vaccari", "X. Zheng", "T. Bailey", "S. Desbled", "A. Goyal", "V. Gonano", "M. Hanset", "W. Kurtz", "S. M. Lim", "L. Mielle", "C. S. Molloy", "R. Roth", "I. A. Terentev", "M. Torres"]}, "294": {"id": "2204.03265v1", "title": "The OmegaWhite Survey for Short-Period Variable Stars VII: High amplitude, short period blue variables", "url": "http://arxiv.org/pdf/2204.03265v1", "date": "2022-04-07 07:40:24", "abs": "Blue Large Amplitude Pulsators (BLAPs) are a relatively new class of blue\nvariable stars showing periodic variations in their light curves with periods\nshorter than a few tens of mins and amplitudes of more than ten percent. We\nreport nine blue variable stars identified in the OmegaWhite survey conducted\nusing ESO's VST, which show a periodic modulation in the range 7-37 min and an\namplitude in the range 0.11-0.28 mag. We have obtained a series of followup\nphotometric and spectroscopic observations made primarily using SALT and\ntelescopes at SAAO. We find four stars which we identify as BLAPs, one of which\nwas previously known. One star, OW J0820--3301, appears to be a member of the\nV361 Hya class of pulsating stars and is spatially close to an extended nebula.\nOne further star, OW J1819--2729, has characteristics similar to the sdAV\npulsators. In contrast, OW J0815--3421 is a binary star containing an sdB and a\nwhite dwarf with an orbital period of 73.7 min, making it only one of six white\ndwarf-sdB binaries with an orbital period shorter than 80 min. Finally, high\ncadence photometry of four of the candidate BLAPs show features which we\ncompare with notch-like features seen in the much longer period Cepheid\npulsators.", "cat": "astro-ph.SR", "authors": ["G. Ramsay", "P. A. Woudt", "T. Kupfer", "J. van Roestel", "K. Patterson", "B. Warner", "D. A. H. Buckley", "P. J. Groot", "U. Heber", "A. Irrgang", "C. S. Jeffery", "M. Motsoaledi", "M. J. Schwartz", "T. Wevers"]}, "295": {"id": "2403.08319v2", "title": "Knowledge Conflicts for LLMs: A Survey", "url": "http://arxiv.org/pdf/2403.08319v2", "date": "2024-06-22 08:31:40", "abs": "This survey provides an in-depth analysis of knowledge conflicts for large\nlanguage models (LLMs), highlighting the complex challenges they encounter when\nblending contextual and parametric knowledge. Our focus is on three categories\nof knowledge conflicts: context-memory, inter-context, and intra-memory\nconflict. These conflicts can significantly impact the trustworthiness and\nperformance of LLMs, especially in real-world applications where noise and\nmisinformation are common. By categorizing these conflicts, exploring the\ncauses, examining the behaviors of LLMs under such conflicts, and reviewing\navailable solutions, this survey aims to shed light on strategies for improving\nthe robustness of LLMs, thereby serving as a valuable resource for advancing\nresearch in this evolving area.", "cat": "cs.CL", "authors": ["Rongwu Xu", "Zehan Qi", "Zhijiang Guo", "Cunxiang Wang", "Hongru Wang", "Yue Zhang", "Wei Xu"]}, "296": {"id": "2104.14751v1", "title": "A Survey on sentiment analysis in Persian: A Comprehensive System Perspective Covering Challenges and Advances in Resources, and Methods", "url": "http://arxiv.org/pdf/2104.14751v1", "date": "2021-04-30 04:31:21", "abs": "Social media has been remarkably grown during the past few years. Nowadays,\nposting messages on social media websites has become one of the most popular\nInternet activities. The vast amount of user-generated content has made social\nmedia the most extensive data source of public opinion. Sentiment analysis is\none of the techniques used to analyze user-generated data. The Persian language\nhas specific features and thereby requires unique methods and models to be\nadopted for sentiment analysis, which are different from those in English\nlanguage. Sentiment analysis in each language has specified prerequisites;\nhence, the direct use of methods, tools, and resources developed for English\nlanguage in Persian has its limitations. The main target of this paper is to\nprovide a comprehensive literature survey for state-of-the-art advances in\nPersian sentiment analysis. In this regard, the present study aims to\ninvestigate and compare the previous sentiment analysis studies on Persian\ntexts and describe contributions presented in articles published in the last\ndecade. First, the levels, approaches, and tasks for sentiment analysis are\ndescribed. Then, a detailed survey of the sentiment analysis methods used for\nPersian texts is presented, and previous relevant works on Persian Language are\ndiscussed. Moreover, we present in this survey the authentic and published\nstandard sentiment analysis resources and advances that have been done for\nPersian sentiment analysis. Finally, according to the state-of-the-art\ndevelopment of English sentiment analysis, some issues and challenges not being\naddressed in Persian texts are listed, and some guidelines and trends are\nprovided for future research on Persian texts. The paper provides information\nto help new or established researchers in the field as well as industry\ndevelopers who aim to deploy an operational complete sentiment analysis system.", "cat": "cs.CL", "authors": ["Zeinab Rajabi", "MohammadReza Valavi"]}, "297": {"id": "1808.03280v1", "title": "A Giant Metrewave Radio Telescope survey for associated HI 21-cm absorption in the Caltech-Jodrell Flat-spectrum sample", "url": "http://arxiv.org/pdf/1808.03280v1", "date": "2018-08-09 18:00:04", "abs": "We report a Giant Metrewave Radio Telescope (GMRT) survey for associated HI\n21-cm absorption from 50 active galactic nuclei (AGNs), at $z \\approx 0.04 -\n3.01$, selected from the Caltech-Jodrell Bank Flat-spectrum (CJF) sample. Clean\nspectra were obtained towards 40 sources, yielding two new absorption\ndetections, at $z = 0.229$ towards TXS 0003+380 and $z = 0.333$ towards TXS\n1456+375, besides confirming an earlier detection, at $z = 1.277$ towards TXS\n1543+480. There are 92 CJF sources, at $0.01 \\lesssim z \\lesssim 3.6$, with\nsearches for associated HI 21-cm absorption, by far the largest\nuniformly-selected AGN sample with searches for such absorption. We find weak\n($\\approx 2\\sigma$) evidence for a lower detection rate of HI 21-cm absorption\nat high redshifts, with detection rates of $28^{+10}_{-8}$\\% and\n$7^{+6}_{-4}$\\% in the low-$z$ ($z < z_{\\rm med}$) and high-$z$ ($z > z_{\\rm\nmed}$) sub-samples, respectively. We use two-sample tests to find that the\nstrength of the HI 21-cm absorption in the AGNs of our sample depends on both\nredshift and AGN luminosity, with a lower detection rate and weaker absorption\nat high redshifts and high ultraviolet/radio AGN luminosities. Unfortunately,\nthe luminosity bias in our sample, with high-luminosity AGNs arising at high\nredshifts, implies that it is not currently possible to identify whether\nredshift evolution or AGN luminosity is the primary cause of the weaker\nabsorption in high-$z$, high-luminosity AGNs. We find that the strength of HI\n21-cm absorption does not depend on AGN colour, suggesting that dust extinction\nis not the main cause of reddening in the CJF sample.", "cat": "astro-ph.GA", "authors": ["J. N. H. S. Aditya", "Nissim Kanekar"]}, "298": {"id": "2008.08339v1", "title": "A Survey of HTTPS Traffic and Services Identification Approaches", "url": "http://arxiv.org/pdf/2008.08339v1", "date": "2020-08-19 09:04:15", "abs": "HTTPS is quickly rising alongside the need of Internet users to benefit from\nsecurity and privacy when accessing the Web, and it becomes the predominant\napplication protocol on the Internet. This migration towards a secure Web using\nHTTPS comes with important challenges related to the management of HTTPS\ntraffic to guarantee basic network properties such as security, QoS,\nreliability, etc. But encryption undermines the effectiveness of standard\nmonitoring techniques and makes it difficult for ISPs and network\nadministrators to properly identify and manage the services behind HTTPS\ntraffic. This survey details the techniques used to monitor HTTPS traffic, from\nthe most basic level of protocol identification (TLS, HTTPS), to the finest\nidentification of precise services. We show that protocol identification is\nwell mastered while more precise levels keep being challenging despite recent\nadvances. We also describe practical solutions that lead us to discuss the\ntrade-off between security and privacy and the research directions to guarantee\nboth of them.", "cat": "cs.CR", "authors": ["Wazen M. Shbair", "Thibault Cholez", "Jerome Francois", "Isabelle Chrisment"]}, "299": {"id": "2103.15512v2", "title": "A proposal for relative in-flight flux self-calibrations for spectro-photometric surveys", "url": "http://arxiv.org/pdf/2103.15512v2", "date": "2021-06-23 14:29:56", "abs": "We present a method for the in-flight relative flux self-calibration of a\nspectro-photometer instrument, general enough to be applied to any upcoming\ngalaxy survey on satellite. The instrument response function, that accounts for\na smooth continuous variation due to telescope optics, on top of a\ndiscontinuous effect due to the segmentation of the detector, is inferred with\na $\\chi^2$ statistics. The method provides unbiased inference of the sources\ncount rates and of the reconstructed relative response function, in the limit\nof high count rates. We simulate a simplified sequence of observations\nfollowing a spatial random pattern and realistic distributions of sources and\ncount rates, with the purpose of quantifying the relative importance of the\nnumber of sources and exposures for correctly reconstructing the instrument\nresponse. We present a validation of the method, with the definition of figures\nof merit to quantify the expected performance, in plausible scenarios.", "cat": "astro-ph.IM", "authors": ["S. Davini", "I. Risso", "M. Scodeggio", "L. Paganin", "S. Caprioli", "M. Bonici", "A. Caminata", "S. Di Domizio", "G. Testera", "S. Tosi", "B. Valerio", "M. Fumana", "P. Franzetti"]}, "300": {"id": "2205.05517v1", "title": "Groups and protocluster candidates in the CLAUDS and HSC-SSP joint deep surveys", "url": "http://arxiv.org/pdf/2205.05517v1", "date": "2022-05-11 14:08:42", "abs": "Using the extended halo-based group finder developed by Yang et al. (2021),\nwhich is able to deal with galaxies via spectroscopic and photometric redshifts\nsimultaneously, we construct galaxy group and candidate protocluster catalogs\nin a wide redshift range ($0 < z < 6$) from the joint CFHT Large Area $U$-band\nDeep Survey (CLAUDS) and Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP)\ndeep data set. Based on a selection of 5,607,052 galaxies with $i$-band\nmagnitude $m_{i} < 26$ and a sky coverage of $34.41\\ {\\rm deg}^2$, we identify\na total of 2,232,134 groups, within which 402,947 groups have at least three\nmember galaxies. We have visually checked and discussed the general properties\nof those richest groups at redshift $z>2.0$. By checking the galaxy number\ndistributions within a $5-7\\ h^{-1}\\mathrm{Mpc}$ projected separation and a\nredshift difference $\\Delta z \\le 0.1$ around those richest groups at redshift\n$z>2$, we identified a list of 761, 343 and 43 protocluster candidates in the\nredshift bins $2\\leq z<3$, $3\\leq z<4$ and $z \\geq 4$, respectively. In\ngeneral, these catalogs of galaxy groups and protocluster candidates will\nprovide useful environmental information in probing galaxy evolution along the\ncosmic time.", "cat": "astro-ph.CO", "authors": ["Qingyang Li", "Xiaohu Yang", "Chengze Liu", "Yipeng Jing", "Min He", "Jiasheng Huang", "Y. Sophia Dai", "Marcin Sawicki", "Stephane Arnouts", "Stephen Gwyn", "Thibaud Moutard", "H. J. Mo", "Kai Wang", "Antonios Katsianis", "Weiguang Cui", "Jiaxin Han", "I-Non Chiu", "Yizhou Gu", "Haojie Xu"]}, "301": {"id": "2404.04925v1", "title": "Multilingual Large Language Model: A Survey of Resources, Taxonomy and Frontiers", "url": "http://arxiv.org/pdf/2404.04925v1", "date": "2024-04-07 11:52:44", "abs": "Multilingual Large Language Models are capable of using powerful Large\nLanguage Models to handle and respond to queries in multiple languages, which\nachieves remarkable success in multilingual natural language processing tasks.\nDespite these breakthroughs, there still remains a lack of a comprehensive\nsurvey to summarize existing approaches and recent developments in this field.\nTo this end, in this paper, we present a thorough review and provide a unified\nperspective to summarize the recent progress as well as emerging trends in\nmultilingual large language models (MLLMs) literature. The contributions of\nthis paper can be summarized: (1) First survey: to our knowledge, we take the\nfirst step and present a thorough review in MLLMs research field according to\nmulti-lingual alignment; (2) New taxonomy: we offer a new and unified\nperspective to summarize the current progress of MLLMs; (3) New frontiers: we\nhighlight several emerging frontiers and discuss the corresponding challenges;\n(4) Abundant resources: we collect abundant open-source resources, including\nrelevant papers, data corpora, and leaderboards. We hope our work can provide\nthe community with quick access and spur breakthrough research in MLLMs.", "cat": "cs.CL", "authors": ["Libo Qin", "Qiguang Chen", "Yuhang Zhou", "Zhi Chen", "Yinghui Li", "Lizi Liao", "Min Li", "Wanxiang Che", "Philip S. Yu"]}, "302": {"id": "2212.03954v1", "title": "Going Beyond XAI: A Systematic Survey for Explanation-Guided Learning", "url": "http://arxiv.org/pdf/2212.03954v1", "date": "2022-12-07 20:59:59", "abs": "As the societal impact of Deep Neural Networks (DNNs) grows, the goals for\nadvancing DNNs become more complex and diverse, ranging from improving a\nconventional model accuracy metric to infusing advanced human virtues such as\nfairness, accountability, transparency (FaccT), and unbiasedness. Recently,\ntechniques in Explainable Artificial Intelligence (XAI) are attracting\nconsiderable attention, and have tremendously helped Machine Learning (ML)\nengineers in understanding AI models. However, at the same time, we started to\nwitness the emerging need beyond XAI among AI communities; based on the\ninsights learned from XAI, how can we better empower ML engineers in steering\ntheir DNNs so that the model's reasonableness and performance can be improved\nas intended? This article provides a timely and extensive literature overview\nof the field Explanation-Guided Learning (EGL), a domain of techniques that\nsteer the DNNs' reasoning process by adding regularization, supervision, or\nintervention on model explanations. In doing so, we first provide a formal\ndefinition of EGL and its general learning paradigm. Secondly, an overview of\nthe key factors for EGL evaluation, as well as summarization and categorization\nof existing evaluation procedures and metrics for EGL are provided. Finally,\nthe current and potential future application areas and directions of EGL are\ndiscussed, and an extensive experimental study is presented aiming at providing\ncomprehensive comparative studies among existing EGL models in various popular\napplication domains, such as Computer Vision (CV) and Natural Language\nProcessing (NLP) domains.", "cat": "cs.AI", "authors": ["Yuyang Gao", "Siyi Gu", "Junji Jiang", "Sungsoo Ray Hong", "Dazhou Yu", "Liang Zhao"]}, "303": {"id": "1307.1733v1", "title": "The NuSTAR Extragalactic Survey: A First Sensitive Look at the High-Energy Cosmic X-ray Background Population", "url": "http://arxiv.org/pdf/1307.1733v1", "date": "2013-07-05 22:41:00", "abs": "We report on the first ten identifications of sources serendipitously\ndetected by the NuSTAR to provide the first sensitive census of the cosmic\nX-ray background (CXB) source population at >10 keV. We find that these\nNuSTAR-detected sources are ~100x fainter than those previously detected at >10\nkeV and have a broad range in redshift and luminosity (z=0.020-2.923 and\nL_10-40 keV~4x10^{41}-5x10^{45} erg/s); the median redshift and luminosity are\nz~0.7 and L_10-40 keV~3x10^{44} erg/s, respectively. We characterize these\nsources on the basis of broad-band ~0.5-32 keV spectroscopy, optical\nspectroscopy, and broad-band ultraviolet-to-mid-infrared SED analyzes. We find\nthat the dominant source population is quasars with L_10-40 keV>10^{44} erg/s,\nof which ~50% are obscured with N_H>10^{22} cm^{-2}. However, none of the ten\nNuSTAR sources are Compton thick (N_H>10^{24} cm^{-2}) and we place a 90%\nconfidence upper limit on the fraction of Compton-thick quasars (L_10-40\nkeV>10^{44} erg/s) selected at >10 keV of ~33% over the redshift range\nz=0.5-1.1. We jointly fitted the rest-frame ~10-40 keV data for all of the\nnon-beamed sources with L_10-40 keV>10^{43} erg/s to constrain the average\nstrength of reflection; we find R<1.4 for \\Gamma=1.8, broadly consistent with\nthat found for local AGNs observed at >10 keV. We also constrain the host\ngalaxy masses and find a median stellar mass of ~10^{11} M_sun, a factor ~5\ntimes higher than the median stellar mass of nearby high-energy selected AGNs,\nwhich may be at least partially driven by the order of magnitude higher X-ray\nluminosities of the NuSTAR sources. Within the low source-statistic limitations\nof our study, our results suggest that the overall properties of the NuSTAR\nsources are broadly similar to those of nearby high-energy selected AGNs but\nscaled up in luminosity and mass.", "cat": "astro-ph.HE", "authors": ["D. M. Alexander", "D. Stern", "A. Del Moro", "G. B. Lansbury", "R. J. Assef", "J. Aird", "M. Ajello", "D. R. Ballantyne", "F. E. Bauer", "S. E. Boggs", "W. N. Brandt", "F. E. Christensen", "F. Civano", "A. Comastri", "W. W. Craig", "M. Elvis", "B. W. Grefenstette", "C. J. Hailey", "F. A. Harrison", "R. C. Hickox", "B. Luo", "K. K. Madsen", "J. R. Mullaney", "M. Perri", "S. Puccetti", "C. Saez", "E. Treister", "C. M. Urry", "W. W. Zhang", "C. R. Bridge", "P. R. M. Eisenhardt", "A. H. Gonzalez", "S. H. Miller", "C. W. Tsar"]}, "304": {"id": "2005.08614v1", "title": "Semi-online Scheduling: A Survey", "url": "http://arxiv.org/pdf/2005.08614v1", "date": "2020-05-18 11:53:23", "abs": "In online scheduling, jobs are available one by one and each job must be\nscheduled irrevocably before the availability of the next job. Semi-online\nscheduling is a relaxed variant of online scheduling, where an additional\nmemory in terms of buffer or an Extra Piece of Information(EPI) is provided\nalong with input data. The EPI may include one or more of the parameter(s) such\nas size of the largest job, total size of all jobs, arrival sequence of the\njobs, optimum makespan value or range of job's processing time. A semi-online\nscheduling algorithm was first introduced in 1997 by Kellerer et al. They\nenvisioned semi-online scheduling as a practically significant model and\nobtained improved results for $2$-identical machine setting. This paper surveys\nscholarly contributions in the design of semi-online scheduling algorithms in\nparallel machine models such as identical and uniformly related by considering\njob's processing formats such as preemptive and non-preemptive with the\noptimality criteria such as Min-Max and Max-Min. The main focus is to present\nstate of the art competitive analysis results of well-known semi-online\nscheduling algorithms in a chronological overview. The survey first introduces\nthe online and semi-online algorithmic frameworks for the multi-processor\nscheduling problem with important applications and research motivation,\nfollowed by a taxonomy for semi-online scheduling. Fifteen well-known\nsemi-online scheduling algorithms are stated. Important competitive analysis\nresults are presented in a chronological way by highlighting the critical ideas\nand intuition behind the results. An evolution time-line of semi-online\nscheduling setups and a classification of the references based on EPI are\noutlined. Finally, the survey concludes with the exploration of some of the\ninteresting research challenges and open problems.", "cat": "cs.DS", "authors": ["Debasis Dwibedy", "Rakesh Mohanty"]}, "305": {"id": "2406.07973v2", "title": "Unique Security and Privacy Threats of Large Language Model: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2406.07973v2", "date": "2024-06-18 05:37:06", "abs": "With the rapid development of artificial intelligence, large language models\n(LLMs) have made remarkable advancements in natural language processing. These\nmodels are trained on vast datasets to exhibit powerful language understanding\nand generation capabilities across various applications, including machine\ntranslation, chatbots, and agents. However, LLMs have revealed a variety of\nprivacy and security issues throughout their life cycle, drawing significant\nacademic and industrial attention. Moreover, the risks faced by LLMs differ\nsignificantly from those encountered by traditional language models. Given that\ncurrent surveys lack a clear taxonomy of unique threat models across diverse\nscenarios, we emphasize the unique privacy and security threats associated with\nfive specific scenarios: pre-training, fine-tuning, retrieval-augmented\ngeneration systems, deployment, and LLM-based agents. Addressing the\ncharacteristics of each risk, this survey outlines potential threats and\ncountermeasures. Research on attack and defense situations can offer feasible\nresearch directions, enabling more areas to benefit from LLMs.", "cat": "cs.CR", "authors": ["Shang Wang", "Tianqing Zhu", "Bo Liu", "Ming Ding", "Xu Guo", "Dayong Ye", "Wanlei Zhou", "Philip S. Yu"]}, "306": {"id": "0704.1388v1", "title": "Why do some intermediate polars show soft X-ray emission? A survey of XMM-Newton spectra", "url": "http://arxiv.org/pdf/0704.1388v1", "date": "2007-04-11 10:11:33", "abs": "We make a systematic analysis of the XMM-Newton X-ray spectra of intermediate\npolars (IPs) and find that, contrary to the traditional picture, most show a\nsoft blackbody component. We compare the results with those from AM Her stars\nand deduce that the blackbody emission arises from reprocessing of hard X-rays,\nrather than from the blobby accretion sometimes seen in AM Hers. Whether an IP\nshows a blackbody component appears to depend primarily on geometric factors: a\nblackbody is not seen in those that have accretion footprints that are always\nobscured by accretion curtains or are only visible when foreshortened on the\nwhite-dwarf limb. Thus we argue against previous suggestions that the blackbody\nemission characterises a separate sub-group of IPs which are more akin to AM\nHers, and develop a unified picture of the blackbody emission in these stars.", "cat": "astro-ph", "authors": ["P. A. Evans", "Coel Hellier"]}, "307": {"id": "1304.3557v1", "title": "Survey of Server Virtualization", "url": "http://arxiv.org/pdf/1304.3557v1", "date": "2013-04-12 07:33:42", "abs": "Virtualization is a term that refers to the abstraction of computer\nresources. The purpose of virtual computing environment is to improve resource\nutilization by providing a unified integrated operating platform for users and\napplications based on aggregation of heterogeneous and autonomous resources.\nMore recently, virtualization at all levels (system, storage, and network)\nbecame important again as a way to improve system security, reliability and\navailability, reduce costs, and provide greater flexibility. Virtualization has\nrapidly become a go-to technology for increasing efficiency in the data center.\nWith virtualization technologies providing tremendous flexibility, even\ndisparate architectures may be deployed on a single machine without\ninterference This paper explains the basics of server virtualization and\naddresses pros and cons of virtualization", "cat": "cs.OS", "authors": ["Radhwan Y Ameen", "Asmaa Y. Hamo"]}, "308": {"id": "0911.4861v2", "title": "The HiZELS/UKIRT large area survey for bright Lyman-alpha emitters at z~9", "url": "http://arxiv.org/pdf/0911.4861v2", "date": "2009-11-28 12:29:46", "abs": "We present the largest area survey to date (1.4 deg2) for Lyman-alpha\nemitters (LAEs) at z~9, as part of the Hi-z Emission Line Survey (HiZELS). The\nsurvey, which primarily targets H-alpha emitters at z < 3, uses the Wide Field\nCAMera on the United Kingdom Infrared Telescope and a custom narrow-band filter\nin the J band to reach a Lyman-alpha luminosity limit of ~10^43.8 erg/s over a\nco-moving volume of 1.12x10^6 Mpc^3 at z = 8.96+-0.06. Two candidates were\nfound out of 1517 line emitters, but those were rejected as LAEs after\nfollow-up observations. This improves the limit on the space density of bright\nLyman-alpha emitters by 3 orders of magnitude and is consistent with\nsuppression of the bright end of the Lyman-alpha luminosity function beyond\nz~6. Combined with upper limits from smaller but deeper surveys, this rules out\nsome of the most extreme models for high-redshift Lyman-alpha emitters. The\npotential contamination of narrow-band Lyman-alpha surveys at z>7 by Galactic\nbrown dwarf stars is also examined, leading to the conclusion that such\ncontamination may well be significant for searches at 7.7 < z < 8.0, 9.1 < z <\n9.5 and 11.7 < z < 12.2.", "cat": "astro-ph.CO", "authors": ["David Sobral", "Philip Best", "Jim Geach", "Ian Smail", "Jaron Kurk", "Michele Cirasuolo", "Mark Casali", "Rob Ivison", "Kristen Coppin", "Gavin Dalton"]}, "309": {"id": "0812.2358v1", "title": "Identifying nearby field T dwarfs in the UKIDSS Galactic Clusters Survey", "url": "http://arxiv.org/pdf/0812.2358v1", "date": "2008-12-12 11:53:31", "abs": "We present the discovery of two new late-T dwarfs identified in the UKIRT\nInfrared Deep Sky Survey (UKIDSS) Galactic Clusters Survey (GCS) Data Release 2\n(DR2). These T dwarfs are nearby old T dwarfs along the line of sight to\nstar-forming regions and open clusters targeted by the UKIDSS GCS. They are\nfound towards the Alpha Per cluster and Orion complex, respectively, from a\nsearch in 54 square degrees surveyed in five filters. Photometric candidates\nwere picked up in two-colour diagrams, in a very similar manner to candidates\nextracted from the UKIDSS Large Area Survey (LAS) but taking advantage of the Z\nfilter employed by the GCS. Both candidates exhibit near-infrared J-band\nspectra with strong methane and water absorption bands characteristic of late-T\ndwarfs. We derive spectral types of T6.5+/-0.5 and T7+/-1 and estimate\nphotometric distances less than 50 pc for UGCS J030013.86+490142.5 and UGCS\nJ053022.52-052447.4, respectively. The space density of T dwarfs found in the\nGCS seems consistent with discoveries in the larger areal coverage of the\nUKIDSS Large Area Survey, indicating one T dwarf in 6-11 square degrees. The\nfinal area surveyed by the GCS, 1000 square degrees in five passbands, will\nallow expansion of the LAS search area by 25%, increase the probability of\nfinding ultracool brown dwarfs, and provide optimal estimates of contamination\nby old field brown dwarfs in deep surveys to identify such objects in open\nclusters and star-forming regions.", "cat": "astro-ph", "authors": ["N. Lodieu", "B. Burningham", "N. C. Hambly", "D. J. Pinfield"]}, "310": {"id": "1910.09533v2", "title": "Extracting key information from spectroscopic galaxy surveys", "url": "http://arxiv.org/pdf/1910.09533v2", "date": "2023-07-05 14:14:50", "abs": "We develop a novel method to extract key cosmological information, which is\nprimarily carried by the baryon acoustic oscillations and redshift space\ndistortions, from spectroscopic galaxy surveys based on a joint principal\ncomponent analysis (PCA) and massive optimized parameter estimation and data\ncompression (MOPED) algorithm. We apply this method to galaxy samples from BOSS\nDR12, and find that a PCA manipulation is effective at extracting the\ninformative modes in the 2D correlation function, giving a tighter constraint\non BAO and RSD parameters compared to that using the lowest three multipole\nmoments by the traditional method; i.e. the Figure of Merit of BAO and RSD\nparameters is improved by $\\sim20\\%$. We then perform a compression of the\ninformative PC modes for BAO and RSD parameters using the MOPED scheme,\nreducing the dimension of the data vector to the number of interesting\nparameters, manifesting the joint PCA and MOPED as a powerful tool for\nclustering analysis with almost no loss of constraining power.", "cat": "astro-ph.CO", "authors": ["Yuting Wang", "Gong-Bo Zhao", "John A. Peacock"]}, "311": {"id": "1312.6552v1", "title": "Socially-Aware Networking: A Survey", "url": "http://arxiv.org/pdf/1312.6552v1", "date": "2013-12-23 14:10:54", "abs": "The widespread proliferation of handheld devices enables mobile carriers to\nbe connected at anytime and anywhere. Meanwhile, the mobility patterns of\nmobile devices strongly depend on the users' movements, which are closely\nrelated to their social relationships and behaviors. Consequently, today's\nmobile networks are becoming increasingly human centric. This leads to the\nemergence of a new field which we call socially-aware networking (SAN). One of\nthe major features of SAN is that social awareness becomes indispensable\ninformation for the design of networking solutions. This emerging paradigm is\napplicable to various types of networks (e.g. opportunistic networks, mobile\nsocial networks, delay tolerant networks, ad hoc networks, etc) where the users\nhave social relationships and interactions. By exploiting social properties of\nnodes, SAN can provide better networking support to innovative applications and\nservices. In addition, it facilitates the convergence of human society and\ncyber physical systems. In this paper, for the first time, to the best of our\nknowledge, we present a survey of this emerging field. Basic concepts of SAN\nare introduced. We intend to generalize the widely-used social properties in\nthis regard. The state-of-the-art research on SAN is reviewed with focus on\nthree aspects: routing and forwarding, incentive mechanisms and data\ndissemination. Some important open issues with respect to mobile social sensing\nand learning, privacy, node selfishness and scalability are discussed.", "cat": "cs.SI", "authors": ["Feng Xia", "Li Liu", "Jie Li", "Jianhua Ma", "Athanasios V. Vasilakos"]}, "312": {"id": "2007.08244v2", "title": "Discovery of a Radio Relic in the Massive Merging Cluster SPT-CL 2023-5535 from the ASKAP-EMU PILOT SURVEY", "url": "http://arxiv.org/pdf/2007.08244v2", "date": "2020-07-18 02:16:20", "abs": "The ASKAP-EMU survey is a deep wide-field radio continuum survey designed to\ncover the entire southern sky and a significant fraction of the northern sky up\nto $+30^{\\circ}$. Here, we report a discovery of a radio relic in the merging\ncluster SPT-CL 2023-5535 at z=0.23 from the ASKAP-EMU pilot 300 sq. deg survey\n(800-1088 MHz). The deep high-resolution data reveal a $\\sim2$ Mpc-scale radio\nhalo elongated in the east-west direction, coincident with the intracluster\ngas. The radio relic is located at the western edge of this radio halo\nstretched $\\sim0.5$ Mpc in the north-south orientation. The integrated spectral\nindex of the radio relic within the narrow bandwidth is $\\alpha^{\\scriptstyle\n\\rm 1088~MHz}_{\\scriptstyle \\rm 800~MHz}=-0.76 \\pm 0.06$. Our weak-lensing\nanalysis shows that the system is massive ($M_{200}=1.04\\pm0.36\\times 10^{15}\nM_{\\odot}$) and composed of at least three subclusters. We suggest a scenario,\nwherein the radio features arise from the collision between the eastern and\nmiddle subclusters. Our discovery illustrates the effectiveness of the\nASKAP-EMU survey in detecting diffuse emissions in galaxy clusters and when\ncompleted, the survey will greatly increase the number of merging cluster\ndetections with diffuse radio emissions.", "cat": "astro-ph.HE", "authors": ["Kim HyeongHan", "M. James Jee", "Lawrence Rudnick", "David Parkinson", "Kyle Finner", "Mijin Yoon", "Wonki Lee", "Gianfranco Brunetti", "Marcus Br\u00fcggen", "Jordan D. Collier", "Andrew M. Hopkins", "Micha\u0142 J. Micha\u0142owski", "Ray P. Norris", "Chris Riseley"]}, "313": {"id": "1011.1129v1", "title": "IGR J16547-1916/1RXS J165443.5-191620 -- a New Intermediate Polar from the INTEGRAL Galactic Survey", "url": "http://arxiv.org/pdf/1011.1129v1", "date": "2010-11-04 12:04:08", "abs": "We present the results of our optical identification of the X-ray source IGR\nJ16547-1916 detected by the INTEGRAL observatory during a deep all-sky survey.\nAnalysis of the spectroscopic data from the SWIFT and INTEGRAL observatories in\nthe X-ray energy band and from the BTA (Special Astrophysical Observatory)\ntelescope in the optical band has shown that the source is most likely an\nintermediate polar -- an accreting white dwarf with the mass of M~0.85 M_Sun in\na low-mass binary system. Subsequent studies of the object's rapid variability\nwith the RTT-150 telescope have confirmed this conclusion by revealing periodic\npulsations of its optical emission with a period of ~550 s.", "cat": "astro-ph.HE", "authors": ["A. Lutovinov", "R. Burenin", "M. Revnivtsev", "V. Suleimanov", "A. Tkachenko"]}, "314": {"id": "1812.08856v10", "title": "Machine Learning for Wireless Link Quality Estimation: A Survey", "url": "http://arxiv.org/pdf/1812.08856v10", "date": "2021-01-18 10:16:21", "abs": "Since the emergence of wireless communication networks, a plethora of\nresearch papers focus their attention on the quality aspects of wireless links.\n The analysis of the rich body of existing literature on link quality\nestimation using models developed from data traces indicates that the\ntechniques used for modeling link quality estimation are becoming increasingly\nsophisticated. A number of recent estimators leverage machine learning (ML)\ntechniques that require a sophisticated design and development process, each of\nwhich has a great potential to significantly affect the overall model\nperformance.\n In this paper, we provide a comprehensive survey on link quality estimators\ndeveloped from empirical data and then focus on the subset that use ML\nalgorithms. We analyze ML-based link quality estimation (LQE) models from two\nperspectives using performance data. Firstly, we focus on how they address\nquality requirements that are important from the perspective of the\napplications they serve. Secondly, we analyze how they approach the standard\ndesign steps commonly used in the ML community. Having analyzed the scientific\nbody of the survey, we review existing open source datasets suitable for LQE\nresearch. Finally, we round up our survey with the lessons learned and design\nguidelines for ML-based LQE development and dataset collection.", "cat": "cs.NI", "authors": ["Gregor Cerar", "Halil Yetgin", "Mihael Mohor\u010di\u010d", "Carolina Fortuna"]}, "315": {"id": "2006.00648v2", "title": "A Survey on 3D LiDAR Localization for Autonomous Vehicles", "url": "http://arxiv.org/pdf/2006.00648v2", "date": "2020-11-21 17:07:12", "abs": "LiDAR sensors are becoming one of the most essential sensors in achieving\nfull autonomy for self driving cars. LiDARs are able to produce rich, dense and\nprecise spatial data, which can tremendously help in localizing and tracking a\nmoving vehicle. In this paper, we review the latest finding in 3D LiDAR\nlocalization for autonomous driving cars, and analyse the results obtained by\neach method, in an effort to guide the research community towards the path that\nseems to be the most promising.", "cat": "cs.CV", "authors": ["Mahdi Elhousni", "Xinming Huang"]}, "316": {"id": "2402.00659v1", "title": "Modeling Freight Mode Choice Using Machine Learning Classifiers: A Comparative Study Using the Commodity Flow Survey (CFS) Data", "url": "http://arxiv.org/pdf/2402.00659v1", "date": "2024-02-01 15:18:48", "abs": "This study explores the usefulness of machine learning classifiers for\nmodeling freight mode choice. We investigate eight commonly used machine\nlearning classifiers, namely Naive Bayes, Support Vector Machine, Artificial\nNeural Network, K-Nearest Neighbors, Classification and Regression Tree, Random\nForest, Boosting and Bagging, along with the classical Multinomial Logit model.\nUS 2012 Commodity Flow Survey data are used as the primary data source; we\naugment it with spatial attributes from secondary data sources. The performance\nof the classifiers is compared based on prediction accuracy results. The\ncurrent research also examines the role of sample size and training-testing\ndata split ratios on the predictive ability of the various approaches. In\naddition, the importance of variables is estimated to determine how the\nvariables influence freight mode choice. The results show that the tree-based\nensemble classifiers perform the best. Specifically, Random Forest produces the\nmost accurate predictions, closely followed by Boosting and Bagging. With\nregard to variable importance, shipment characteristics, such as shipment\ndistance, industry classification of the shipper and shipment size, are the\nmost significant factors for freight mode choice decisions.", "cat": "cs.LG", "authors": ["Majbah Uddin", "Sabreena Anowar", "Naveen Eluru"]}, "317": {"id": "2406.06702v1", "title": "NEATH III: a molecular line survey of a simulated star-forming cloud", "url": "http://arxiv.org/pdf/2406.06702v1", "date": "2024-06-10 18:04:39", "abs": "We present synthetic line observations of a simulated molecular cloud,\nutilising a self-consistent treatment of the dynamics and time-dependent\nchemical evolution. We investigate line emission from the three most common CO\nisotopologues ($^{12}$CO, $^{13}$CO, C$^{18}$O) and six supposed tracers of\ndense gas (NH$_3$, HCN, N$_2$H$^+$, HCO$^+$, CS, HNC). Our simulation produces\na range of line intensities consistent with that observed in real molecular\nclouds. The HCN-to-CO intensity ratio is relatively invariant with column\ndensity, making HCN (and chemically-similar species such as CS) a poor tracer\nof high-density material in the cloud. The ratio of N$_2$H$^+$ to HCN or CO, on\nthe other hand, is highly selective of regions with densities above $10^{22} \\,\n{\\rm cm^{-2}}$, and the N$_2$H$^+$ line is a very good tracer of the dynamics\nof high volume density ($>10^4 \\, {\\rm cm^{-3}}$) material. Focusing on cores\nformed within the simulated cloud, we find good agreement with the line\nintensities of an observational sample of prestellar cores, including\nreproducing observed CS line intensities with an undepleted elemental abundance\nof sulphur. However, agreement between cores formed in the simulation, and\nmodels of isolated cores which have otherwise-comparable properties, is poor.\nThe formation from and interaction with the large-scale environment has a\nsignificant impact on the line emission properties of the cores, making\nisolated models unsuitable for interpreting observational data.", "cat": "astro-ph.GA", "authors": ["F. D. Priestley", "P. C. Clark", "S. C. O. Glover", "S. E. Ragan", "O. Feh\u00e9r", "L. R. Prole", "R. S. Klessen"]}, "318": {"id": "2203.06083v1", "title": "Ages of Main-Sequence Turn-Off Stars from the GALAH Survey", "url": "http://arxiv.org/pdf/2203.06083v1", "date": "2022-03-11 17:05:57", "abs": "Main sequence turn-off (MSTO) stars are good tracers of Galactic populations\nsince their ages can be reliably estimated from atmospheric parameters. Based\non the GALAH survey, we use the Yale Rotation Evolution Code to determine ages\nof 2926 MSTO stars with mean age uncertainty $\\sim$10\\% considering the\nvariation of C and O abundances. Ages of CO-poor stars are systematically\naffected by $\\sim$10\\% due to the C and O abundances, globally shifting to\n$\\sim$0.5 Gyr older compared to the results using solar metal-mixture. Of the\nstars with \\mbox{[Fe/H] $\\sim$0.3-0.5} or \\mbox{[O/Fe]~$\\leq$~-0.25}, many have\nfractional age differences~$\\geq$~20\\%, and even reach up to 36\\%. The\nage-metallicity relation appears to possibly exist two distinct sequences: a\nyoung sequence of stars with age mostly $<$ 7 Gyr, and a relatively older\nsequence of stars with age mostly $>$ 7 Gyr, overlapping at 5 Gyr\n$\\leq$~age~$\\leq$ 7 Gyr. Moreover, the trends of abundances to age ratios show\ntwo corresponding sequences, especially in [O/Fe]-age plane. We also find that\n[Y/Mg] is a good chemical clock in disk populations. The young sequence and the\nold sequence can not be separated based on chemistry or kinematics, therefore\nstellar age is an important parameter to distinguish these two sequences in our\nsample.", "cat": "astro-ph.SR", "authors": ["Xunzhou Chen", "Zhishuai Ge", "Yuqin Chen", "Shaolan Bi", "Jie Yu", "Wuming Yang", "Jason W. Ferguson", "Yaqian Wu", "Yaguang Li"]}, "319": {"id": "1108.2711v1", "title": "Galaxy pairs in the Sloan Digital Sky Survey - IV: Interactions trigger AGN", "url": "http://arxiv.org/pdf/1108.2711v1", "date": "2011-08-12 20:08:15", "abs": "Galaxy-galaxy interactions are predicted to cause gas inflows leading to\nenhanced nuclear star formation. In this paper we test the further prediction\nthat the gas inflows lead to enhanced accretion onto the central supermassive\nblack hole, triggering activity in the nucleus. Based on a sample of 11,060\nSDSS galaxies with a close companion (rp < 80 kpc, Delta V < 200 km/s), we\nclassify AGN based either on emission line ratios or on spectral classification\nas a quasar. The AGN fraction in the close pairs sample is compared to a\ncontrol sample of 110,600 mass- and redshift-matched control galaxies with no\nnearby companion. We find a clear increase in the AGN fraction in close pairs\nof galaxies with projected separations < 40 kpc by up to a factor of 2.5\nrelative to the control sample (although the enhancement depends on the chosen\nS/N cut of the sample). The increase in AGN fraction is strongest in equal mass\ngalaxy pairings, and weakest in the lower mass component of an unequal mass\npairing. The increased AGN fraction at small separations is accompanied by an\nenhancement in the number of `composite' galaxies whose spectra are the result\nof photoionization by both AGN and stars. Our results indicate that AGN\nactivity occurs (at least in some cases) well before final coalescence and\nconcurrently with ongoing star formation. Finally, we find a marked increase at\nsmall projected separations of the fraction of pairs in which BOTH galaxies\nharbour AGN. We demonstrate that the fraction of double AGN exceeds the\nexpected random fraction, indicating that some pairs undergo correlated nuclear\nactivity. Taken together with complimentary studies, we favour an\ninterpretation where interactions trigger AGN, but are not the only cause of\nnuclear activity.", "cat": "astro-ph.CO", "authors": ["Sara L. Ellison", "David R. Patton", "J. Trevor Mendel", "Jillian M. Scudder"]}, "320": {"id": "1807.07904v1", "title": "Observational signatures of dark energy produced in an ancestor vacuum: Forecast for galaxy surveys", "url": "http://arxiv.org/pdf/1807.07904v1", "date": "2018-07-20 15:40:51", "abs": "We study observational consequences of the model for dark energy proposed in\n[1] (Aoki et al., Phys.Rev. D97 (2018) no.4, 043517). We assume our universe\nhas been created by bubble nucleation, and consider quantum fluctuations of an\nultralight scalar field. Residual effects of fluctuations generated in an\nancestor vacuum (de Sitter space in which the bubble was formed) is interpreted\nas dark energy. Its equation of state parameter w(z) has a characteristic form,\napproaching -1 in the future, but -1/3 in the past. A novel feature of our\nmodel is that dark energy effectively increases the magnitude of the negative\nspatial curvature in the evolution of the Hubble parameter, though it does not\nalter the definition of the angular diameter distance. We perform Fisher\nanalysis and forecast the constraints for our model from future galaxy surveys\nby Square Kilometre Array and Euclid. Due to degeneracy between dark energy and\nthe spatial curvature, galaxy surveys alone can determine these parameters only\nfor optimistic choices of their values, but combination with other independent\nobservations, such as CMB, will greatly improve the chance of determining them.", "cat": "astro-ph.CO", "authors": ["Daisuke Yamauchi", "Hajime Aoki", "Satoshi Iso", "Da-Shin Lee", "Yasuhiro Sekino", "Chen-Pin Yeh"]}, "321": {"id": "2304.05482v3", "title": "Computational Pathology: A Survey Review and The Way Forward", "url": "http://arxiv.org/pdf/2304.05482v3", "date": "2024-01-27 21:27:51", "abs": "Computational Pathology CPath is an interdisciplinary science that augments\ndevelopments of computational approaches to analyze and model medical\nhistopathology images. The main objective for CPath is to develop\ninfrastructure and workflows of digital diagnostics as an assistive CAD system\nfor clinical pathology, facilitating transformational changes in the diagnosis\nand treatment of cancer that are mainly address by CPath tools. With\nevergrowing developments in deep learning and computer vision algorithms, and\nthe ease of the data flow from digital pathology, currently CPath is witnessing\na paradigm shift. Despite the sheer volume of engineering and scientific works\nbeing introduced for cancer image analysis, there is still a considerable gap\nof adopting and integrating these algorithms in clinical practice. This raises\na significant question regarding the direction and trends that are undertaken\nin CPath. In this article we provide a comprehensive review of more than 800\npapers to address the challenges faced in problem design all-the-way to the\napplication and implementation viewpoints. We have catalogued each paper into a\nmodel-card by examining the key works and challenges faced to layout the\ncurrent landscape in CPath. We hope this helps the community to locate relevant\nworks and facilitate understanding of the field's future directions. In a\nnutshell, we oversee the CPath developments in cycle of stages which are\nrequired to be cohesively linked together to address the challenges associated\nwith such multidisciplinary science. We overview this cycle from different\nperspectives of data-centric, model-centric, and application-centric problems.\nWe finally sketch remaining challenges and provide directions for future\ntechnical developments and clinical integration of CPath\n(https://github.com/AtlasAnalyticsLab/CPath_Survey).", "cat": "eess.IV", "authors": ["Mahdi S. Hosseini", "Babak Ehteshami Bejnordi", "Vincent Quoc-Huy Trinh", "Danial Hasan", "Xingwen Li", "Taehyo Kim", "Haochen Zhang", "Theodore Wu", "Kajanan Chinniah", "Sina Maghsoudlou", "Ryan Zhang", "Stephen Yang", "Jiadai Zhu", "Lyndon Chan", "Samir Khaki", "Andrei Buin", "Fatemeh Chaji", "Ala Salehi", "Bich Ngoc Nguyen", "Dimitris Samaras", "Konstantinos N. Plataniotis"]}, "322": {"id": "1711.01794v1", "title": "The Green Bank Ammonia Survey: Unveiling the Dynamics of the Barnard 59 star-forming Clump", "url": "http://arxiv.org/pdf/1711.01794v1", "date": "2017-11-06 09:19:07", "abs": "Understanding the early stages of star formation is a research field of\nongoing development, both theoretically and observationally. In this context,\nmolecular data have been continuously providing observational constraints on\nthe gas dynamics at different excitation conditions and depths in the sources.\nWe have investigated the Barnard 59 core, the only active site of star\nformation in the Pipe Nebula, to achieve a comprehensive view of the kinematic\nproperties of the source. These information were derived by simultaneously\nfitting ammonia inversion transition lines (1,1) and (2,2). Our analysis\nunveils the imprint of protostellar feedback, such as increasing line widths,\ntemperature and turbulent motions in our molecular data. Combined with\ncomplementary observations of dust thermal emission, we estimate that the core\nis gravitationally bound following a virial analysis. If the core is not\ncontracting, another source of internal pressure, most likely the magnetic\nfield, is supporting it against gravitational collapse and limits its star\nformation efficiency.", "cat": "astro-ph.GA", "authors": ["E. Redaelli", "F. O. Alves", "P. Caselli", "J. E. Pineda", "R. K. Friesen", "A. Chac\u00f3n-Tanarro", "C. D. Matzner", "A. Ginsburg", "E. Rosolowsky", "J. Keown", "S. S. R. Offner", "J. Di Francesco", "H. Kirk", "P. C. Myers", "A. Hacar", "A. Cimatti", "H. H. Chen", "M. C. Chen", "Y. M. Seo", "K. I. Lee"]}, "323": {"id": "1010.6195v1", "title": "The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes", "url": "http://arxiv.org/pdf/1010.6195v1", "date": "2010-10-29 12:59:16", "abs": "XMM and Chandra opened a new area for the study of clusters of galaxies. Not\nonly for cluster physics but also, for the detection of faint and distant\nclusters that were inaccessible with previous missions. This article presents\n66 spectroscopically confirmed clusters (0.051042 erg/s) although they do not show any clear signature\nof nuclear activity in the optical spectrum.", "cat": "astro-ph.HE", "authors": ["N. Cappelluti", "M. Brusa", "G. Hasinger", "A. Comastri", "G. Zamorani", "A. Finoguenov", "R. Gilli", "S. Puccetti", "T. Miyaji", "M. Salvato", "C. Vignali", "T. Aldcroft", "H. Boehringer", "H. Brunner", "F. Civano", "M. Elvis", "F. Fiore", "A. Fruscione", "R. E. Griffiths", "L. Guzzo", "A. Iovino", "A. M. Koekemoer", "V. Mainieri", "N. Z. Scoville", "P. Shopbell", "J. Silverman", "C. M. Urry"]}, "336": {"id": "2102.05343v1", "title": "Is Secure Coding Education in the Industry Needed? An Investigation Through a Large Scale Survey", "url": "http://arxiv.org/pdf/2102.05343v1", "date": "2021-02-10 09:33:21", "abs": "The Department of Homeland Security in the United States estimates that 90%\nof software vulnerabilities can be traced back to defects in design and\nsoftware coding. The financial impact of these vulnerabilities has been shown\nto exceed 380 million USD in industrial control systems alone. Since software\ndevelopers write software, they also introduce these vulnerabilities into the\nsource code. However, secure coding guidelines exist to prevent software\ndevelopers from writing vulnerable code. This study focuses on the human\nfactor, the software developer, and secure coding, in particular secure coding\nguidelines. We want to understand the software developers' awareness and\ncompliance to secure coding guidelines and why, if at all, they aren't\ncompliant or aware. We base our results on a large-scale survey on secure\ncoding guidelines, with more than 190 industrial software developers. Our\nwork's main contribution motivates the need to educate industrial software\ndevelopers on secure coding guidelines, and it gives a list of fifteen\nactionable items to be used by practitioners in the industry. We also make our\nraw data openly available for further research.", "cat": "cs.SE", "authors": ["Tiago Espinha Gasiba", "Ulrike Lechner", "Maria Pinto-Albuquerque", "Daniel Mendez"]}, "337": {"id": "2402.03436v1", "title": "Euclid preparation. Optical emission-line predictions of intermediate-z galaxy populations in GAEA for the Euclid Deep and Wide Surveys", "url": "http://arxiv.org/pdf/2402.03436v1", "date": "2024-02-05 19:00:03", "abs": "In anticipation of the Euclid Wide and Deep Surveys, we present optical\nemission-line predictions at intermediate redshifts from 0.4 to 2.5. Our\napproach combines a mock light cone from the GAEA semi-analytic model to\nself-consistently model nebular emission from HII regions, narrow-line regions\nof active galactic nuclei (AGN), and evolved stellar populations. Our analysis\nfocuses on seven optical emission lines: H$\\alpha$, H$\\beta$,\n[SII]$\\lambda\\lambda 6717, 6731$, [NII]$\\lambda 6584$, [OI]$\\lambda 6300$,\n[OIII]$\\lambda 5007$, and [OII]$\\lambda\\lambda 3727, 3729$. We find that Euclid\nwill predominantly observe massive, star-forming, and metal-rich line-emitters.\nInterstellar dust, modelled using a Calzetti law with mass-dependent scaling,\nmay decrease observable percentages by a further 20-30% with respect to our\nunderlying emission-line populations from GAEA. We predict Euclid to observe\naround 30-70% of H$\\alpha$-, [NII]-, [SII]-, and [OIII]-emitting galaxies at\nredshift below 1 and under 10% at higher redshift. Observability of H$\\beta$-,\n[OII]-, and [OI]- emission is limited to below 5%. For the Euclid-observable\nsample, we find that BPT diagrams can effectively distinguish between different\ngalaxy types up to around redshift 1.8, attributed to the bias toward\nmetal-rich systems. Moreover, we show that the relationships of H$\\alpha$ and\n[OIII]+H$\\beta$ to the star-formation rate, and the [OIII]-AGN luminosity\nrelation, exhibit minimal changes with increasing redshift. Based on line\nratios [NII]/H$\\alpha$, [NII]/[OII], and [NII]/[SII], we further propose novel\nz-invariant tracers for the black hole accretion rate-to-star formation rate\nratio. Lastly, we find that commonly used metallicity estimators display\ngradual shifts in normalisations with increasing redshift, while maintaining\nthe overall shape of local calibrations. This is in tentative agreement with\nrecent JWST data.", "cat": "astro-ph.GA", "authors": ["Euclid Collaboration", "L. Scharr\u00e9", "M. Hirschmann", "G. De Lucia", "S. Charlot", "F. Fontanot", "M. Spinelli", "L. Xie", "A. Feltre", "V. Allevato", "A. Plat", "M. N. Bremer", "S. Fotopoulou", "L. Gabarra", "B. R. Granett", "M. Moresco", "C. Scarlata", "L. Pozzetti", "L. Spinoglio", "M. Talia", "G. Zamorani", "B. Altieri", "A. Amara", "S. Andreon", "N. Auricchio", "M. Baldi", "S. Bardelli", "D. Bonino", "E. Branchini", "M. Brescia", "J. Brinchmann", "S. Camera", "V. Capobianco", "C. Carbone", "J. Carretero", "S. Casas", "F. J. Castander", "M. Castellano", "S. Cavuoti", "A. Cimatti", "G. Congedo", "C. J. Conselice", "L. Conversi", "Y. Copin", "L. Corcione", "F. Courbin", "H. M. Courtois", "A. Da Silva", "H. Degaudenzi", "J. Dinis", "M. Douspis", "F. Dubath", "X. Dupac", "S. Dusini", "M. Farina", "S. Farrens", "S. Ferriol", "M. Frailis", "E. Franceschi", "S. Galeotta", "B. Garilli", "B. Gillis", "C. Giocoli", "A. Grazian", "F. Grupp", "L. Guzzo", "S. V. H. Haugan", "W. Holmes", "I. Hook", "F. Hormuth", "A. Hornstrup", "K. Jahnke", "E. Keih\u00e4nen", "S. Kermiche", "A. Kiessling", "T. Kitching", "B. Kubik", "M. K\u00fcmmel", "M. Kunz", "H. Kurki-Suonio", "S. Ligori", "P. B. Lilje", "V. Lindholm", "I. Lloro", "D. Maino", "E. Maiorano", "O. Mansutti", "O. Marggraf", "K. Markovic", "N. Martinet", "F. Marulli", "R. Massey", "S. Maurogordato", "H. J. McCracken", "E. Medinaceli", "S. Mei", "Y. Mellier", "M. Meneghetti", "E. Merlin", "G. Meylan", "L. Moscardini", "E. Munari", "S. -M. Niemi", "C. Padilla", "S. Paltani", "F. Pasian", "K. Pedersen", "V. Pettorino", "G. Polenta", "M. Poncet", "L. A. Popa", "F. Raison", "A. Renzi", "J. Rhodes", "G. Riccio", "E. Romelli", "M. Roncarelli", "E. Rossetti", "R. Saglia", "D. Sapone", "B. Sartoris", "M. Schirmer", "P. Schneider", "A. Secroun", "G. Seidel", "S. Serrano", "C. Sirignano", "G. Sirri", "L. Stanco", "C. Surace", "P. Tallada-Cresp\u00ed", "A. N. Taylor", "H. I. Teplitz", "I. Tereno", "R. Toledo-Moreo", "F. Torradeflot", "I. Tutusaus", "L. Valenziano", "T. Vassallo", "A. Veropalumbo", "Y. Wang", "J. Weller", "J. Zoubian", "E. Zucca", "A. Biviano", "M. Bolzonella", "E. Bozzo", "C. Burigana", "C. Colodro-Conde", "D. Di Ferdinando", "R. Farinelli", "J. Graci\u00e1-Carpio", "G. Mainetti", "M. Martinelli", "N. Mauri", "C. Neissner", "A. A. Nucita", "Z. Sakr", "V. Scottez", "M. Tenti", "M. Viel", "M. Wiesmann", "Y. Akrami", "S. Anselmi", "C. Baccigalupi", "M. Ballardini", "M. Bethermin", "A. Blanchard", "S. Borgani", "A. S. Borlaff", "S. Bruton", "R. Cabanac", "A. Calabro", "G. Ca\u00f1as-Herrera", "A. Cappi", "C. S. Carvalho", "G. Castignani", "T. Castro", "K. C. Chambers", "S. Contarini", "T. Contini", "A. R. Cooray", "J. Coupon", "O. Cucciati", "G. Desprez", "S. Di Domizio", "H. Dole", "A. D\u00edaz-S \u00e1nchez", "J. A. Escartin Vigo", "S. Escoffier", "I. Ferrero", "K. Ganga", "J. Garc\u00eda-Bellido", "E. Gaztanaga", "K. George", "F. Giacomini", "G. Gozaliasl", "A. Gregorio", "A. Hall", "H. Hildebrandt", "J. J. E. Kajava", "V. Kansal", "C. C. Kirkpatrick", "L. Legrand", "A. Loureiro", "J. Macias-Perez", "M. Magliocchetti", "C. Mancini", "F. Mannucci", "R. Maoli", "C. J. A. P. Martins", "S. Matthew", "L. Maurin", "R. B. Metcalf", "M. Migliaccio", "P. Monaco", "G. Morgante", "Nicholas A. Walton", "M. P\u00f6ntinen", "V. Popa", "C. Porciani", "D. Potter", "I. Risso", "P. -F. Rocci", "M. Sahl\u00e9n", "A. G. S\u00e1nchez", "A. Schneider", "M. Schultheis", "M. Sereno", "P. Simon", "J. Steinwagner", "G. Testera", "M. Tewes", "R. Teyssier", "S. Toft", "S. Tosi", "A. Troja", "M. Tucci", "J. Valiviita", "D. Vergani", "G. Verza", "I. A. Zinchenko"]}, "338": {"id": "2402.08132v2", "title": "On the Resurgence of Recurrent Models for Long Sequences -- Survey and Research Opportunities in the Transformer Era", "url": "http://arxiv.org/pdf/2402.08132v2", "date": "2024-02-14 13:04:28", "abs": "A longstanding challenge for the Machine Learning community is the one of\ndeveloping models that are capable of processing and learning from very long\nsequences of data. The outstanding results of Transformers-based networks\n(e.g., Large Language Models) promotes the idea of parallel attention as the\nkey to succeed in such a challenge, obfuscating the role of classic sequential\nprocessing of Recurrent Models. However, in the last few years, researchers who\nwere concerned by the quadratic complexity of self-attention have been\nproposing a novel wave of neural models, which gets the best from the two\nworlds, i.e., Transformers and Recurrent Nets. Meanwhile, Deep Space-State\nModels emerged as robust approaches to function approximation over time, thus\nopening a new perspective in learning from sequential data, followed by many\npeople in the field and exploited to implement a special class of (linear)\nRecurrent Neural Networks. This survey is aimed at providing an overview of\nthese trends framed under the unifying umbrella of Recurrence. Moreover, it\nemphasizes novel research opportunities that become prominent when abandoning\nthe idea of processing long sequences whose length is known-in-advance for the\nmore realistic setting of potentially infinite-length sequences, thus\nintersecting the field of lifelong-online learning from streamed data.", "cat": "cs.LG", "authors": ["Matteo Tiezzi", "Michele Casoni", "Alessandro Betti", "Tommaso Guidi", "Marco Gori", "Stefano Melacci"]}, "339": {"id": "1105.0586v1", "title": "The Spitzer Extragalactic Representative Volume Survey (SERVS): The Environments of High-z SDSS Quasi-Stellar-Objects", "url": "http://arxiv.org/pdf/1105.0586v1", "date": "2011-05-03 13:54:07", "abs": "This paper presents a study of the environments of SDSS Quasi-Stellar-Objects\n(QSOs) in the Spitzer Extragalactic Representative Volume Survey (SERVS). We\nconcentrate on the high-redshift QSOs as these have not been studied in large\nnumbers with data of this depth before. We use the IRAC 3.6-4.5{\\mu}m colour of\nobjects and ancillary r-band data to filter out as much foreground\ncontamination as possible. This technique allows us to find a significant (>\n4-{\\sigma}) over-density of galaxies around QSOs in a redshift bin centred on z\n~ 2.0 and a (> 2-{\\sigma}) over-density of galaxies around QSOs in a redshift\nbin centred on z ~ 3.3. We compare our findings to the predictions of a\nsemi-analytic galaxy formation model, based on the {\\Lambda}CDM millennium\nsimulation, and find for both redshift bins that the model predictions match\nwell the source-density we have measured from the SERVS data.", "cat": "astro-ph.CO", "authors": ["J. T. Falder", "J. A. Stevens", "Matt J. Jarvis", "D. G. Bonfield", "M. Lacy", "D. Farrah", "S. Oliver", "J. Surace", "J. -C. Mauduit", "M. Vaccari", "L. Marchetti", "E. Gonz\u00e1lez-Solares", "J. Afonso", "A. Cava", "N. Seymour"]}, "340": {"id": "2107.07919v2", "title": "A Survey on Bias in Visual Datasets", "url": "http://arxiv.org/pdf/2107.07919v2", "date": "2022-06-23 13:46:10", "abs": "Computer Vision (CV) has achieved remarkable results, outperforming humans in\nseveral tasks. Nonetheless, it may result in significant discrimination if not\nhandled properly as CV systems highly depend on the data they are fed with and\ncan learn and amplify biases within such data. Thus, the problems of\nunderstanding and discovering biases are of utmost importance. Yet, there is no\ncomprehensive survey on bias in visual datasets. Hence, this work aims to: i)\ndescribe the biases that might manifest in visual datasets; ii) review the\nliterature on methods for bias discovery and quantification in visual datasets;\niii) discuss existing attempts to collect bias-aware visual datasets. A key\nconclusion of our study is that the problem of bias discovery and\nquantification in visual datasets is still open, and there is room for\nimprovement in terms of both methods and the range of biases that can be\naddressed. Moreover, there is no such thing as a bias-free dataset, so\nscientists and practitioners must become aware of the biases in their datasets\nand make them explicit. To this end, we propose a checklist to spot different\ntypes of bias during visual dataset collection.", "cat": "cs.CV", "authors": ["Simone Fabbrizzi", "Symeon Papadopoulos", "Eirini Ntoutsi", "Ioannis Kompatsiaris"]}, "341": {"id": "2401.11024v1", "title": "The MeerKAT 1.3 GHz Survey of the Small Magellanic Cloud", "url": "http://arxiv.org/pdf/2401.11024v1", "date": "2024-01-19 20:46:47", "abs": "We present new radio continuum images and a source catalogue from the MeerKAT\nsurvey in the direction of the Small Magellanic Cloud (SMC). The observations,\nat a central frequency of 1.3 GHz across a bandwidth of 0.8 GHz, encompass a\nfield of view ~7 x 7 degrees and result in images with resolution of 8 arcsec.\nThe median broad-band Stokes I image Root Mean Squared noise value is ~11\nmicroJy/beam. The catalogue produced from these images contains 108,330 point\nsources and 517 compact extended sources. We also describe a UHF (544-1088 MHz)\nsingle pointing observation. We report the detection of a new confirmed\nSupernova Remnant (SNR) (MCSNR J0100-7211) with an X-ray magnetar at its centre\nand 10 new SNR candidates. This is in addition to the detection of 21\npreviously confirmed SNRs and two previously noted SNR candidates. Our new SNR\ncandidates have typical surface brightness an order of magnitude below those\npreviously known, and on the whole they are larger. The high sensitivity of the\nMeerKAT survey also enabled us to detect the bright end of the SMC Planetary\nNebulae (PNe) sample - point-like radio emission is associated with 38 of 102\noptically known PNe, of which 19 are new detections. Lastly, we present the\ndetection of three foreground radio stars amidst 11 circularly polarised\nsources, and a few examples of morphologically interesting background radio\ngalaxies from which the radio ring galaxy ESO 029-G034 may represent a new type\nof radio object.", "cat": "astro-ph.GA", "authors": ["W. Cotton", "M. D. Filipovic", "F. Camilo", "R. Indebetouw", "R. Z. E. Alsaberi", "J. O. Anih", "M. Baker", "T . S. Bastian", "I. Bojicic", "E. Carli", "F. Cavallaro", "E. J. Crawford", "S. Dai", "F. Haberl", "L. Levin", "K. Luken", "C . M. Pennock", "N. Rajabpour", "B. W. Stappers", "J. Th. van Loon", "A. A. Zijlstra", "S. Buchner", "M. Geyer", "S. Goedhart", "M. Serylak"]}, "342": {"id": "2211.07333v1", "title": "WALLABY Pilot Survey: Public release of HI kinematic models for more than 100 galaxies from phase 1 of ASKAP pilot observations", "url": "http://arxiv.org/pdf/2211.07333v1", "date": "2022-11-14 13:13:54", "abs": "We present the Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY)\nPilot Phase I HI kinematic models. This first data release consists of HI\nobservations of three fields in the direction of the Hydra and Norma clusters,\nand the NGC 4636 galaxy group. In this paper, we describe how we generate and\npublicly release flat-disk tilted-ring kinematic models for 109/592 unique HI\ndetections in these fields. The modelling method adopted here - which we call\nthe WALLABY Kinematic Analysis Proto-Pipeline (WKAPP) and for which the\ncorresponding scripts are also publicly available - consists of combining\nresults from the homogeneous application of the FAT and 3DBAROLO algorithms to\nthe subset of 209 detections with sufficient resolution and S/N in order to\ngenerate optimized model parameters and uncertainties. The 109 models presented\nhere tend to be gas rich detections resolved by at least 3-4 synthesized beams\nacross their major axes, but there is no obvious environmental bias in the\nmodelling. The data release described here is the first step towards the\nderivation of similar products for thousands of spatially-resolved WALLABY\ndetections via a dedicated kinematic pipeline. Such a large publicly available\nand homogeneously analyzed dataset will be a powerful legacy product that that\nwill enable a wide range of scientific studies.", "cat": "astro-ph.GA", "authors": ["N. Deg", "K. Spekkens", "T. Westmeier", "T. N. Reynolds", "P. Venkataraman", "S. Goliath", "A. X. Shen", "R. Halloran", "A. Bosma", "B. Catinella", "W. J. G. de Blok", "H. D\u00e9nes", "E. M. Di Teodoro", "A. Elagali", "B. -Q. For", "C. Howlett", "G. I. G. J\u00f3zsa", "P. Kamphuis", "D. Kleiner", "B. Koribalski", "K. Lee-Waddell", "F. Lelli", "X. Lin", "C. Murugeshan", "S. Oh", "J. Rhee", "T. C. Scott", "L. Staveley-Smith", "J. M. van der Hulst", "L. Verdes-Montenegro", "J. Wang", "O. I. Wong"]}, "343": {"id": "0905.3449v1", "title": "Post-AGB stars in the AKARI survey", "url": "http://arxiv.org/pdf/0905.3449v1", "date": "2009-05-21 07:47:05", "abs": "Obscured by their circumstellar dusty envelopes post-AGB stars emit a large\nfraction of their energy in the infrared and thus, infrared sky surveys like\nIRAS were essential for discoveries of post-AGBs in the past. Now, with the\nAKARI infrared sky survey we can extend our knowledge about the late stages of\nstellar evolution. The long-term goal of our work is to define new photometric\ncriteria to distinguish new post-AGB candidates from the AKARI data.", "cat": "astro-ph.SR", "authors": ["Natasza Siodmiak", "Nick Cox", "Ryszard Szczerba", "Pedro Garcia-Lario"]}, "344": {"id": "1310.6468v1", "title": "Measurement of $H(z)$ and $D_A(z)$ from the two-dimensional power spectrum of Sloan Digital Sky Survey luminous red galaxies", "url": "http://arxiv.org/pdf/1310.6468v1", "date": "2013-10-24 02:53:31", "abs": "We present a method to measure the Hubble parameter $H(z)$ and the angular\ndiameter distance $D_A(z)$ simultaneously from the two-dimensional matter power\nspectrum from galaxy surveys with broad sky coverage. We validate this method\nby applying it to the LasDamas mock galaxy catalogs. Then we apply this method\nto Sloan Digital Sky Survey (SDSS) Data Release 7 and obtain measurements of\n$\\Omega_mh^2=0.1268 \\pm 0.0085$, $H(z=0.35)=81.3\\pm 3.8$km/s/Mpc, $D_A(z=0.35)\n= 1037\\pm44$Mpc, without assuming a dark energy model or a flat universe. We\nalso find that the derived parameters $H(0.35)r_s(z_d)/c=0.0431 \\pm 0.0018$ and\n$D_A(0.35)/r_s(z_d)=6.48 \\pm 0.25$. These are in excellent agreement with\nsimilar measurements from the two-dimensional correlation function of the same\ndata.", "cat": "astro-ph.CO", "authors": ["Maddumage Don P. Hemantha", "Yun Wang", "Chia-Hsun Chuang"]}, "345": {"id": "1510.01631v1", "title": "The VISTA Carina Nebula Survey II. Spatial distribution of the infrared-excess-selected young stellar population", "url": "http://arxiv.org/pdf/1510.01631v1", "date": "2015-10-06 15:35:46", "abs": "We performed a deep wide-field (6.76 deg^2) near-infrared survey with the\nVISTA telescope that covers the entire extent of the Carina nebula complex\n(CNC). The point-source catalog created from these data contains around four\nmillion individual objects down to masses of 0.1 M_sun. We present a\nstatistical study of the large-scale spatial distribution and an investigation\nof the clustering properties of infrared-excesses objects, which are used to\ntrace disk-bearing young stellar objects (YSOs). We find that a (J - H) versus\n(Ks - [4.5]) color-color diagram is well suited to tracing the population of\nYSO-candidates (cYSOs) by their infrared excess. We identify 8781 sources with\nstrong infrared excess, which we consider as cYSOs. This sample is used to\ninvestigate the spatial distribution of the cYSOs with a nearest-neighbor\nanalysis. The surface density distribution of cYSOs agrees well with the shape\nof the clouds as seen in our Herschel far-infrared survey. The strong decline\nin the surface density of excess sources outside the area of the clouds\nsupports the hypothesis that our excess-selected sample consists predominantly\nof cYSOs with a low level of background contamination. This analysis allows us\nto identify 14 groups of cYSOs outside the central area. Our results suggest\nthat the total population of cYSOs in the CNC comprises about 164000 objects,\nwith a substantial fraction (~35%) located in the northern, still not well\nstudied parts. Our cluster analysis suggests that roughly half of the cYSOs\nconstitute a non-clustered, dispersed population.", "cat": "astro-ph.SR", "authors": ["Peter Zeidler", "Thomas Preibisch", "Thorsten Ratzka", "Veronica Roccatagliata", "Monika G. Petr-Gotzens"]}, "346": {"id": "2102.13027v4", "title": "A Survey of RDF Stores & SPARQL Engines for Querying Knowledge Graphs", "url": "http://arxiv.org/pdf/2102.13027v4", "date": "2021-10-13 06:15:01", "abs": "RDF has seen increased adoption in recent years, prompting the\nstandardization of the SPARQL query language for RDF, and the development of\nlocal and distributed engines for processing SPARQL queries. This survey paper\nprovides a comprehensive review of techniques and systems for querying RDF\nknowledge graphs. While other reviews on this topic tend to focus on the\ndistributed setting, the main focus of the work is on providing a comprehensive\nsurvey of state-of-the-art storage, indexing and query processing techniques\nfor efficiently evaluating SPARQL queries in a local setting (on one machine).\nTo keep the survey self-contained, we also provide a short discussion on graph\npartitioning techniques used in the distributed setting. We conclude by\ndiscussing contemporary research challenges for further improving SPARQL query\nengines. This extended version also provides a survey of over one hundred\nSPARQL query engines and the techniques they use, along with twelve benchmarks\nand their features.", "cat": "cs.DB", "authors": ["Waqas Ali", "Muhammad Saleem", "Bin Yao", "Aidan Hogan", "Axel-Cyrille Ngonga Ngomo"]}, "347": {"id": "1403.0975v4", "title": "A Near-Infrared Survey of the Inner Galactic Plane for Wolf-Rayet Stars III. New Methods: Faintest WR Stars", "url": "http://arxiv.org/pdf/1403.0975v4", "date": "2015-06-15 14:55:52", "abs": "A new method of image subtraction is applied to images from a J, K, and\nnarrow-band imaging survey of 300 square degrees of the plane of the Galaxy,\nsearching for new Wolf-Rayet stars. Our survey spans 150 degrees in Galactic\nlongitude and reaches 1 degree above and below the Galactic plane. The survey\nhas a useful limiting magnitude of K =15 over most of the observed Galactic\nplane, and K =14 (due to severe crowding) within a few degrees of the Galactic\ncenter. The new image subtraction method described here (better than aperture\nor even point-spread-function photometry in very crowded fields) detected\nseveral thousand emission-line candidates. In June and July 2011 and 2012, we\nspectroscopically followed up on 333 candidates with MDM-TIFKAM and IRTF-SPEX,\ndiscovering 89 emission-line sources. These include 49 Wolf-Rayet stars, 43 of\nthem previously unidentified, including the most distant known Galactic WR\nstars, more than doubling the number on the far side of the Milky Way. We also\ndemonstrate our survey's ability to detect very faint PNe and other NIR\nemission objects.", "cat": "astro-ph.SR", "authors": ["Graham C. Kanarek", "Michael M. Shara", "Jacqueline K. Faherty", "David Zurek", "Anthony F. J. Moffat"]}, "348": {"id": "2211.12523v2", "title": "Constraints on modified gravity from the BOSS galaxy survey", "url": "http://arxiv.org/pdf/2211.12523v2", "date": "2023-03-19 18:30:20", "abs": "We develop a pipeline to set new constraints on scale-independent modified\ngravity, from the galaxy power spectrum in redshift space of BOSS DR12. The\nlatter is modelled using the effective field theory of large-scale structure up\nto 1-loop order in perturbation theory. We test our pipeline on synthetic and\nsimulated data, to assess systematic biases on the inferred cosmological\nparameters due to marginalization and theoretical errors, and we apply it to\nthe normal branch of the DGP model with a $\\Lambda$CDM background. When applied\nto synthetic data and cosmological simulations, we observe biased posteriors\ndue to the strong degeneracy between the nDGP parameter $\\Omega_{\\rm rc}$ and\nthe primordial amplitude of fluctuations $A_s$. Fixing the latter to the Planck\ncentral value, we obtain a posterior distribution with $\\Omega_{\\rm rc}\\lesssim\n0.65$ at 95$\\%$ C.L., under the assumption of a flat prior on $\\log_{10}\n\\Omega_{\\rm rc}$. This upper bound, however, depends strongly on the prior on\n$\\Omega_{\\rm rc}$. To alleviate this effect, we provide an upper bound based on\nthe Bayes factor between the nDGP model and $\\Lambda$CDM model, which gives\n$\\Omega_{\\rm rc}\\lesssim 0.2$ at 95$\\%$ C.L..", "cat": "astro-ph.CO", "authors": ["Lorenzo Piga", "Marco Marinucci", "Guido D'Amico", "Massimo Pietroni", "Filippo Vernizzi", "Bill S. Wright"]}, "349": {"id": "2103.09274v1", "title": "A survey of deep neural network watermarking techniques", "url": "http://arxiv.org/pdf/2103.09274v1", "date": "2021-03-16 18:35:07", "abs": "Protecting the Intellectual Property Rights (IPR) associated to Deep Neural\nNetworks (DNNs) is a pressing need pushed by the high costs required to train\nsuch networks and the importance that DNNs are gaining in our society.\nFollowing its use for Multimedia (MM) IPR protection, digital watermarking has\nrecently been considered as a mean to protect the IPR of DNNs. While DNN\nwatermarking inherits some basic concepts and methods from MM watermarking,\nthere are significant differences between the two application areas, calling\nfor the adaptation of media watermarking techniques to the DNN scenario and the\ndevelopment of completely new methods. In this paper, we overview the most\nrecent advances in DNN watermarking, by paying attention to cast it into the\nbulk of watermarking theory developed during the last two decades, while at the\nsame time highlighting the new challenges and opportunities characterizing DNN\nwatermarking. Rather than trying to present a comprehensive description of all\nthe methods proposed so far, we introduce a new taxonomy of DNN watermarking\nand present a few exemplary methods belonging to each class. We hope that this\npaper will inspire new research in this exciting area and will help researchers\nto focus on the most innovative and challenging problems in the field.", "cat": "cs.CR", "authors": ["Yue Li", "Hongxia Wang", "Mauro Barni"]}, "350": {"id": "2402.02455v1", "title": "A Survey on Decentralized Identifiers and Verifiable Credentials", "url": "http://arxiv.org/pdf/2402.02455v1", "date": "2024-02-04 11:55:14", "abs": "Digital identity has always been considered the keystone for implementing\nsecure and trustworthy communications among parties. The ever-evolving digital\nlandscape has gone through many technological transformations that have also\naffected the way entities are digitally identified. During this digital\nevolution, identity management has shifted from centralized to decentralized\napproaches. The last era of this journey is represented by the emerging\nSelf-Sovereign Identity (SSI), which gives users full control over their data.\nSSI leverages decentralized identifiers (DIDs) and verifiable credentials\n(VCs), which have been recently standardized by the World Wide Web Community\n(W3C). These technologies have the potential to build more secure and\ndecentralized digital identity systems, remarkably contributing to\nstrengthening the security of communications that typically involve many\ndistributed participants. It is worth noting that the scope of DIDs and VCs\nextends beyond individuals, encompassing a broad range of entities including\ncloud, edge, and Internet of Things (IoT) resources. However, due to their\nnovelty, existing literature lacks a comprehensive survey on how DIDs and VCs\nhave been employed in different application domains, which go beyond SSI\nsystems. This paper provides readers with a comprehensive overview of such\ntechnologies from different perspectives. Specifically, we first provide the\nbackground on DIDs and VCs. Then, we analyze available implementations and\noffer an in-depth review of how these technologies have been employed across\ndifferent use-case scenarios. Furthermore, we examine recent regulations and\ninitiatives that have been emerging worldwide. Finally, we present some\nchallenges that hinder their adoption in real-world scenarios and future\nresearch directions.", "cat": "cs.CR", "authors": ["Carlo Mazzocca", "Abbas Acar", "Selcuk Uluagac", "Rebecca Montanari", "Paolo Bellavista", "Mauro Conti"]}, "351": {"id": "0809.3981v1", "title": "Surveying Pseudomoduli: the Good, the Bad and the Incalculable", "url": "http://arxiv.org/pdf/0809.3981v1", "date": "2008-09-23 18:50:43", "abs": "We classify possible types of pseudomoduli which arise when supersymmetry is\ndynamically broken in infrared-free low-energy theories. We show that, even if\nthe pseudomoduli potential is generated only at higher loops, there is a regime\nwhere the potential can be simply determined from a combination of one-loop\nrunning data. In this regime, we compute whether the potential for the various\ntypes of pseudomoduli is safe, has a dangerous runaway to the UV cutoff of the\nlow-energy theory, or is incalculable. Our results are applicable to building\nnew models of supersymmetry breaking. We apply the results to survey large\nclasses of models.", "cat": "hep-th", "authors": ["Kenneth Intriligator", "David Shih", "Matthew Sudano"]}, "352": {"id": "2310.14414v2", "title": "Vision Language Models in Autonomous Driving: A Survey and Outlook", "url": "http://arxiv.org/pdf/2310.14414v2", "date": "2024-06-20 19:36:38", "abs": "The applications of Vision-Language Models (VLMs) in the field of Autonomous\nDriving (AD) have attracted widespread attention due to their outstanding\nperformance and the ability to leverage Large Language Models (LLMs). By\nincorporating language data, driving systems can gain a better understanding of\nreal-world environments, thereby enhancing driving safety and efficiency. In\nthis work, we present a comprehensive and systematic survey of the advances in\nvision language models in this domain, encompassing perception and\nunderstanding, navigation and planning, decision-making and control, end-to-end\nautonomous driving, and data generation. We introduce the mainstream VLM tasks\nin AD and the commonly utilized metrics. Additionally, we review current\nstudies and applications in various areas and summarize the existing\nlanguage-enhanced autonomous driving datasets thoroughly. Lastly, we discuss\nthe benefits and challenges of VLMs in AD and provide researchers with the\ncurrent research gaps and future trends.", "cat": "cs.CV", "authors": ["Xingcheng Zhou", "Mingyu Liu", "Ekim Yurtsever", "Bare Luka Zagar", "Walter Zimmer", "Hu Cao", "Alois C. Knoll"]}, "353": {"id": "1012.1727v1", "title": "Cross-correlation of the 2XMMi catalogue with Data Release 7 of the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1012.1727v1", "date": "2010-12-08 10:11:25", "abs": "The Survey Science Centre of the XMM-Newton satellite released the first\nincremental version of the 2XMM catalogue in August 2008 . With more than\n220,000 X-ray sources, the 2XMMi was at that time the largest catalogue of\nX-ray sources ever published and thus constitutes an unprecedented resource for\nstudying the high-energy properties of various classes of X-ray emitters such\nas AGN and stars. The advent of the 7th release of the Sloan Digital Sky Survey\noffers the opportunity to cross-match two major surveys and extend the spectral\nenergy distribution of many 2XMMi sources towards the optical bands. We here\npresent a cross-matching algorithm based on the classical likelihood ratio\nestimator. The method developed has the advantage of providing true\nprobabilities of identifications without resorting to Monte-Carlo simulations.\nOver 30,000 2XMMi sources have SDSS counterparts with individual probabilities\nof identification higher than 90%. Using spectroscopic identifications from the\nSDSS DR7 catalogue supplemented by extraction from other catalogues, we build\nan identified sample from which the way the various classes of X-ray emitters\ngather in the multi dimensional parameter space can be analysed. We investigate\ntwo scientific use cases. In the first example we show how these\nmulti-wavelength data can be used to search for new QSO2s. Although no specific\nrange of observed properties allows us to identify Compton Thick QSO2s, we show\nthat the prospects are much better for Compton Thin AGN2 and discuss several\npossible multi-parameter selection strategies. In a second example, we confirm\nthe hardening of the mean X-ray spectrum with increasing X-ray luminosity on a\nsample of over 500 X-ray active stars and reveal that on average X-ray active M\nstars display bluer $g-r$ colour indexes than less active ones (abridged).", "cat": "astro-ph.HE", "authors": ["F. -X. Pineau", "C. Motch", "F. Carrera", "R. Della Ceca", "S. Derriere", "L. Michel", "A. Schwope", "M. G. Watson"]}, "354": {"id": "1507.02657v1", "title": "The population of galaxy-galaxy strong lenses in forthcoming optical imaging surveys", "url": "http://arxiv.org/pdf/1507.02657v1", "date": "2015-07-09 19:06:07", "abs": "Ongoing and future imaging surveys represent significant improvements in\ndepth, area and seeing compared to current data-sets. These improvements offer\nthe opportunity to discover up to three orders of magnitude more galaxy-galaxy\nstrong lenses than are currently known. In this work we forecast the number of\nlenses discoverable in forthcoming surveys and simulate their properties. We\ngenerate a population of statistically realistic strong lenses and simulate\nobservations of this population for the Dark Energy Survey (DES), Large\nSynoptic Survey Telescope (LSST) and Euclid surveys. We verify our model\nagainst the galaxy-scale lens search of the Canada-France-Hawaii Telescope\nLegacy Survey (CFHTLS), predicting 250 discoverable lenses compared to 220\nfound by Gavazzi et al (2014). The predicted Einstein radius distribution is\nalso remarkably similar to that found by Sonnenfeld et al (2013). For future\nsurveys we find that, assuming Poisson limited lens galaxy subtraction,\nsearches in DES, LSST and Euclid datasets should discover 2400, 120000, and\n170000 galaxy-galaxy strong lenses respectively. Finders using blue minus red\n(g-i) difference imaging for lens subtraction can discover 1300 and 62000\nlenses in DES and LSST. The uncertainties on the model are dominated by the\nhigh redshift source population which typically gives fractional errors on the\ndiscoverable lens number at the tens of percent level. We find that doubling\nthe signal-to-noise ratio required for a lens to be detectable, approximately\nhalves the number of detectable lenses in each survey, indicating the\nimportance of understanding the selection function and sensitivity of future\nlens finders in interpreting strong lens statistics. We make our population\nforecasting and simulated observation codes publicly available so that the\nselection function of strong lens finders can easily be calibrated.", "cat": "astro-ph.CO", "authors": ["Thomas E Collett"]}, "355": {"id": "1211.0748v1", "title": "FAST low frequency pulsar survey", "url": "http://arxiv.org/pdf/1211.0748v1", "date": "2012-11-05 02:47:53", "abs": "The Five-hundred-meter Aperture Spherical radio Telescope (FAST) is under\nconstruction and will be commissioned in September 2016. A low frequency 7-beam\nreceiver working around 400 MHz is proposed for FAST early science. It will be\noptimized for a whole FAST sky drift-scan pulsar survey. Simulations show that\nabout 1500 new normal pulsars will be discovered, as while as about 200\nmillisecond pulsars.", "cat": "astro-ph.IM", "authors": ["Youling Yue", "Di Li", "Rendong Nan"]}, "356": {"id": "1201.5393v2", "title": "SN 2006oz: rise of a super-luminous supernova observed by the SDSS-II SN Survey", "url": "http://arxiv.org/pdf/1201.5393v2", "date": "2012-05-18 23:13:46", "abs": "We study SN 2006oz, a newly-recognized member of the class of H-poor,\nsuper-luminous supernovae. We present multi-color light curves from the SDSS-II\nSN Survey, that cover the rise time, as well as an optical spectrum that shows\nthat the explosion occurred at z~0.376. We fitted black body functions to\nestimate the temperature and radius evolution of the photosphere and used the\nparametrized code SYNOW to model the spectrum. We constructed a bolometric\nlight curve and compared it with explosion models. The very early light curves\nshow a dip in the g- and r-bands and a possible initial cooling phase in the\nu-band before rising to maximum light. The bolometric light curve shows a\nprecursor plateau with a duration of 6-10 days in the rest-frame. A lower limit\nof M_u < -21.5 can be placed on the absolute peak luminosity of the SN, while\nthe rise time is constrained to be at least 29 days. During our observations,\nthe emitting sphere doubled its radius to 2x10^15 cm, while the temperature\nremained hot at 15000 K. As for other similar SNe, the spectrum is best modeled\nwith elements including O II and Mg II, while we tentatively suggest that Fe\nIII might be present. We suggest that the precursor plateau might be related to\na recombination wave in a circumstellar medium (CSM) and discuss whether this\nis a common property of all similar explosions. The subsequent rise can be\nequally well described by input from a magnetar or by ejecta-CSM interaction,\nbut the models are not well constrained owing to the lack of post-maximum\nobservations, and CSM interaction has difficulties accounting for the precursor\nplateau self-consistently. Radioactive decay is less likely to be the mechanism\nthat powers the luminosity. The host galaxy, detected in deep imaging with the\n10 m GTC, is a moderately young and star-forming, but not a starburst, galaxy.\nIt has an absolute magnitude of M_g = -16.9.", "cat": "astro-ph.SR", "authors": ["G. Leloudas", "E. Chatzopoulos", "B. Dilday", "J. Gorosabel", "J. Vinko", "A. Gallazzi", "J. C. Wheeler", "B. Bassett", "J. A. Fischer", "J. A. Frieman", "J. P. U. Fynbo", "A. Goobar", "M. Jelinek", "D. Malesani", "R. C. Nichol", "J. Nordin", "L. Ostman", "M. Sako", "D. P. Schneider", "M. Smith", "J. Sollerman", "M. D. Stritzinger", "C. C. Thoene", "A. de Ugarte Postigo"]}, "357": {"id": "2011.03556v1", "title": "Void Probability Function of Simulated Surveys of high-redshift Lyman-Alpha Emitters", "url": "http://arxiv.org/pdf/2011.03556v1", "date": "2020-11-06 19:00:05", "abs": "We calculate the void probability function (VPF) in simulations of\nLyman-$\\alpha$ emitters (LAEs) across a wide redshift range ($z=3.1,\\ 4.5,\\\n5.7,\\ 6.6$). The VPF measures the zero-point correlation function (i.e. places\ndevoid of galaxies) and naturally connects to higher order correlation\nfunctions while being computationally simple to calculate. We explore the\nPoissonian and systematic errors on the VPF, specify its accuracy as a function\nof average source density and the volume probed, and provide the appropriate\nsize scales to measure the VPF. At small radii the accuracy of the VPF is\nlimited by galaxy density, while at large radii the VPF is limited by the\nnumber of independent volumes probed. We also offer guidelines for\nunderstanding and quantifying the error in the VPF. We approximate the error in\nthe VPF by using independent sub-volumes of the catalogs, after finding that\njackknife statistics underestimate the uncertainty. We use the VPF to probe the\nstrength of higher order correlation functions by measuring and examining the\nhierarchical scaling between the correlation functions using count-in-cells.\nThe negative binomial model (NBM) has been shown to best describe the scaling\nbetween the two point correlation function and VPF for low-redshift galaxy\nobservations. We further test the fit of the NBM by directly deriving the\nvolume averaged two-point correlation function from the VPF and vice versa. We\nfind the NBM best describes the $z=3.1, 4.5, 5.7$ simulated LAEs, with a\n1$\\sigma$ deviation from the model in the $z=6.6$ catalog. This suggests that\nLAEs show higher order clustering terms similar to those of normal low redshift\ngalaxies.", "cat": "astro-ph.GA", "authors": ["Lucia A. Perez", "Sangeeta Malhotra", "James E. Rhoads", "Vithal Tilvi"]}, "358": {"id": "1903.10768v2", "title": "The MURALES survey II. Presentation of MUSE observations of 20 3C low-z radio galaxies and first results", "url": "http://arxiv.org/pdf/1903.10768v2", "date": "2019-10-15 06:17:36", "abs": "We present observations of a complete sub-sample of 20 radio galaxies from\nthe Third Cambridge Catalog (3C) with redshift <0.3 obtained from VLT/MUSE\noptical integral field spectrograph. These data have been obtained as part of\nthe survey MURALES (a MUse RAdio Loud Emission line Snapshot survey) with the\nmain goal of exploring the Active Galactic Nuclei (AGN) feedback process in a\nsizeable sample of the most powerful radio sources at low redshift. We present\nthe data analysis and, for each source, the resulting emission line images and\nthe 2D gas velocity field. Thanks to their unprecedented depth (the median 3\nsigma surface brightness limit in the emission line maps is 6X10^-18 erg s-1\ncm-2 arcsec-2, these observations reveal emission line structures extending to\nseveral tens of kiloparsec in most objects. In nine sources the gas velocity\nshows ordered rotation, but in the other cases it is highly complex. 3C sources\nshow a connection between radio morphology and emission line properties.\nWhereas, in three of the four Fanaroff and Riley Class I radio galaxies (FRIs),\nthe line emission regions are compact, ~1 kpc in size; in all but one of the\nClass II radiogalaxies FRIIs, we detected large scale structures of ionized gas\nwith a median extent of 17 kpc. Among the FRIIs, those of high and low\nexcitation show extended gas structures with similar morphological properties,\nsuggesting that they both inhabit regions characterized by a rich gaseous\nenvironment on kpc scale.", "cat": "astro-ph.GA", "authors": ["B. Balmaverde", "A. Capetti", "A. Marconi", "G. Venturi", "M. Chiaberge", "R. Baldi", "S. Baum", "R. Gilli", "P. Grandi", "E. Meyer", "G. Miley", "C. O'Dea", "W. Sparks", "E. Torresi", "G. Tremblay"]}, "359": {"id": "0901.2248v1", "title": "Analysis of the RC catalog sample in the region overlapping with the regions of the FIRST and SDSS surveys: I. Identification of sources with the VLSS, TXS, NVSS, FIRST, and GB6 catalogs", "url": "http://arxiv.org/pdf/0901.2248v1", "date": "2009-01-15 15:19:35", "abs": "Radio sources of the RC catalog produced in 1980--1985 at RATAN-600 radio\ntelescope based on a deep survey of a sky strip centered on the declination of\nthe SS 433 source are optically identified in the region overlapping with FIRST\nand SDSS surveys (about 132 square degrees). The NVSS catalog was used as the\nreference catalog for refining the coordinates of the radio sources. The\nmorphology is found for about 75% of the objects of the sample and the ratio of\nsingle, double and multicomponent radio sources is computed based on FIRST\nradio maps. The 74, 365, 1400, and 4850 MHz data of the VLSS, TXS, NVSS, FIRST,\nand GB6 catalogs are used to analyze the shape of the spectra.", "cat": "astro-ph.CO", "authors": ["O. P. Zhelenkova", "A. I. Kopylov"]}, "360": {"id": "2006.11391v1", "title": "Computer Vision with Deep Learning for Plant Phenotyping in Agriculture: A Survey", "url": "http://arxiv.org/pdf/2006.11391v1", "date": "2020-06-18 14:21:19", "abs": "In light of growing challenges in agriculture with ever growing food demand\nacross the world, efficient crop management techniques are necessary to\nincrease crop yield. Precision agriculture techniques allow the stakeholders to\nmake effective and customized crop management decisions based on data gathered\nfrom monitoring crop environments. Plant phenotyping techniques play a major\nrole in accurate crop monitoring. Advancements in deep learning have made\npreviously difficult phenotyping tasks possible. This survey aims to introduce\nthe reader to the state of the art research in deep plant phenotyping.", "cat": "cs.CV", "authors": ["Akshay L Chandra", "Sai Vikas Desai", "Wei Guo", "Vineeth N Balasubramanian"]}, "361": {"id": "1604.06462v1", "title": "The Next Generation Virgo Cluster Survey (NGVS). XIII. The Luminosity and Mass Function of Galaxies in the Core of the Virgo Cluster and the Contribution from Disrupted Satellites", "url": "http://arxiv.org/pdf/1604.06462v1", "date": "2016-04-21 20:00:05", "abs": "We present measurements of the galaxy luminosity and stellar mass function in\na 3.71 deg$^2$ (0.3 Mpc$^2$) area in the core of the Virgo cluster, based on\n$ugriz$ data from the Next Generation Virgo Cluster Survey (NGVS). The galaxy\nsample consists of 352 objects brighter than $M_g=-9.13$ mag, the 50%\ncompleteness limit of the survey. Using a Bayesian analysis, we find a best-fit\nfaint end slope of $\\alpha=-1.33 \\pm 0.02$ for the g-band luminosity function;\nconsistent results are found for the stellar mass function as well as the\nluminosity function in the other four NGVS bandpasses. We discuss the\nimplications for the faint-end slope of adding 92 ultra compact dwarfs galaxies\n(UCDs) -- previously compiled by the NGVS in this region -- to the galaxy\nsample, assuming that UCDs are the stripped remnants of nucleated dwarf\ngalaxies. Under this assumption, the slope of the luminosity function (down to\nthe UCD faint magnitude limit, $M_g = -9.6$ mag) increases dramatically, up to\n$\\alpha = -1.60 \\pm 0.06$ when correcting for the expected number of disrupted\nnon-nucleated galaxies. We also calculate the total number of UCDs and globular\nclusters that may have been deposited in the core of Virgo due to the\ndisruption of satellites, both nucleated and non-nucleated. We estimate that\n~150 objects with $M_g\\lesssim-9.6$ mag and that are currently classified as\nglobular clusters, might, in fact, be the nuclei of disrupted galaxies. We\nfurther estimate that as many as 40% of the (mostly blue) globular clusters in\nthe core of Virgo might once have belonged to such satellites; these same\ndisrupted satellites might have contributed ~40% of the total luminosity in\ngalaxies observed in the core region today. Finally, we use an updated Local\nGroup galaxy catalog to provide a new measurement of the luminosity function of\nLocal Group satellites, $\\alpha=-1.21\\pm0.05$.", "cat": "astro-ph.GA", "authors": ["Laura Ferrarese", "Patrick Cote", "Ruben Sanchez-Janssen", "Joel Roediger", "Alan W. McConnachie", "Patrick R. Durrell", "Lauren A. MacArthur", "John P. Blakeslee", "Pierre-Alain Duc", "S. Boissier", "Alessandro Boselli", "Stephane Courteau", "Jean-Charles Cuillandre", "Eric Emsellem", "S. D. J. Gwyn", "Puragra Guhathakurta", "Andres Jordan", "Ariane Lancon", "Chengze Liu", "Simona Mei", "J. Christopher Mihos", "Thomas H. Puzia", "James E. Taylor", "Hongxin Zhang"]}, "362": {"id": "2108.04087v1", "title": "Reinforcement Learning for Intelligent Healthcare Systems: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2108.04087v1", "date": "2021-08-05 18:47:17", "abs": "The rapid increase in the percentage of chronic disease patients along with\nthe recent pandemic pose immediate threats on healthcare expenditure and\nelevate causes of death. This calls for transforming healthcare systems away\nfrom one-on-one patient treatment into intelligent health systems, to improve\nservices, access and scalability, while reducing costs. Reinforcement Learning\n(RL) has witnessed an intrinsic breakthrough in solving a variety of complex\nproblems for diverse applications and services. Thus, we conduct in this paper\na comprehensive survey of the recent models and techniques of RL that have been\ndeveloped/used for supporting Intelligent-healthcare (I-health) systems. This\npaper can guide the readers to deeply understand the state-of-the-art regarding\nthe use of RL in the context of I-health. Specifically, we first present an\noverview for the I-health systems challenges, architecture, and how RL can\nbenefit these systems. We then review the background and mathematical modeling\nof different RL, Deep RL (DRL), and multi-agent RL models. After that, we\nprovide a deep literature review for the applications of RL in I-health\nsystems. In particular, three main areas have been tackled, i.e., edge\nintelligence, smart core network, and dynamic treatment regimes. Finally, we\nhighlight emerging challenges and outline future research directions in driving\nthe future success of RL in I-health systems, which opens the door for\nexploring some interesting and unsolved problems.", "cat": "cs.LG", "authors": ["Alaa Awad Abdellatif", "Naram Mhaisen", "Zina Chkirbene", "Amr Mohamed", "Aiman Erbad", "Mohsen Guizani"]}, "363": {"id": "2011.08305v3", "title": "Dynamically Tagged Groups of Very Metal-poor Halo Stars from the HK and Hamburg/ESO Surveys", "url": "http://arxiv.org/pdf/2011.08305v3", "date": "2021-04-26 16:54:51", "abs": "We analyze the dynamical properties of $\\sim$1500 very metal-poor (VMP;\n[Fe/H] $\\lesssim -2.0$) halo stars, based primarily on medium-resolution\nspectroscopic data from the HK and Hamburg/ESO surveys. These data, collected\nover the past thirty years, are supplemented by a number of calibration stars\nand other small samples, along with astrometric information from $Gaia$ DR2. We\napply a clustering algorithm to the 4-D energy-action space of the sample, and\nidentify a set of 38 Dynamically Tagged Groups (DTGs), containing between 5 and\n30 member stars. Many of these DTGs can be associated with previously known\nprominent substructures such as $Gaia$-Sausage/Enceladus (GSE), Sequoia, the\nHelmi Stream (HStr), and Thamnos. Others are associated with previously\nidentified smaller dynamical groups of stars and streams. We identify 10 new\nDTGs as well, many of which have strongly retrograde orbits. We also\ninvestigate possible connections between our DTGs and $\\sim$300 individual\n$r$-process-enhanced (RPE) stars from a recent literature compilation. We find\nthat several of these objects have similar dynamical properties to GSE (5), the\nHStr (4), Sequoia (1), and Rg5 (1), indicating that their progenitors might\nhave been important sources of RPE stars in the Galaxy. Additionally, a number\nof our newly identified DTGs are shown to be associated with at least two RPE\nstars each (DTG-2: 3, DTG-7: 2; DTG-27: 2). Taken as a whole, these results are\nconsistent with ultra-faint and/or dwarf spheroidal galaxies as birth\nenvironments in which $r$-process nucleosynthesis took place, and then were\ndisrupted by the Milky Way.", "cat": "astro-ph.GA", "authors": ["Guilherme Limberg", "Silvia Rossi", "Timothy C. Beers", "H\u00e9lio D. Perottoni", "Angeles P\u00e9rez-Villegas", "Rafael M. Santucci", "Yuri Abuchaim", "Vinicius M. Placco", "Young Sun Lee", "Norbert Christlieb", "John E. Norris", "Michael S. Bessell", "Sean G. Ryan", "Ronald Wilhelm", "Jaehyon Rhee", "Anna Frebel"]}, "364": {"id": "1804.04589v1", "title": "A Survey on Neural Network-Based Summarization Methods", "url": "http://arxiv.org/pdf/1804.04589v1", "date": "2018-03-19 18:49:16", "abs": "Automatic text summarization, the automated process of shortening a text\nwhile reserving the main ideas of the document(s), is a critical research area\nin natural language processing. The aim of this literature review is to survey\nthe recent work on neural-based models in automatic text summarization. We\nexamine in detail ten state-of-the-art neural-based summarizers: five\nabstractive models and five extractive models. In addition, we discuss the\nrelated techniques that can be applied to the summarization tasks and present\npromising paths for future research in neural-based summarization.", "cat": "cs.CL", "authors": ["Yue Dong"]}, "365": {"id": "2007.07413v1", "title": "A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS", "url": "http://arxiv.org/pdf/2007.07413v1", "date": "2020-07-15 00:22:46", "abs": "We have conducted a comprehensive survey of emission-line galaxies at\n$z\\lesssim1.6$ based on narrowband (NB) imaging data taken with Hyper\nSuprime-Cam (HSC) on the Subaru telescope. In this paper, we update the\ncatalogs of H$\\alpha$, [OIII], and [OII] emission-line galaxies using the data\nfrom the second Public Data Release (PDR2) of Subaru Strategic Program (SSP) of\nHSC and Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS) survey along\nwith the spectroscopic redshifts for 2,019 emission-line galaxies selected with\nthe PDR1 data. The wider effective coverage of NB816 and NB921, 16.3 deg$^2$\nand 16.9 deg$^2$ respectively, are available in the Deep and UltraDeep layers\nof HSC-SSP from the PDR2. The CHORUS survey provides us with data with\nadditional three NBs (NB527, NB718, and NB973) in the COSMOS field in the\nUltraDeep layer (1.37 deg$^2$). The five NB datasets allow us to investigate\nthe star-forming galaxies presenting emission-lines at 14 specific redshifts\nranging from $z\\sim1.6$ down to $z\\sim0.05$. We revisit the distribution of\nlarge-scale structures and luminosity functions (LFs) for the emission-line\ngalaxies with the large samples of 75,377 emission-line galaxies selected. The\nredshift revolution of LFs shows that the star formation rate densities (SFRDs)\ndecreases monotonically from $z\\sim1.6$, which is consistent with the cosmic\nSFRD ever known. Our samples of emission-line galaxies covering a sufficiently\nlarge survey volume are useful to investigate the evolution of star-forming\ngalaxies since the cosmic noon in a wide range of environments including galaxy\nclusters, filaments, and voids.", "cat": "astro-ph.GA", "authors": ["Masao Hayashi", "Rhythm Shimakawa", "Masayuki Tanaka", "Masato Onodera", "Yusei Koyama", "Akio K. Inoue", "Yutaka Komiyama", "Chien-Hsiu Lee", "Yen-Ting Lin", "Kiyoto Yabe"]}, "366": {"id": "1709.00553v2", "title": "Dynamic Shortest Path and Transitive Closure Algorithms: A Survey", "url": "http://arxiv.org/pdf/1709.00553v2", "date": "2017-10-29 15:15:14", "abs": "Algorithms which compute properties over graphs have always been of interest\nin computer science, with some of the fundamental algorithms, such as\nDijkstra's algorithm, dating back to the 50s. Since the 70s there as been\ninterest in computing over graphs which are constantly changing, in a way which\nis more efficient than simple recomputing after each time the graph changes. In\nthis paper we provide a survey of both the foundational, and the state of the\nart, algorithms which solve either shortest path or transitive closure problems\nin either fully or partially dynamic graphs. We balance this with the known\nconditional lowerbounds.", "cat": "cs.DS", "authors": ["Daniel P. Martin"]}, "367": {"id": "2307.07861v1", "title": "Radar Odometry for Autonomous Ground Vehicles: A Survey of Methods and Datasets", "url": "http://arxiv.org/pdf/2307.07861v1", "date": "2023-07-15 17:58:38", "abs": "Radar odometry has been gaining attention in the last decade. It stands as\none of the best solutions for robotic state estimation in unfavorable\nconditions; conditions where other interoceptive and exteroceptive sensors may\nfall short. Radars are widely adopted, resilient to weather and illumination,\nand provide Doppler information which make them very attractive for such tasks.\nThis article presents an extensive survey of the latest work on ground-based\nradar odometry for autonomous robots. It covers technologies, datasets,\nmetrics, and approaches that have been developed in the last decade in addition\nto in-depth analysis and categorization of the various methods and techniques\napplied to tackle this problem. This article concludes with challenges and\nfuture recommendations to advance the field of radar odometry making it a great\nstarting point for newcomers and a valuable reference for experienced\nresearchers.", "cat": "cs.RO", "authors": ["Nader J. Abu-Alrub", "Nathir A. Rawashdeh"]}, "368": {"id": "2009.00153v2", "title": "The Separation and H-alpha Contrasts of Massive Accreting Planets in the Gaps of Transitional Disks: Predicted H-alpha Protoplanet Yields for Adaptive Optics Surveys", "url": "http://arxiv.org/pdf/2009.00153v2", "date": "2020-09-03 18:06:51", "abs": "We present a massive accreting gap (MAG) planet model that ensures large gaps\nin transitional disks are kept dust free by the scattering action of three\nco-planar quasi-circular planets in a 1:2:4 Mean Motion Resonance (MMR). This\nmodel uses the constraint of the observed gap size, and the dust-free nature of\nthe gap, to determine within ~10% the possible orbits for 3 massive planets in\nan MMR. Calculated orbits are consistent with the observed orbits and H-alpha\nemission (the brightest line to observe these planets) for LkCa 15 b and PDS 70\nb and PDS 70 c within observational errors. Moreover, the model suggests that\nthe scarcity of detected H-alpha planets is likely a selection effect of the\ncurrent limitations of non-coronagraphic, low (<10%) Strehl, H-alpha imaging\nwith Adaptive Optics (AO) systems used in past H-alpha surveys. We predict that\nas higher Strehl AO systems (with high-performance custom coronagraphs; like\n6.5-m Magellan Telescope MagAO-X system) are utilized at H-alpha the number of\ndetected gap planets will substantially increase by more than tenfold. For\nexample, we show that >25 new H-alpha \"gap planets\" are potentially\ndiscoverable by a survey of the best 19 transitional disks with MagAO-X.\nDetections of these accreting protoplanets will significantly improve our\nunderstanding of planet formation, planet growth and accretion, solar system\narchitectures, and planet disk interactions.", "cat": "astro-ph.EP", "authors": ["Laird M. Close"]}, "369": {"id": "2404.17693v1", "title": "A Survey Selection Correction using Nonrandom Followup with an Application to the Gender Entrepreneurship Gap", "url": "http://arxiv.org/pdf/2404.17693v1", "date": "2024-04-26 20:45:02", "abs": "Selection into samples undermines efforts to describe populations and to\nestimate relationships between variables. We develop a simple method for\ncorrecting for sample selection that explains differences in survey responses\nbetween early and late respondents with correlation between potential responses\nand preference for survey response. Our method relies on researchers observing\nthe number of data collection attempts prior to each individual's survey\nresponse rather than covariates that affect response rates without affecting\npotential responses. Applying our method to a survey of entrepreneurial\naspirations among undergraduates at University of Wisconsin-Madison, we find\nsuggestive evidence that the entrepreneurial aspiration rate is larger among\nsurvey respondents than the population, as well as the male-female gender gap\nin the entrepreneurial aspiration rate, which we estimate as 21 percentage\npoints in the sample and 19 percentage points in the population. Our results\nsuggest that the male-female gap in entrepreneurial aspirations arises prior to\ndirect exposure to the labor market.", "cat": "econ.EM", "authors": ["Clint Harris", "Jon Eckhardt", "Brent Goldfarb"]}, "370": {"id": "1507.05559v1", "title": "Lambda Bootis stars in the SuperWASP survey", "url": "http://arxiv.org/pdf/1507.05559v1", "date": "2015-07-20 16:44:59", "abs": "We have analysed around 170 000 individual photometric WASP measurements of\n15 well established lambda Bootis stars to search for variability. The lambda\nBootis stars are a small group of late-B to early-F, Pop. I, stars that show\nmoderate to extreme (surface) underabundances (up to a factor 100) of most\nFe-peak elements, but solar abundances of lighter elements (C, N, O and S).\nThey are excellent laboratories for the study of fundamental astrophysical\nprocesses such as diffusion, meridional circulation, stellar winds, and\naccretion in the presence of pulsation. From the 15 targets, eight are variable\nand seven are apparently constant with upper limits between 0.8 and 3.0 mmag.\nWe present a detailed time series analysis and a comparison with previously\npublished results. From an asteroseismologic study we conclude that the found\nchemical peculiarities are most probably restricted to the surface.", "cat": "astro-ph.SR", "authors": ["E. Paunzen", "M. Skarka", "P. Walczak", "D. L. Holdsworth", "B. Smalley", "R. G. West", "J. Janik"]}, "371": {"id": "2308.12499v3", "title": "Unveiling the solution to the final-parsec problem by combining milli-Hertz gravitational-wave observation and AGN survey", "url": "http://arxiv.org/pdf/2308.12499v3", "date": "2023-11-22 03:18:09", "abs": "Massive black hole binaries (MBHBs) could be the loudest gravitational-wave\n(GW) sources in milli-Hertz (mHz) GW band, but their dynamical evolution may\nstall when the black holes reach the innermost parsec of a galaxy. Such a\n\"final-parsec problem\" could be solved if MBHB forms in a gas-rich environment,\nsuch as an active galactic nucleus (AGN), but other solutions not involving\nAGNs also exist. Testing the correlation between these mHz GW sources and AGNs\nis difficult in real observation because AGNs are ubiquitous. To overcome this\ndifficult, we use a statistical method, first designed to constrain the host\ngalaxies of stellar-mass binary black holes, to search for a MBHB-AGN\ncorrelation in different astrophysical scenarios. We find that by detecting\nonly one MBHB at $z \\lesssim 0.5$, a mHz GW detector, such as the Laser\nInterferometer Space Antenna (LISA), can already distinguish different merger\nscenarios thanks to the precise localization of the source. Future detector\nnetworks and deeper AGNs surveys can further testify the MBHB-AGN correlation\nup to a redshift of $z\\sim 2$ even if only a small fraction of MBHBs merge\ninside AGNs. These constraints will help settle the long-standing debate on the\npossible solutions to the final-parsec problem.", "cat": "astro-ph.HE", "authors": ["Liang-Gui Zhu", "Xian Chen"]}, "372": {"id": "2012.01502v1", "title": "The SEDIGISM survey: Molecular clouds in the inner Galaxy", "url": "http://arxiv.org/pdf/2012.01502v1", "date": "2020-12-02 20:08:50", "abs": "We use the 13CO(2-1) emission from the SEDIGISM high-resolution spectral-line\nsurvey of the inner Galaxy, to extract the molecular cloud population with a\nlarge dynamic range in spatial scales, using the SCIMES algorithm. This work\ncompiles a cloud catalogue with a total of 10663 molecular clouds, 10300 of\nwhich we were able to assign distances and compute physical properties. We\nstudy some of the global properties of clouds using a science sample,\nconsisting of 6664 well resolved sources and for which the distance estimates\nare reliable. In particular, we compare the scaling relations retrieved from\nSEDIGISM to those of other surveys, and we explore the properties of clouds\nwith and without high-mass star formation. Our results suggest that there is no\nsingle global property of a cloud that determines its ability to form massive\nstars, although we find combined trends of increasing mass, size, surface\ndensity and velocity dispersion for the sub-sample of clouds with ongoing\nhigh-mass star formation. We then isolate the most extreme clouds in the\nSEDIGISM sample (i.e. clouds in the tails of the distributions) to look at\ntheir overall Galactic distribution, in search for hints of environmental\neffects. We find that, for most properties, the Galactic distribution of the\nmost extreme clouds is only marginally different to that of the global cloud\npopulation. The Galactic distribution of the largest clouds, the turbulent\nclouds and the high-mass star-forming clouds are those that deviate most\nsignificantly from the global cloud population. We also find that the least\ndynamically active clouds (with low velocity dispersion or low virial\nparameter) are situated further afield, mostly in the least populated areas.\nHowever, we suspect that part of these trends may be affected by some\nobservational biases, and thus require further follow up work in order to be\nconfirmed.", "cat": "astro-ph.GA", "authors": ["A. Duarte-Cabral", "D. Colombo", "J. S. Urquhart", "A. Ginsburg", "D. Russeil", "F. Schuller", "L. D. Anderson", "P. J. Barnes", "M. T. Beltran", "H. Beuther", "S. Bontemps", "L. Bronfman", "T. Csengeri", "C. L. Dobbs", "D. Eden", "A. Giannetti", "J. Kauffmann", "M. Mattern", "S. -N. X. Medina", "K. M. Menten", "M. -Y. Lee", "A. R. Pettitt", "M. Riener", "A. J. Rigby", "A. Trafficante", "V. S. Veena", "M. Wienen", "F. Wyrowski", "C. Agurto", "F. Azagra", "R. Cesaroni", "R. Finger", "E. Gonzalez", "T. Henning", "A. K. Hernandez", "J. Kainulainen", "S. Leurini", "S. Lopez", "F. Mac-Auliffe", "P. Mazumdar", "S. Molinari", "F. Motte", "E. Muller", "Q. Nguyen-Luong", "R. Parra", "J. -P. Perez-Beaupuits", "F. M. Montenegro-Montes", "T. J. T. Moore", "S. E. Ragan", "A. Sanchez-Monge", "A. Sanna", "P. Schilke", "E. Schisano", "N. Schneider", "S. Suri", "L. Testi", "K. Torstensson", "P. Venegas", "K. Wang", "A. Zavagno"]}, "373": {"id": "1712.03681v3", "title": "Revisiting the determinacy on New Keynesian Models: A survey", "url": "http://arxiv.org/pdf/1712.03681v3", "date": "2024-01-09 15:39:48", "abs": "The goal of this paper is to review some analytic techniques that are\npotentially useful to shed light on the determinacy question that arises in New\nKeynesian models as result of a combination of several monetary policy rules;\nin these models, we provide conditions to guarantee existence and uniqueness of\nequilibrium by means of results that are obtained from theoretical analysis. In\nparticular, these methods confirm the well known fact that Taylor--like rules\nin interest rate setting are not the only way to reach determinacy of the\nrational expectations equilibrium in the New Keynesian setting. The key\ntechnical tool we use for that purposes is the so--called Budan--Fourier\nTheorem, that we review along the paper. All the ideas and techniques presented\nhave been already used, our contribution that might be original here are the\norganization and emphasis.", "cat": "q-fin.EC", "authors": ["Alberto F. Boix", "Adri\u00e1n Segura Moreiras"]}, "374": {"id": "2110.06071v1", "title": "The SEDIGISM survey: The influence of spiral arms on the molecular gas distribution of the inner Milky Way", "url": "http://arxiv.org/pdf/2110.06071v1", "date": "2021-10-12 15:20:12", "abs": "The morphology of the Milky Way is still a matter of debate. In order to shed\nlight on uncertainties surrounding the structure of the Galaxy, in this paper,\nwe study the imprint of spiral arms on the distribution and properties of its\nmolecular gas. To do so, we take full advantage of the SEDIGISM survey that\nobserved a large area of the inner Galaxy in the $^{13}$CO(2-1) line at an\nangular resolution of 28\". We analyse the influences of the spiral arms by\nconsidering the features of the molecular gas emission as a whole across the\nlongitude-velocity map built from the full survey. Additionally, we examine the\nproperties of the molecular clouds in the spiral arms compared to the\nproperties of their counterparts in the inter-arm regions. Through flux and\nluminosity probability distribution functions, we find that the molecular gas\nemission associated with the spiral arms does not differ significantly from the\nemission between the arms. On average, spiral arms show masses per unit length\nof $\\sim10^5-10^6$ M$_{\\odot} $kpc$^{-1}$. This is similar to values inferred\nfrom data sets in which emission distributions were segmented into molecular\nclouds. By examining the cloud distribution across the Galactic plane, we infer\nthat the molecular mass in the spiral arms is a factor of 1.5 higher than that\nof the inter-arm medium, similar to what is found for other spiral galaxies in\nthe local Universe. We observe that only the distributions of cloud mass\nsurface densities and aspect ratio in the spiral arms show significant\ndifferences compared to those of the inter-arm medium; other observed\ndifferences appear instead to be driven by a distance bias. By comparing our\nresults with simulations and observations of nearby galaxies, we conclude that\nthe measured quantities would classify the Milky Way as a flocculent spiral\ngalaxy, rather than as a grand-design one.", "cat": "astro-ph.GA", "authors": ["D. Colombo", "A. Duarte-Cabral", "A. R. Pettitt", "J. S. Urquhart", "F. Wyrowski", "T. Csengeri", "K. R. Neralwar", "F. Schuller", "K. M. Menten", "L. Anderson", "P. Barnes", "H. Beuther", "L. Bronfman", "D. Eden", "A. Ginsburg", "T. Henning", "C. Koenig", "M. -Y. Lee", "M. Mattern", "S. Medina", "S. E. Ragan", "A. J. Rigby", "A. Sanchez-Monge", "A. Traficante", "A. Y. Yang", "M. Wienen"]}, "375": {"id": "1503.06216v2", "title": "Hydra II: a faint and compact Milky Way dwarf galaxy found in the Survey of the Magellanic Stellar History", "url": "http://arxiv.org/pdf/1503.06216v2", "date": "2015-04-02 18:45:49", "abs": "We present the discovery of a new dwarf galaxy, Hydra II, found\nserendipitously within the data from the ongoing Survey of the MAgellanic\nStellar History (SMASH) conducted with the Dark Energy Camera on the Blanco 4m\nTelescope. The new satellite is compact (r_h = 68 +/- 11 pc) and faint (M_V =\n-4.8 +/- 0.3), but well within the realm of dwarf galaxies. The stellar\ndistribution of HydraII in the color-magnitude diagram is well-described by a\nmetal-poor ([Fe/H] = -2.2) and old (13 Gyr) isochrone and shows a distinct blue\nhorizontal branch, some possible red clump stars, and faint stars that are\nsuggestive of blue stragglers. At a heliocentric distance of 134 +/- 10 kpc,\nHydra II is located in a region of the Galactic halo that models have suggested\nmay host material from the leading arm of the Magellanic Stream. A comparison\nwith N-body simulations hints that the new dwarf galaxy could be or could have\nbeen a satellite of the Magellanic Clouds.", "cat": "astro-ph.GA", "authors": ["Nicolas F. Martin", "David L. Nidever", "Gurtina Besla", "Knut Olsen", "Alistair R. Walker", "A. Katherina Vivas", "Robert A. Gruendl", "Catherine C. Kaleida", "Ricardo R. Mu\u00f1oz", "Robert D. Blum", "Abhijit Saha", "Blair C. Conn", "Eric F. Bell", "You-Hua Chu", "Maria-Rosa L. Cioni", "Thomas J. L. de Boer", "Carme Gallart", "Shoko Jin", "Andrea Kunder", "Steven R. Majewski", "David Martinez-Delgado", "Antonela Monachesi", "Matteo Monelli", "Lara Monteagudo", "Noelia E. D. No\u00ebl", "Edward W. Olszewski", "Guy S. Stringfellow", "Roeland P. van der Marel", "Denis Zaritsky"]}, "376": {"id": "1802.02583v1", "title": "The dragonfly nearby galaxies survey. Iv. A giant stellar disk in ngc 2841", "url": "http://arxiv.org/pdf/1802.02583v1", "date": "2018-02-07 19:00:02", "abs": "Neutral gas is commonly believed to dominate over stars in the outskirts of\ngalaxies, and investigations of the disk-halo interface are generally\nconsidered to be in the domain of radio astronomy. This may simply be a\nconsequence of the fact that deep HI observations typically probe to a lower\nmass surface density than visible wavelength data. This paper presents low\nsurface brightness optimized visible wavelength observations of the extreme\noutskirts of the nearby spiral galaxy NGC 2841. We report the discovery of an\nenormous low-surface brightness stellar disk in this object. When azimuthally\naveraged, the stellar disk can be traced out to a radius of $\\sim$70 kpc (5\n$R_{25}$ or 23 inner disk scale lengths). The structure in the stellar disk\ntraces the morphology of HI emission and extended UV emission. Contrary to\nexpectations, the stellar mass surface density does not fall below that of the\ngas mass surface density at any radius. In fact, at all radii greater than\n$\\sim$20 kpc, the ratio of the stellar to gas mass surface density is a\nconstant 3:1. Beyond $\\sim$30 kpc, the low surface brightness stellar disk\nbegins to warp, which may be an indication of a physical connection between the\noutskirts of the galaxy and infall from the circumgalactic medium. A\ncombination of stellar migration, accretion and in-situ star formation might be\nresponsible for building up the outer stellar disk, but whatever mechanisms\nformed the outer disk must also explain the constant ratio between stellar and\ngas mass in the outskirts of this galaxy.", "cat": "astro-ph.GA", "authors": ["Jielai Zhang", "Roberto Abraham", "Pieter van Dokkum", "Allison Merritt", "Steven Janssens"]}, "377": {"id": "1312.2949v1", "title": "A Survey of Embedded Software Profiling Methodologies", "url": "http://arxiv.org/pdf/1312.2949v1", "date": "2013-12-10 05:15:32", "abs": "Embedded Systems combine one or more processor cores with dedicated logic\nrunning on an ASIC or FPGA to meet design goals at reasonable cost. It is\nachieved by profiling the application with variety of aspects like performance,\nmemory usage, cache hit versus cache miss, energy consumption, etc. Out of\nthese, performance estimation is more important than others. With ever\nincreasing system complexities, it becomes quite necessary to carry out\nperformance estimation of embedded software implemented in a particular\nprocessor for fast design space exploration. Such profiled data also guides the\ndesigner how to partition the system for Hardware (HW) and Software (SW)\nenvironments. In this paper, we propose a classification for currently\navailable Embedded Software Profiling Tools, and we present different academic\nand industrial approaches in this context. Based on these observations, it will\nbe easy to identify such common principles and needs which are required for a\ntrue Software Profiling Tool for a particular application.", "cat": "cs.PF", "authors": ["Rajendra Patel", "Arvind Rajwat"]}, "378": {"id": "1801.09961v3", "title": "Modeling Influence with Semantics in Social Networks: a Survey", "url": "http://arxiv.org/pdf/1801.09961v3", "date": "2018-10-04 07:16:23", "abs": "The discovery of influential entities in all kinds of networks (e.g. social,\ndigital, or computer) has always been an important field of study. In recent\nyears, Online Social Networks (OSNs) have been established as a basic means of\ncommunication and often influencers and opinion makers promote politics,\nevents, brands or products through viral content. In this work, we present a\nsystematic review across i) online social influence metrics, properties, and\napplications and ii) the role of semantic in modeling OSNs information. We end\nup with the conclusion that both areas can jointly provide useful insights\ntowards the qualitative assessment of viral user-generated content, as well as\nfor modeling the dynamic properties of influential content and its flow\ndynamics.", "cat": "cs.IR", "authors": ["Gerasimos Razis", "Ioannis Anagnostopoulos", "Sherali Zeadally"]}, "379": {"id": "2005.04094v1", "title": "Parallel Programming Models for Heterogeneous Many-Cores : A Survey", "url": "http://arxiv.org/pdf/2005.04094v1", "date": "2020-05-05 13:39:05", "abs": "Heterogeneous many-cores are now an integral part of modern computing systems\nranging from embedding systems to supercomputers. While heterogeneous many-core\ndesign offers the potential for energy-efficient high-performance, such\npotential can only be unlocked if the application programs are suitably\nparallel and can be made to match the underlying heterogeneous platform. In\nthis article, we provide a comprehensive survey for parallel programming models\nfor heterogeneous many-core architectures and review the compiling techniques\nof improving programmability and portability. We examine various software\noptimization techniques for minimizing the communicating overhead between\nheterogeneous computing devices. We provide a road map for a wide variety of\ndifferent research areas. We conclude with a discussion on open issues in the\narea and potential research directions. This article provides both an\naccessible introduction to the fast-moving area of heterogeneous programming\nand a detailed bibliography of its main achievements.", "cat": "cs.DC", "authors": ["Jianbin Fang", "Chun Huang", "Tao Tang", "Zheng Wang"]}, "380": {"id": "1510.04453v1", "title": "A NuSTAR Survey of Nearby Ultraluminous Infrared Galaxies", "url": "http://arxiv.org/pdf/1510.04453v1", "date": "2015-10-15 09:13:13", "abs": "We present a NuSTAR, Chandra, and XMM--Newton survey of nine of the nearest\nultraluminous infrared galaxies (ULIRGs). The unprecedented sensitivity of\nNuSTAR at energies above 10 keV enables spectral modeling with far better\nprecision than was previously possible. Six of the nine sources observed were\ndetected sufficiently well by NuSTAR to model in detail their broadband X-ray\nspectra, and recover the levels of obscuration and intrinsic X-ray\nluminosities. Only one source (IRAS 13120--5453) has a spectrum consistent with\na Compton--thick AGN, but we cannot rule out that a second source (Arp 220)\nharbors an extremely highly obscured AGN as well. Variability in column density\n(reduction by a factor of a few compared to older observations) is seen in IRAS\n05189--2524 and Mrk 273, altering the classification of these border-line\nsources from Compton-thick to Compton-thin. The ULIRGs in our sample have\nsurprisingly low observed fluxes in high energy (>10 keV) X-rays, especially\ncompared to their bolometric luminosities. They have lower ratios of unabsorbed\n2--10 keV to bolometric luminosity, and unabsorbed 2--10 keV to mid-IR [O IV]\nline luminosity than do Seyfert 1 galaxies. We identify IRAS 08572+3915 as\nanother candidate intrinsically X-ray weak source, similar to Mrk 231. We\nspeculate that the X-ray weakness of IRAS 08572+3915 is related to its powerful\noutflow observed at other wavelengths.", "cat": "astro-ph.GA", "authors": ["Stacy H. Teng", "Jane R. Rigby", "Daniel Stern", "Andrew Ptak", "D. M. Alexander", "Franz E. Bauer", "Stephen E. Boggs", "W. Niel Brandt", "Finn E. Christensen", "Andrea Comastri", "William W. Craig", "Duncan Farrah", "Poshak Gandhi", "Charles J. Hailey", "Fiona A. Harrison", "Ryan C. Hickox", "Michael Koss", "Bin Luo", "Ezequiel Treister", "William W. Zhang"]}, "381": {"id": "2107.00244v2", "title": "The Galaxy Activity, Torus and Outflow Survey (GATOS): II. Torus and polar dust emission in nearby Seyfert galaxies", "url": "http://arxiv.org/pdf/2107.00244v2", "date": "2021-07-02 14:12:27", "abs": "We compare mid-IR and ALMA far-IR images of 12 nearby Seyferts selected from\nGATOS. The mid-IR unresolved emission contributes more than 60% of the nuclear\nemission in most galaxies. By contrast, the ALMA 870micron continuum emission\nis mostly resolved and typically along the torus equatorial direction (Paper I,\nGarcia-Burillo et al. 2021). The Eddington ratios and nuclear hydrogen column\ndensities NH of half the sample are favorable to launching polar and/or\nequatorial dusty winds, according to simulations. Six show mid-IR extended\nemission in the polar direction as traced by the NLR and perpendicular to the\nALMA emission. In a few, the nuclear NH might be too high to uplift large\nquantities of dusty material along the polar direction. Five galaxies have low\nNH and/or Eddington ratios and thus polar dusty winds are not likely. We\ngenerate new CAT3D-WIND disk-wind model images. At low wind-to-disk cloud\nratios the far-IR model images have disk- and ring-like morphologies. The\nX-shape associated with dusty winds is seen better in the far-IR at\nintermediate-high inclinations for the extended-wind configurations. In most\nmodels, the mid-IR emission comes from the inner part of the disk/cone.\nExtended bi-conical and one-sided polar mid-IR emission is seen in\nextended-wind configurations and high wind-to-disk cloud ratios. When convolved\nto our resolution, the model images reproduce qualitative aspects of the\nobserved morphologies. Low-intermediate wind-to-disk ratios are required to\naccount for the large fractions of unresolved mid-IR emission. This work and\nPaper I provide observational support for the torus+wind scenario. The wind\ncomponent is more relevant at high Eddington ratios and/or AGN luminosities,\nand polar dust emission is predicted at NH of up to $10^{24}$cm$^{-2}$. The\ntorus/disk component, on the other hand, prevails at low luminosities and/or\nEddington ratios. (Abridged)", "cat": "astro-ph.GA", "authors": ["A. Alonso-Herrero", "S. Garc\u00eda-Burillo", "S. F. Hoenig", "I. Garc\u00eda-Bernete", "C. Ramos Almeida", "O. Gonz\u00e1lez-Mart\u00edn", "E. L\u00f3pez-Rodr\u00edguez", "P. G. Boorman", "A. J. Bunker", "L. Burtscher", "F. Combes", "R. Davies", "T. D\u00edaz-Santos", "P. Gandhi", "B. Garc\u00eda-Lorenzo", "E. K. S. Hicks", "L. K. Hunt", "K. Ichikawa", "M. Imanishi", "T. Izumi", "A. Labiano", "N. A. Levenson", "C. Packham", "M. Pereira-Santaella", "C. Ricci", "D. Rigopoulou", "P. Roche", "D. J. Rosario", "D. Rouan", "T. Shimizu", "M. Stalevski", "K. Wada", "D. Williamson"]}, "382": {"id": "2407.12585v2", "title": "A global view on star formation: The GLOSTAR Galactic plane survey. XI. Radio source catalog IV: $2^\\circ < \\ell < 28^\\circ$, $36^\\circ < \\ell < 60^\\circ$ and $|b| < 1^\\circ$", "url": "http://arxiv.org/pdf/2407.12585v2", "date": "2024-08-08 09:31:39", "abs": "The GLOSTAR survey studies star formation with the VLA and the Effelsberg\n100m telescope in the Galactic plane (-2d2 mag/arcsec^2. Contrasting non-parametric elliptical isophote\nfitting with simple parametric models also shows that two-component fits (e.g.,\nS\\'ersic plus exponential) are insufficient to describe late-type galaxies with\nhigh fidelity. It is established that elliptical isophote fitting, and in\nparticular AutoProf, is ideally suited for a broad range of automated isophotal\nanalysis tasks. AutoProf is freely available to the community at:\nhttps://github.com/ConnorStoneAstro/AutoProf", "cat": "astro-ph.GA", "authors": ["Connor Stone", "Nikhil Arora", "St\u00e9phane Courteau", "Jean-Charles Cuillandre"]}, "389": {"id": "2310.10315v2", "title": "A Survey on Quantum Machine Learning: Current Trends, Challenges, Opportunities, and the Road Ahead", "url": "http://arxiv.org/pdf/2310.10315v2", "date": "2024-07-27 08:08:45", "abs": "Quantum Computing (QC) claims to improve the efficiency of solving complex\nproblems, compared to classical computing. When QC is integrated with Machine\nLearning (ML), it creates a Quantum Machine Learning (QML) system. This paper\naims to provide a thorough understanding of the foundational concepts of QC and\nits notable advantages over classical computing. Following this, we delve into\nthe key aspects of QML in a detailed and comprehensive manner.\n In this survey, we investigate a variety of QML algorithms, discussing their\napplicability across different domains. We examine quantum datasets,\nhighlighting their unique characteristics and advantages. The survey also\ncovers the current state of hardware technologies, providing insights into the\nlatest advancements and their implications for QML. Additionally, we review the\nsoftware tools and simulators available for QML development, discussing their\nfeatures and usability.\n Furthermore, we explore practical applications of QML, illustrating how it\ncan be leveraged to solve real-world problems more efficiently than classical\nML methods. This paper serves as a valuable resource for readers seeking to\nunderstand the current state-of-the-art techniques in the QML field, offering a\nsolid foundation to embark on further exploration and development in this\nrapidly evolving area.", "cat": "quant-ph", "authors": ["Kamila Zaman", "Alberto Marchisio", "Muhammad Abdullah Hanif", "Muhammad Shafique"]}, "390": {"id": "1403.7854v1", "title": "A Comparative Study of Infrared Asteroid Surveys: IRAS, AKARI, and WISE", "url": "http://arxiv.org/pdf/1403.7854v1", "date": "2014-03-31 02:37:47", "abs": "We present a comparative study of three infrared asteroid surveys based on\nthe size and albedo data from the Infrared Astronomical Satellite (IRAS), the\nJapanese infrared satellite AKARI, and the Wide-field Infrared Survey Explorer\n(WISE). Our study showed that: (i) the total number of asteroids detected with\ndiameter and albedo information with these three surveyors is 138,285, which is\nlargely contributed by WISE; (ii) the diameters and albedos measured by the\nthree surveyors for 1,993 commonly detected asteroids are in good agreement,\nand within +/-10% in diameter and +/-22% in albedo at 1sigma deviation level.\nIt is true that WISE offers size and albedo of a large fraction (>20%) of known\nasteroids down to a few km bodies, but we would suggest that the IRAS and AKARI\ncatalogs compensate for larger asteroids up to several hundred km, especially\nin the main belt region. We discuss the complementarity of these three catalogs\nin order to facilitate the use of these data sets for characterizing the\nphysical properties of minor planets.", "cat": "astro-ph.EP", "authors": ["Fumihiko Usui", "Sunao Hasegawa", "Masateru Ishiguro", "Thomas G. Mueller", "Takafumi Ootsubo"]}, "391": {"id": "2111.06077v2", "title": "A Survey on Hyperdimensional Computing aka Vector Symbolic Architectures, Part I: Models and Data Transformations", "url": "http://arxiv.org/pdf/2111.06077v2", "date": "2023-07-31 22:40:51", "abs": "This two-part comprehensive survey is devoted to a computing framework most\ncommonly known under the names Hyperdimensional Computing and Vector Symbolic\nArchitectures (HDC/VSA). Both names refer to a family of computational models\nthat use high-dimensional distributed representations and rely on the algebraic\nproperties of their key operations to incorporate the advantages of structured\nsymbolic representations and vector distributed representations. Notable models\nin the HDC/VSA family are Tensor Product Representations, Holographic Reduced\nRepresentations, Multiply-Add-Permute, Binary Spatter Codes, and Sparse Binary\nDistributed Representations but there are other models too. HDC/VSA is a highly\ninterdisciplinary field with connections to computer science, electrical\nengineering, artificial intelligence, mathematics, and cognitive science. This\nfact makes it challenging to create a thorough overview of the field. However,\ndue to a surge of new researchers joining the field in recent years, the\nnecessity for a comprehensive survey of the field has become extremely\nimportant. Therefore, amongst other aspects of the field, this Part I surveys\nimportant aspects such as: known computational models of HDC/VSA and\ntransformations of various input data types to high-dimensional distributed\nrepresentations. Part II of this survey is devoted to applications, cognitive\ncomputing and architectures, as well as directions for future work. The survey\nis written to be useful for both newcomers and practitioners.", "cat": "cs.AI", "authors": ["Denis Kleyko", "Dmitri A. Rachkovskij", "Evgeny Osipov", "Abbas Rahimi"]}, "392": {"id": "0902.3326v1", "title": "Two distant brown dwarfs in the UKIRT Infrared Deep Sky Survey Deep Extragalactic Survey Data Release 2", "url": "http://arxiv.org/pdf/0902.3326v1", "date": "2009-02-19 09:28:13", "abs": "We present the discovery of two brown dwarfs in the UKIRT Infrared Deep Sky\nSurvey (UKIDSS) Deep Extragalactic Survey (DXS) Data Release 2. Both objects\nwere selected photometrically from six square degrees in DXS for their blue J-K\ncolour and the lack of optical counterparts in the Sloan Digital Sky Survey\n(SDSS) Stripe 82. Additional optical photometry provided by the\nCanada-France-Hawaii Telescope Legacy Survey (CFHT-LS) corroborated the\npossible substellarity of these candidates. Subsequent methane imaging of UDXS\nJ221611.51+003308.1 and UDXS J221903.10+002418.2, has confirmed them as\nT7$\\pm$1 and T6$\\pm$1 dwarfs at photometric distances of 81 (52-118 pc) and 60\n(44-87 pc; 2 sigma confidence level). A similar search in the second data\nrelease of the Ultra Deep Survey over a smaller area (0.77 square degree) and\nshallower depth didn't return any late-T dwarf candidate. The numbers of late-T\ndwarfs in our study are broadly in line with a declining mass function when\nconsidering the current area and depth of the DXS and UDS. These brown dwarfs\nare the first discovered in the VIMOS 4 field and among the few T dwarfs found\nin pencil-beam surveys. They are valuable to investigate the scale height of T\ndwarfs.", "cat": "astro-ph.GA", "authors": ["N. Lodieu", "P. D. Dobbie", "N. R. Deacon", "B. P. Venemans", "M. Durant"]}, "393": {"id": "2309.01014v1", "title": "Searching for Variable Stars Using the Large Array Survey Telescope (LAST)", "url": "http://arxiv.org/pdf/2309.01014v1", "date": "2023-09-02 20:25:38", "abs": "This paper introduces a novel variability report generator developed for the\nLarge Array Survey Telescope (LAST), a cost-effective multi-purpose telescope\narray conducting a wide survey of the variable sky in the visible-light\nspectrum. Designed to automate variability detection, the report generator\nidentifies candidate variable stars by employing adjustable thresholds to\ndetect periodic and non-periodic variables. The program outputs a visual and\ntabular photometric report for each candidate variable source from a given LAST\nsub-image. Functioning as a whitepaper, this document also provides a concise\noverview of LAST, discussing its design, data workflow, and variability search\nperformance.", "cat": "astro-ph.IM", "authors": ["Barkotel Zemenu"]}, "394": {"id": "0802.1528v1", "title": "Bayesian Galaxy Shape Measurement for Weak Lensing Surveys -II. Application to Simulations", "url": "http://arxiv.org/pdf/0802.1528v1", "date": "2008-02-12 20:54:15", "abs": "We extend the Bayesian model fitting shape measurement method presented in\nMiller et al. (2007) and use the method to estimate the shear from the Shear\nTEsting Programme simulations (STEP). The method uses a fast model fitting\nalgorithm which uses realistic galaxy profiles and analytically marginalises\nover the position and amplitude of the model by doing the model fitting in\nFourier space. This is used to find the full posterior probability in\nellipticity so that the shear can be estimated in a fully Bayesian way. The\nBayesian shear estimation allows measurement bias arising from the presence of\nrandom noise to be removed. In this paper we introduce an iterative algorithm\nthat can be used to estimate the intrinsic ellipticity prior and show that this\nis accurate and stable. By using the method to estimate the shear from the\nSTEP1 simulations we find the method to have a shear bias of m ~ 0.005 and a\nvariation in shear offset with PSF type of sigma_c ~ 0.0002. These values are\nsmaller than for any method presented in the STEP1 publication that behaves\nlinearly with shear. Using the method to estimate the shear from the STEP2\nsimulations we find than the shear bias and offset are m ~ 0.002 and c ~\n-0.0007 respectively. In addition we find that the bias and offset are stable\nto changes in magnitude and size of the galaxies. Such biases should yield any\ncosmological constraints from future weak lensing surveys robust to systematic\neffects in shape measurement.", "cat": "astro-ph", "authors": ["T. D. Kitching", "L. Miller", "C. E. Heymans", "L. van Waerbeke", "A. F. Heavens"]}, "395": {"id": "1609.08018v1", "title": "Small near-Earth asteroids in the Palomar Transient Factory survey: A real-time streak-detection system", "url": "http://arxiv.org/pdf/1609.08018v1", "date": "2016-09-26 15:15:09", "abs": "Near-Earth asteroids (NEAs) in the 1-100 meter size range are estimated to be\n$\\sim$1,000 times more numerous than the $\\sim$15,000 currently-catalogued\nNEAs, most of which are in the 0.5-10 kilometer size range. Impacts from 10-100\nmeter size NEAs are not statistically life-threatening but may cause\nsignificant regional damage, while 1-10 meter size NEAs with low velocities\nrelative to Earth are compelling targets for space missions. We describe the\nimplementation and initial results of a real-time NEA-discovery system\nspecialized for the detection of small, high angular rate (visually-streaked)\nNEAs in Palomar Transient Factory (PTF) images. PTF is a 1.2-m aperture,\n7.3-deg$^2$ field-of-view optical survey designed primarily for the discovery\nof extragalactic transients (e.g., supernovae) in 60-second exposures reaching\n$\\sim$20.5 visual magnitude. Our real-time NEA discovery pipeline uses a\nmachine-learned classifier to filter a large number of false-positive streak\ndetections, permitting a human scanner to efficiently and remotely identify\nreal asteroid streaks during the night. Upon recognition of a streaked NEA\ndetection (typically within an hour of the discovery exposure), the scanner\ntriggers follow-up with the same telescope and posts the observations to the\nMinor Planet Center for worldwide confirmation. We describe our ten initial\nconfirmed discoveries, all small NEAs that passed 0.3-15 lunar distances from\nEarth. Lastly, we derive useful scaling laws for comparing\nstreaked-NEA-detection capabilities of different surveys as a function of their\nhardware and survey-pattern characteristics. This work most directly informs\nestimates of the streak-detection capabilities of the Zwicky Transient Facility\n(ZTF, planned to succeed PTF in 2017), which will apply PTF's current\nresolution and sensitivity over a 47-deg$^2$ field-of-view.", "cat": "astro-ph.EP", "authors": ["Adam Waszczak", "Thomas A. Prince", "Russ Laher", "Frank Masci", "Brian Bue", "Umaa Rebbapragada", "Tom Barlow", "Jason Surace", "George Helou", "Shrinivas Kulkarni"]}, "396": {"id": "1310.0037v2", "title": "Probing Neutrinos from Planck and Forthcoming Galaxy Redshift Surveys", "url": "http://arxiv.org/pdf/1310.0037v2", "date": "2013-12-12 15:17:54", "abs": "We investigate how much the constraints on the neutrino properties can be\nimproved by combining the CMB, the photometric and spectroscopic galaxy\nredshift surveys which include the CMB lensing, galaxy lensing tomography,\ngalaxy clustering and redshift space distortion observables. We pay a\nparticular attention to the constraint on the neutrino mass in view of the\nforthcoming redshift surveys such as the Euclid satellite and the LSST survey\nalong with the Planck CMB lensing measurements. Combining the transverse mode\ninformation from the angular power spectrum and the longitudinal mode\ninformation from the spectroscopic survey with the redshift space distortion\nmeasurements can determine the total neutrino mass with the projected error of\nO(0.02)eV. Our analysis fixes the mass splittings among the neutrino species to\nbe consistent with the neutrino oscillation data, and we accordingly study the\nsensitivity of our parameter estimations on the minimal neutrino mass. The\ncosmological measurement of the total neutrino mass can distinguish between the\nnormal and inverted mass hierarchy scenarios if the minimal neutrino mass <\n0.005 eV with the predicted 1-{\\sigma} uncertainties taken into account.", "cat": "astro-ph.CO", "authors": ["Yoshitaka Takeuchi", "Kenji Kadota"]}, "397": {"id": "0907.1305v1", "title": "An HST/WFPC Survey of Bright Young Clusters in M31. II. Photometry of Less Luminous Clusters in the Fields", "url": "http://arxiv.org/pdf/0907.1305v1", "date": "2009-07-07 21:23:54", "abs": "We report on the properties of 89 low mass star clusters located in the\nvicinity of luminous young clusters (blue globulars) in the disk of M31. 82 of\nthe clusters are newly detected. We have determined their integrated magnitudes\nand colors, based on a series of Hubble Space Telescope Wide Field/Planetary\nCamera 2 exposures in blue and red (HST filters F450W and F814W). The\nintegrated apparent magnitudes range from F450W = 17.5 to 22.5, and the colors\nindicate a wide range of ages. Stellar color-magnitude diagrams for all\nclusters were obtained and those with bright enough stars were fit to\ntheoretical isochrones to provide age estimates. The ages range from 12 Myr to\n>500 Myr. Reddenings, which average E(F450 - F814) = 0.59 with a dispersion of\n0.21 magnitudes, were derived from the main sequence fitting for those\nclusters. Comparison of these ages and integrated colors with single population\ntheoretical models with solar abundances suggests a color offset of 0.085\nmagnitudes at the ages tested. Estimated ages for the remaining clusters are\nbased on their measured colors. The age-frequency diagram shows a steep decline\nof number with age, with a large decrease in number per age interval between\nthe youngest and the oldest clusters detected.", "cat": "astro-ph.GA", "authors": ["P. W. Hodge", "O. K. Krienke", "M. Bellazzini", "S. Perina", "P. Barmby", "J. G. Cohen", "T. H. Puzia", "J. Strader"]}, "398": {"id": "2001.04840v1", "title": "Hybrid LiFi and WiFi Networks: A Survey", "url": "http://arxiv.org/pdf/2001.04840v1", "date": "2020-01-14 15:03:10", "abs": "To tackle the rapidly growing number of mobile devices and their expanding\ndemands for Internet services, network convergence is envisaged to integrate\ndifferent technology domains. A recently proposed and promising approach to\nindoor wireless communications is integrating light fidelity (LiFi) and\nwireless fidelity (WiFi), namely a hybrid LiFi and WiFi network (HLWNet). This\ntype of network combines the high-speed data transmission of LiFi and the\nubiquitous coverage of WiFi. In this paper, we present a survey-style\nintroduction to HLWNets, starting with a framework including the network\nstructure, cell deployment, multiple access schemes, modulation techniques,\nillumination requirements and backhauling. Then, key performance metrics and\nrecent achievements are reviewed. Further, the unique challenges faced by\nHLWNets are elaborated in many research directions, including user behavior\nmodeling, interference management, handover and load balancing. Finally, we\ndiscuss the potential of HLWNets in application areas such as indoor\npositioning and physical layer security.", "cat": "cs.IT", "authors": ["Xiping Wu", "Mohammad Dehghani Soltani", "Lai Zhou", "Majid Safari", "Harald Haas"]}, "399": {"id": "2310.13054v1", "title": "CAPOS: The bulge Cluster APOgee Survey IV. Elemental Abundances of the bulge globular cluster NGC 6558", "url": "http://arxiv.org/pdf/2310.13054v1", "date": "2023-10-19 18:00:03", "abs": "This study presents the results concerning six red giant stars members of the\nglobular cluster NGC 6558. Our analysis utilized high-resolution near-infrared\nspectra obtained through the CAPOS initiative (the APOgee Survey of Clusters in\nthe Galactic Bulge), which focuses on surveying clusters within the Galactic\nBulge, as a component of the Apache Point Observatory Galactic Evolution\nExperiment II survey (APOGEE-2). We employ the BACCHUS (Brussels Automatic Code\nfor Characterizing High accUracy Spectra) code to provide line-by-line\nelemental-abundances for Fe-peak (Fe, Ni), $\\alpha$-(O, Mg, Si, Ca, Ti),\nlight-(C, N), odd-Z (Al), and the $s$-process element (Ce) for the 4 stars with\nhigh signal-to-noise ratios. This is the first reliable measure of the CNO\nabundances for NGC 6558. Our analysis yields a mean metallicity for NGC 6558 of\n$\\langle$[Fe/H]$\\rangle$ = $-$1.15 $\\pm$ 0.08, with no evidence for a\nmetallicity spread. We find a Solar Ni abundance, $\\langle$[Ni/Fe]$\\rangle$\n$\\sim$ $+$0.01, and a moderate enhancement of $\\alpha$-elements, ranging\nbetween $+$0.16 to $<+$0.42, and a slight enhancement of the $s$-process\nelement $\\langle$[Ce/Fe]$\\rangle$ $\\sim$ $+$0.19. We also found low levels of\n$\\langle$[Al/Fe]$\\rangle \\sim $+$0.09$, but with a strong enrichment of\nnitrogen, [N/Fe]$>+$0.99, along with a low level of carbon, [C/Fe]$<-$0.12.\nThis behaviour of Nitrogen-Carbon is a typical chemical signature for the\npresence of multiple stellar populations in virtually all GCs; this is the\nfirst time that it is reported in NGC 6558. We also observed a remarkable\nconsistency in the behaviour of all the chemical species compared to the other\nCAPOS bulge GCs of the same metallicity.", "cat": "astro-ph.GA", "authors": ["Danilo Gonz\u00e1lez-D\u00edaz", "Jos\u00e9 G. Fern\u00e1ndez-Trincado", "Sandro Villanova", "Doug Geisler", "Beatriz Barbuy", "Dante Minniti", "Timothy C. Beers", "Christian Moni Bidin", "Francesco Mauro", "Cesar Mu\u00f1oz", "Baitian Tang", "Mario Soto", "Antonela Monachesi", "Richard R. Lane", "Heinz Frelijj"]}, "400": {"id": "2007.02106v2", "title": "Automatic Target Recognition on Synthetic Aperture Radar Imagery: A Survey", "url": "http://arxiv.org/pdf/2007.02106v2", "date": "2020-12-12 21:11:18", "abs": "Automatic Target Recognition (ATR) for military applications is one of the\ncore processes towards enhancing intelligencer and autonomously operating\nmilitary platforms. Spurred by this and given that Synthetic Aperture Radar\n(SAR) presents several advantages over its counterpart data domains, this paper\nsurveys and assesses current SAR ATR architectures that employ the most popular\ndataset for the SAR domain, namely the Moving and Stationary Target Acquisition\nand Recognition (MSTAR) dataset. Based on the current methodology trends, we\npropose a taxonomy for the SAR ATR architectures, along with a direct\ncomparison of the strengths and weaknesses of each method under both standard\nand extended operational conditions. Additionally, despite MSTAR being the\nstandard SAR ATR benchmarking dataset we also highlight its weaknesses and\nsuggest future research directions.", "cat": "cs.CV", "authors": ["O. Kechagias-Stamatis", "N. Aouf"]}, "401": {"id": "2408.03374v1", "title": "The ALMA-CRISTAL Survey: Spatial extent of [CII] line emission in star-forming galaxies at $z=4-6$", "url": "http://arxiv.org/pdf/2408.03374v1", "date": "2024-08-06 18:00:07", "abs": "We investigate the spatial extent of the [CII] line emission in a sample of\n34 galaxies at $z=4-6$ from the ALMA-CRISTAL Survey. By modeling the [CII] line\nemission in the visibility data directly, we derive the effective radius of\n[CII] line emission assuming exponential distribution. These measurements\ncomprise not only isolated galaxies but also interacting systems, identified\nthanks to the high spatial resolution of the data. The [CII] line radius ranges\nfrom 0.5 to 3.5 kpc with an average value of 1.9 kpc. We compare the [CII]\nsizes with the sizes of UV and FIR continua, which were measured from the HST\nF160W and ALMA Band-7 continuum images, respectively. We confirm that the [CII]\nline emission is more spatially extended than the continuum emission, with\naverage size ratios of $R_{e,[CII]}/R_{e,UV}=2.90$ and\n$R_{e,[CII]}/R_{e,FIR}=1.54$, although about half of the FIR-detected sample\nshow comparable spatial extent between [CII] line and FIR continuum emission\n($R_{e,[CII]}\\approx R_{e, FIR}$). The residual visibility data of the best-fit\nmodel do not show evidence of flux excesses either individually or in stacking\nanalysis. This indicates that the [CII] line emission in star-forming galaxies\ncan be characterized by an extended exponential disk profile. Overall, our\nresults suggest that the spatial extent of [CII] line emission can primarily be\nexplained by photodissociation regions associated with star formation activity,\nwhile the contribution from diffuse neutral medium (atomic gas) and the effects\nof mergers may further expand the [CII] line distributions, causing their\nvariations among our sample. We report the correlations between the [CII] line,\ndust, and Lya line properties, which may be in line with our scenario. Future\n3D-analysis of Lya and Ha lines will shed light on the association of the\nextended [CII] line emission with atomic gas and outflows.", "cat": "astro-ph.GA", "authors": ["Ryota Ikeda", "Ken-ichi Tadaki", "Ikki Mitsuhashi", "Manuel Aravena", "Ilse De Looze", "Natascha M. F\u00f6rster Schreiber", "Jorge Gonz\u00e1lez-L\u00f3pez", "Rodrigo Herrera-Camus", "Justin Spilker", "Loreto Barcos-Mu\u00f1oz", "Elisabete da Cunha", "Rebecca Davies", "Tanio D\u00edaz-Santos", "Andrea Ferrara", "Meghana Killi", "Lilian L. Lee", "Juno Li", "Dieter Lutz", "Renske Smit", "Manuel Solimano", "Kseniia Telikova", "Hannah \u00dcbler", "Sylvain Veilleux", "Vicente Villanueva"]}, "402": {"id": "1607.03438v1", "title": "A spectroscopic analysis of a sample of narrow-line Seyfert 1 galaxies selected from the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1607.03438v1", "date": "2016-07-12 16:51:42", "abs": "We revisited the spectroscopic characteristics of narrow-line Seyfert 1\ngalaxies (NLS1s) by analysing a homogeneous sample of 296 NLS1s at redshift\nbetween 0.028 and 0.345, extracted from the Sloan Digital Sky Survey (SDSS-DR7)\npublic archive. We confirm that NLS1s are mostly characterized by Balmer lines\nwith Lorentzian profiles, lower black hole masses and higher Eddington ratios\nthan classic broad-line Seyfert 1 (BLS1s), but they also appear to be active\ngalactic nuclei (AGNs) contiguous with BLS1s and sharing with them common\nproperties. Strong Fe II emission does not seem to be a distinctive property of\nNLS1s, as low values of Fe II/H$\\beta$ are equally observed in these AGNs. Our\ndata indicate that Fe II and Ca II kinematics are consistent with the one of\nH$\\beta$. On the contrary, O I $\\lambda$8446 seems to be systematically\nnarrower and it is likely emitted by gas of the broad-line region more distant\nfrom the ionizing source and showing different physical properties. Finally,\nalmost all NLS1s of our sample show radial motions of the narrow-line region\nhighly-ionised gas. The mechanism responsible for this effect is not yet clear,\nbut there are hints that very fast outflows require high continuum luminosities\n(> $10^{44}$ erg/s) or high Eddington ratios (log(L$_{\\rm bol}$/L$_{\\rm Edd}$)\n> -0.1).", "cat": "astro-ph.GA", "authors": ["V. Cracco", "S. Ciroi", "M. Berton", "F. Di Mille", "L. Foschini", "G. La Mura", "P. Rafanelli"]}, "403": {"id": "2202.03142v1", "title": "A Comprehensive Survey on the Internet of Things with the Industrial Marketplace", "url": "http://arxiv.org/pdf/2202.03142v1", "date": "2022-01-19 08:29:19", "abs": "There is no doubt that new technology has become one of the crucial parts of\nmost people's lives around the world. By and large, in this era, the Internet\nand the Internet of Things (IoT) have become the most indispensable parts of\nour lives. Recently, IoT technologies have been regarded as the most broadly\nused tools among other technologies. The tools and the facilities of IoT\ntech-nologies within the marketplace are part of Industry 4.0. The marketplace\nis too regarded as a new area that can be used with IoT technologies. One of\nthe main purposes of this paper is to highlight using IoT technologies in\nIndustry 4.0, and the Industrial Internet of Things (IIoT) is another feature\nrevised. This paper focuses on the value of the IoT in the industrial domain in\ngeneral; it reviews the IoT and focuses on its benefits and drawbacks, and\npresents some of the IoT applications, such as in transportation and\nhealthcare. In addition, the trends and facts that are related to the IoT\ntechnologies on the marketplace are reviewed. Finally, the role of IoT in\ntelemedicine and healthcare and the benefits of IoT technologies for COVID-19\nare presented as well.", "cat": "cs.NI", "authors": ["Kazhan Othman Mohammed Salih", "Tarik A. Rashid", "Dalibor Radovanovic", "Nebojsa Bacanin"]}, "404": {"id": "0704.3842v1", "title": "MMT observations of new extremely metal-poor emission-line galaxies in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/0704.3842v1", "date": "2007-04-29 13:25:45", "abs": "We present 6.5-meter MMT spectrophotometry of 20 H II regions in 13 extremely\nmetal-poor emission-line galaxies selected from the Data Release 5 of the Sloan\nDigital Sky Survey to have [O III] 4959/Hbeta < 1 and [N II] 6583/Hbeta < 0.05.\nThe electron temperature-sensitive emission line [O III] 4363 is detected in 13\nH II regions allowing a direct abundance determination. The oxygen abundance in\nthe remaining H II regions is derived using a semi-empirical method. The oxygen\nabundance of the galaxies in our sample ranges from 12+logO/H ~ 7.1 to ~ 7.8,\nwith 10 H II regions having an oxygen abundance lower than 7.5. The lowest\noxygen abundances, 12+logO/H = 7.14+/-0.03 and 7.13+/-0.07, are found in two H\nII regions of the blue compact dwarf galaxy SDSSJ0956+2849=DDO 68, making it\nthe second most-metal deficient emission-line galaxy known, after SBS\n0335-052W.", "cat": "astro-ph", "authors": ["Y. I. Izotov", "T. X. Thuan"]}, "405": {"id": "2102.12983v1", "title": "Observations of Her X-1 in low states during SRG/eROSITA all-sky survey", "url": "http://arxiv.org/pdf/2102.12983v1", "date": "2021-02-25 16:35:26", "abs": "eROSITA (extended ROentgen Survey with an Imaging Telescope Array) instrument\nonboard the Russian-German `Spectrum-Roentgen-Gamma' (SRG) mission observed the\nHer X-1/HZ Her binary system in multiple scans over the source during the first\nand second SRG all-sky surveys. Both observations occurred during a low state\nof the X-ray source when the outer parts of the accretion disk blocked the\nneutron star from view. The orbital modulation of the X-ray flux was detected\nduring the low states. We argue that the detected X-ray radiation results from\nscattering of the emission of the central source by three distinct regions: (a)\nan optically thin hot corona with temperature $\\sim (2-4) \\times 10^6$ K above\nthe irradiated hemisphere of the optical star; (b) an optically thin hot halo\nabove the accretion disk; and (c) the optically thick cold atmosphere of the\noptical star. The latter region effectively scatters photons with energies\nabove $5-6$ keV.", "cat": "astro-ph.HE", "authors": ["N. I. Shakura", "D. A. Kolesnikov", "P. S. Medvedev", "R. A. Sunyaev", "M. R. Gilfanov", "K. A. Postnov", "S. V. Molkov"]}, "406": {"id": "1609.04172v1", "title": "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties", "url": "http://arxiv.org/pdf/1609.04172v1", "date": "2016-09-14 08:41:08", "abs": "At about 1000 days after the launch of Gaia we present the first Gaia data\nrelease, Gaia DR1, consisting of astrometry and photometry for over 1 billion\nsources brighter than magnitude 20.7. We summarize Gaia DR1 and provide\nillustrations of the scientific quality of the data, followed by a discussion\nof the limitations due to the preliminary nature of this release. Gaia DR1\nconsists of: a primary astrometric data set which contains the positions,\nparallaxes, and mean proper motions for about 2 million of the brightest stars\nin common with the Hipparcos and Tycho-2 catalogues and a secondary astrometric\ndata set containing the positions for an additional 1.1 billion sources. The\nsecond component is the photometric data set,consisting of mean G-band\nmagnitudes for all sources. The G-band light curves and the characteristics of\n~3000 Cepheid and RR Lyrae stars, observed at high cadence around the south\necliptic pole, form the third component. For the primary astrometric data set\nthe typical uncertainty is about 0.3 mas for the positions and parallaxes, and\nabout 1 mas/yr for the proper motions. A systematic component of ~0.3 mas\nshould be added to the parallax uncertainties. For the subset of ~94000\nHipparcos stars in the primary data set, the proper motions are much more\nprecise at about 0.06 mas/yr. For the secondary astrometric data set, the\ntypical uncertainty of the positions is ~10 mas. The median uncertainties on\nthe mean G-band magnitudes range from the mmag level to ~0.03 mag over the\nmagnitude range 5 to 20.7. Gaia DR1 represents a major advance in the mapping\nof the heavens and the availability of basic stellar data that underpin\nobservational astrophysics. Nevertheless, the very preliminary nature of this\nfirst Gaia data release does lead to a number of important limitations to the\ndata quality which should be carefully considered before drawing conclusions\nfrom the data.", "cat": "astro-ph.IM", "authors": ["Gaia Collaboration", "A. G. A. Brown", "A. Vallenari", "T. Prusti", "J. de Bruijne", "F. Mignard", "R. Drimmel", "585 co-authors"]}, "407": {"id": "1512.05049v1", "title": "An HST Survey of the Highest-Velocity Ejecta in Cassiopeia A", "url": "http://arxiv.org/pdf/1512.05049v1", "date": "2015-12-16 04:53:26", "abs": "We present Hubble Space Telescope WFC3/IR images of the Cassiopeia A\nsupernova remnant that survey its high-velocity, S-rich debris in the NE jet\nand SW counterjet regions through [S III] 9069, 9531 and [S II] 10,287 - 10,370\nline emissions. We identify nearly 3400 sulfur emitting knots concentrated in\n~120 degree wide opposing streams, almost triple the number previously known.\nThe vast majority of these ejecta knots lie at projected distances well out\nahead of the remnant's forward blast wave and main shell ejecta, extending to\nangular distance of 320\" to the NE and 260\" to the SW from the center of\nexpansion. Such angular distances imply undecelerated ejecta knot transverse\nvelocities of 15,600 and 12,700 km/s respectively, assuming an explosion date\n~1670 AD and a distance of 3.4 kpc. Optical spectra of knots near the outermost\ntip of the NE ejecta stream show strong emission lines of S, Ca, and Ar. We\nestimate a total mass ~0.1 Msun and a kinetic energy of at least ~1 x10^50 erg\nfor S-rich ejecta in the NE jet and SW counterjet. Although their broadness and\nkinetic energy argue against the Cas~A SN being a jet-induced explosion, the\njets are kinematically and chemically distinct from the rest of the remnant.\nThis may reflect an origin in a jet-like mechanism that accelerated interior\nmaterial from a Si,S,Ar,Ca-rich region near the progenitor's core up through\nthe mantle and H,He,N and O-rich outer layers with velocities that greatly\nexceeded that of the rapidly expanding photosphere.", "cat": "astro-ph.HE", "authors": ["Robert A. Fesen", "Dan Milisavljevic"]}, "408": {"id": "2006.00632v2", "title": "Neural Unsupervised Domain Adaptation in NLP---A Survey", "url": "http://arxiv.org/pdf/2006.00632v2", "date": "2020-10-28 08:24:14", "abs": "Deep neural networks excel at learning from labeled data and achieve\nstate-of-the-art resultson a wide array of Natural Language Processing tasks.\nIn contrast, learning from unlabeled data, especially under domain shift,\nremains a challenge. Motivated by the latest advances, in this survey we review\nneural unsupervised domain adaptation techniques which do not require labeled\ntarget domain data. This is a more challenging yet a more widely applicable\nsetup. We outline methods, from early traditional non-neural methods to\npre-trained model transfer. We also revisit the notion of domain, and we\nuncover a bias in the type of Natural Language Processing tasks which received\nmost attention. Lastly, we outline future directions, particularly the broader\nneed for out-of-distribution generalization of future NLP.", "cat": "cs.CL", "authors": ["Alan Ramponi", "Barbara Plank"]}, "409": {"id": "2309.01955v2", "title": "A Survey on Interpretable Cross-modal Reasoning", "url": "http://arxiv.org/pdf/2309.01955v2", "date": "2023-09-14 13:10:34", "abs": "In recent years, cross-modal reasoning (CMR), the process of understanding\nand reasoning across different modalities, has emerged as a pivotal area with\napplications spanning from multimedia analysis to healthcare diagnostics. As\nthe deployment of AI systems becomes more ubiquitous, the demand for\ntransparency and comprehensibility in these systems' decision-making processes\nhas intensified. This survey delves into the realm of interpretable cross-modal\nreasoning (I-CMR), where the objective is not only to achieve high predictive\nperformance but also to provide human-understandable explanations for the\nresults. This survey presents a comprehensive overview of the typical methods\nwith a three-level taxonomy for I-CMR. Furthermore, this survey reviews the\nexisting CMR datasets with annotations for explanations. Finally, this survey\nsummarizes the challenges for I-CMR and discusses potential future directions.\nIn conclusion, this survey aims to catalyze the progress of this emerging\nresearch area by providing researchers with a panoramic and comprehensive\nperspective, illuminating the state of the art and discerning the\nopportunities. The summarized methods, datasets, and other resources are\navailable at\nhttps://github.com/ZuyiZhou/Awesome-Interpretable-Cross-modal-Reasoning.", "cat": "cs.AI", "authors": ["Dizhan Xue", "Shengsheng Qian", "Zuyi Zhou", "Changsheng Xu"]}, "410": {"id": "1605.01439v1", "title": "A Systematic Survey of Protoclusters at $z\\sim3\\mathrm{-}6$ in the CFHTLS Deep Fields", "url": "http://arxiv.org/pdf/1605.01439v1", "date": "2016-05-04 21:21:36", "abs": "We present the discovery of three protoclusters at $z\\sim3\\mathrm{-}4$ with\nspectroscopic confirmation in the Canada-France-Hawaii Telescope (CFHT) Legacy\nSurvey Deep Fields. In these fields, we investigate the large-scale projected\nsky distribution of $z\\sim3\\mathrm{-}6$ Lyman break galaxies and identify 21\nprotocluster candidates from regions that are overdense at more than $4\\sigma$\noverdensity significance. Based on cosmological simulations, it is expected\nthat more than $76\\%$ of these candidates will evolve into a galaxy cluster of\nat least a halo mass of $10^{14}\\,\\mathrm{M_\\odot}$ at $z=0$. We perform\nfollow-up spectroscopy for eight of the candidates using Subaru/FOCAS,\nKeckII/DEIMOS, and Gemini-N/GMOS. In total we target 462 dropout candidates and\nobtain 138 spectroscopic redshifts. We confirm three real protoclusters at\n$z=3\\mathrm{-}4$ with more than five members spectroscopically identified, and\nfind one to be an incidental overdense region by mere chance alignment. The\nother four candidate regions at $z\\sim5\\mathrm{-}6$ require more spectroscopic\nfollow-up in order to be conclusive. A $z=3.67$ protocluster, which has eleven\nspectroscopically confirmed members, shows a remarkable core-like structure\ncomposed of a central small region ($<0.5\\,\\mathrm{physical\\>Mpc}$) and an\noutskirts region ($\\sim1.0\\,\\mathrm{physical\\>Mpc}$). The Ly$\\alpha$ equivalent\nwidths of members of the protocluster are significantly smaller than those of\nfield galaxies at the same redshift while there is no difference in the UV\nluminosity distributions. These results imply that some environmental effects\nstart operating as early as at $z\\sim4$ along with the growth of the\nprotocluster structure.", "cat": "astro-ph.GA", "authors": ["Jun Toshikawa", "Nobunari Kashikawa", "Roderik Overzier", "Matthew A. Malkan", "Hisanori Furusawa", "Shogo Ishikawa", "Masafusa Onoue", "Kazuaki Ota", "Masayuki Tanaka", "Yuu Niino", "Hisakazu Uchiyama"]}, "411": {"id": "2404.07461v1", "title": "\"Confidently Nonsensical?'': A Critical Survey on the Perspectives and Challenges of 'Hallucinations' in NLP", "url": "http://arxiv.org/pdf/2404.07461v1", "date": "2024-04-11 03:51:29", "abs": "We investigate how hallucination in large language models (LLM) is\ncharacterized in peer-reviewed literature using a critical examination of 103\npublications across NLP research. Through a comprehensive review of\nsociological and technological literature, we identify a lack of agreement with\nthe term `hallucination.' Additionally, we conduct a survey with 171\npractitioners from the field of NLP and AI to capture varying perspectives on\nhallucination. Our analysis underscores the necessity for explicit definitions\nand frameworks outlining hallucination within NLP, highlighting potential\nchallenges, and our survey inputs provide a thematic understanding of the\ninfluence and ramifications of hallucination in society.", "cat": "cs.CL", "authors": ["Pranav Narayanan Venkit", "Tatiana Chakravorti", "Vipul Gupta", "Heidi Biggs", "Mukund Srinath", "Koustava Goswami", "Sarah Rajtmajer", "Shomir Wilson"]}, "412": {"id": "1611.04671v1", "title": "The high-redshift evolution of the Red Sequence scatter from joint simulations and HAWK-I Cluster Survey", "url": "http://arxiv.org/pdf/1611.04671v1", "date": "2016-11-15 01:58:05", "abs": "We study the evolution of the Red Sequence (RS) scatter in galaxy clusters\nand groups simultaneously using predictions from our simulations (cosmological\nhydrodynamic + semi-analytical) as well as observational data from the HAWK-I\nCluster Survey (HCS), a sample of galaxy clusters at redshifts $0.8 < z < 1.5$.\nWe analyze the intrinsic scatter of the RS to investigate whether the stellar\nage can be its main effective driver, at the same time assessing the role of\nmetallicity variations in shaping the RS building at around epoch $z\\sim$1 and\nbeyond. To this purpose we rely on various methods to derive the average age\nand age spread from the RS colour scatter of the HCS sample, with the aid of\npopulation synthesis models. The RS scatter predicted by the models at $z< 0.7$\nis found to not depend on the star formation history adopted, whilst at $z>the\ncorrelation found between age and rest-frame colour scatters is quite robust,\nalthough all age scatter estimations ultimately depend on the definition of RS\nas well as on the completeness limits adopted. We find that the age spread of\nRS galaxies predicted by both hydrodynamical simulations and SAM increases with\ncosmic epoch, while the ratio between the age spread and the average age\nremains approximately constant. Both trends are in agreement with observational\nresults from both the HCS and other literature samples.", "cat": "astro-ph.GA", "authors": ["A. D. Romeo", "P. Cerulo", "Kang Xi", "E. Contini", "J. Sommer-Larsen", "I. Gavignaud"]}, "413": {"id": "2201.06310v1", "title": "A survey study of success factors in data science projects", "url": "http://arxiv.org/pdf/2201.06310v1", "date": "2022-01-17 09:50:46", "abs": "In recent years, the data science community has pursued excellence and made\nsignificant research efforts to develop advanced analytics, focusing on solving\ntechnical problems at the expense of organizational and socio-technical\nchallenges. According to previous surveys on the state of data science project\nmanagement, there is a significant gap between technical and organizational\nprocesses. In this article we present new empirical data from a survey to 237\ndata science professionals on the use of project management methodologies for\ndata science. We provide additional profiling of the survey respondents' roles\nand their priorities when executing data science projects. Based on this survey\nstudy, the main findings are: (1) Agile data science lifecycle is the most\nwidely used framework, but only 25% of the survey participants state to follow\na data science project methodology. (2) The most important success factors are\nprecisely describing stakeholders' needs, communicating the results to\nend-users, and team collaboration and coordination. (3) Professionals who\nadhere to a project methodology place greater emphasis on the project's\npotential risks and pitfalls, version control, the deployment pipeline to\nproduction, and data security and privacy.", "cat": "cs.DB", "authors": ["I\u00f1igo Martinez", "Elisabeth Viles", "Igor G. Olaizola"]}, "414": {"id": "0905.3410v2", "title": "Optimizing baryon acoustic oscillation surveys II: curvature, redshifts, and external datasets", "url": "http://arxiv.org/pdf/0905.3410v2", "date": "2009-10-05 21:44:11", "abs": "We extend our study of the optimization of large baryon acoustic oscillation\n(BAO) surveys to return the best constraints on the dark energy, building on\nPaper I of this series (Parkinson et al. 2007). The survey galaxies are assumed\nto be pre-selected active, star-forming galaxies observed by their line\nemission with a constant number density across the redshift bin. Star-forming\ngalaxies have a redshift desert in the region 1.6 < z < 2, and so this redshift\nrange was excluded from the analysis. We use the Seo & Eisenstein (2007)\nfitting formula for the accuracies of the BAO measurements, using only the\ninformation for the oscillatory part of the power spectrum as distance and\nexpansion rate rulers. We go beyond our earlier analysis by examining the\neffect of including curvature on the optimal survey configuration and updating\nthe expected `prior' constraints from Planck and SDSS. We once again find that\nthe optimal survey strategy involves minimizing the exposure time and\nmaximizing the survey area (within the instrumental constraints), and that all\ntime should be spent observing in the low-redshift range (z<1.6) rather than\nbeyond the redshift desert, z>2. We find that when assuming a flat universe the\noptimal survey makes measurements in the redshift range 0.1 < z <0.7, but that\nincluding curvature as a nuisance parameter requires us to push the maximum\nredshift to 1.35, to remove the degeneracy between curvature and evolving dark\nenergy. The inclusion of expected other data sets (such as WiggleZ, BOSS and a\nstage III SN-Ia survey) removes the necessity of measurements below redshift\n0.9, and pushes the maximum redshift up to 1.5. We discuss considerations in\ndetermining the best survey strategy in light of uncertainty in the true\nunderlying cosmological model.", "cat": "astro-ph.CO", "authors": ["David Parkinson", "Martin Kunz", "Andrew R. Liddle", "Bruce A. Bassett", "Robert C. Nichol", "Mihran Vardanyan"]}, "415": {"id": "2001.02358v2", "title": "Characterization of unresolved and unclassified sources detected in radio continuum surveys of the Galactic plane", "url": "http://arxiv.org/pdf/2001.02358v2", "date": "2020-02-01 07:05:53", "abs": "The continuum emission from 1 to 2 GHz of The HI/OH/Recombination line survey\nof the inner Milky Way (THOR) at $\\lesssim$18\" resolution covers $\\sim 132$\nsquare degrees of the Galactic plane and detects 10387 sources. Similarly, the\nfirst data release of the Global View of Star Formation in the Milky Way\n(GLOSTAR) surveys covers $\\sim 16$ square degrees of the Galactic plane from\n4-8 GHz at 18\" resolution and detects 1575 sources. However, a large fraction\nof the unresolved discrete sources detected in these radio continuum surveys of\nthe Galactic plane remain unclassified. Here, we study the Euclidean-normalized\ndifferential source counts of unclassified and unresolved sources detected in\nthese surveys and compare them with simulated extragalactic radio source\npopulations as well as previously established source counts. We find that the\ndifferential source counts for THOR and GLOSTAR surveys are in excellent\nagreement with both simulation and previous observations. We also estimate the\nangular two-point correlation function of unclassified and unresolved sources\ndetected in THOR survey. We find a higher clustering amplitude in comparison\nwith the Faint Images of the Radio Sky at Twenty-cm (FIRST) survey up to the\nangular separation of $5^{\\circ}$. The decrease in angular correlation with\nincreasing flux cut and the excellent agreement of clustering pattern of\nsources above 1 mJy with high $z$ samples ($z >0.5$) of the FIRST survey\nindicates that these sources might be high $z$ extragalactic compact objects.\nThe similar pattern of one-point and two-point statistics of unclassified and\ncompact sources with extragalactic surveys and simulations confirms the\nextragalactic origin of these sources.", "cat": "astro-ph.GA", "authors": ["Arnab Chakraborty", "Nirupam Roy", "Y. Wang", "Abhirup Datta", "H. Beuther", "S. -N. X. Medina", "K. M. Menten", "J. S. Urquhart", "A. Brunthaler", "S. A. Dzib"]}, "416": {"id": "0707.2537v1", "title": "A Combined Spitzer and Chandra Survey of Young Stellar Objects in the Serpens Cloud Core", "url": "http://arxiv.org/pdf/0707.2537v1", "date": "2007-07-17 15:07:02", "abs": "We present Spitzer and Chandra observations of the nearby (~260 pc) embedded\nstellar cluster in the Serpens Cloud Core. We observed, using Spitzer's IRAC\nand MIPS instruments, in six wavelength bands from 3 to 70 ${\\mu}m$, to detect\nthermal emission from circumstellar disks and protostellar envelopes, and to\nclassify stars using color-color diagrams and spectral energy distributions\n(SEDs). These data are combined with Chandra observations to examine the\neffects of circumstellar disks on stellar X-ray properties. Young diskless\nstars were also identified from their increased X-ray emission. We have\nidentified 138 YSOs in Serpens: 22 class 0/I, 16 flat spectrum, 62 class II, 17\ntransition disk, and 21 class III stars; 60 of which exhibit X-ray emission.\nOur primary results are the following: 1.) ten protostars detected previously\nin the sub-millimeter are detected at lambda < 24 microns, seven at lambda < 8\nmicrons, 2.) the protostars are more closely grouped than more evolved YSOs\n(median separation : ~0.024 pc, and 3.) the luminosity and temperature of the\nX-ray emitting plasma around these YSOs does not show any significant\ndependence on evolutionary class. We combine the infrared derived values of AK\nand X-ray values of NH for 8 class III objects and find that the column density\nof hydrogen gas per mag of extinctions is less than half the standard\ninterstellar value, for AK > 1. This may be the result of grain growth through\ncoagulation and/or the accretion of volatiles in the Serpens cloud core.", "cat": "astro-ph", "authors": ["E. Winston", "S. T. Megeath", "S. J. Wolk", "J. Muzerolle", "R. Gutermuth", "J. L. Hora", "L. E. Allen", "B. Spitzbart", "P. Myers", "G. G. Fazio"]}, "417": {"id": "2109.02349v1", "title": "Smart Grids Co-Simulations: Survey & Research Directions", "url": "http://arxiv.org/pdf/2109.02349v1", "date": "2021-09-06 10:38:54", "abs": "The integration of renewable sources, communication and power networks with\ninformation and communication technologies is one of the main challenges in\nSmart Grids (SG) large-scale testing. For this reason, the coupling of\nsimulators is commonly used to dynamically simulate several aspects of the SG\ninfrastructure, in the so-called co-simulations. In this paper, we provide a\nscoping review of research of co-simulations in the context of Smart Grids: i)\nresearch areas and research problems addressed by co-simulations, ii) specific\nco-simulation aspects focus of research, iii) typical coupling of simulators in\nco-simulation studies. Based on the results, we discuss research directions of\nfuture SG co-simulation research in each of the identified areas.", "cat": "cs.OH", "authors": ["Peter Mihal", "Martin Schvarcbacher", "Bruno Rossi", "Tom\u00e1\u0161 Pitner"]}, "418": {"id": "1607.03808v2", "title": "The ALMA Frontier Fields survey I: 1.1 mm continuum detections in Abell 2744, MACSJ0416.1-2403 and MACSJ1149.5+2223", "url": "http://arxiv.org/pdf/1607.03808v2", "date": "2016-10-24 16:15:35", "abs": "Dusty star-forming galaxies are among the most prodigious systems at high\nredshift (z>1), characterized by high star formation rates and huge dust\nreservoirs. The bright end of this population has been well characterized in\nrecent years, but considerable uncertainties remain for fainter dusty\nstar-forming galaxies, which are responsible for the bulk of star formation at\nhigh redshift and thus play a key role in galaxy growth and evolution.\n In this first paper of our series, we describe our methods for finding high\nredshift faint dusty galaxies using millimeter observations with ALMA. We\nobtained ALMA 1.1 mm mosaic images for three strong-lensing galaxy clusters\nfrom the Frontier Fields survey. The 2'x2' mosaics overlap with the deep HST\nWFC3/IR footprints and encompass the high magnification regions of each\ncluster. The combination of extremely high ALMA sensitivity and the\nmagnification power of these clusters allows us to systematically probe the\nsub-mJy population of dusty star-forming galaxies over a large surveyed area.\n We present a description of the reduction and analysis of the ALMA continuum\nobservations for the galaxy clusters Abell 2744 (z=0.308), MACSJ0416.1-2403\n(z=0.396) and MACSJ1149.5+2223 (z=0.543), for which we reach observed rms\nsensitivities of 55, 59 and 71 $\\mu$Jy beam$^{-1}$ respectively. We detect 12\ndusty star-forming galaxies at S/N>5.0 across the three clusters, all of them\npresenting coincidence with NIR detected counterparts in the HST images. None\nof the sources fall close to the lensing caustics, thus they are not strongly\nlensed. The observed 1.1 mm flux densities for the total sample of galaxies\nrange from 0.41 to 2.82 mJy, with observed effective radii spanning <0.05\" to\n0.37\"$\\pm$0.21\". The lensing-corrected sizes of the detected sources appear to\nbe in the same range as those measured in brighter samples, albeit with\npossibly larger dispersion.", "cat": "astro-ph.GA", "authors": ["J. Gonz\u00e1lez-L\u00f3pez", "F. E. Bauer", "C. Romero-Ca\u00f1izales", "R. Kneissl", "E. Villard", "R. Carvajal", "S. Kim", "N. Laporte", "T. Anguita", "M. Aravena", "R. J. Bouwens", "L. Bradley", "M. Carrasco", "R. Demarco", "H. Ford", "E. Ibar", "L. Infante", "H. Messias", "A. M. Mu\u00f1oz Arancibia", "N. Nagar", "N. Padilla", "E. Treister", "P. Troncoso", "A. Zitrin"]}, "419": {"id": "2009.08395v1", "title": "A Multimodal Memes Classification: A Survey and Open Research Issues", "url": "http://arxiv.org/pdf/2009.08395v1", "date": "2020-09-17 16:13:21", "abs": "Memes are graphics and text overlapped so that together they present concepts\nthat become dubious if one of them is absent. It is spread mostly on social\nmedia platforms, in the form of jokes, sarcasm, motivating, etc. After the\nsuccess of BERT in Natural Language Processing (NLP), researchers inclined to\nVisual-Linguistic (VL) multimodal problems like memes classification, image\ncaptioning, Visual Question Answering (VQA), and many more. Unfortunately, many\nmemes get uploaded each day on social media platforms that need automatic\ncensoring to curb misinformation and hate. Recently, this issue has attracted\nthe attention of researchers and practitioners. State-of-the-art methods that\nperformed significantly on other VL dataset, tends to fail on memes\nclassification. In this context, this work aims to conduct a comprehensive\nstudy on memes classification, generally on the VL multimodal problems and\ncutting edge solutions. We propose a generalized framework for VL problems. We\ncover the early and next-generation works on VL problems. Finally, we identify\nand articulate several open research issues and challenges. This is the first\nstudy that presents the generalized view of the advanced classification\ntechniques concerning memes classification to the best of our knowledge. We\nbelieve this study presents a clear road-map for the Machine Learning (ML)\nresearch community to implement and enhance memes classification techniques.", "cat": "cs.CV", "authors": ["Tariq Habib Afridi", "Aftab Alam", "Muhammad Numan Khan", "Jawad Khan", "Young-Koo Lee"]}, "420": {"id": "1009.3928v1", "title": "The X-Ray Properties of the Optically Brightest Mini-BAL Quasars from the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1009.3928v1", "date": "2010-09-20 20:00:01", "abs": "We have compiled a sample of 14 of the optically brightest radio-quiet\nquasars ($m_{i}$~$\\le$~17.5 and $z$~$\\ge$~1.9) in the Sloan Digital Sky Survey\nData Release 5 quasar catalog that have C IV mini-BALs present in their\nspectra. X-ray data for 12 of the objects were obtained via a Chandra snapshot\nsurvey using ACIS-S, while data for the other two quasars were obtained from\narchival XMM-Newton observations. Joint X-ray spectral analysis shows the\nmini-BAL quasars have a similar average power-law photon index\n($\\Gamma\\approx1.9$) and level of intrinsic absorption ($N_H \\lesssim 8\\times\n10^{21} \\ {\\rm cm}^{-2}$) as non-BMB (neither BAL nor mini-BAL) quasars.\nMini-BAL quasars are more similar to non-BMB quasars than to BAL quasars in\ntheir distribution of relative X-ray brightness (assessed with\n$\\Delta\\alpha_{\\rm ox}$). Relative colors indicate mild dust reddening in the\noptical spectra of mini-BAL quasars. Significant correlations between\n$\\Delta\\alpha_{\\rm ox}$ and UV absorption properties are confirmed for a sample\nof 56 sources combining mini-BAL and BAL quasars with high signal-to-noise\nratio rest-frame UV spectra, which generally supports models in which X-ray\nabsorption is important in enabling driving of the UV absorption-line wind. We\nalso propose alternative parametrizations of the UV absorption properties of\nmini-BAL and BAL quasars, which may better describe the broad absorption\ntroughs in some respects.", "cat": "astro-ph.CO", "authors": ["Jianfeng Wu", "W. N. Brandt", "M. L. Comins", "Robert R. Gibson", "Ohad Shemmer", "Gordon P. Garmire", "Donald P. Schneider"]}, "421": {"id": "1606.04107v2", "title": "The MOSDEF Survey: Detection of [OIII]$\u03bb$4363 and the direct-method oxygen abundance of a star-forming galaxy at z=3.08", "url": "http://arxiv.org/pdf/1606.04107v2", "date": "2016-06-16 17:27:20", "abs": "We present measurements of the electron-temperature based oxygen abundance\nfor a highly star-forming galaxy at z=3.08, COSMOS-1908. This is the highest\nredshift at which [OIII]$\\lambda$4363 has been detected, and the first time\nthat this line has been measured at z>2. We estimate an oxygen abundance of\n12+log(O/H)$=8.00^{+0.13}_{-0.14}$. This galaxy is a low-mass ($10^{9.3}$\nM$_{\\odot}$), highly star-forming ($\\sim50$ M$_{\\odot}$ yr$^{-1}$) system that\nhosts a young stellar population ($\\sim160$ Myr). We investigate the physical\nconditions of the ionized gas in COSMOS-1908 and find that this galaxy has a\nhigh ionization parameter, little nebular reddening ($E(B-V)_{\\rm gas}<0.14$),\nand a high electron density ($n_e\\sim500$ cm$^{-3}$). We compare the ratios of\nstrong oxygen, neon, and hydrogen lines to the direct-method oxygen abundance\nfor COSMOS-1908 and additional star-forming galaxies at z=0-1.8 with\n[OIII]$\\lambda$4363 measurements, and show that galaxies at z$\\sim$1-3 follow\nthe same strong-line correlations as galaxies in the local universe. This\nagreement suggests that the relationship between ionization parameter and O/H\nis similar for z$\\sim$0 and high-redshift galaxies. These results imply that\nmetallicity calibrations based on lines of oxygen, neon, and hydrogen do not\nstrongly evolve with redshift and can reliably estimate abundances out to\nz$\\sim$3, paving the way for robust measurements of the evolution of the\nmass-metallicity relation to high redshift.", "cat": "astro-ph.GA", "authors": ["Ryan L. Sanders", "Alice E. Shapley", "Mariska Kriek", "Naveen A. Reddy", "William R. Freeman", "Alison L. Coil", "Brian Siana", "Bahram Mobasher", "Irene Shivaei", "Sedona H. Price", "Laura de Groot"]}, "422": {"id": "2112.07545v1", "title": "Assessment of [Fe/H] determinations for FGK stars in spectroscopic surveys", "url": "http://arxiv.org/pdf/2112.07545v1", "date": "2021-12-14 16:53:00", "abs": "The number of stars with a measured value of [Fe/H] is considerably\nincreasing thanks to spectroscopic surveys. However different methodologies,\ninputs and assumptions used in spectral analyses lead to different precisions\nin [Fe/H] and possibly to systematic differences that need to be evaluated. It\nis essential to understand the characteristics of each survey to fully exploit\ntheir potential, in particular if the surveys are combined. The purpose of this\nstudy is to compare [Fe/H] determinations from the largest spectroscopic\nsurveys (APOGEE, GALAH, the Gaia ESO survey, RAVE, LAMOST, SEGUE ) to other\ncatalogues taken as reference. Offsets and dispersions of the residuals are\nexamined as well as their trends with other parameters. We use reference\nsamples providing independent determinations of [Fe/H] which are compared to\nthose from the surveys for common stars. The distribution of the residuals is\nassessed through simple statistics that measures the offset between two\ncatalogues and the dispersion representative of the precision of both\ncatalogues. When relevant, linear fits are performed. A large sample of\nFGK-type stars with [Fe/H] based on high-resolution, high signal to noise\nspectroscopy was built from the PASTEL catalogue to provide a reference sample.\nWe also use FGK members in open and globular clusters to assess the internal\nconsistency of [Fe/H] of each survey. The agreement of median [Fe/H] values for\nclusters observed by different surveys is discussed. All the surveys\noverestimate the low metallicities, and some of them also underestimate the\nhigh metallicities. They perform well in the most populated intermediate\nmetallicity range, whatever the resolution. In most cases the typical precision\nthat we deduce from the comparisons is in good agreement with the uncertainties\nquoted in the catalogues. Some exceptions to this general behaviour are\ndiscussed.", "cat": "astro-ph.SR", "authors": ["Caroline Soubiran", "Nathalie Brouillet", "Laia Casamiquela"]}, "423": {"id": "2012.04830v4", "title": "Machine Learning for Cataract Classification and Grading on Ophthalmic Imaging Modalities: A Survey", "url": "http://arxiv.org/pdf/2012.04830v4", "date": "2022-04-02 01:52:37", "abs": "Cataracts are the leading cause of visual impairment and blindness globally.\nOver the years, researchers have achieved significant progress in developing\nstate-of-the-art machine learning techniques for automatic cataract\nclassification and grading, aiming to prevent cataracts early and improve\nclinicians' diagnosis efficiency. This survey provides a comprehensive survey\nof recent advances in machine learning techniques for cataract\nclassification/grading based on ophthalmic images. We summarize existing\nliterature from two research directions: conventional machine learning methods\nand deep learning methods. This survey also provides insights into existing\nworks of both merits and limitations. In addition, we discuss several\nchallenges of automatic cataract classification/grading based on machine\nlearning techniques and present possible solutions to these challenges for\nfuture research.", "cat": "eess.IV", "authors": ["Xiaoqing Zhang", "Yan Hu", "Zunjie Xiao", "Jiansheng Fang", "Risa Higashita", "Jiang Liu"]}, "424": {"id": "2011.09329v1", "title": "A VLBA Survey of radio stars in the Orion Nebula Cluster: I. The nonthermal radio population", "url": "http://arxiv.org/pdf/2011.09329v1", "date": "2020-11-18 15:08:32", "abs": "We present first results of a four-epoch VLBA survey for nonthermal emission\ntoward all 556 compact radio sources previously identified in a deep VLA survey\nof the Orion Nebula Cluster (ONC). We identify VLBA counterparts toward an\nunprecedented 123 sources. Of these, 41 do not have X-ray counterparts, of\nwhich 34 also do not display near-infrared counterparts. Since these cannot be\nexplained by extragalactic background sources, this suggests a component of the\nONC population of young stellar objects that are too deeply embedded for even\nX-rays to be detectable. We find pervasive variability and detect even most of\nthe highest-S/N sources in only one out of four epochs. Neither a negative\nspectral index nor extreme variability in the VLA data is a good predictor of a\nVLBA detection.", "cat": "astro-ph.SR", "authors": ["Jan Forbrich", "Sergio A. Dzib", "Mark J. Reid", "Karl M. Menten"]}, "425": {"id": "2201.03397v2", "title": "A Survey on the k-Path Vertex Cover Problem", "url": "http://arxiv.org/pdf/2201.03397v2", "date": "2022-01-12 08:08:06", "abs": "Given a graph $G=(V,E)$ and a positive integer $k\\ge2$, a $k$-path vertex\ncover is a subset of vertices $F$ such that every path on $k$ vertices in $G$\ncontains at least one vertex from $F$. A minimum $k$-path vertex cover in $G$\nis a $k$-path vertex cover with minimum cardinality and its cardinality is\ncalled the {\\it $k$-path vertex cover number} of $G$. In the {\\it $k$-path\nvertex cover problem}, it is required to find a minimum $k$-path vertex cover\nin a given graph. In this paper, we present a brief survey of the current state\nof the art in the study of the $k$-path vertex cover problem and the $k$-path\nvertex cover number.", "cat": "math.CO", "authors": ["Jianhua Tu"]}, "426": {"id": "2202.07893v2", "title": "A Survey of Pretraining on Graphs: Taxonomy, Methods, and Applications", "url": "http://arxiv.org/pdf/2202.07893v2", "date": "2022-03-21 01:52:33", "abs": "Pretrained Language Models (PLMs) such as BERT have revolutionized the\nlandscape of Natural Language Processing (NLP). Inspired by their\nproliferation, tremendous efforts have been devoted to Pretrained Graph Models\n(PGMs). Owing to the powerful model architectures of PGMs, abundant knowledge\nfrom massive labeled and unlabeled graph data can be captured. The knowledge\nimplicitly encoded in model parameters can benefit various downstream tasks and\nhelp to alleviate several fundamental issues of learning on graphs. In this\npaper, we provide the first comprehensive survey for PGMs. We firstly present\nthe limitations of graph representation learning and thus introduce the\nmotivation for graph pre-training. Then, we systematically categorize existing\nPGMs based on a taxonomy from four different perspectives. Next, we present the\napplications of PGMs in social recommendation and drug discovery. Finally, we\noutline several promising research directions that can serve as a guideline for\nfuture research.", "cat": "cs.LG", "authors": ["Jun Xia", "Yanqiao Zhu", "Yuanqi Du", "Stan Z. Li"]}, "427": {"id": "2401.17309v3", "title": "The hot circumgalactic medium in the eROSITA All-Sky Survey II. Scaling relations between X-ray luminosity and galaxies' mass", "url": "http://arxiv.org/pdf/2401.17309v3", "date": "2024-08-18 15:58:26", "abs": "Understanding how the properties of galaxies relate to the properties of the\nhot circum-galactic medium (CGM) around them can constrain galaxy evolution\nmodels. We measured the X-ray luminosity of the hot CGM based on the surface\nbrightness profiles of central galaxy samples measured from Spectrum Roentgen\nGamma (SRG)/eROSITA all-sky survey data. We related the X-ray luminosity to the\ngalaxies' stellar and halo mass, and we compared the observed relations to the\nself-similar model and intrinsic (i.e., not forward-modeled) output of the\nIllustrisTNG, EAGLE, and SIMBA simulations. The average hot CGM X-ray\nluminosity ($L_{\\rm X,CGM}$) correlates with the galaxy's stellar mass ($M_*$).\nIt increases from $(1.6 \\pm 2.1)\\times10^{39} \\rm erg\\,s^{-1}$ to $(3.4 \\pm\n0.3)\\times10^{41} \\rm erg\\,s^{-1}$, when $\\log(M_*)$ increases from 10.0 to\n11.5. A power law describes the correlation as $\\log(L_{\\rm X,CGM})= (2.4\\pm\n0.1)\\times \\log(M_*)+(14.6\\pm1.5)$. The hot CGM X-ray luminosity as a function\nof halo mass is measured within $\\log(M_{\\rm 500c})=11.3-13.7$, extending our\nknowledge of the scaling relation by more than two orders of magnitude. $L_{\\rm\nX,CGM}$ increases with $M_{\\rm 500c}$ from $(3.0 \\pm 1.6)\\times10^{39}\\ \\rm\nerg\\,s^{-1}$ at $\\log(M_{\\rm 500c})=11.3$ to $(1.3 \\pm 0.1)\\times10^{42}\\ \\rm\nerg\\,s^{-1}$ at $\\log(M_{\\rm 500c})=13.7$. The relation follows a power law of\n$\\log(L_{\\rm X,CGM})= (1.32\\pm 0.05)\\times \\log(M_{\\rm 500c})+(24.1\\pm0.7)$.\nOur observations highlight the necessity of non-gravitational processes at the\ngalaxy group scale while suggesting these processes are sub-dominant at the\ngalaxy scale. We show that the outputs of current cosmological galaxy\nsimulations generally align with the observational results uncovered here but\nwith possibly important deviations in selected mass ranges.", "cat": "astro-ph.GA", "authors": ["Yi Zhang", "Johan Comparat", "Gabriele Ponti", "Andrea Merloni", "Kirpal Nandra", "Frank Haberl", "Nhut Truong", "Annalisa Pillepich", "Nicola Locatelli", "Xiaoyuan Zhang", "Jeremy Sanders", "Xueying Zheng", "Ang Liu", "Paola Popesso", "Teng Liu", "Peter Predehl", "Mara Salvato", "Soumya Shreeram", "Michael C. H. Yeung"]}, "428": {"id": "2107.10059v1", "title": "Automated Identification of Security Discussions in Microservices Systems: Industrial Surveys and Experiments", "url": "http://arxiv.org/pdf/2107.10059v1", "date": "2021-07-21 13:03:08", "abs": "Lack of awareness and knowledge of microservices-specific security challenges\nand solutions often leads to ill-informed security decisions in microservices\nsystem development. We claim that identifying and leveraging security\ndiscussions scattered in existing microservices systems can partially close\nthis gap. We define security discussion as \"a paragraph from developer\ndiscussions that includes design decisions, challenges, or solutions relating\nto security\". We first surveyed 67 practitioners and found that securing\nmicroservices systems is a unique challenge and that having access to security\ndiscussions is useful for making security decisions. The survey also confirms\nthe usefulness of potential tools that can automatically identify such security\ndiscussions. We developed fifteen machine/deep learning models to automatically\nidentify security discussions. We applied these models on a manually\nconstructed dataset consisting of 4,813 security discussions and 12,464\nnon-security discussions. We found that all the models can effectively identify\nsecurity discussions: an average precision of 84.86%, recall of 72.80%,\nF1-score of 77.89%, AUC of 83.75% and G-mean 82.77%. DeepM1, a deep learning\nmodel, performs the best, achieving above 84% in all metrics and significantly\noutperforms three baselines. Finally, the practitioners' feedback collected\nfrom a validation survey reveals that security discussions identified by DeepM1\nhave promising applications in practice.", "cat": "cs.SE", "authors": ["Ali Rezaei Nasab", "Mojtaba Shahin", "Peng Liang", "Mohammad Ehsan Basiri", "Seyed Ali Hoseyni Raviz", "Hourieh Khalajzadeh", "Muhammad Waseem", "Amine Naseri"]}, "429": {"id": "2402.03093v3", "title": "AI-Enhanced Virtual Reality in Medicine: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2402.03093v3", "date": "2024-07-11 06:50:50", "abs": "With the rapid advance of computer graphics and artificial intelligence\ntechnologies, the ways we interact with the world have undergone a\ntransformative shift. Virtual Reality (VR) technology, aided by artificial\nintelligence (AI), has emerged as a dominant interaction media in multiple\napplication areas, thanks to its advantage of providing users with immersive\nexperiences. Among those applications, medicine is considered one of the most\npromising areas. In this paper, we present a comprehensive examination of the\nburgeoning field of AI-enhanced VR applications in medical care and services.\nBy introducing a systematic taxonomy, we meticulously classify the pertinent\ntechniques and applications into three well-defined categories based on\ndifferent phases of medical diagnosis and treatment: Visualization Enhancement,\nVR-related Medical Data Processing, and VR-assisted Intervention. This\ncategorization enables a structured exploration of the diverse roles that\nAI-powered VR plays in the medical domain, providing a framework for a more\ncomprehensive understanding and evaluation of these technologies. To our best\nknowledge, this is the first systematic survey of AI-powered VR systems in\nmedical settings, laying a foundation for future research in this\ninterdisciplinary domain.", "cat": "cs.CV", "authors": ["Yixuan Wu", "Kaiyuan Hu", "Danny Z. Chen", "Jian Wu"]}, "430": {"id": "1210.0363v1", "title": "Status and results from the RAVE survey", "url": "http://arxiv.org/pdf/1210.0363v1", "date": "2012-10-01 12:16:09", "abs": "RAVE, the RAdial Velocity Experiment, is a large spectroscopic survey which\ncollects spectroscopic data for stars in the southern hemisphere. RAVE uses the\nAAO Schmidt telescope with a wavelength coverage similar to Gaia but a lower\nresolution of R=7,500. Since 2003, RAVE collected over 500,000 spectra\nproviding an unprecedented dataset to study the structure and kinematics of the\nMilky Way and its stellar populations. In this review, we will summarize the\nmain results obtained using the RAVE catalogues.", "cat": "astro-ph.GA", "authors": ["A. Siebert"]}, "431": {"id": "2302.13442v2", "title": "Understanding URDF: A Survey Based on User Experience", "url": "http://arxiv.org/pdf/2302.13442v2", "date": "2023-03-12 20:49:43", "abs": "With the increasing complexity of robot systems, it is necessary to simulate\nthem before deployment. To do this, a model of the robot's kinematics or\ndynamics is required. One of the most commonly used formats for modeling robots\nis the Unified Robot Description Format (URDF). The goal of this article is to\nunderstand how URDF is currently used, what challenges people face when working\nwith it, and how the community sees the future of URDF. The outcome can\npotentially be used to guide future research. This article presents the results\nfrom a survey based on 510 anonymous responses from robotic developers of\ndifferent backgrounds and levels of experience. We find that 96.8% of the\nparticipants have simulated robots before, and of them 95.5% had used URDF. We\nidentify a number of challenges and limitations that complicate the use of\nURDF, such as the inability to model parallel linkages and closed-chain\nsystems, no real standard, lack of documentation, and a limited number of\ndynamic parameters to model the robot. Future perspectives for URDF are also\ndetermined, where 53.5% believe URDF will be more commonly used in the future,\n12.2% believe other standards or tools will make URDF obsolete, and 34.4% are\nnot sure what the future of URDF will be. Most participants agree that there is\na need for better tooling to ensure URDF's future use.", "cat": "cs.RO", "authors": ["Daniella Tola", "Peter Corke"]}, "432": {"id": "2205.11422v3", "title": "The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars", "url": "http://arxiv.org/pdf/2205.11422v3", "date": "2023-01-03 14:48:35", "abs": "We present $\\sim10-40\\,\\mu$m SOFIA-FORCAST images of 11 isolated protostars\nas part of the SOFIA Massive (SOMA) Star Formation Survey, with this\nmorphological classification based on 37 $\\mu$m imaging. We develop an\nautomated method to define source aperture size using the gradient of its\nbackground-subtracted enclosed flux and apply this to build spectral energy\ndistributions (SEDs). We fit the SEDs with radiative transfer models, developed\nwithin the framework of turbulent core accretion (TCA) theory, to estimate key\nprotostellar properties. Here, we release the sedcreator python package that\ncarries out these methods. The SEDs are generally well fitted by the TCA\nmodels, from which we infer initial core masses $M_c$ ranging from\n$20-430\\:M_\\odot$, clump mass surface densities $\\Sigma_{\\rm\ncl}\\sim0.3-1.7\\:{\\rm{g\\:cm}}^{-2}$ and current protostellar masses\n$m_*\\sim3-50\\:M_\\odot$. From a uniform analysis of the 40 sources in the full\nSOMA survey to date, we find that massive protostars form across a wide range\nof clump mass surface density environments, placing constraints on theories\nthat predict a minimum threshold $\\Sigma_{\\rm cl}$ for massive star formation.\nHowever, the upper end of the $m_*-\\Sigma_{\\rm cl}$ distribution follows trends\npredicted by models of internal protostellar feedback that find greater star\nformation efficiency in higher $\\Sigma_{\\rm cl}$ conditions. We also\ninvestigate protostellar far-IR variability by comparison with IRAS data,\nfinding no significant variation over an $\\sim$40 year baseline.", "cat": "astro-ph.GA", "authors": ["Ruben Fedriani", "Jonathan C. Tan", "Zoie Telkamp", "Yichen Zhang", "Yao-Lun Yang", "Mengyao Liu", "Chi-Yan Law", "Maria T. Beltran", "Viviana Rosero", "Kei E. I. Tanaka", "Giuliana Cosentino", "Prasanta Gorai", "Juan Farias", "Jan E. Staff", "James M. De Buizer", "Barbara Whitney"]}, "433": {"id": "1704.07455v2", "title": "Systematic Identification of LAEs for Visible Exploration and Reionization Research Using Subaru HSC (SILVERRUSH). I. Program Strategy and Clustering Properties of ~2,000 Lya Emitters at z=6-7 over the 0.3-0.5 Gpc$^2$ Survey Area", "url": "http://arxiv.org/pdf/1704.07455v2", "date": "2017-07-15 12:23:04", "abs": "We present the SILVERRUSH program strategy and clustering properties\ninvestigated with $\\sim 2,000$ Ly$\\alpha$ emitters at $z=5.7$ and $6.6$ found\nin the early data of the Hyper Suprime-Cam (HSC) Subaru Strategic Program\nsurvey exploiting the carefully designed narrowband filters. We derive angular\ncorrelation functions with the unprecedentedly large samples of LAEs at $z=6-7$\nover the large total area of $14-21$ deg$^2$ corresponding to $0.3-0.5$\ncomoving Gpc$^2$. We obtain the average large-scale bias values of $b_{\\rm\navg}=4.1\\pm 0.2$ ($4.5\\pm 0.6$) at $z=5.7$ ($z=6.6$) for $\\gtrsim L^*$ LAEs,\nindicating the weak evolution of LAE clustering from $z=5.7$ to $6.6$. We\ncompare the LAE clustering results with two independent theoretical models that\nsuggest an increase of an LAE clustering signal by the patchy ionized bubbles\nat the epoch of reionization (EoR), and estimate the neutral hydrogen fraction\nto be $x_{\\rm HI}=0.15^{+0.15}_{-0.15}$ at $z=6.6$. Based on the halo\noccupation distribution models, we find that the $\\gtrsim L^*$ LAEs are hosted\nby the dark-matter halos with the average mass of $\\log (\\left < M_{\\rm h}\n\\right >/M_\\odot) =11.1^{+0.2}_{-0.4}$ ($10.8^{+0.3}_{-0.5}$) at $z=5.7$\n($6.6$) with a Ly$\\alpha$ duty cycle of 1 % or less, where the results of\n$z=6.6$ LAEs may be slightly biased, due to the increase of the clustering\nsignal at the EoR. Our clustering analysis reveals the low-mass nature of\n$\\gtrsim L^*$ LAEs at $z=6-7$, and that these LAEs probably evolve into massive\nsuper-$L^*$ galaxies in the present-day universe.", "cat": "astro-ph.GA", "authors": ["Masami Ouchi", "Yuichi Harikane", "Takatoshi Shibuya", "Kazuhiro Shimasaku", "Yoshiaki Taniguchi", "Akira Konno", "Masakazu Kobayashi", "Masaru Kajisawa", "Tohru Nagao", "Yoshiaki Ono", "Akio K. Inoue", "Masayuki Umemura", "Masao Mori", "Kenji Hasegawa", "Ryo Higuchi", "Yutaka Komiyama", "Yuichi Matsuda", "Kimihiko Nakajima", "Tomoki Saito", "Shiang-Yu Wang"]}, "434": {"id": "1601.03668v1", "title": "The ALHAMBRA survey: evolution of galaxy spectral segregation", "url": "http://arxiv.org/pdf/1601.03668v1", "date": "2016-01-14 17:18:31", "abs": "We study the clustering of galaxies as a function of spectral type and\nredshift in the range $0.35 < z < 1.1$ using data from the Advanced Large\nHomogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The data\ncover 2.381 deg$^2$ in 7 fields, after applying a detailed angular selection\nmask, with accurate photometric redshifts [$\\sigma_z < 0.014(1+z)$] down to\n$I_{AB} < 24$. From this catalog we draw five fixed number density,\nredshift-limited bins. We estimate the clustering evolution for two different\nspectral populations selected using the ALHAMBRA-based photometric templates:\nquiescent and star-forming galaxies. For each sample, we measure the real-space\nclustering using the projected correlation function. Our calculations are\nperformed over the range $[0.03,10.0] h^{-1}$ Mpc, allowing us to find a\nsteeper trend for $r_p \\lesssim 0.2 h^{-1}$ Mpc, which is especially clear for\nstar-forming galaxies. Our analysis also shows a clear early differentiation in\nthe clustering properties of both populations: star-forming galaxies show\nweaker clustering with evolution in the correlation length over the analysed\nredshift range, while quiescent galaxies show stronger clustering already at\nhigh redshifts, and no appreciable evolution. We also perform the bias\ncalculation where similar segregation is found, but now it is among the\nquiescent galaxies where a growing evolution with redshift is clearer. These\nfindings clearly corroborate the well known colour-density relation, confirming\nthat quiescent galaxies are mainly located in dark matter halos that are more\nmassive than those typically populated by star-forming galaxies.", "cat": "astro-ph.GA", "authors": ["Ll. Hurtado-Gil", "P. Arnalte-Mur", "V. J. Mart\u00ednez", "A. Fern\u00e1ndez-Soto", "M. Stefanon", "B. Ascaso", "C. L\u00f3pez-Sanjuan", "I. M\u00e1rquez", "M. Povic", "K. Viironen", "J. A. L. Aguerri", "E. Alfaro", "T. Aparicio-Villegas", "N. Ben\u00edtez", "T. Broadhurst", "J. Cabrera-Ca\u00f1o", "F. J. Castander", "J. Cepa", "M. Cervi\u00f1o", "D. Crist\u00f3bal-Hornillos", "R. M. Gonz\u00e1lez Delgado", "C. Husillos", "L. Infante", "J. Masegosa", "M. Moles", "A. Molino", "A. del Olmo", "S. Paredes", "J. Perea", "F. Prada", "J. M. Quintana"]}, "435": {"id": "0709.3113v1", "title": "Point Sources from a Spitzer IRAC Survey of the Galactic Center", "url": "http://arxiv.org/pdf/0709.3113v1", "date": "2007-09-19 21:42:50", "abs": "We have obtained Spitzer/IRAC observations of the central 2.0 x 1.4 degrees\n(~280 x 200 pc) of the Galaxy at 3.6-8.0 microns. A point source catalog of\n1,065,565 objects is presented. The catalog includes magnitudes for the point\nsources at 3.6, 4.5, 5.8, and 8.0 microns, as well as JHK photometry from\n2MASS. The point source catalog is confusion limited with average limits of\n12.4, 12.1, 11.7, and 11.2 magnitudes for [3.6], [4.5], [5.8], and [8.0],\nrespectively. We find that the confusion limits are spatially variable because\nof stellar surface density, background surface brightness level, and extinction\nvariations across the survey region. The overall distribution of point source\ndensity with Galactic latitude and longitude is essentially constant, but\nstructure does appear when sources of different magnitude ranges are selected.\nBright stars show a steep decreasing gradient with Galactic latitude, and a\nslow decreasing gradient with Galactic longitude, with a peak at the position\nof the Galactic center. From IRAC color-magnitude and color-color diagrams, we\nconclude that most of the point sources in our catalog have IRAC magnitudes and\ncolors characteristic of red giant and AGB stars.", "cat": "astro-ph", "authors": ["Solange V. Ramirez", "Richard G. Arendt", "Kris Sellgren", "Susan R. Stolovy", "Angela Cotera", "Howard A. Smith", "Farhad Yusef-Zadeh"]}, "436": {"id": "1412.6733v1", "title": "Weather on Other Worlds. III. A Survey for T Dwarfs with High Amplitude Optical Variability", "url": "http://arxiv.org/pdf/1412.6733v1", "date": "2014-12-21 06:41:44", "abs": "We have monitored twelve T dwarfs with the Kitt Peak 2.1m telescope using an\nf814w filter (0.7-0.95 microns) to place in context the remarkable 10-20%\nvariability exhibited by the nearby T dwarf Luhman 16B in this wavelength\nregime. The motivation was the poorly known red optical behavior of T dwarfs,\nwhich have been monitored almost exclusively at infrared wavelengths, where\nvariability amplitudes greater than 10% have been found to be very rare. We\ndetect highly significant variability in two T dwarfs. The T2.5 dwarf 2MASS\n13243559+6358284 shows consistent ~17% variability on two consecutive nights.\nThe T2 dwarf 2MASS J16291840+0335371 exhibits ~10% variability that may evolve\nfrom night to night, similarly to Luhman 16B. Both objects were previously\nknown to be variable in the infrared, but with considerably lower amplitudes.\nWe also find evidence for variability in the T6 dwarf J162414.37+002915.6, but\nsince it has lower significance, we conservatively refrain from claiming this\nobject as a variable. We explore and rule out various telluric effects,\ndemonstrating that the variations we detect are astrophysically real. We\nsuggest that high-amplitude photometric variability for T dwarfs is likely more\ncommon in the red optical than at longer wavelengths. The two new members of\nthe growing class of high-amplitude variable T dwarfs offer excellent prospects\nfor further study of cloud structures and their evolution.", "cat": "astro-ph.SR", "authors": ["Aren N. Heinze", "Stanimir Metchev", "Kendra Kellogg"]}, "437": {"id": "2206.06089v3", "title": "Graph Neural Networks Intersect Probabilistic Graphical Models: A Survey", "url": "http://arxiv.org/pdf/2206.06089v3", "date": "2023-01-30 10:47:31", "abs": "Graphs are a powerful data structure to represent relational data and are\nwidely used to describe complex real-world data structures. Probabilistic\nGraphical Models (PGMs) have been well-developed in the past years to\nmathematically model real-world scenarios in compact graphical representations\nof distributions of variables. Graph Neural Networks (GNNs) are new inference\nmethods developed in recent years and are attracting growing attention due to\ntheir effectiveness and flexibility in solving inference and learning problems\nover graph-structured data. These two powerful approaches have different\nadvantages in capturing relations from observations and how they conduct\nmessage passing, and they can benefit each other in various tasks. In this\nsurvey, we broadly study the intersection of GNNs and PGMs. Specifically, we\nfirst discuss how GNNs can benefit from learning structured representations in\nPGMs, generate explainable predictions by PGMs, and how PGMs can infer object\nrelationships. Then we discuss how GNNs are implemented in PGMs for more\nefficient inference and structure learning. In the end, we summarize the\nbenchmark datasets used in recent studies and discuss promising future\ndirections.", "cat": "cs.AI", "authors": ["Chenqing Hua", "Sitao Luan", "Qian Zhang", "Jie Fu"]}, "438": {"id": "1606.00283v1", "title": "Synthetic data products for future HI galaxy surveys: a tool for characterising source confusion in spectral line stacking experiments", "url": "http://arxiv.org/pdf/1606.00283v1", "date": "2016-06-01 13:38:14", "abs": "Much of our current understanding of neutral, atomic gas in galaxies comes\nfrom radio observations of the nearby Universe. Until the next generation of\ninstruments allow us to push to much higher redshifts, we must rely mostly upon\ntheoretical models of galaxy formation to provide us with key insights into the\nlikely cosmic evolution of HI in the Universe, and its links to molecular\nclouds and star formation. In this work, we present a new set of methods to\nconvert mock galaxy catalogues into synthetic data cubes containing model\ngalaxies with realistic spatial and spectral HI distributions over large\ncosmological volumes. Such synthetic data products can be used to guide\nobserving and data handling/analysis strategies for forthcoming HI galaxy\nsurveys. As a demonstration of the potential use of our simulated products we\nuse them to conduct several mock HI stacking experiments for both low and\nhigh-redshift galaxy samples. The stacked spectra can be accurately decomposed\ninto contributions from target and non-target galaxies, revealing in all\nco-added spectra large fractions of contaminant mass due to source confusion.\nOur results are consistent with similar estimates extrapolated from z=0\nobservational data. The amount of confused mass in a stacked spectrum grows\nalmost linearly with the size of the observational beam, suggesting potential\nover-estimates of Omega_HI by some recent HI stacking experiments. Our\nsimulations will allow the study of subtle redshift-dependent effects in future\nstacking analyses.", "cat": "astro-ph.GA", "authors": ["E. C. Elson", "S. L. Blyth", "A. J. Baker"]}, "439": {"id": "1611.09511v1", "title": "Naming the Pain in Requirements Engineering: A Design for a Global Family of Surveys and First Results from Germany", "url": "http://arxiv.org/pdf/1611.09511v1", "date": "2016-11-29 06:51:02", "abs": "For many years, we have observed industry struggling in defining a high\nquality requirements engineering (RE) and researchers trying to understand\nindustrial expectations and problems. Although we are investigating the\ndiscipline with a plethora of empirical studies, they still do not allow for\nempirical generalisations. To lay an empirical and externally valid foundation\nabout the state of the practice in RE, we aim at a series of open and\nreproducible surveys that allow us to steer future research in a problem-driven\nmanner. We designed a globally distributed family of surveys in joint\ncollaborations with different researchers and completed the first run in\nGermany. The instrument is based on a theory in the form of a set of hypotheses\ninferred from our experiences and available studies. We test each hypothesis in\nour theory and identify further candidates to extend the theory by correlation\nand Grounded Theory analysis. In this article, we report on the design of the\nfamily of surveys, its underlying theory, and the full results obtained from\nGermany with participants from 58 companies. The results reveal, for example, a\ntendency to improve RE via internally defined qualitative methods rather than\nrelying on normative approaches like CMMI. We also discovered various RE\nproblems that are statistically significant in practice. For instance, we could\ncorroborate communication flaws or moving targets as problems in practice. Our\nresults are not yet fully representative but already give first insights into\ncurrent practices and problems in RE, and they allow us to draw lessons learnt\nfor future replications. Our results obtained from this first run in Germany\nmake us confident that the survey design and instrument are well-suited to be\nreplicated and, thereby, to create a generalisable empirical basis of RE in\npractice.", "cat": "cs.SE", "authors": ["D. M\u00e9ndez Fern\u00e1ndez", "S. Wagner"]}, "440": {"id": "2205.09425v2", "title": "NIR spectroscopic survey of protostellar jets in the star forming region IC 1396N", "url": "http://arxiv.org/pdf/2205.09425v2", "date": "2022-06-01 15:05:22", "abs": "Abridged. The bright-rimmed cloud IC1396N hosts CO, H$_2$, and Herbig-Haro\noutflows powered by millimetre compact sources. We aim to characterise the\nkinematics and physical conditions of the H$_2$ emission features spread over\nIC1396N, which appear as chains of knots with a jet-like morphology, tracing\ndifferent H$_2$ outflows, and to obtain further information about (and an\nidentification of) the driving sources. Low-resolution, long-slit near-infrared\nspectra were acquired with NICS at the TNG, using grisms KB (R~1200), HK and JH\n(R~500). Several slit pointings and PA were used throughout IC1396N to sample a\nnumber of the H$_2$ knots previously detected in deep H$_2$ 2.12 $\\mu$m images.\nThe knots exhibit rich ro-vibrational spectra of H$_2$, consistent with\nshock-excited excitation, from which radial velocities and relevant physical\nconditions of the IC1396N H$_2$ outflows were derived. These also allowed\nestimating extinction ranges towards several features. [FeII] emission was only\ndetected towards a few knots, which also display unusually large H$_2$ 1-0\nS(3)/S(1) flux ratios. The obtained radial velocities confirm that most of the\noutflows are close to the plane of the sky. Nearby knots in the same chain\noften display different radial velocities, both blue-shifted and red-shifted,\nwhich we interpret as due to ubiquitous jet precession in the driving sources\nor the development of oblique shocks. One of the chains (strand A) appears as a\nset of features trailing a leading bow-shock structure consistent with the\nresults of 3-D magneto-hydrodynamical models. Either side of the leading\nbow-shock (A15) exhibits a different radial velocity, whose possible\nexplanations are discussed in the paper. Our data cannot confirm whether\nstrands A and B have both been originated by the intermediate mass young\nstellar object BIMA 2.", "cat": "astro-ph.GA", "authors": ["Fabrizio Massi", "Rosario L\u00f3pez", "Maria T. Beltr\u00e1n", "Robert Estalella", "Josep M. Girart"]}, "441": {"id": "0910.5418v1", "title": "Photometric redshifts and cluster tomography in the ESO Distant Cluster Survey", "url": "http://arxiv.org/pdf/0910.5418v1", "date": "2009-10-28 16:30:36", "abs": "This paper reports the results obtained on the photometric redshifts\nmeasurement and accuracy, and cluster tomography in the ESO Distant Cluster\nSurvey (EDisCS) fields. Photometric redshifts were computed using two\nindependent codes (Hyperz and G. Rudnick's code). The accuracy of photometric\nredshifts was assessed by comparing our estimates with the spectroscopic\nredshifts of ~1400 galaxies in the 0.31). We apply this method on the fourth GES\ninternal data release and detect 354 SBn candidates (342 SB2, 11 SB3 and even\none SB4), including only 9 SB2 known in the literature. This implies that about\n98% of these SBn candidates are new (because of their faint visual magnitude\nthat can reach V=19). Visual inspection of the SBn candidate spectra reveals\nthat the most probable candidates have indeed a composite spectrum. Among SB2\ncandidates, an orbital solution could be computed for two previously unknown\nbinaries: 06404608+0949173 (known as V642 Mon) in NGC 2264 and 19013257-0027338\nin Berkeley 81. A detailed analysis of the unique SB4 (four peaks in the CCF)\nreveals that HD 74438 in the open cluster IC 2391 is a physically bound stellar\nquadruple system. The SB candidates belonging to stellar clusters are reviewed\nin detail to discard false detections. We warn against the use of atmospheric\nparameters for these system components rather than by SB-specific pipelines.\nOur implementation of an automatic detection of spectroscopic binaries within\nthe GES has allowed an efficient discovery of many new multiple systems.", "cat": "astro-ph.SR", "authors": ["T. Merle", "S. Van Eck", "A. Jorissen", "M. Van der Swaelmen", "T. Masseron", "T. Zwitter", "D. Hatzidimitriou", "A. Klutsch", "D. Pourbaix", "R. Blomme", "C. C. Worley", "G. Sacco", "J. Lewis", "C. Abia", "G. Traven", "R. Sordo", "A. Bragaglia", "R. Smiljanic", "E. Pancino", "F. Damiani", "A. Hourihane", "G. Gilmore", "S. Randich", "S. Koposov", "A. Casey", "L. Morbidelli", "E. Franciosini", "L. Magrini", "P. Jofre", "M. T. Costado", "R. D. Jeffries", "M. Bergemann", "A. C. Lanzafame", "A. Bayo", "G. Carraro", "E. Flaccomio", "L. Monaco", "S. Zaggia"]}, "458": {"id": "0909.2795v1", "title": "Data reduction strategy of the Effelsberg-Bonn HI Survey (EBHIS)", "url": "http://arxiv.org/pdf/0909.2795v1", "date": "2009-09-15 12:53:28", "abs": "Since autumn 2008 a new L-band 7-Feed-Array receiver is used for an HI 21-cm\nline survey performed with the 100-m Effelsberg telescope. The survey will\ncover the whole northern hemisphere comprising both, the galactic and\nextragalactic sky in parallel. Using state-of-the-art FPGA based digital Fast\nFourier Transform spectrometers, superior in dynamic range and temporal\nresolution, allows to apply sophisticated radio frequency interferences (RFI)\nmitigation schemes to the survey data.\n The EBHIS data reduction software includes the RFI mitigation, gain-curve\ncorrection, intensity calibration, stray-radiation correction, gridding, and\nsource detection. We discuss the severe degradation of radio astronomical HI\ndata by RFI signals and the gain in scientific yield when applying modern RFI\nmitigation schemes. For this aim simulations of the galaxy distribution within\nthe local volume (z<0.07) with and without RFI degradation were performed.\nThese simulations, allow us to investigate potential biases and selection\neffects introduced by the data reduction software and the applied source\nparametrization methods.", "cat": "astro-ph.IM", "authors": ["B. Winkel", "J. Kerp", "P. M. W. Kalberla"]}, "459": {"id": "1711.08675v1", "title": "Stellar parameters and H$\u03b1$ line profile variability of Be stars in the BeSOS survey", "url": "http://arxiv.org/pdf/1711.08675v1", "date": "2017-11-23 12:56:14", "abs": "The Be phenomenon is present in about 20$\\%$ of the B-type stars. Be stars\nshow variability on a broad range of timescales, which in most cases is related\nto the presence of a circumstellar disk of variable size and structure. For\nthis reason a time resolved survey is highly desirable in order to understand\nthe mechanisms of disk formation which are still poorly understood. In\naddition, a complete observational sample would improve the statistical\nsignificance of the study of the stellar and disk parameters. The \"Be Stars\nObservation Survey\" (BeSOS) is a survey containing reduced spectra obtained\nusing the echelle spectrograph PUCHEROS with a spectral resolution of 17000 in\nthe range of 4260-7300 $\\text{\\AA}$. BeSOS's main objective is to offer\nconsistent spectroscopic and time resolved data obtained with one instrument.\nThe user can download or plot the data and get the stellar parameters directly\nfrom the website. We also provide a star-by-star analysis based on photometric,\nspectroscopic and interferometric data as well as general information about the\nwhole BeSOS sample. Recently, BeSOS led to the discovery of a new Be star HD\n42167 and facilitated study of the V/R variation of HD 35165 and HD 120324, the\nsteady disk of HD 110335 and the Be shell status of HD 127972. Optical spectra\nused in this work, as well as the derived stellar parameters are available\nonline in \\url{http://besos.ifa.uv.cl}.", "cat": "astro-ph.SR", "authors": ["C. Arcos", "S. Kanaan", "J. Ch\u00e1vez", "L. Vanzi", "I. Araya", "M. Cur\u00e9"]}, "460": {"id": "1708.01537v2", "title": "Dark Energy Survey Year 1 Results: Galaxy-Galaxy Lensing", "url": "http://arxiv.org/pdf/1708.01537v2", "date": "2018-09-04 13:58:22", "abs": "We present galaxy-galaxy lensing measurements from 1321 sq. deg. of the Dark\nEnergy Survey (DES) Year 1 (Y1) data. The lens sample consists of a selection\nof 660,000 red galaxies with high-precision photometric redshifts, known as\nredMaGiC, split into five tomographic bins in the redshift range $0.15 < z <\n0.9$. We use two different source samples, obtained from the Metacalibration\n(26 million galaxies) and Im3shape (18 million galaxies) shear estimation\ncodes, which are split into four photometric redshift bins in the range $0.2 <\nz < 1.3$. We perform extensive testing of potential systematic effects that can\nbias the galaxy-galaxy lensing signal, including those from shear estimation,\nphotometric redshifts, and observational properties. Covariances are obtained\nfrom jackknife subsamples of the data and validated with a suite of log-normal\nsimulations. We use the shear-ratio geometric test to obtain independent\nconstraints on the mean of the source redshift distributions, providing\nvalidation of those obtained from other photo-$z$ studies with the same data.\nWe find consistency between the galaxy bias estimates obtained from our\ngalaxy-galaxy lensing measurements and from galaxy clustering, therefore\nshowing the galaxy-matter cross-correlation coefficient $r$ to be consistent\nwith one, measured over the scales used for the cosmological analysis. The\nresults in this work present one of the three two-point correlation functions,\nalong with galaxy clustering and cosmic shear, used in the DES cosmological\nanalysis of Y1 data, and hence the methodology and the systematics tests\npresented here provide a critical input for that study as well as for future\ncosmological analyses in DES and other photometric galaxy surveys.", "cat": "astro-ph.CO", "authors": ["J. Prat", "C. S\u00e1nchez", "Y. Fang", "D. Gruen", "J. Elvin-Poole", "N. Kokron", "L. F. Secco", "B. Jain", "R. Miquel", "N. MacCrann", "M. A. Troxel", "A. Alarcon", "D. Bacon", "G. M. Bernstein", "J. Blazek", "R. Cawthon", "C. Chang", "M. Crocce", "C. Davis", "J. De Vicente", "J. P. Dietrich", "A. Drlica-Wagner", "O. Friedrich", "M. Gatti", "W. G. Hartley", "B. Hoyle", "E. M. Huff", "M. Jarvis", "M. M. Rau", "R. P. Rollins", "A. J. Ross", "E. Rozo", "E. S. Rykoff", "S. Samuroff", "E. Sheldon", "T. N. Varga", "P. Vielzeuf", "J. Zuntz", "T. M. C. Abbott", "F. B. Abdalla", "S. Allam", "J. Annis", "K. Bechtol", "A. Benoit-L\u00e9vy", "E. Bertin", "D. Brooks", "E. Buckley-Geer", "D. L. Burke", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "F. J. Castander", "C. E. Cunha", "C. B. D'Andrea", "L. N. da Costa", "S. Desai", "H. T. Diehl", "S. Dodelson", "T. F. Eifler", "E. Fernandez", "B. Flaugher", "P. Fosalba", "J. Frieman", "J. Garc\u00eda-Bellido", "E. Gaztanaga", "D. W. Gerdes", "T. Giannantonio", "D. A. Goldstein", "R. A. Gruendl", "J. Gschwend", "G. Gutierrez", "K. Honscheid", "D. J. James", "T. Jeltema", "M. W. G. Johnson", "M. D. Johnson", "D. Kirk", "E. Krause", "K. Kuehn", "S. Kuhlmann", "O. Lahav", "T. S. Li", "M. Lima", "M. A. G. Maia", "M. March", "J. L. Marshall", "P. Martini", "P. Melchior", "F. Menanteau", "J. J. Mohr", "R. C. Nichol", "B. Nord", "A. A. Plazas", "A. K. Romer", "A. Roodman", "M. Sako", "E. Sanchez", "V. Scarpine", "R. Schindler", "M. Schubnell", "I. Sevilla-Noarbe", "M. Smith", "R. C. Smith", "M. Soares-Santos", "F. Sobreira", "E. Suchyta", "M. E. C. Swanson", "G. Tarle", "D. Thomas", "D. L. Tucker", "V. Vikram", "A. R. Walker", "R. H. Wechsler", "B. Yanny", "Y. Zhang"]}, "461": {"id": "1710.09900v1", "title": "A Spectroscopic Survey of the Fields of 28 Strong Gravitational Lenses: Implications for $H_0$", "url": "http://arxiv.org/pdf/1710.09900v1", "date": "2017-10-26 20:15:16", "abs": "Strong gravitational lensing provides an independent measurement of the\nHubble parameter ($H_0$). One remaining systematic is a bias from the\nadditional mass due to a galaxy group at the lens redshift or along the\nsightline. We quantify this bias for more than 20 strong lenses that have\nwell-sampled sightline mass distributions, focusing on the convergence $\\kappa$\nand shear $\\gamma$. In 23% of these fields, a lens group contributes a $\\ge$1%\nconvergence bias; in 57%, there is a similarly significant line-of-sight group.\nFor the nine time delay lens systems, $H_0$ is overestimated by 11$^{+3}_{-2}$%\non average when groups are ignored. In 67% of fields with total $\\kappa \\ge$\n0.01, line-of-sight groups contribute $\\gtrsim 2\\times$ more convergence than\ndo lens groups, indicating that the lens group is not the only important mass.\nLens environment affects the ratio of four (quad) to two (double) image\nsystems; all seven quads have lens groups while only three of 10 doubles do,\nand the highest convergences due to lens groups are in quads. We calibrate the\n$\\gamma$-$\\kappa$ relation: $\\log(\\kappa_{\\rm{tot}}) = (1.94 \\pm 0.34)\n\\log(\\gamma_{\\rm{tot}}) + (1.31 \\pm 0.49)$ with a rms scatter of 0.34 dex.\nShear, which, unlike convergence, can be measured directly from lensed images,\ncan be a poor predictor of $\\kappa$; for 19% of our fields, $\\kappa$ is\n$\\gtrsim 2\\gamma$. Thus, accurate cosmology using strong gravitational lenses\nrequires precise measurement and correction for all significant structures in\neach lens field.", "cat": "astro-ph.GA", "authors": ["Michelle L. Wilson", "Ann I. Zabludoff", "Charles R. Keeton", "Kenneth C. Wong", "Kurtis A. Williams", "K. Decker French", "Ivelina G. Momcheva"]}, "462": {"id": "2002.02473v2", "title": "A Novel Survey for Young Substellar Objects with the W-band filter II. The Coolest and Lowest Mass Members of the Serpens-South Star-forming Region", "url": "http://arxiv.org/pdf/2002.02473v2", "date": "2020-04-03 14:09:42", "abs": "Given its relative proximity (~430 pc), compact size (< 20'), young age (~\n0.5 Myr) and rich number of young stellar objects, the Serpens-South star\nforming region is a promising site for studying young sub-stellar objects, yet\nthe low-mass members of this region remain largely undiscovered. In this paper\nwe report on a deep photometric survey using a custom 1.45 um filter (W-band),\nas well as standard J and H near-IR filters, in order to identify candidate\nlow-mass young brown-dwarfs in the Serpens-South region. We constructed a\nreddening-insensitive index (Q) by combining J, H and W-band photometry for\nsurvey objects, in order to identify candidate low-mass members of Serpens\nbased on the strength of the water absorption feature at 1.45 um in the\natmospheres of mid-M and later objects. We then conducted spectroscopic follow\nup to confirm youth and spectral type for our candidates. This is the first\nsurvey to identify the very low-mass and coolest members of Serpens-South. We\nidentify 4 low-mass candidate Serpens members, which all display IR excess\nemission, indicating the likely presence of circumstellar disks around them.\nOne of the four candidate low-mass members in our list, SERP182918-020245,\nexhibits Pa_beta and Br_gamma emission features, confirming its youth and\nongoing magnetospheric accretion. Our new candidate members have spectral types\n>M4 and are the coolest and lowest mass candidate members yet identified in\nSerpens-South.", "cat": "astro-ph.SR", "authors": ["Jessy Jose", "Beth A. Biller", "Lo\u0131c Albert", "Sophie Dubber", "Katelyn Allers", "Gregory J. Herczeg", "Michael C. Liu", "Samuel Pearson", "Bhavana Lalchand", "Wen-Ping Chen", "Mickael Bonnefoy", "Etienne Artigau", "Philippe Delorme", "Po-shih Chiang", "Zhoujian Zhang", "Yumiko Oasa"]}, "463": {"id": "2308.15501v1", "title": "The AIMS Site Survey", "url": "http://arxiv.org/pdf/2308.15501v1", "date": "2023-08-29 09:34:53", "abs": "This paper reports site survey results for the Infrared System for the\nAccurate Measurement of Solar Magnetic Field, especially in Saishiteng\nMountain, Qinghai, China. Since 2017, we have installed weather station,\nspectrometer for precipitable water vapor (PWV) and S-DIMM and carried out\nobservation on weather elements, precipitable water vapor and daytime seeing\ncondition for more than one year in almost all candidates. At Mt. Saishiteng,\nthe median value of daytime precipitable water vapor is 5.25 mm and its median\nvalue in winter season is 2.1 mm. The median value of Fried parameter of\ndaytime seeing observation at Saishiteng Mountain is 3.42 cm. Its solar direct\nradiation data shows that solar average observable time is 446 minutes per day\nand premium time is 401 minutes per day in August 2019.", "cat": "astro-ph.IM", "authors": ["Xingming Bao", "Jian Wang", "Shuai Jing", "Yuanyong Deng", "Dongguang Wang"]}, "464": {"id": "2001.11231v1", "title": "Survey of Deep Reinforcement Learning for Motion Planning of Autonomous Vehicles", "url": "http://arxiv.org/pdf/2001.11231v1", "date": "2020-01-30 09:47:22", "abs": "Academic research in the field of autonomous vehicles has reached high\npopularity in recent years related to several topics as sensor technologies,\nV2X communications, safety, security, decision making, control, and even legal\nand standardization rules. Besides classic control design approaches,\nArtificial Intelligence and Machine Learning methods are present in almost all\nof these fields. Another part of research focuses on different layers of Motion\nPlanning, such as strategic decisions, trajectory planning, and control. A wide\nrange of techniques in Machine Learning itself have been developed, and this\narticle describes one of these fields, Deep Reinforcement Learning (DRL). The\npaper provides insight into the hierarchical motion planning problem and\ndescribes the basics of DRL. The main elements of designing such a system are\nthe modeling of the environment, the modeling abstractions, the description of\nthe state and the perception models, the appropriate rewarding, and the\nrealization of the underlying neural network. The paper describes vehicle\nmodels, simulation possibilities and computational requirements. Strategic\ndecisions on different layers and the observation models, e.g., continuous and\ndiscrete state representations, grid-based, and camera-based solutions are\npresented. The paper surveys the state-of-art solutions systematized by the\ndifferent tasks and levels of autonomous driving, such as car-following,\nlane-keeping, trajectory following, merging, or driving in dense traffic.\nFinally, open questions and future challenges are discussed.", "cat": "cs.LG", "authors": ["Szil\u00e1rd Aradi"]}, "465": {"id": "2404.13244v1", "title": "Intelligent Agents for Auction-based Federated Learning: A Survey", "url": "http://arxiv.org/pdf/2404.13244v1", "date": "2024-04-20 03:05:25", "abs": "Auction-based federated learning (AFL) is an important emerging category of\nFL incentive mechanism design, due to its ability to fairly and efficiently\nmotivate high-quality data owners to join data consumers' (i.e., servers') FL\ntraining tasks. To enhance the efficiency in AFL decision support for\nstakeholders (i.e., data consumers, data owners, and the auctioneer),\nintelligent agent-based techniques have emerged. However, due to the highly\ninterdisciplinary nature of this field and the lack of a comprehensive survey\nproviding an accessible perspective, it is a challenge for researchers to enter\nand contribute to this field. This paper bridges this important gap by\nproviding a first-of-its-kind survey on the Intelligent Agents for AFL (IA-AFL)\nliterature. We propose a unique multi-tiered taxonomy that organises existing\nIA-AFL works according to 1) the stakeholders served, 2) the auction mechanism\nadopted, and 3) the goals of the agents, to provide readers with a\nmulti-perspective view into this field. In addition, we analyse the limitations\nof existing approaches, summarise the commonly adopted performance evaluation\nmetrics, and discuss promising future directions leading towards effective and\nefficient stakeholder-oriented decision support in IA-AFL ecosystems.", "cat": "cs.LG", "authors": ["Xiaoli Tang", "Han Yu", "Xiaoxiao Li", "Sarit Kraus"]}, "466": {"id": "2004.11138v3", "title": "The Creation and Detection of Deepfakes: A Survey", "url": "http://arxiv.org/pdf/2004.11138v3", "date": "2020-09-13 22:44:33", "abs": "Generative deep learning algorithms have progressed to a point where it is\ndifficult to tell the difference between what is real and what is fake. In\n2018, it was discovered how easy it is to use this technology for unethical and\nmalicious applications, such as the spread of misinformation, impersonation of\npolitical leaders, and the defamation of innocent individuals. Since then,\nthese `deepfakes' have advanced significantly.\n In this paper, we explore the creation and detection of deepfakes and provide\nan in-depth view of how these architectures work. The purpose of this survey is\nto provide the reader with a deeper understanding of (1) how deepfakes are\ncreated and detected, (2) the current trends and advancements in this domain,\n(3) the shortcomings of the current defense solutions, and (4) the areas which\nrequire further research and attention.", "cat": "cs.CV", "authors": ["Yisroel Mirsky", "Wenke Lee"]}, "467": {"id": "1110.0005v1", "title": "Unsupervised self-organised mapping: a versatile empirical tool for object selection, classification and redshift estimation in large surveys", "url": "http://arxiv.org/pdf/1110.0005v1", "date": "2011-09-30 20:01:49", "abs": "We present an application of unsupervised machine learning - the\nself-organised map (SOM) - as a tool for visualising, exploring and mining the\ncatalogues of large astronomical surveys. Self-organisation culminates in a\nlow-resolution representation of the 'topology' of a parameter volume, and this\ncan be exploited in various ways pertinent to astronomy. Using data from the\nCosmological Evolution Survey (COSMOS), we demonstrate two key astronomical\napplications of the SOM: (i) object classification and selection, using the\nexample of galaxies with active galactic nuclei as a demonstration, and (ii)\nphotometric redshift estimation, illustrating how SOMs can be used as totally\nempirical predictive tools. With a training set of ~3800 galaxies with\nz_spec<1, we achieve photometric redshift accuracies competitive with other\n(mainly template fitting) techniques that use a similar number of photometric\nbands (sigma(Dz)=0.03 with a ~2% outlier rate when using u*-band to 8um\nphotometry). We also test the SOM as a photo-z tool using the PHoto-z Accuracy\nTesting (PHAT) synthetic catalogue of Hildebrandt et al. (2010), which compares\nseveral different photo-z codes using a common input/training set. We find that\nthe SOM can deliver accuracies that are competitive with many of the\nestablished template-fitting and empirical methods. This technique is not\nwithout clear limitations, which are discussed, but we suggest it could be a\npowerful tool in the era of extremely large - 'petabyte' - databases where\nefficient data-mining is a paramount concern.", "cat": "astro-ph.IM", "authors": ["James E. Geach"]}, "468": {"id": "2401.01313v3", "title": "A Comprehensive Survey of Hallucination Mitigation Techniques in Large Language Models", "url": "http://arxiv.org/pdf/2401.01313v3", "date": "2024-01-08 16:19:17", "abs": "As Large Language Models (LLMs) continue to advance in their ability to write\nhuman-like text, a key challenge remains around their tendency to hallucinate\ngenerating content that appears factual but is ungrounded. This issue of\nhallucination is arguably the biggest hindrance to safely deploying these\npowerful LLMs into real-world production systems that impact people's lives.\nThe journey toward widespread adoption of LLMs in practical settings heavily\nrelies on addressing and mitigating hallucinations. Unlike traditional AI\nsystems focused on limited tasks, LLMs have been exposed to vast amounts of\nonline text data during training. While this allows them to display impressive\nlanguage fluency, it also means they are capable of extrapolating information\nfrom the biases in training data, misinterpreting ambiguous prompts, or\nmodifying the information to align superficially with the input. This becomes\nhugely alarming when we rely on language generation capabilities for sensitive\napplications, such as summarizing medical records, financial analysis reports,\netc. This paper presents a comprehensive survey of over 32 techniques developed\nto mitigate hallucination in LLMs. Notable among these are Retrieval Augmented\nGeneration (Lewis et al, 2021), Knowledge Retrieval (Varshney et al,2023),\nCoNLI (Lei et al, 2023), and CoVe (Dhuliawala et al, 2023). Furthermore, we\nintroduce a detailed taxonomy categorizing these methods based on various\nparameters, such as dataset utilization, common tasks, feedback mechanisms, and\nretriever types. This classification helps distinguish the diverse approaches\nspecifically designed to tackle hallucination issues in LLMs. Additionally, we\nanalyze the challenges and limitations inherent in these techniques, providing\na solid foundation for future research in addressing hallucinations and related\nphenomena within the realm of LLMs.", "cat": "cs.CL", "authors": ["S. M Towhidul Islam Tonmoy", "S M Mehedi Zaman", "Vinija Jain", "Anku Rani", "Vipula Rawte", "Aman Chadha", "Amitava Das"]}, "469": {"id": "2011.00183v1", "title": "The CARMA-NRO Orion Survey: Filament Formation via Collision-Induced Magnetic Reconnection -- The Stick in Orion A", "url": "http://arxiv.org/pdf/2011.00183v1", "date": "2020-10-31 04:23:30", "abs": "A unique filament is identified in the {\\it Herschel} maps of the Orion A\ngiant molecular cloud. The filament, which, we name the Stick, is\nruler-straight and at an early evolutionary stage. Transverse position-velocity\ndiagrams show two velocity components closing in on the Stick. The filament\nshows consecutive rings/forks in C$^{18}$O(1-0) channel maps, which is\nreminiscent of structures generated by magnetic reconnection. We propose that\nthe Stick formed via collision-induced magnetic reconnection (CMR). We use the\nmagnetohydrodynamics (MHD) code Athena++ to simulate the collision between two\ndiffuse molecular clumps, each carrying an anti-parallel magnetic field. The\nclump collision produces a narrow, straight, dense filament with a factor of\n$>$200 increase in density. The production of the dense gas is seven times\nfaster than free-fall collapse. The dense filament shows ring/fork-like\nstructures in radiative transfer maps. Cores in the filament are confined by\nsurface magnetic pressure. CMR can be an important dense-gas-producing\nmechanism in the Galaxy and beyond.", "cat": "astro-ph.GA", "authors": ["Shuo Kong", "Volker Ossenkopf-Okada", "H\u00e9ctor G. Arce", "John Bally", "\u00c1lvaro S\u00e1nchez-Monge", "Peregrine McGehee", "S\u00fcmeyye Suri", "Ralf S. Klessen", "John M. Carpenter", "Dariusz C. Lis", "Fumitaka Nakamura", "Peter Schilke", "Rowan J. Smith", "Steve Mairs", "Alyssa Goodman", "Mar\u00eda Jos\u00e9 Maureira"]}, "470": {"id": "0705.2906v1", "title": "Investigating high-mass star formation through maser surveys", "url": "http://arxiv.org/pdf/0705.2906v1", "date": "2007-05-21 02:36:14", "abs": "Interstellar masers are unique probes of the environments in which they\narise. In studies of high-mass star formation their primary function has been\nas signposts of these regions and they have been used as probes of the\nkinematics and physical conditions in only a few sources. With a few notable\nexceptions, we know relatively little about the evolutionary phase the\ndifferent maser species trace, nor their location with respect to other star\nformation tracers. While detailed studies of a small number of maser regions\ncan reveal much about them, other information can only be obtained through\nlarge, systematic searches. In particular, such surveys are vital in efforts to\ndetermine an evolutionary sequence for the common maser species, and there is\ngrowing evidence that methanol masers may trace an earlier phase than the other\ncommon maser species of OH and water.", "cat": "astro-ph", "authors": ["S. P. Ellingsen", "M. A. Voronkov", "D. M. Cragg", "A. M. Sobolev", "S. L. Breen", "P. D. Godfrey"]}, "471": {"id": "1502.03020v1", "title": "GLACE survey: OSIRIS/GTC Tuneable Filter H$\u03b1$ imaging of the rich galaxy cluster ZwCl 0024.0+1652 at z = 0.395. Part I -- Survey presentation, TF data reduction techniques and catalogue", "url": "http://arxiv.org/pdf/1502.03020v1", "date": "2015-02-10 18:01:07", "abs": "The cores of clusters at 0 $\\lesssim$ z $\\lesssim$ 1 are dominated by\nquiescent early-type galaxies, whereas the field is dominated by star-forming\nlate-type ones. Galaxy properties, notably the star formation (SF) ability, are\naltered as they fall into overdense regions. The critical issues to understand\nthis evolution are how the truncation of SF is connected to the morphological\ntransformation and the responsible physical mechanism. The GaLAxy Cluster\nEvolution Survey (GLACE) is conducting a study on the variation of galaxy\nproperties (SF, AGN, morphology) as a function of environment in a\nrepresentative sample of clusters. A deep survey of emission line galaxies\n(ELG) is being performed, mapping a set of optical lines ([OII], [OIII],\nH$\\beta$ and H$\\alpha$/[NII]) in several clusters at z $\\sim$ 0.40, 0.63 and\n0.86. Using the Tunable Filters (TF) of OSIRIS/GTC, GLACE applies the technique\nof TF tomography: for each line, a set of images at different wavelengths are\ntaken through the TF, to cover a rest frame velocity range of several thousands\nkm/s. The first GLACE results target the H$\\alpha$/[NII] lines in the cluster\nZwCl 0024.0+1652 at z = 0.395 covering $\\sim$ 2 $\\times$ r$_{vir}$. We discuss\nthe techniques devised to process the TF tomography observations to generate\nthe catalogue of H$\\alpha$ emitters of 174 unique cluster sources down to a SFR\nbelow 1 M$_{\\odot}$/yr. The AGN population is discriminated using different\ndiagnostics and found to be $\\sim$ 37% of the ELG population. The median SFR is\n1.4 M$_{\\odot}$/yr. We have studied the spatial distribution of ELG, confirming\nthe existence of two components in the redshift space. Finally, we have\nexploited the outstanding spectral resolution of the TF to estimate the cluster\nmass from ELG dynamics, finding M$_{200}$ = 4.1 $\\times$ 10$^{14}$ M$_{\\odot}\nh^{-1}$, in agreement with previous weak-lensing estimates.", "cat": "astro-ph.GA", "authors": ["Miguel S\u00e1nchez-Portal", "Irene Pintos-Castro", "Ricardo P\u00e9rez-Mart\u00ednez", "Jordi Cepa", "Ana M. P\u00e9rez Garc\u00eda", "Helena Dom\u00ednguez-S\u00e1nchez", "\u00c1ngel Bongiovanni", "Ana L. Serra", "Emilio Alfaro", "Bruno Altieri", "Alfonso Arag\u00f3n-Salamanca", "Chantal Balkowski", "Andrea Biviano", "Malcom Bremer", "Francisco Castander", "H\u00e9ctor Casta\u00f1eda", "Nieves Castro-Rodr\u00edguez", "Ana L. Chies-Santos", "Daniela Coia", "Antonaldo Diaferio", "Pierre-Alain Duc", "Alessandro Ederoclite", "James Geach", "Ignacio Gonz\u00e1lez-Serrano", "Chris. P. Haines", "Brian McBreen", "Leo Metcalfe", "Iv\u00e1n Oteo", "Ismael P\u00e9rez-Fourn\u00f3n", "Bianca Poggianti", "Jana Polednikova", "Marina Ram\u00f3n-P\u00e9rez", "Jos\u00e9 M. Rodr\u00edguez-Espinosa", "Joana S. Santos", "Ian Smail", "Graham P. Smith", "Sonia Temporin", "Ivan Valtchanov"]}, "472": {"id": "1005.5570v1", "title": "The Sloan Digital Sky Survey Quasar Lens Search. IV. Statistical Lens Sample from the Fifth Data Release", "url": "http://arxiv.org/pdf/1005.5570v1", "date": "2010-05-31 00:43:02", "abs": "We present the second report of our systematic search for strongly lensed\nquasars from the data of the Sloan Digital Sky Survey (SDSS). From extensive\nfollow-up observations of 136 candidate objects, we find 36 lenses in the full\nsample of 77,429 spectroscopically confirmed quasars in the SDSS Data Release\n5. We then define a complete sample of 19 lenses, including 11 from our\nprevious search in the SDSS Data Release 3, from the sample of 36,287 quasars\nwith i<19.1 in the redshift range 0.6 0.2 mag of ~ 8.0,\n7.7, and 1.8 deg^-2 for quasars, AGNs, and RR Lyrae stars, respectively. We\nalso calculate a surface density rate in the UV for transient sources, using\nthe effective survey time at the cadence appropriate to each class, of ~ 15 and\n52 deg^-2 yr^-1 for M dwarfs and extragalactic transients, respectively.\n(Abridged.)", "cat": "astro-ph.CO", "authors": ["S. Gezari", "D. C. Martin", "K. Forster", "J. D. Neill", "M. Huber", "T. Heckman", "L. Bianchi", "P. Morrissey", "S. G. Neff", "M. Seibert", "D. Schiminovich", "T. K. Wyder", "W. S. Burgett", "K. C. Chambers", "N. Kaiser", "E. A. Magnier", "P. A. Price", "J. L. Tonry"]}, "483": {"id": "0812.0163v1", "title": "The UKIDSS-2MASS Proper Motion Survey I: Ultracool dwarfs from UKIDSS DR4", "url": "http://arxiv.org/pdf/0812.0163v1", "date": "2008-11-30 19:10:07", "abs": "The UKIRT Infrared Deep Sky Survey (UKIDSS) is the first of a new generation\nof infrared surveys. Here we combine the data from two UKIDSS components, the\nLarge Area Survey (LAS) and the Galactic Cluster Survey (GCS), with 2MASS data\nto produce an infrared proper motion survey for low mass stars and brown\ndwarfs. In total we detect 267 low mass stars and brown dwarfs with significant\nproper motions. We recover all ten known single L dwarfs and the one known T\ndwarf above the 2MASS detection limit in our LAS survey area and identify eight\nadditional new candidate L dwarfs. We also find one new candidate L dwarf in\nour GCS sample. Our sample also contains objects from eleven potential common\nproper motion binaries. Finally we test our proper motions and find that while\nthe LAS objects have proper motions consistent with absolute proper motions,\nthe GCS stars may have proper motions which are significantly under-estimated.\nThis is due possibly to the bulk motion of some of the local astrometric\nreference stars used in the proper motion determination.", "cat": "astro-ph", "authors": ["N. R. Deacon", "N. C. Hambly", "R. R. King", "M. J. McCaughrean"]}, "484": {"id": "1412.3254v2", "title": "A survey on structural Ramsey theory and topological dynamics with the Kechris-Pestov-Todorcevic correspondence in mind", "url": "http://arxiv.org/pdf/1412.3254v2", "date": "2014-12-12 10:34:25", "abs": "In 2005, Kechris, Pestov and Todorcevic established a surprising\ncorrespondence between structural Ramsey theory and topological dynamics. As an\nimmediate consequence, it triggered a new interest for structural Ramsey\ntheory. The purpose of the present paper is to present a self-contained survey\nof the corresponding developments.", "cat": "math.CO", "authors": ["Lionel Nguyen Van Th\u00e9"]}, "485": {"id": "1610.04577v1", "title": "A Survey on Various Data Mining Techniques for ECG Meta Analysis", "url": "http://arxiv.org/pdf/1610.04577v1", "date": "2016-04-22 11:41:23", "abs": "Data Mining is the process of examining the information from different point\nof view and compressing it for the relevant data. This data can also be\nutilized to build the incomes. Data Mining is also known as Data or Knowledge\nDiscovery. The basic purpose of data mining is to search patterns which have\nminimal user inputs and efforts. Data Mining plays a very crucial role in the\nvarious fields. There are various data mining procedures which can be connected\nin different fields of innovation. By using data mining techniques, it is\nobserved that less time is taken for the prediction of any disease with more\naccuracy. In this paper we would review various data mining techniques which\nare categorized under classification, regression and clustering and apply these\nalgorithms over an ECG dataset. The purpose of this work is to determine the\nmost suitable data mining technique and use it to improve the accuracy of\nanalyzing ECG data for better decision making.", "cat": "cs.DB", "authors": ["Kratika Tyagi", "Prof. Sanjeev Thakur"]}, "486": {"id": "1505.04106v1", "title": "Fourier analysis of multi-tracer cosmological surveys", "url": "http://arxiv.org/pdf/1505.04106v1", "date": "2015-05-15 16:15:42", "abs": "We present optimal quadratic estimators for the Fourier analysis of\ncosmological surveys that detect several different types of tracers of\nlarge-scale structure. Our estimators can be used to simultaneously fit the\nmatter power spectrum and the biases of the tracers - as well as redshift-space\ndistortions (RSDs), non-Gaussianities (NGs), or any other effects that are\nmanifested through differences between the clusterings of distinct species of\ntracers. Our estimators reduce to the one by Feldman, Kaiser & Peacock (ApJ\n1994, FKP) in the case of a survey consisting of a single species of tracer. We\nshow that the multi-tracer estimators are unbiased, and that their covariance\nis given by the inverse of the multi-tracer Fisher matrix (Abramo, MNRAS 2013;\nAbramo & Leonard, MNRAS 2013). When the biases, RSDs and NGs are fixed to their\nfiducial values, and one is only interested in measuring the underlying power\nspectrum, our estimators are projected into the estimator found by Percival,\nVerde & Peacock (MNRAS 2003). We have tested our estimators on simple\n(lognormal) simulated galaxy maps, and we show that it performs as expected,\nbeing either equivalent or superior to the FKP method in all cases we analyzed.\nFinally, we have shown how to extend the multi-tracer technique to include the\n1-halo term of the power spectrum.", "cat": "astro-ph.CO", "authors": ["L. Raul Abramo", "Lucas F. Secco", "Arthur Loureiro"]}, "487": {"id": "2011.06731v1", "title": "The JCMT BISTRO survey: alignment between outflows and magnetic fields in dense cores/clumps", "url": "http://arxiv.org/pdf/2011.06731v1", "date": "2020-11-13 02:45:24", "abs": "We compare the directions of molecular outflows of 62 low-mass Class 0 and I\nprotostars in nearby (<450 pc) star-forming regions with the mean orientations\nof the magnetic fields on 0.05-0.5 pc scales in the dense cores/clumps where\nthey are embedded. The magnetic field orientations were measured using the JCMT\nPOL-2 data taken by the BISTRO-1 survey and from the archive. The outflow\ndirections were observed with interferometers in the literature. The observed\ndistribution of the angles between the outflows and the magnetic fields peaks\nbetween 15 and 35 degrees. After considering projection effects, our results\ncould suggest that the outflows tend to be misaligned with the magnetic fields\nby 50+/-15 degrees in three-dimensional space and are less likely (but not\nruled out) randomly oriented with respect to the magnetic fields. There is no\ncorrelation between the misalignment and the bolometric temperatures in our\nsample. In several sources, the small-scale (1000-3000 au) magnetic fields is\nmore misaligned with the outflows than their large-scale magnetic fields,\nsuggesting that the small-scale magnetic field has been twisted by the\ndynamics. In comparison with turbulent MHD simulations of core formation, our\nobservational results are more consistent with models in which the energy\ndensities in the magnetic field and the turbulence of the gas are comparable.\nOur results also suggest that the misalignment alone cannot sufficiently reduce\nthe efficiency of magnetic braking to enable formation of the observed number\nof large Keplerian disks with sizes larger than 30-50 au.", "cat": "astro-ph.GA", "authors": ["Hsi-Wei Yen", "Patrick M. Koch", "Charles L. H. Hull", "Derek Ward-Thompson", "Pierre Bastien", "Tetsuo Hasegawa", "Woojin Kwon", "Shih-Ping Lai", "Keping Qiu", "Tao-Chung Ching", "Eun Jung Chung", "Simon Coude", "James Di Francesco", "Pham Ngoc Diep", "Yasuo Doi", "Chakali Eswaraiah", "Sam Falle", "Gary Fuller", "Ray S. Furuya", "Ilseung Han", "Jennifer Hatchell", "Martin Houde", "Shu-ichiro Inutsuka", "Doug Johnstone", "Ji-hyun Kang", "Miju Kang", "Kee-Tae Kim", "Florian Kirchschlager", "Jungmi Kwon", "Chang Won Lee", "Chin-Fei Lee", "Hong-Li Liu", "Tie Liu", "A-Ran Lyo", "Nagayoshi Ohashi", "Takashi Onaka", "Kate Pattle", "Sarah Sadavoy", "Hiro Saito", "Hiroko Shinnaga", "Archana Soam", "Mehrnoosh Tahani", "Motohide Tamura", "Ya-Wen Tang", "Xindi Tang", "Chuan-Peng Zhang"]}, "488": {"id": "2210.10805v1", "title": "TFAW survey II: 6 Newly Validated Planets and 13 Planet Candidates from K2", "url": "http://arxiv.org/pdf/2210.10805v1", "date": "2022-10-19 18:00:08", "abs": "Searching for Earth-sized planets in data from Kepler's extended mission (K2)\nis a niche that still remains to be fully exploited. The TFAW survey is an\nongoing project that aims to re-analyze all light curves in K2 C1-C8 and\nC12-C18 campaigns with a wavelet-based detrending and denoising method, and the\nperiod search algorithm TLS to search for new transit candidates not detected\nin previous works. We have analyzed a first subset of 24 candidate planetary\nsystems around relatively faint host stars (10.9 < $K_{p}$ < 15.4) to allow for\nfollow-up speckle imaging observations. Using VESPA and TRICERATOPS, we\nstatistically validate six candidates orbiting four unique host stars by\nobtaining false-positive probabilities smaller than 1% with both methods. We\nalso present 13 vetted planet candidates that might benefit from other, more\nprecise follow-up observations. All of these planets are sub-Neptune-sized,\nwith two validated planets and three candidates with sub-Earth sizes, and have\norbital periods between 0.81 and 23.98 days. Some interesting systems include\ntwo ultra-short-period planets, three multi-planetary systems, three\nsub-Neptunes that appear to be within the small planet Radius Gap, and two\nvalidated and one candidate sub-Earths (EPIC 210706310, EPIC 210768568, and\nEPIC 246078343) orbiting metal-poor stars.", "cat": "astro-ph.EP", "authors": ["D. del Ser", "O. Fors", "M. del Alc\u00e1zar", "V. Dyachenko", "E. P. Horch", "A. Tokovinin", "C. Ziegler", "G. T. van Belle", "C. A. Clark", "Z. D. Hartman"]}, "489": {"id": "2201.08071v3", "title": "Temporal Sentence Grounding in Videos: A Survey and Future Directions", "url": "http://arxiv.org/pdf/2201.08071v3", "date": "2023-03-13 13:55:30", "abs": "Temporal sentence grounding in videos (TSGV), \\aka natural language video\nlocalization (NLVL) or video moment retrieval (VMR), aims to retrieve a\ntemporal moment that semantically corresponds to a language query from an\nuntrimmed video. Connecting computer vision and natural language, TSGV has\ndrawn significant attention from researchers in both communities. This survey\nattempts to provide a summary of fundamental concepts in TSGV and current\nresearch status, as well as future research directions. As the background, we\npresent a common structure of functional components in TSGV, in a tutorial\nstyle: from feature extraction from raw video and language query, to answer\nprediction of the target moment. Then we review the techniques for multimodal\nunderstanding and interaction, which is the key focus of TSGV for effective\nalignment between the two modalities. We construct a taxonomy of TSGV\ntechniques and elaborate the methods in different categories with their\nstrengths and weaknesses. Lastly, we discuss issues with the current TSGV\nresearch and share our insights about promising research directions.", "cat": "cs.CV", "authors": ["Hao Zhang", "Aixin Sun", "Wei Jing", "Joey Tianyi Zhou"]}, "490": {"id": "2007.14989v2", "title": "Analytic marginalization of $N(z)$ uncertainties in tomographic galaxy surveys", "url": "http://arxiv.org/pdf/2007.14989v2", "date": "2020-09-24 08:49:50", "abs": "We present a new method to marginalize over uncertainties in redshift\ndistributions, $N(z)$, within tomographic cosmological analyses applicable to\ncurrent and upcoming photometric galaxy surveys. We allow for arbitrary\ndeviations from the best-guess $N(z)$ governed by a general covariance matrix\ndescribing the uncertainty in our knowledge of redshift distributions. In\nprinciple, this is marginalization over hundreds or thousands of new parameters\ndescribing potential deviations as a function of redshift and tomographic bin.\nHowever, by linearly expanding the theory predictions around a fiducial model,\nthis marginalization can be performed analytically, resulting in a modified\ndata covariance matrix that effectively downweights the modes of the data\nvector that are more sensitive to redshift distribution variations. We showcase\nthis method by applying it to the galaxy clustering measurements from the Hyper\nSuprime-Cam first data release. We illustrate how to marginalize over\nsample-variance of the calibration sample and a large general systematic\nuncertainty in photometric estimation methods, and explore the impact of priors\nimposing smoothness in the redshift distributions.", "cat": "astro-ph.CO", "authors": ["Boryana Hadzhiyska", "David Alonso", "Andrina Nicola", "An\u017ee Slosar"]}, "491": {"id": "2307.11882v1", "title": "Astrometry and Photometry for $\\approx$1000 L, T, and Y Dwarfs from the UKIRT Hemisphere Survey", "url": "http://arxiv.org/pdf/2307.11882v1", "date": "2023-07-21 19:43:57", "abs": "We present positions, proper motions, and near-infrared photometry for 966\nknown objects with spectral types later than M observed as part of the the\nUKIRT Hemisphere Survey (UHS). We augment the photometry and astrometry from\nUHS with information from Gaia DR3, Pan-STARRS DR2, and CatWISE 2020 to produce\na database of homogeneous photometry and astrometry for this sample. The\nmulti-epoch survey strategy of UHS allows us to determine proper motions for\nmost sources, with a median proper motion uncertainty of $\\sim$3.6 mas\nyr$^{-1}$. Our UHS proper motion measurements are generally in good agreement\nwith those from Gaia DR3, Pan-STARRS, and CatWISE 2020, with UHS proper motions\ntypically more precise than those from CatWISE 2020 and Pan-STARRS but not Gaia\nDR3. We critically analyze publicly available spectra for 406 members of this\nsample and provide updated near-infrared spectral types for $\\sim$100 objects.\nWe determine typical colors as a function of spectral type and provide absolute\nmagnitude vs. spectral type relations for UHS $J$- and $K$-band photometry.\nUsing newly determined proper motions, we highlight several objects of\ninterest, such as objects with large tangential velocities, widely separated\nco-moving companions, and potential members of young nearby associations.", "cat": "astro-ph.SR", "authors": ["Adam C. Schneider", "Jeffrey A. Munn", "Frederick J. Vrba", "Justice Bruursema", "Scott E. Dahm", "Stephen J. Williams", "Michael C. Liu", "Bryan N. Dorland"]}, "492": {"id": "0708.1227v1", "title": "H-alpha Survey of the Local Volume: Isolated Southern Galaxies", "url": "http://arxiv.org/pdf/0708.1227v1", "date": "2007-08-09 10:11:59", "abs": "We present our H-alpha observations of 11 isolated southern galaxies: SDIG,\nPGC 51659, E 222-010, E 272-025, E 137-018, IC 4662, Sag DIG, IC 5052, IC 5152,\nUGCA 438, and E149-003, with distances from 1 to 7 Mpc. We have determined the\ntotal H-alpha fluxes from these galaxies. The star formation rates in these\ngalaxies range from 10^{-1} (IC 4662) to 10^{-4}_{\\odot}/yr (SDIG) and the gas\ndepletion time at the observed star formation rates lies within the range from\n1/6 to 24 Hubble times H_0^{-1} .", "cat": "astro-ph", "authors": ["S. S. Kaisin", "A. V. Kasparova", "A. Yu. Knyazev", "I. D. Karachentsev"]}, "493": {"id": "2304.09805v1", "title": "A Survey of Corpora for Germanic Low-Resource Languages and Dialects", "url": "http://arxiv.org/pdf/2304.09805v1", "date": "2023-04-19 16:45:16", "abs": "Despite much progress in recent years, the vast majority of work in natural\nlanguage processing (NLP) is on standard languages with many speakers. In this\nwork, we instead focus on low-resource languages and in particular\nnon-standardized low-resource languages. Even within branches of major language\nfamilies, often considered well-researched, little is known about the extent\nand type of available resources and what the major NLP challenges are for these\nlanguage varieties. The first step to address this situation is a systematic\nsurvey of available corpora (most importantly, annotated corpora, which are\nparticularly valuable for NLP research). Focusing on Germanic low-resource\nlanguage varieties, we provide such a survey in this paper. Except for\ngeolocation (origin of speaker or document), we find that manually annotated\nlinguistic resources are sparse and, if they exist, mostly cover morphosyntax.\nDespite this lack of resources, we observe that interest in this area is\nincreasing: there is active development and a growing research community. To\nfacilitate research, we make our overview of over 80 corpora publicly\navailable. We share a companion website of this overview at\nhttps://github.com/mainlp/germanic-lrl-corpora .", "cat": "cs.CL", "authors": ["Verena Blaschke", "Hinrich Sch\u00fctze", "Barbara Plank"]}, "494": {"id": "0707.4211v1", "title": "Expansion of the Planet Detection Channels in Next-Generation Microlensing Surveys", "url": "http://arxiv.org/pdf/0707.4211v1", "date": "2007-07-28 04:58:24", "abs": "We classify various types of planetary lensing signals and the channels of\ndetecting them. We estimate the relative frequencies of planet detections\nthrough the individual channels with special emphasis on the new channels to be\nadditionally provided by future lensing experiments that will survey wide\nfields continuously at high cadence by using very large-format imaging cameras.\n From this investigation, we find that the fraction of wide-separation planets\nthat would be discovered through the new channels of detecting planetary\nsignals as independent and repeating events would be substantial. We estimate\nthat the fraction of planets detectable through the new channels would comprise\n~15 -- 30% of all planets depending on the models of the planetary separation\ndistribution and mass ratios of planets. Considering that a significant\nfraction of planets might exist in the form of free-floating planets, the\nfrequency of planets to be detected through the new channel would be even\nhigher. With the expansion of the channels of detecting planet, future lensing\nsurveys will greatly expand the range of planets to be probed.", "cat": "astro-ph", "authors": ["Cheongho Han"]}, "495": {"id": "1002.1526v2", "title": "The ASTE Galactic Center CO J=3-2 Survey: Probing Shocked Molecular Gas in the CMZ", "url": "http://arxiv.org/pdf/1002.1526v2", "date": "2010-02-12 10:12:32", "abs": "Large-scale CO surveys have revealed that the central molecular zone (CMZ) of\nour Galaxy is characterized by a number of expanding shells/arcs, and by a\npeculiar population of compact clouds with large velocity widths --\nhigh-velocity compact clouds (HVCCs). We have performed a large-scale CO J=3-2\nsurvey of the CMZ from 2005 to 2008 with the Atacama Submillimeter-wave\nTelescope Experiment (ASTE). The data cover almost the full extent of the CMZ\nand the Clump 2 with a 34 arcsec grid spacing. The CO J=3-2 data were compared\nwith the CO J=1--0 data taken with the Nobeyama Radio Observatory 45 m\ntelescope. Molecular gas in the CMZ exhibits higher J=3-2/J=1-0 intensity\nratios [R(3-2/1-0)=0.7] than that in the Galactic disk [R(3-2/1-0)=0.4]. We\nextracted highly excited, optically thin gas by the criterion, R(3-2/1-0)>=1.5.\nClumps of high R(3-2/1-0) gas were found in the Sgr A and Sgr C regions, near\nSNR G 0.9+0.1, and three regions with energetic HVCCs; CO 1.27+0.01, CO\n-0.41-0.23, and CO -1.21-0.12. We also found a number of small spots of high\nR(3-2/1-0) gas over the CMZ. Many of these high R(3-2/1-0) clumps and spots\nhave large velocity widths, and some apparently coincides with HVCCs,\nsuggesting that they are spots of shocked molecular gas. Their origin should be\nlocal explosive events, possibly supernova explosions. These suggest that the\nenergetic HVCCs are associated with massive compact clusters, which have been\nformed by microbursts of star formation. Rough estimates of the energy flow\nfrom large to small scale suggest that the supernova shocks can make a\nsignificant contribution to turbulence activation and gas heating in the CMZ.", "cat": "astro-ph.GA", "authors": ["Tomoharu Oka", "Kunihiko Tanaka", "Shinji Matsumura", "Makoto Nagai", "Kazuhisa Kamegai", "Tetsuo Hasegawa"]}, "496": {"id": "2307.15224v1", "title": "AI in Software Engineering: A Survey on Project Management Applications", "url": "http://arxiv.org/pdf/2307.15224v1", "date": "2023-07-27 23:02:24", "abs": "Artificial Intelligence (AI) refers to the intelligence demonstrated by\nmachines, and within the realm of AI, Machine Learning (ML) stands as a notable\nsubset. ML employs algorithms that undergo training on data sets, enabling them\nto carry out specific tasks autonomously. Notably, AI holds immense potential\nin the field of software engineering, particularly in project management and\nplanning. In this literature survey, we explore the use of AI in Software\nEngineering and summarize previous works in this area. We first review eleven\ndifferent publications related to this subject, then compare the surveyed\nworks. We then comment on the possible challenges present in the utilization of\nAI in software engineering and suggest possible further research avenues and\nthe ways in which AI could evolve with software engineering in the future.", "cat": "cs.SE", "authors": ["Talia Crawford", "Scott Duong", "Richard Fueston", "Ayorinde Lawani", "Samuel Owoade", "Abel Uzoka", "Reza M. Parizi", "Abbas Yazdinejad"]}, "497": {"id": "1612.04883v3", "title": "Graph Summarization Methods and Applications: A Survey", "url": "http://arxiv.org/pdf/1612.04883v3", "date": "2018-01-16 18:10:26", "abs": "While advances in computing resources have made processing enormous amounts\nof data possible, human ability to identify patterns in such data has not\nscaled accordingly. Efficient computational methods for condensing and\nsimplifying data are thus becoming vital for extracting actionable insights. In\nparticular, while data summarization techniques have been studied extensively,\nonly recently has summarizing interconnected data, or graphs, become popular.\nThis survey is a structured, comprehensive overview of the state-of-the-art\nmethods for summarizing graph data. We first broach the motivation behind, and\nthe challenges of, graph summarization. We then categorize summarization\napproaches by the type of graphs taken as input and further organize each\ncategory by core methodology. Finally, we discuss applications of summarization\non real-world graphs and conclude by describing some open problems in the\nfield.", "cat": "cs.IR", "authors": ["Yike Liu", "Tara Safavi", "Abhilash Dighe", "Danai Koutra"]}, "498": {"id": "1504.06174v1", "title": "A Survey of Extended H$_2$ Emission from Massive YSOs", "url": "http://arxiv.org/pdf/1504.06174v1", "date": "2015-04-23 13:29:35", "abs": "We present the results from a survey, designed to investigate the accretion\nprocess of massive young stellar objects (MYSOs) through near infrared narrow\nband imaging using the H$_2$ $\\nu$=1-0 S(1) transition filter. A sample of 353\nMassive Young Stellar Object (MYSO) candidates was selected from the Red MSX\nSource survey using photometric criteria at longer wavelengths (infrared and\nsubmillimeter) and chosen with positions throughout the Galactic Plane. Our\nsurvey was carried out at the SOAR Telescope in Chile and CFHT in Hawaii\ncovering both hemispheres. The data reveal that extended H$_2$ emission is a\ngood tracer of outflow activity, which is a signpost of accretion process on\nyoung massive stars. Almost half of the sample exhibit extended H$_2$ emission\nand 74 sources (21\\%) have polar morphology, suggesting collimated outflows.\nThe polar-like structures are more likely to appear on radio-quiet sources,\nindicating these structures occur during the pre-UCHII phase. We also found an\nimportant fraction of sources associated with fluorescent H$_2$ diffuse\nemission that could be due to a more evolved phase. The images also indicate\nonly $\\sim$23\\% (80) of the sample is associated with extant (young) stellar\nclusters. These results support the scenario in which massive stars are formed\nby accretion disks, since the merging of low mass stars would not produce\noutflow structures.", "cat": "astro-ph.SR", "authors": ["Felipe Navarete", "Augusto Damineli", "Cassio L. Barbosa", "Robert D. Blum"]}, "499": {"id": "1110.5221v1", "title": "A spectroscopic survey of thick disc stars outside the solar neighbourhood", "url": "http://arxiv.org/pdf/1110.5221v1", "date": "2011-10-24 13:09:12", "abs": "We performed a spectroscopic survey of nearly 700 stars probing the galactic\nthick disc far from the solar neighbourhood towards the galactic coordinates\n(l~277, b~47). The derived effective temperatures, surface gravities and\noverall metallicities were then combined with stellar evolution isochrones,\nradial velocities and proper motions to derive the distances, kinematics and\norbital parameters of the sample stars. The targets belonging to each galactic\ncomponent (thin disc, thick disc, halo) were selected either on their\nkinematics or according to their position above the galactic plane, and the\nvertical gradients were also estimated. We present here atmospheric parameters,\ndistances and kinematics for this sample, and a comparison of our kinematic and\nmetallicity distributions with the Besancon model of the Milky Way. The thick\ndisc far from the solar neighbourhood is found to differ only slightly from the\nthick disc properties as derived in the solar vicinity. For regions where the\nthick disc dominates, we measured vertical velocity and metallicity trends of\nd(V_phi)/dZ = 19 +/- 8 km/s/kpc and d[M/H]/dZ = -0.14 +/- 0.05 dex/kpc,\nrespectively. These trends can be explained as a smooth transition between the\ndifferent galactic components, although intrinsic gradients could not be\nexcluded. In addition, a correlation d(V_phi)/d[M/H] = -45 +/- 12 km/s/dex\nbetween the orbital velocity and the metallicity of the thick disc is detected.\nThis gradient is inconsistent with the SDSS photometric survey analysis, which\ndid not detect any such trend, and challenges radial migration models of thick\ndisc formation. Estimations of the scale heights and scale lengths for\ndifferent metallicity bins of the thick disc result in consistent values, with\nhR~3.4 \\pm 0.7 kpc, and hZ~694 \\pm 45 pc, showing no evidence of relics of\ndestroyed massive satellites.", "cat": "astro-ph.GA", "authors": ["G. Kordopatis", "A. Recio-Blanco", "P. de Laverny", "G. Gilmore", "V. Hill", "R. F. G. Wyse", "A. Helmi", "A. Bijaoui", "M. Zoccali", "O. Bienaym\u00e9"]}, "500": {"id": "0812.3588v2", "title": "A multi-wavelength survey of AGN in the XMM-LSS field: I. Quasar selection via the KX technique", "url": "http://arxiv.org/pdf/0812.3588v2", "date": "2009-02-24 18:41:45", "abs": "AIMS: We present a sample of candidate quasars selected using the\nKX-technique. The data cover 0.68 deg^2 of the X-ray Multi-Mirror (XMM)\nLarge-Scale Structure (LSS) survey area where overlapping multi-wavelength\nimaging data permits an investigation of the physical nature of selected\nsources. METHODS: The KX method identifies quasars on the basis of their\noptical (R and z') to near-infrared (Ks) photometry and point-like morphology.\nWe combine these data with optical (u*,g'r',i',z') and mid-infrared (3.6-24\nmicron) wavebands to reconstruct the spectral energy distributions (SEDs) of\ncandidate quasars. RESULTS: Of 93 sources selected as candidate quasars by the\nKX method, 25 are classified as quasars by the subsequent SED analysis.\nSpectroscopic observations are available for 12/25 of these sources and confirm\nthe quasar hypothesis in each case. Even more, 90% of the SED-classified\nquasars show X-ray emission, a property not shared by any of the false\ncandidates in the KX-selected sample. Applying a photometric redshift analysis\nto the sources without spectroscopy indicates that the 25 sources classified as\nquasars occupy the interval 0.7 < z < 2.5. The remaining 68/93 sources are\nclassified as stars and unresolved galaxies.", "cat": "astro-ph", "authors": ["Th. Nakos", "J. P. Willis", "S. Andreon", "J. Surdej", "P. Riaud", "E. Hatziminaoglou", "O. Garcet", "D. Alloin", "M. Baes", "G. Galaz", "M. Pierre", "H. Quintana", "M. J. Page", "J. A. Tedds", "M. T. Ceballos", "A. Corral", "J. Ebrero", "M. Krumpe", "S. Mateos"]}, "501": {"id": "2204.09059v2", "title": "A deep survey of short GRB host galaxies over $z\\sim0-2$: implications for offsets, redshifts, and environments", "url": "http://arxiv.org/pdf/2204.09059v2", "date": "2022-07-11 19:14:01", "abs": "A significant fraction (30\\%) of well-localized short gamma-ray bursts\n(sGRBs) lack a coincident host galaxy. This leads to two main scenarios:\n\\textit{i}) that the progenitor system merged outside of the visible light of\nits host, or \\textit{ii}) that the sGRB resided within a faint and distant\ngalaxy that was not detected by follow-up observations. Discriminating between\nthese scenarios has important implications for constraining the formation\nchannels of neutron star mergers, the rate and environments of gravitational\nwave sources, and the production of heavy elements in the Universe. In this\nwork, we present the results of our observing campaign targeted at 31 sGRBs\nthat lack a putative host galaxy. Our study effectively doubles the sample of\nwell-studied sGRB host galaxies, now totaling 72 events of which $28\\%$ lack a\ncoincident host to deep limits ($r$\\,$\\gtrsim$\\,$26$ or\n$F110W$\\,$\\gtrsim$\\,$27$ AB mag), and represents the largest homogeneously\nselected catalog of sGRB offsets to date. We find that 70\\% of sub-arcsecond\nlocalized sGRBs occur within 10 kpc of their host's nucleus, with a median\nprojected physical offset of $5.6$ kpc. Using this larger population, we\ndiscover an apparent redshift evolution in their locations: bursts at low-$z$\noccur at $2\\times$ larger offsets compared to those at $z$\\,$>$\\,$0.5$. This\nevolution could be due to a physical evolution of the host galaxies themselves\nor a bias against faint high-$z$ galaxies. Furthermore, we discover a sample of\nhostless sGRBs at $z$\\,$\\gtrsim$\\,$1$ that are indicative of a larger high-$z$\npopulation, constraining the redshift distribution and disfavoring log-normal\ndelay time models.", "cat": "astro-ph.HE", "authors": ["B. O'Connor", "E. Troja", "S. Dichiara", "P. Beniamini", "S. B. Cenko", "C. Kouveliotou", "J. Becerra Gonzalez", "J. Durbak", "P. Gatkine", "A. Kutyrev", "T. Sakamoto", "R. Sanchez-Ramirez", "S. Veilleux"]}, "502": {"id": "2401.17764v1", "title": "The GRAVITY young stellar object survey XIII. Tracing the time-variable asymmetric disk structure in the inner AU of the Herbig star HD98922", "url": "http://arxiv.org/pdf/2401.17764v1", "date": "2024-01-31 11:43:24", "abs": "Temporal variability in the photometric and spectroscopic properties of\nprotoplanetary disks is common in YSO. However, evidence pointing toward\nchanges in their morphology over short timescales has only been found for a few\nsources, mainly due to a lack of high cadence observations at mas resolution.\nWe combine GRAVITY multi-epoch observations of HD98922 at mas resolution with\nPIONIER archival data covering a total time span of 11 years. We interpret the\ninterferometric visibilities and spectral energy distribution with geometrical\nmodels and through radiative transfer techniques. We investigated\nhigh-spectral-resolution quantities to obtain information on the properties of\nthe HI BrG-line-emitting region. The observations are best fitted by a model of\na crescent-like asymmetric dust feature located at 1 au and accounting for 70%\nof the NIR emission. The feature has an almost constant magnitude and orbits\nthe central star with a possible sub-Keplerian period of 12 months, although a\n9 month period is another, albeit less probable, solution. The radiative\ntransfer models show that the emission originates from a small amount of\ncarbon-rich (25%) silicates, or quantum-heated particles located in a\nlow-density region. Among different possible scenarios, we favor hydrodynamical\ninstabilities in the inner disk that can create a large vortex. The high\nspectral resolution differential phases in the BrG-line show that the hot-gas\ncomponent is offset from the star and in some cases is located between the star\nand the crescent feature. The scale of the emission does not favor\nmagnetospheric accretion as a driving mechanism. The scenario of an asymmetric\ndisk wind or a massive accreting substellar or planetary companion is\ndiscussed. With this unique observational data set for HD98922, we reveal\nmorphological variability in the innermost 2 au of its disk region.", "cat": "astro-ph.SR", "authors": ["GRAVITY Collaboration", "V. Ganci", "L. Labadie", "K. Perraut", "A. Wojtczak", "J. Kaufhold", "M. Benisty", "E. Alecian", "G. Bourdarot", "W. Brandner", "A. Caratti o Garatti", "C. Dougados", "R. Garcia Lopez", "J. Sanchez-Bermudez", "A. Soulain", "A. Amorim", "J. -P. Berger", "P. Caselli", "Y. Cl\u00e9net", "A. Drescher", "A. Eckart", "F. Eisenhauer", "M. Fabricius", "H. Feuchtgruber", "P. Garcia", "E. Gendron", "R. Genzel", "S. Gillessen", "S. Grant", "G. Hei\u00dfel", "T. Henning", "M. Horrobin", "L. Jocou", "P. Kervella", "S. Lacour", "V. Lapeyr\u00e8re", "J. -B. Le Bouquin", "P. L\u00e9na", "D. Lutz", "F. Mang", "N. Moruj\u00e3o", "T. Ott", "T. Paumard", "G. Perrin", "D. Ribeiro", "M. Sadun Bordoni", "S. Scheithauer", "J. Shangguan", "T. Shimizu", "C. Straubmeier", "E. Sturm", "L. Tacconi", "E. van Dishoeck", "F. Vincent", "J. Woillez"]}, "503": {"id": "1807.01092v1", "title": "Barlenses in the CALIFA survey: combining the photometric and stellar population analysis", "url": "http://arxiv.org/pdf/1807.01092v1", "date": "2018-07-03 11:35:18", "abs": "We investigate barlenses in the Calar Alto Legacy Integral Field Area\n(CALIFA) survey galaxies, studying their morphologies, stellar populations and\nmetallicities. Multi-component decompositions are made using the Sloan Digital\nSky Survey (SDSS) images and making GALFIT models, fitting besides bulges,\ndisks and bars, also barlenses, which are the face-on counterparts of\nBoxy/Peanut bulges. Similar GALFIT models as were made for the galaxies, were\nmade also for the simulation snap-shots. For the stellar populations and\nmetallicities in the various structure components CALIFA IFU-observations are\nused. We show that, when present, barlenses account for a significant portion\nof light of photometric bulges (i.e. the excess light on top of the disks),\nwhich highlights the importance of bars in accumulating the central galaxy mass\nconcentrations in the cosmic timescale. Bars and barlenses are found to have\nsimilar cumulative stellar age and metallicity distributions. This is the first\ntime that a combined morphological and stellar population analysis is used to\nstudy barlenses. We show that their stars are accumulated in a prolonged time\nperiod, concurrently with the evolution of the narrow bar.", "cat": "astro-ph.GA", "authors": ["E. Laurikainen", "H. Salo", "J. Laine", "J. Janz"]}, "504": {"id": "2002.05543v1", "title": "A mid-infrared interferometric survey of the planet-forming region around young Sun-like stars", "url": "http://arxiv.org/pdf/2002.05543v1", "date": "2020-02-13 14:52:12", "abs": "We present our results from a mid-infrared interferometric survey targeted at\nthe planet-forming region in the circumstellar disks around low- and\nintermediate-mass young stars. Our sample consist of 82 objects, including T\nTauri stars, Herbig Ae stars, and young eruptive stars. Our main results are:\n1) Disks around T Tauri stars are similar to those around Herbig Ae stars, but\nare relatively more extended once we account for stellar luminosity. 2) From\nthe distribution of the sizes of the mid-infrared emitting region we find that\ninner dusty disk holes may be present in roughly half of the sample. 3) Our\nanalysis of the silicate spectral feature reveals that the dust in the inner\n$\\sim$1 au region of disks is generally more processed than that in the outer\nregions. 4) The dust in the disks of T Tauri stars typically show weaker\nsilicate emission in the N band spectrum, compared to Herbig Ae stars, which\nmay indicate a general difference in the disk structure. Our data products are\navailable at VizieR, and at the following web page:\nhttp://konkoly.hu/MIDI_atlas", "cat": "astro-ph.SR", "authors": ["J. Varga", "P. \u00c1brah\u00e1m", "L. Chen", "Th. Ratzka", "K. \u00c9. Gab\u00e1nyi", "\u00c1. K\u00f3sp\u00e1l"]}, "505": {"id": "1210.5465v1", "title": "CARMENES. I. A radial-velocity survey for terrestrial planets in the habitable zones of M dwarfs. A historical overview", "url": "http://arxiv.org/pdf/1210.5465v1", "date": "2012-10-19 16:18:10", "abs": "CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with\nNear-infrared and optical Echelle Spectrographs) is a next generation\ninstrument being built for the 3.5-m telescope at the Calar Alto Observatory by\na consortium of eleven Spanish and German institutions. Conducting a five-year\nexoplanet survey targeting 300 M dwarfs with the completed instrument is an\nintegral part of the project. The CARMENES instrument consists of two separate\nechelle spectrographs covering the wavelength range from 550 to 1700 nm at a\nspectral resolution of R=82,000, fed by fibers from the Cassegrain focus of the\ntelescope. The spectrographs are housed in vacuum tanks providing the\ntemperature-stabilized environments necessary to enable a 1 m/s radial velocity\nprecision employing a simultaneous calibration with emission-line lamps.", "cat": "astro-ph.IM", "authors": ["P. J. Amado", "A. Quirrenbach", "I. Ribas", "J. A. Caballero", "M. A. S\u00e1nchez-Carrasco", "A. Reiners", "W. Seifert", "R. Mundt", "H. Mandel", "the CARMENES Consortium"]}, "506": {"id": "1410.2172v1", "title": "The extended ROSAT-ESO Flux-Limited X-ray Galaxy Cluster Survey (REFLEX II) V. Exploring a local underdensity in the Southern Sky", "url": "http://arxiv.org/pdf/1410.2172v1", "date": "2014-10-08 15:50:50", "abs": "Several claims have been made that we are located in a locally underdense\nregion of the Universe based on observations of supernovae and galaxy density\ndistributions. Two recent studies of K-band galaxy surveys have provided new\nsupport for a local underdensity in the galaxy distribution out to distances of\n200 - 300 Mpc. If confirmed, such large local underdensities would have\nimportant implications on the interpretation of local measurements of\ncosmological parameters. Galaxy clusters have been shown to be ideal probes to\ntrace the large-scale structure of the Universe. In this paper we study the\nlocal density distribution in the southern sky with the X-ray detected galaxy\nclusters from the REFLEX II cluster survey. From the normalized comoving number\ndensity of clusters we find an average underdensity of ~30 - 40% in the\nredshift range out to z ~0.04 (~170 Mpc) in the southern extragalactic sky with\na significance larger than 3.4sigma. On larger scales from 300 Mpc to over 1\nGpc the density distribution appears remarkably homogeneous. The local\nunderdensity seems to be dominated by the South Galactic Cap region. A\ncomparison of the cluster distribution with that of galaxies in the K-band from\na recent study shows that galaxies and clusters trace each other very closely\nin density. In the South Galactic Cap region both surveys find a local\nunderdensity in the redshift range z= 0 to 0.05 and no significant underdensity\nin the North Galactic Cap at southern latitudes. Our results to not support\ncosmological models that attempt to interpret the cosmic acceleration by a\nlarge local void, since the local underdensity we find is not isotropic and\nlimited to a size significantly smaller than 300 Mpc radius.", "cat": "astro-ph.CO", "authors": ["Hans Boehringer", "Gayoung Chon", "Martyn Bristow", "Chris A. Collins"]}, "507": {"id": "2004.08255v1", "title": "A Survey of Approximate Quantile Computation on Large-scale Data (Technical Report)", "url": "http://arxiv.org/pdf/2004.08255v1", "date": "2020-04-17 14:10:00", "abs": "As data volume grows extensively, data profiling helps to extract metadata of\nlarge-scale data. However, one kind of metadata, order statistics, is difficult\nto be computed because they are not mergeable or incremental. Thus, the\nlimitation of time and memory space does not support their computation on\nlarge-scale data. In this paper, we focus on an order statistic, quantiles, and\npresent a comprehensive analysis of studies on approximate quantile\ncomputation. Both deterministic algorithms and randomized algorithms that\ncompute approximate quantiles over streaming models or distributed models are\ncovered. Then, multiple techniques for improving the efficiency and performance\nof approximate quantile algorithms in various scenarios, such as skewed data\nand high-speed data streams, are presented. Finally, we conclude with coverage\nof existing packages in different languages and with a brief discussion of the\nfuture direction in this area.", "cat": "cs.DS", "authors": ["Zhiwei Chen", "Aoqian Zhang"]}, "508": {"id": "2401.09994v1", "title": "Bayesian modeling of spatial ordinal data from health surveys", "url": "http://arxiv.org/pdf/2401.09994v1", "date": "2024-01-18 14:10:49", "abs": "Health surveys allow exploring health indicators that are of great value from\na public health point of view and that cannot normally be studied from regular\nhealth registries. These indicators are usually coded as ordinal variables and\nmay depend on covariates associated with individuals. In this paper, we propose\na Bayesian individual-level model for small-area estimation of survey-based\nhealth indicators. A categorical likelihood is used at the first level of the\nmodel hierarchy to describe the ordinal data, and spatial dependence among\nsmall areas is taken into account by using a conditional autoregressive (CAR)\ndistribution. Post-stratification of the results of the proposed\nindividual-level model allows extrapolating the results to any administrative\nareal division, even for small areas. We apply this methodology to the analysis\nof the Health Survey of the Region of Valencia (Spain) of 2016 to describe the\ngeographical distribution of a self-perceived health indicator of interest in\nthis region.", "cat": "stat.ME", "authors": ["Miguel \u00c1ngel Beltr\u00e1n S\u00e1nchez", "Miguel \u00c1ngel Mart\u00ednez Beneito", "Ana Corber\u00e1n Vallet"]}, "509": {"id": "2303.01438v1", "title": "Radio detections of two unusual cataclysmic variables in the VLA Sky Survey", "url": "http://arxiv.org/pdf/2303.01438v1", "date": "2023-03-02 17:51:53", "abs": "We report two new radio detections of cataclysmic variables (CVs), and place\nthem in context with radio and X-ray detections of other CVs. We detected QS\nVir, a low accretion-rate CV; V2400 Oph, a diskless intermediate polar (IP);\nand recovered the polar AM Her in the Very Large Array Sky Survey (VLASS) 2-4\nGHz radio images. The radio luminosities of these systems are higher than\ntypically expected from coronal emission from stars of similar spectral types,\nand neither system is expected to produce jets, leaving the origin of the radio\nemission a puzzle. The radio emission mechanism for these two CVs may be\nelectron-cyclotron maser emission, synchrotron radiation, or a more exotic\nprocess. We compile published radio detections of CVs, and X-ray measurements\nof these CVs, to illustrate their locations in the radio - X-ray luminosity\nplane, a diagnostic tool often used for X-ray binaries, active galactic nuclei,\nand radio stars. Several radio-emitting CVs, including these two newly detected\nCVs, seem to lie near the principal radio/X-ray track followed by black hole\nX-ray binaries (BHXBs) at low luminosity, suggesting additional complexity in\nclassifying unknown systems using their radio and X-ray luminosities alone.", "cat": "astro-ph.HE", "authors": ["Margaret E Ridder", "Craig O Heinke", "Gregory R Sivakoff", "Andrew K Hughes"]}, "510": {"id": "1410.3892v2", "title": "Radio-Quiet Quasars in the VIDEO Survey: Evidence for AGN-powered radio emission at S_1.4GHz < 1 mJy", "url": "http://arxiv.org/pdf/1410.3892v2", "date": "2015-01-19 21:20:10", "abs": "Understanding the interplay between black-hole accretion and star formation,\nand how to disentangle the two, is crucial to our understanding of galaxy\nformation and evolution. To investigate, we use a combination of optical and\nnear-infrared photometry to select a sample of 74 quasars from the VISTA Deep\nExtragalactic Observations (VIDEO) Survey, over 1 deg$^2$. The depth of VIDEO\nallows us to study very low accretion rates and/or lower-mass black holes, and\n26 per cent of the candidate quasar sample has been spectroscopically\nconfirmed. We use a radio-stacking technique to sample below the nominal\nflux-density threshold using data from the Very Large Array at 1.4 GHz and\nfind, in agreement with other work, that a power-law fit to the quasar-related\nradio source counts is inadequate at low flux density. By comparing with a\ncontrol sample of galaxies (where we match in terms of stellar mass), and by\nestimating the star formation rate, we suggest that this radio emission is\npredominantly caused by accretion activity rather than star-formation activity.", "cat": "astro-ph.GA", "authors": ["Sarah V. White", "Matt J. Jarvis", "Boris H\u00e4u\u00dfler", "Natasha Maddox"]}, "511": {"id": "1609.00025v2", "title": "A VLA Survey For Faint Compact Radio Sources in the Orion Nebula Cluster", "url": "http://arxiv.org/pdf/1609.00025v2", "date": "2016-09-02 16:45:29", "abs": "We present Karl G. Janksy Very Large Array (VLA) 1.3 cm, 3.6 cm, and 6 cm\ncontinuum maps of compact radio sources in the Orion Nebular Cluster. We\nmosaicked 34 square arcminutes at 1.3 cm, 70 square arcminutes at 3.6 cm and\n109 square arcminutes at 6 cm, containing 778 near-infrared detected YSOs and\n190 HST-identified proplyds (with significant overlap between those\ncharacterizations). We detected radio emission from 175 compact radio sources\nin the ONC, including 26 sources that were detected for the first time at these\nwavelengths. For each detected source we fit a simple free-free and dust\nemission model to characterize the radio emission. We extrapolate the free-free\nemission spectrum model for each source to ALMA bands to illustrate how these\nmeasurements could be used to correctly measure protoplanetary disk dust masses\nfrom sub-millimeter flux measurements. Finally, we compare the fluxes measured\nin this survey with previously measured fluxes for our targets, as well as four\nseparate epochs of 1.3 cm data, to search for and quantify variability of our\nsources.", "cat": "astro-ph.GA", "authors": ["Patrick D. Sheehan", "Josh A. Eisner", "Rita K. Mann", "Jonathan P. Williams"]}, "512": {"id": "1212.0034v1", "title": "GEOS RR Lyr Survey: Blazhko Period Measurement of Three RRab Stars - CX Lyrae, NU Aurigae and VY Corona Borealis", "url": "http://arxiv.org/pdf/1212.0034v1", "date": "2012-11-30 22:45:33", "abs": "We present the results of collaborative observations of three RR Lyrae stars\n(CX Lyr, NU Aur and VY CrB) which have a strong Blazhko effect. This work has\nbeen initiated and performed in the framework of the GEOS RR Lyr Survey (Groupe\nEurop\\'een d'Observations Stellaires). From the measured light curves, we have\ndetermined the times and the magnitudes at maximum. The times of maxima have\nbeen compared to ephemerides to obtain the (O-C) values and from a period\nanalysis of these (O-C) values, the Blazhko period is derived. The Blazhko\nperiods of NU Aur (114.8 days) and VY CrB (32.3 days) are reported here for the\nfirst time and a more accurate period for CX Lyr (68.3 days) has been obtained.\nThe three stars are subject to strong Blazhko effect, but this effect has\ndifferent characteristics for each of them. When we compare the variations of\nmagnitude at maximum and variations of (O-C) values with respect to the Blazhko\nphase, these variations are either in phase, in opposition, or even in\nquadrature.", "cat": "astro-ph.SR", "authors": ["Pierre de Ponthiere", "Jean-Francois Le Borgne", "F. Fumagalli", "Franz-Josef Hambsch", "Tom Krajci", "J-M Llapasset", "Kenneth Menzies", "Marco Nobile", "Richard Sabo"]}, "513": {"id": "1709.05076v1", "title": "Stellar atmospheric parameters and the Gaia-ESO Survey experience with multiple analysis pipelines", "url": "http://arxiv.org/pdf/1709.05076v1", "date": "2017-09-15 07:07:37", "abs": "To use libraries of observed stellar spectra, one needs to know the\natmospheric parameters of the stars associated to those spectra. It is,\nhowever, hard to know what are the real levels of precision and accuracy of\nthese parameters. To overcome this very same problem in a stellar survey, the\nGaia-ESO Survey implements a comprehensive calibration effort together with the\nuse of multiple parallel analysis methodologies. Here, we discuss the multiple\nanalyses approach and the effort to understand the accuracy and precision of\nthe provided stellar atmospheric parameters.", "cat": "astro-ph.SR", "authors": ["R. Smiljanic", "A. J. Korn", "A. R. Casey", "the Gaia-ESO Survey consortium"]}, "514": {"id": "2111.05193v2", "title": "A Survey on Green Deep Learning", "url": "http://arxiv.org/pdf/2111.05193v2", "date": "2021-11-10 02:28:08", "abs": "In recent years, larger and deeper models are springing up and continuously\npushing state-of-the-art (SOTA) results across various fields like natural\nlanguage processing (NLP) and computer vision (CV). However, despite promising\nresults, it needs to be noted that the computations required by SOTA models\nhave been increased at an exponential rate. Massive computations not only have\na surprisingly large carbon footprint but also have negative effects on\nresearch inclusiveness and deployment on real-world applications.\n Green deep learning is an increasingly hot research field that appeals to\nresearchers to pay attention to energy usage and carbon emission during model\ntraining and inference. The target is to yield novel results with lightweight\nand efficient technologies. Many technologies can be used to achieve this goal,\nlike model compression and knowledge distillation. This paper focuses on\npresenting a systematic review of the development of Green deep learning\ntechnologies. We classify these approaches into four categories: (1) compact\nnetworks, (2) energy-efficient training strategies, (3) energy-efficient\ninference approaches, and (4) efficient data usage. For each category, we\ndiscuss the progress that has been achieved and the unresolved challenges.", "cat": "cs.LG", "authors": ["Jingjing Xu", "Wangchunshu Zhou", "Zhiyi Fu", "Hao Zhou", "Lei Li"]}, "515": {"id": "2009.10661v1", "title": "Decoding Starlight with Big Survey Data, Machine Learning, and Cosmological Simulations", "url": "http://arxiv.org/pdf/2009.10661v1", "date": "2020-09-22 16:32:43", "abs": "Stars, and collections of stars, encode rich signatures of stellar physics\nand galaxy evolution. With properties influenced by both their environment and\nintrinsic nature, stars retain information about astrophysical phenomena that\nare not otherwise directly observable. In the time-domain, the observed\nbrightness variability of a star can be used to investigate physical processes\noccurring at the stellar surface and in the stellar interior. On a galactic\nscale, the properties of stars, including chemical abundances and stellar ages,\nserve as a multi-dimensional record of the origin of the galaxy. In the Milky\nWay, together with orbital properties, this informs the details of the\nevolution of our Galaxy since its formation. Extending beyond the Local Group,\nthe attributes of unresolved stellar populations allow us to study the\ndiversity of galaxies in the Universe.\n By examining the properties of stars, and how they vary across a range of\nspatial and temporal scales, this Dissertation connects the information\nresiding within stars to global processes in galactic formation and evolution.\nWe develop new approaches to determine stellar properties, including rotation\nand surface gravity, from the variability that we directly observe. We offer\nnew insight into the chemical enrichment history of the Milky Way, tracing\ndifferent stellar explosions that capture billions of years of evolution. We\nadvance knowledge and understanding of how stars and galaxies are linked, by\nexamining differences in the initial stellar mass distributions comprising\ngalaxies, as they form. In building up this knowledge, we highlight current\ntensions between data and theory. By synthesizing numerical simulations, large\nobservational data sets, and machine learning techniques, this work makes\nvaluable methodological contributions to maximize insights from diverse\nensembles of current and future stellar observations.", "cat": "astro-ph.GA", "authors": ["Kirsten Blancato"]}, "516": {"id": "2109.03784v1", "title": "A Survey on Machine Learning Techniques for Auto Labeling of Video, Audio, and Text Data", "url": "http://arxiv.org/pdf/2109.03784v1", "date": "2021-09-08 17:15:34", "abs": "Machine learning has been utilized to perform tasks in many different domains\nsuch as classification, object detection, image segmentation and natural\nlanguage analysis. Data labeling has always been one of the most important\ntasks in machine learning. However, labeling large amounts of data increases\nthe monetary cost in machine learning. As a result, researchers started to\nfocus on reducing data annotation and labeling costs. Transfer learning was\ndesigned and widely used as an efficient approach that can reasonably reduce\nthe negative impact of limited data, which in turn, reduces the data\npreparation cost. Even transferring previous knowledge from a source domain\nreduces the amount of data needed in a target domain. However, large amounts of\nannotated data are still demanded to build robust models and improve the\nprediction accuracy of the model. Therefore, researchers started to pay more\nattention on auto annotation and labeling. In this survey paper, we provide a\nreview of previous techniques that focuses on optimized data annotation and\nlabeling for video, audio, and text data.", "cat": "cs.LG", "authors": ["Shikun Zhang", "Omid Jafari", "Parth Nagarkar"]}, "517": {"id": "1308.6818v1", "title": "Host Galaxy Spectra and Consequences for SN Typing From The SDSS SN Survey", "url": "http://arxiv.org/pdf/1308.6818v1", "date": "2013-08-30 18:40:07", "abs": "We present the spectroscopy from 5254 galaxies that hosted supernovae (SNe)\nor other transient events in the Sloan Digital Sky Survey II (SDSS-II).\nObtained during SDSS-I, SDSS-II, and the Baryon Oscillation Spectroscopic\nSurvey (BOSS), this sample represents the largest systematic, unbiased,\nmagnitude limited spectroscopic survey of supernova (SN) host galaxies. Using\nthe host galaxy redshifts, we test the impact of photometric SN classification\nbased on SDSS imaging data with and without using spectroscopic redshifts of\nthe host galaxies. Following our suggested scheme, there are a total of 1166\nphotometrically classified SNe Ia when using a flat redshift prior and 1126 SNe\nIa when the host spectroscopic redshift is assumed. For 1024 (87.8%) candidates\nclassified as likely SNe Ia without redshift information, we find that the\nclassification is unchanged when adding the host galaxy redshift. Using\nphotometry from SDSS imaging data and the host galaxy spectra, we also report\nhost galaxy properties for use in future nalysis of SN astrophysics. Finally,\nwe investigate the differences in the interpretation of the light curve\nproperties with and without knowledge of the redshift. When using the SALT2\nlight curve fitter, we find a 21% increase in the number of fits that converge\nwhen using the spectroscopic redshift. Without host galaxy redshifts, we find\nthat SALT2 light curve fits are systematically biased towards lower photometric\nredshift estimates and redder colors in the limit of low signal-to-noise data.\nThe general improvements in performance of the light curve fitter and the\nincreased diversity of the host galaxy sample highlights the importance of host\ngalaxy spectroscopy for current photometric SN surveys such as the Dark Energy\nSurvey and future surveys such as the Large Synoptic Survey Telescope.", "cat": "astro-ph.CO", "authors": ["Matthew D. Olmstead", "Peter J. Brown", "Masao Sako", "Bruce Bassett", "J. Brinkmann", "Joel R. Brownstein", "Howard Brewington", "Heather Campbell", "Chris B. D'Andrea", "Kyle S. Dawson", "Garrett L. Ebelke", "Joshua A. Frieman", "Llu\u00eds Galbany", "Peter Garnavich", "Ravi R. Gupta", "Renee Hlozek", "Saurabh W. Jha", "Martin Kunz", "Hubert Lampeitl", "Elena Malanushenko", "Viktor Malanushenko", "John Marriner", "Ramon Miquel", "Antonio D. Montero-Dorta", "Robert C. Nichol", "Daniel J. Oravetz", "Kaike Pan", "Donald P. Schneider", "Audrey E. Simmons", "Mathew Smith", "Stephanie A. Snedden"]}, "518": {"id": "1811.04937v1", "title": "MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters -- IV. cataclysmic variables -- properties of bright and faint populations", "url": "http://arxiv.org/pdf/1811.04937v1", "date": "2018-11-12 19:00:01", "abs": "We investigate here populations of cataclysmic variables (CVs) in a set of\n288 globular cluster (GC) models evolved with the MOCCA code. This is by far\nthe largest sample of GC models ever analysed with respect to CVs. Contrary to\nwhat has been argued for a long time, we found that dynamical destruction of\nprimordial CV progenitors is much stronger in GCs than dynamical formation of\nCVs, and that dynamically formed CVs and CVs formed under no/weak influence of\ndynamics have similar white dwarf mass distributions. In addition, we found\nthat, on average, the detectable CV population is predominantly composed of CVs\nformed via typical common envelope phase (CEP) ($\\gtrsim70$ per cent), that\nonly $\\approx2-4$ per cent of all CVs in a GC is likely to be detectable, and\nthat core-collapsed models tend to have higher fractions of bright CVs than\nnon-core-collapsed ones. We also consistently show, for the first time, that\nthe properties of bright and faint CVs can be understood by means of the pre-CV\nand CV formation rates, their properties at their formation times and cluster\nhalf-mass relaxation times. Finally, we show that models following the initial\nbinary population proposed by Kroupa and set with low CEP efficiency better\nreproduce the observed amount of CVs and CV candidates in NGC 6397, NGC 6752\nand 47 Tuc. To progress with comparisons, the essential next step is to\nproperly characterize the candidates as CVs (e.g. by obtaining orbital periods\nand mass ratios).", "cat": "astro-ph.GA", "authors": ["Diogo Belloni", "Mirek Giersz", "Liliana E. Rivera Sandoval", "Abbas Askar", "Pawe\u0142 Cieciel\u0105g"]}, "519": {"id": "1605.09395v2", "title": "Radio Counterparts of Compact Binary Mergers detectable in Gravitational Waves: A Simulation for an Optimized Survey", "url": "http://arxiv.org/pdf/1605.09395v2", "date": "2016-09-04 13:54:47", "abs": "Mergers of binary neutron stars and black hole-neutron star binaries produce\ngravitational-wave (GW) emission and outflows with significant kinetic\nenergies. These outflows result in radio emissions through synchrotron\nradiation. We explore the detectability of these synchrotron generated radio\nsignals by follow-up observations of GW merger events lacking a detection of\nelectromagnetic counterparts in other wavelengths. We model radio light curves\narising from (i) sub-relativistic merger ejecta and (ii) ultra-relativistic\njets. The former produces radio remnants on timescales of a few years and the\nlatter produces $\\gamma$-ray bursts in the direction of the jet and\norphan-radio afterglows extending over wider angles on timescales of weeks.\nBased on the derived light curves, we suggest an optimized survey at $1.4$ GHz\nwith five epochs separated by a logarithmic time interval. We estimate the\ndetectability of the radio counterparts of simulated GW-merger events to be\ndetected by advanced LIGO and Virgo by current and future radio facilities. The\ndetectable distances for these GW merger events could be as high as 1 Gpc.\n$20$--$60\\%$ of the long-lasting radio remnants will be detectable in the case\nof the moderate kinetic energy of $3\\cdot 10^{50}$ erg and a circum-merger\ndensity of $0.1 {\\rm cm^{-3}}$ or larger, while $5$--$20\\%$ of the orphan radio\nafterglows with kinetic energy of $10^{48}$ erg will be detectable. The\ndetection likelihood increases if one focuses on the well-localizable GW\nevents. We discuss the background noise due to radio fluxes of host galaxies\nand false positives arising from extragalactic radio transients and variable\nActive Galactic Nuclei and we show that the quiet radio transient sky is of\ngreat advantage when searching for the radio counterparts.", "cat": "astro-ph.HE", "authors": ["Kenta Hotokezaka", "Samaya Nissanke", "Gregg Hallinan", "T. Joseph W. Lazio", "Ehud Nakar", "Tsvi Piran"]}, "520": {"id": "2311.05804v1", "title": "Model-as-a-Service (MaaS): A Survey", "url": "http://arxiv.org/pdf/2311.05804v1", "date": "2023-11-10 00:35:00", "abs": "Due to the increased number of parameters and data in the pre-trained model\nexceeding a certain level, a foundation model (e.g., a large language model)\ncan significantly improve downstream task performance and emerge with some\nnovel special abilities (e.g., deep learning, complex reasoning, and human\nalignment) that were not present before. Foundation models are a form of\ngenerative artificial intelligence (GenAI), and Model-as-a-Service (MaaS) has\nemerged as a groundbreaking paradigm that revolutionizes the deployment and\nutilization of GenAI models. MaaS represents a paradigm shift in how we use AI\ntechnologies and provides a scalable and accessible solution for developers and\nusers to leverage pre-trained AI models without the need for extensive\ninfrastructure or expertise in model training. In this paper, the introduction\naims to provide a comprehensive overview of MaaS, its significance, and its\nimplications for various industries. We provide a brief review of the\ndevelopment history of \"X-as-a-Service\" based on cloud computing and present\nthe key technologies involved in MaaS. The development of GenAI models will\nbecome more democratized and flourish. We also review recent application\nstudies of MaaS. Finally, we highlight several challenges and future issues in\nthis promising area. MaaS is a new deployment and service paradigm for\ndifferent AI-based models. We hope this review will inspire future research in\nthe field of MaaS.", "cat": "cs.AI", "authors": ["Wensheng Gan", "Shicheng Wan", "Philip S. Yu"]}, "521": {"id": "2303.03576v1", "title": "A Survey of Numerical Algorithms that can Solve the Lasso Problems", "url": "http://arxiv.org/pdf/2303.03576v1", "date": "2023-03-07 01:12:59", "abs": "In statistics, the least absolute shrinkage and selection operator (Lasso) is\na regression method that performs both variable selection and regularization.\nThere is a lot of literature available, discussing the statistical properties\nof the regression coefficients estimated by the Lasso method. However, there\nlacks a comprehensive review discussing the algorithms to solve the\noptimization problem in Lasso. In this review, we summarize five representative\nalgorithms to optimize the objective function in Lasso, including the iterative\nshrinkage threshold algorithm (ISTA), fast iterative shrinkage-thresholding\nalgorithms (FISTA), coordinate gradient descent algorithm (CGDA), smooth L1\nalgorithm (SLA), and path following algorithm (PFA). Additionally, we also\ncompare their convergence rate, as well as their potential strengths and\nweakness.", "cat": "stat.CO", "authors": ["Yujie Zhao", "Xiaoming Huo"]}, "522": {"id": "1303.7467v3", "title": "Optimizing Throughput on Guaranteed-Bandwidth WAN Networks for the Large Synoptic Survey Telescope (LSST)", "url": "http://arxiv.org/pdf/1303.7467v3", "date": "2013-06-21 21:45:42", "abs": "The Large Synoptic Survey Telescope (LSST) is a proposed 8.4-meter telescope\nthat will be located in the Andes mountains in Chile. Every 17 seconds, a 6.4\nGB image is transferred to Illinois for immediate processing. That transfer\nneeds to complete within approximately five seconds. LSST is provisioning an\ninternational WAN with a 10Gbps bandwidth guarantee for this and other\nproject-related data transfers. The stringent latency requirement drives a\nre-examination of TCP congestion control for this use case. Specifically, prior\nwork on dedicated Long Fat Networks (LFNs) does not go far enough in fully\nleveraging the opportunity provided by the bandwidth guarantee. This paper\npresents an approach for how optimal network throughput can be obtained for the\nLSST use case, and the conditions under which any project can achieve data\nthroughput rates on long-distance networks approaching wire speed.", "cat": "cs.NI", "authors": ["D. Michael Freemon"]}, "523": {"id": "2301.13350v1", "title": "A Survey on Digital Twins: Architecture, Enabling Technologies, Security and Privacy, and Future Prospects", "url": "http://arxiv.org/pdf/2301.13350v1", "date": "2023-01-31 00:58:46", "abs": "By interacting, synchronizing, and cooperating with its physical counterpart\nin real time, digital twin is promised to promote an intelligent, predictive,\nand optimized modern city. Via interconnecting massive physical entities and\ntheir virtual twins with inter-twin and intra-twin communications, the Internet\nof digital twins (IoDT) enables free data exchange, dynamic mission\ncooperation, and efficient information aggregation for composite insights\nacross vast physical/virtual entities. However, as IoDT incorporates various\ncutting-edge technologies to spawn the new ecology, severe known/unknown\nsecurity flaws and privacy invasions of IoDT hinders its wide deployment.\nBesides, the intrinsic characteristics of IoDT such as \\emph{decentralized\nstructure}, \\emph{information-centric routing} and \\emph{semantic\ncommunications} entail critical challenges for security service provisioning in\nIoDT. To this end, this paper presents an in-depth review of the IoDT with\nrespect to system architecture, enabling technologies, and security/privacy\nissues. Specifically, we first explore a novel distributed IoDT architecture\nwith cyber-physical interactions and discuss its key characteristics and\ncommunication modes. Afterward, we investigate the taxonomy of security and\nprivacy threats in IoDT, discuss the key research challenges, and review the\nstate-of-the-art defense approaches. Finally, we point out the new trends and\nopen research directions related to IoDT.", "cat": "cs.CR", "authors": ["Yuntao Wang", "Zhou Su", "Shaolong Guo", "Minghui Dai", "Tom H. Luan", "Yiliang Liu"]}, "524": {"id": "1206.4715v2", "title": "Transit Detection in the MEarth Survey of Nearby M Dwarfs: Bridging the Clean-First, Search-Later Divide", "url": "http://arxiv.org/pdf/1206.4715v2", "date": "2012-09-04 20:25:53", "abs": "In the effort to characterize the masses, radii, and atmospheres of\npotentially habitable exoplanets, there is an urgent need to find examples of\nsuch planets transiting nearby M dwarfs. The MEarth Project is an ongoing\neffort to do so, as a ground-based photometric survey designed to detect\nexoplanets as small as 2 Earth radii transiting mid-to-late M dwarfs within 33\npc of the Sun. Unfortunately, identifying transits of such planets in\nphotometric monitoring is complicated both by the intrinsic stellar variability\nthat is common among these stars and by the nocturnal cadence, atmospheric\nvariations, and instrumental systematics that often plague Earth-bound\nobservatories. Here we summarize the properties of MEarth data gathered so far,\nand we present a new framework to detect shallow exoplanet transits in wiggly\nand irregularly-spaced light curves. In contrast to previous methods that clean\ntrends from light curves before searching for transits, this framework assesses\nthe significance of individual transits simultaneously while modeling\nvariability, systematics, and the photometric quality of individual nights. Our\nMethod for Including Starspots and Systematics in the Marginalized Probability\nof a Lone Eclipse (MISS MarPLE) uses a computationally efficient semi-Bayesian\napproach to explore the vast probability space spanned by the many parameters\nof this model, naturally incorporating the uncertainties in these parameters\ninto its evaluation of candidate events. We show how to combine individual\ntransits processed by MISS MarPLE into periodic transiting planet candidates\nand compare our results to the popular Box-fitting Least Squares (BLS) method\nwith simulations. By applying MISS MarPLE to observations from the MEarth\nProject, we demonstrate the utility of this framework for robustly assessing\nthe false alarm probability of transit signals in real data. [slightly\nabridged]", "cat": "astro-ph.EP", "authors": ["Zachory K. Berta", "Jonathan Irwin", "David Charbonneau", "Christopher J. Burke", "Emilio E. Falco"]}, "525": {"id": "1306.4336v2", "title": "The VMC survey -IX. Pilot study of the proper motion of stellar populations in the LMC from 2MASS and VISTA data", "url": "http://arxiv.org/pdf/1306.4336v2", "date": "2013-11-01 14:07:23", "abs": "We use multi-epoch near-infrared observations from the VISTA survey of the\nMagellanic Cloud system (VMC) to measure the proper motion of stars of the LMC,\nin one tile of 1.5 deg^2 centred at (alpha, delta) = (05:59:23.136,\n-66:20:28.68) and including the South Ecliptic Pole, with respect to their\n2MASS position over a time baseline of ~10 years and from VMC observations\nonly, spanning a time range of ~1 year. Stars of different ages are selected\nfrom the (J-Ks) vs. Ks diagram and their average coordinate displacement is\ncomputed from the difference between Ks band observations for stars as faint as\nKs=19 mag. Proper motions are derived by averaging up to seven 2MASS-VMC\ncombinations in the first case and from the slope of the best fit line among\nthe seven VMC epochs in the second case. Separate proper motion values are\nobtained for variable stars in the field. The proper motion of ~40,000 LMC\nstars in the tile, with respect to ~8000 background galaxies, obtained from VMC\ndata alone, is mu_alpha cos(delta) = +2.20+/-0.06 (stat) +/-0.29 (sys) and\nmu_delta = +1.70+/-0.06 (stat) +/-0.30 (sys) mas/yr. This value agrees with\nrecent ground-based determinations in a nearby field but is larger than studies\nwith the HST; the cause of this discrepancy may be due to additional systematic\nerrors in the data. The LMC proper motion is also clearly distinct from the\nproper motion derived for stars of the Milky Way. The relative proper motion\nbetween the foreground stars and the LMC stars is ~5 mas/yr. Furthermore, we\nmeasure a decrease of the proper motion with increasing logarithm of stellar\nage for LMC stars. This study, based on just one VMC tile, shows the potential\nof the 2MASS-VMC and VMC-VMC combinations for a comprehensive investigation of\nthe proper motion across the Magellanic system. (Abridged)", "cat": "astro-ph.GA", "authors": ["M. -R. L. Cioni", "L. Girardi", "M. I. Moretti", "T. Piffl", "V. Ripepi", "S. Rubele", "R. -D. Scholz", "K. Bekki", "G. Clementini", "V. D. Ivanov", "J. M. Oliveira", "J. Th. van Loon"]}, "526": {"id": "1608.04378v3", "title": "Hadronic matter at the edge: A survey of some theoretical approaches to the physics of the QCD phase diagram", "url": "http://arxiv.org/pdf/1608.04378v3", "date": "2016-08-19 19:34:17", "abs": "In the past few years a wealth of high quality data has made possible to test\ncurrent theoretical ideas about the properties of hadrons subject to extreme\nconditions of density and temperature. The relativistic heavy-ion program\ncarried out at the CERN-SPS and under development at the BNL-RHIC and CERN-LHC\nhas provided results that probe the evolution of collisions of hadronic matter\nat high energies from the initially large density to the late dilute stages. In\naddition, QCD on the lattice has produced results complementing these findings\nwith first principles calculations for observables in a regime where\nperturbative techniques cannot describe the nature of strongly coupled systems.\nThis work aims to review some recent developments that make use of field\ntheoretical methods to describe the physics of hadrons at finite temperature\nand density. I concentrate on two of the main topics that have been explored in\nthe last few years: (1) The search for the structure of the phase diagram and\n(2) analytical signals linked to the chiral symmetry restoration/deconfinement.", "cat": "hep-ph", "authors": ["Alejandro Ayala"]}, "527": {"id": "2109.09478v1", "title": "A Survey of Text Games for Reinforcement Learning informed by Natural Language", "url": "http://arxiv.org/pdf/2109.09478v1", "date": "2021-09-20 12:32:57", "abs": "Reinforcement Learning has shown success in a number of complex virtual\nenvironments. However, many challenges still exist towards solving problems\nwith natural language as a core component. Interactive Fiction Games (or Text\nGames) are one such problem type that offer a set of partially observable\nenvironments where natural language is required as part of the reinforcement\nlearning solutions.\n Therefore, this survey's aim is to assist in the development of new Text Game\nproblem settings and solutions for Reinforcement Learning informed by natural\nlanguage. Specifically, this survey summarises: 1) the challenges introduced in\nText Game Reinforcement Learning problems, 2) the generation tools for\nevaluating Text Games and the subsequent environments generated and, 3) the\nagent architectures currently applied are compared to provide a systematic\nreview of benchmark methodologies and opportunities for future researchers.", "cat": "cs.AI", "authors": ["Philip Osborne", "Heido N\u00f5mm", "Andre Freitas"]}, "528": {"id": "1906.07332v1", "title": "Bo\u00f6tes IV: A New Milky Way Satellite Discovered in the Subaru Hyper Suprime-Cam Survey and Implications for the Missing Satellite Problem", "url": "http://arxiv.org/pdf/1906.07332v1", "date": "2019-06-18 01:35:24", "abs": "We report on the discovery of a new Milky Way (MW) satellite in Bo\\\"otes\nbased on data from the on-going Hyper Suprime-Cam (HSC) Subaru Strategic\nProgram (SSP). This satellite, named Bo\\\"otes IV, is the third ultra-faint\ndwarf that we have discovered in the HSC-SSP. We have identified a\nstatistically significant (32.3$\\sigma$) overdensity of stars having\ncharacteristics of a metal-poor, old stellar population. The distance to this\nstellar system is $D_{\\odot}=209^{+20}_{-18}$ kpc with a $V$-band absolute\nmagnitude of $M_V=-4.53^{+0.23}_{-0.21}$ mag. Bo\\\"otes IV has a half-light\nradius of $r_h=462^{+98}_{-84}$ pc and an ellipticity of\n$0.64^{+0.05}_{-0.05}$, which clearly suggests that this is a dwarf satellite\ngalaxy. We also found another overdensity that appears to be a faint globular\ncluster with $M_V=-0.20^{+0.59}_{-0.83}$ mag and $r_h=5.9^{+1.5}_{-1.3}$ pc\nlocated at $D_{\\odot}=46^{+4}_{-4}$ kpc. Adopting the recent prediction for the\ntotal population of satellites in a MW-sized halo by Newton et al. (2018),\nwhich combined the characteristics of the observed satellites by SDSS and DES\nwith the subhalos obtained in $\\Lambda$CDM models, we estimate that there\nshould be about two MW satellites at $M_V\\le0$ in the $\\sim676$ deg$^2$ covered\nby HSC-SSP, whereas that area includes six satellites. Thus, the observed\nnumber of satellites is larger than the theoretical prediction. On the face of\nit, we have a problem of too many satellites, instead of the well-known missing\nsatellites problem whereby the $\\Lambda$CDM theory overpredicts the number of\nsatellites in a MW-sized halo. This may imply that the models need more\nrefinements for the assignment of subhalos to satellites such as considering\nthose found by the current deeper survey. [abridged]", "cat": "astro-ph.GA", "authors": ["Daisuke Homma", "Masashi Chiba", "Yutaka Komiyama", "Masayuki Tanaka", "Sakurako Okamoto", "Mikito Tanaka", "Miho N. Ishigaki", "Kohei Hayashi", "Nobuo Arimoto", "Scott G. Carlsten", "Robert H. Lupton", "Michael A. Strauss", "Satoshi Miyazaki", "Gabriel Torrealba", "Shiang-Yu Wang", "Hitoshi Murayama"]}, "529": {"id": "2106.15518v1", "title": "An expert survey to assess the current status and future challenges of energy system analysis", "url": "http://arxiv.org/pdf/2106.15518v1", "date": "2021-06-22 09:23:58", "abs": "Decision support systems like computer-aided energy system analysis (ESA) are\nconsidered one of the main pillars for developing sustainable and reliable\nenergy transformation strategies. Although today's diverse tools can already\nsupport decision-makers in a variety of research questions, further\ndevelopments are still necessary. Intending to identify opportunities and\nchallenges in the field, we classify modelling capabilities (32), methodologies\n(15) implementation issues (15) and management issues (7) from an extensive\nliterature review. Based on a quantitative expert survey of energy system\nmodellers (N=61) mainly working with simulation and optimisation models, the\nstatus of development and the complexity of realisation of those modelling\ntopics are assessed. While the rated items are considered to be more complex\nthan actually represented, no significant outliers are determinable, showing\nthat there is no consensus about particular aspects of ESA that are lacking\ndevelopment. Nevertheless, a classification of the items in terms of a\nspecially defined modelling strategy matrix identifies capabilities like\nland-use planning patterns, equity and distributional effects and endogenous\ntechnological learning as \"low hanging fruits\" for enhancement, as well as a\nlarge number of complex topics that are already well implemented. The remaining\n\"tough nuts\" regarding modelling capabilities include non-energy sector and\nsocial behaviour interaction effects. In general, the optimisation and\nsimulation models differ in their respective strengths, justifying the\nexistence of both. While methods were generally rated as quite well developed,\ncombinatorial optimisation approaches, as well as machine learning, are\nidentified as important research methods to be developed further for ESA.", "cat": "physics.soc-ph", "authors": ["Fabian Scheller", "Frauke Wiese", "Jann Michael Weinand", "Dominik Franjo Dominkovi\u0107", "Russell McKenna"]}, "530": {"id": "1111.6596v2", "title": "Thinking Outside the Box: Effects of Modes Larger than the Survey on Matter Power Spectrum Covariance", "url": "http://arxiv.org/pdf/1111.6596v2", "date": "2012-03-27 10:00:16", "abs": "Considering the matter power spectrum covariance matrix, it has recently been\nfound that there is a potentially dominant effect on mildly non-linear scales\ndue to power in modes of size equal to and larger than the survey volume. This\n{\\it beat coupling} effect has been derived analytically in perturbation theory\nand while it has been tested with simulations, some questions remain\nunanswered. Moreover, there is an additional effect of these large modes, which\nhas so far not been included in analytic studies, namely the effect on the\nestimated {\\it average} density which enters the power spectrum estimate. In\nthis article, we work out analytic, perturbation theory based expressions\nincluding both the beat coupling and this {\\it local average effect} and we\nshow that while, when isolated, beat coupling indeed causes large excess\ncovariance in agreement with the literature, in a realistic scenario this is\ncompensated almost entirely by the local average effect, leaving only $\\sim 10\n%$ of the excess. We test our analytic expressions by comparison to a suite of\nlarge N-body simulations. For the variances, we find excellent agreement with\nthe analytic expressions for $k < 0.2 h$Mpc$^{-1}$ at $z=0.5$, while the\ncorrelation coefficients agree to beyond $k=0.4 h$Mpc$^{-1}$. As expected, the\nrange of agreement increases towards higher redshift and decreases slightly\ntowards $z=0$. We finish by including the large-mode effects in a full\ncovariance matrix description for arbitrary survey geometry and confirming its\nvalidity using simulations. This may be useful as a stepping stone towards\nbuilding an actual galaxy (or other tracer's) power spectrum covariance matrix.\n[abridged]", "cat": "astro-ph.CO", "authors": ["Roland de Putter", "Christian Wagner", "Olga Mena", "Licia Verde", "Will Percival"]}, "531": {"id": "2310.03321v1", "title": "Hunting Gamma-ray emitting FR0 radio galaxies in wide-field sky surveys", "url": "http://arxiv.org/pdf/2310.03321v1", "date": "2023-10-05 05:31:24", "abs": "The latest entry in the jetted active galactic nuclei (AGN) family is the\nFanaroff-Riley type 0 (FR0) radio galaxies. They share several observational\ncharacteristics, e.g., nuclear emission and host galaxy morphology, with FR I\nsources; however, they lack extended, kiloparsec-scale radio structures, which\nare the defining features of canonical FR I and II sources. Here we report the\nidentification of 7 gamma-ray emitting AGN as FR0 radio sources by utilizing\nthe high-quality observations delivered by ongoing multi-wavelength wide-field\nsky surveys, e.g., Very Large Array Sky Survey. The broadband observational\nproperties of these objects are found to be similar to their gamma-ray\nundetected counterparts. In the gamma-ray band, FR0 radio galaxies exhibit\nspectral features similar to more common FR I and II radio galaxies, indicating\na common gamma-ray production mechanism and the presence of misaligned jets.\nAlthough the parsec-scale radio structure of FR0s generally exhibits a wide\nrange, with about half having emission on opposite sides of the core, the\ngamma-ray detected FR0s tend to have dominant cores with core-jet structures.\nWe conclude that dedicated, high-resolution observations are needed to unravel\nthe origin of relativistic jets in this enigmatic class of faint yet numerous\npopulation of compact radio sources.", "cat": "astro-ph.HE", "authors": ["Meghana Pannikkote", "Vaidehi S. Paliya", "D. J. Saikia"]}, "532": {"id": "1808.04466v1", "title": "A survey of some of the recent developments in Leavitt path algebras", "url": "http://arxiv.org/pdf/1808.04466v1", "date": "2018-08-13 20:59:07", "abs": "This survey of the recent developments in the investigations of a Leavitt\npath algebra L of an arbitrary graph E over a field K consists of two parts. In\nthe first part describes how very often a single graph property of E implies\nmultiple ring properties of L, thus making Leavitt path algebras effective\ntools in constructing rings of various desirable properties. The second part\ndescribes methods of constructing simple modules over L and characterizes\nLeavitt path algebras all of whose simple modules possess some specific\nproperties such as being flat, finitely presented,being graded, injective etc.", "cat": "math.RA", "authors": ["Kulumani M. Rangaswamy"]}, "533": {"id": "2310.15826v1", "title": "One or Two Things We know about Concept Drift -- A Survey on Monitoring Evolving Environments", "url": "http://arxiv.org/pdf/2310.15826v1", "date": "2023-10-24 13:25:19", "abs": "The world surrounding us is subject to constant change. These changes,\nfrequently described as concept drift, influence many industrial and technical\nprocesses. As they can lead to malfunctions and other anomalous behavior, which\nmay be safety-critical in many scenarios, detecting and analyzing concept drift\nis crucial. In this paper, we provide a literature review focusing on concept\ndrift in unsupervised data streams. While many surveys focus on supervised data\nstreams, so far, there is no work reviewing the unsupervised setting. However,\nthis setting is of particular relevance for monitoring and anomaly detection\nwhich are directly applicable to many tasks and challenges in engineering. This\nsurvey provides a taxonomy of existing work on drift detection. Besides, it\ncovers the current state of research on drift localization in a systematic way.\nIn addition to providing a systematic literature review, this work provides\nprecise mathematical definitions of the considered problems and contains\nstandardized experiments on parametric artificial datasets allowing for a\ndirect comparison of different strategies for detection and localization.\nThereby, the suitability of different schemes can be analyzed systematically\nand guidelines for their usage in real-world scenarios can be provided.\nFinally, there is a section on the emerging topic of explaining concept drift.", "cat": "cs.LG", "authors": ["Fabian Hinder", "Valerie Vaquet", "Barbara Hammer"]}, "534": {"id": "1212.4363v1", "title": "Mirror symmetry breaking with limited enantioselective autocatalysis and temperature gradients: a stability survey", "url": "http://arxiv.org/pdf/1212.4363v1", "date": "2012-12-18 14:33:46", "abs": "We analyze limited enantioselective (LES) autocatalysis in a temperature\ngradient and with internal flow/recycling of hot and cold material.\nMicroreversibility forbids broken mirror symmetry for LES in the presence of a\ntemperature gradient alone. This symmetry can be broken however when the\nauto-catalysis and limited enantioselective catalysis are each localized within\nthe regions of low and high temperature, respectively. This scheme has been\nrecently proposed as a plausible model for spontaneous emergence of chirality\nin abyssal hydrothermal vents. Regions in chemical parameter space are mapped\nout in which the racemic state is unstable and bifurcates to chiral solutions.", "cat": "physics.chem-ph", "authors": ["Celia Blanco", "Josep M. Rib\u00f3", "Joaquim Crusats", "Zoubir El-Hachemi", "Albert Moyano", "David Hochberg"]}, "535": {"id": "1404.5508v1", "title": "Discovery of new magnetic early-B stars within the MiMeS HARPSpol survey", "url": "http://arxiv.org/pdf/1404.5508v1", "date": "2014-04-22 14:18:08", "abs": "To understand the origin of the magnetic fields in massive stars as well as\ntheir impact on stellar internal structure, evolution, and circumstellar\nenvironment, within the MiMeS project, we searched for magnetic objects among a\nlarge sample of massive stars, and build a sub-sample for in-depth follow-up\nstudies required to test the models and theories of fossil field origins,\nmagnetic wind confinement and magnetospheric properties, and magnetic star\nevolution.\n We obtained high-resolution spectropolarimetric observations of a large\nnumber of OB stars thanks to three large programs that have been allocated on\nthe high-resolution spectropolarimeters ESPaDOnS, Narval, and the polarimetric\nmodule HARPSpol of the HARPS spectrograph. We report here on the methods and\nfirst analysis of the HARPSpol magnetic detections. We identified the magnetic\nstars using a multi-line analysis technique. Then, when possible, we monitored\nthe new discoveries to derive their rotation periods, which are critical for\nfollow-up and magnetic mapping studies. We also performed a first-look analysis\nof their spectra and identified obvious spectral anomalies (e.g., abundance\npeculiarities, Halpha emission), which are also of interest for future studies.\n In this paper, we focus on eight of the 11 stars in which we discovered or\nconfirmed a magnetic field from the HARPSpol LP sample (the remaining three\nwere published in a previous paper). Seven of the stars were detected in\nearly-type Bp stars, while the last star was detected in the Ap companion of a\nnormal early B-type star. We report obvious spectral and multiplicity\nproperties, as well as our measurements of their longitudinal field strengths,\nand their rotation periods when we are able to derive them. We also discuss the\npresence or absence of Halpha emission with respect to the theory of\ncentrifugally-supported magnetospheres. (Abriged)", "cat": "astro-ph.SR", "authors": ["E. Alecian", "O. Kochukhov", "V. Petit", "J. Grunhut", "J. Landstreet", "M. E. Oksala", "G. A. Wade", "G. Hussain", "C. Neiner", "D. Bohlender", "the MiMeS Collaboration"]}, "536": {"id": "2406.05424v1", "title": "Recent advancements in computational morphology : A comprehensive survey", "url": "http://arxiv.org/pdf/2406.05424v1", "date": "2024-06-08 10:07:33", "abs": "Computational morphology handles the language processing at the word level.\nIt is one of the foundational tasks in the NLP pipeline for the development of\nhigher level NLP applications. It mainly deals with the processing of words and\nword forms. Computational Morphology addresses various sub problems such as\nmorpheme boundary detection, lemmatization, morphological feature tagging,\nmorphological reinflection etc. In this paper, we present exhaustive survey of\nthe methods for developing computational morphology related tools. We survey\nthe literature in the chronological order starting from the conventional\nmethods till the recent evolution of deep neural network based approaches. We\nalso review the existing datasets available for this task across the languages.\nWe discuss about the effectiveness of neural model compared with the\ntraditional models and present some unique challenges associated with building\nthe computational morphology tools. We conclude by discussing some recent and\nopen research issues in this field.", "cat": "cs.CL", "authors": ["Jatayu Baxi", "Brijesh Bhatt"]}, "537": {"id": "2105.04703v2", "title": "Friends and Foes: Conditional Occurrence Rates of Exoplanet Companions and their Impact on Radial Velocity Follow-up Surveys", "url": "http://arxiv.org/pdf/2105.04703v2", "date": "2021-10-06 23:19:24", "abs": "Population studies of Kepler's multi-planet systems have revealed a\nsurprising degree of structure in their underlying architectures. Information\nfrom a detected transiting planet can be combined with a population model to\nmake predictions about the presence and properties of additional planets in the\nsystem. Using a statistical model for the distribution of planetary systems (He\net al. 2020; arXiv:2007.14473), we compute the conditional occurrence of\nplanets as a function of the period and radius of Kepler-detectable planets.\nAbout half ($0.52 \\pm 0.03$) of the time, the detected planet is not the planet\nwith the largest semi-amplitude $K$ in the system, so efforts to measure the\nmass of the transiting planet with radial velocity (RV) follow-up will have to\ncontend with additional planetary signals in the data. We simulate RV\nobservations to show that assuming a single-planet model to measure the $K$ of\nthe transiting planet often requires significantly more observations than in\nthe ideal case with no additional planets, due to the systematic errors from\nunseen planet companions. Our results show that planets around 10-day periods\nwith $K$ close to the single-measurement RV precision ($\\sigma_{1,\\rm obs}$)\ntypically require $\\sim 100$ observations to measure their $K$ to within 20%\nerror. For a next generation RV instrument achieving $\\sigma_{1,\\rm obs} = 10$\ncm/s, about $\\sim 200$ ($600$) observations are needed to measure the $K$ of a\ntransiting Venus in a Kepler-like system to better than 20% (10%) error, which\nis $\\sim 2.3$ times as many as what would be necessary for a Venus without any\nplanetary companions.", "cat": "astro-ph.EP", "authors": ["Matthias Y. He", "Eric B. Ford", "Darin Ragozzine"]}, "538": {"id": "1607.04828v2", "title": "Using 21-cm absorption surveys to measure the average HI spin temperature in distant galaxies", "url": "http://arxiv.org/pdf/1607.04828v2", "date": "2016-08-06 12:32:21", "abs": "We present a statistical method for measuring the average HI spin temperature\nin distant galaxies using the expected detection yields from future wide-field\n21cm absorption surveys. As a demonstrative case study we consider a simulated\nall-southern-sky survey of 2-h per pointing with the Australian Square\nKilometre Array Pathfinder for intervening HI absorbers at intermediate\ncosmological redshifts between $z = 0.4$ and $1$. For example, if such a survey\nyielded $1000$ absorbers we would infer a harmonic-mean spin temperature of\n$\\overline{T}_\\mathrm{spin} \\sim 100$K for the population of damped Lyman\n$\\alpha$ (DLAs) absorbers at these redshifts, indicating that more than $50$\nper cent of the neutral gas in these systems is in a cold neutral medium (CNM).\nConversely, a lower yield of only 100 detections would imply\n$\\overline{T}_\\mathrm{spin} \\sim 1000$K and a CNM fraction less than $10$ per\ncent. We propose that this method can be used to provide independent\nverification of the spin temperature evolution reported in recent 21cm surveys\nof known DLAs at high redshift and for measuring the spin temperature at\nintermediate redshifts below $z \\approx 1.7$, where the Lyman-$\\alpha$ line is\ninaccessible using ground-based observatories. Increasingly more sensitive and\nlarger surveys with the Square Kilometre Array should provide stronger\nstatistical constraints on the average spin temperature. However, these will\nultimately be limited by the accuracy to which we can determine the HI column\ndensity frequency distribution, the covering factor and the redshift\ndistribution of the background radio source population.", "cat": "astro-ph.GA", "authors": ["J. R. Allison", "M. A. Zwaan", "S. W. Duchesne", "S. J. Curran"]}, "539": {"id": "2109.12404v1", "title": "Deep learning tackles single-cell analysis A survey of deep learning for scRNA-seq analysis", "url": "http://arxiv.org/pdf/2109.12404v1", "date": "2021-09-25 17:08:06", "abs": "Since its selection as the method of the year in 2013, single-cell\ntechnologies have become mature enough to provide answers to complex research\nquestions. With the growth of single-cell profiling technologies, there has\nalso been a significant increase in data collected from single-cell profilings,\nresulting in computational challenges to process these massive and complicated\ndatasets. To address these challenges, deep learning (DL) is positioning as a\ncompetitive alternative for single-cell analyses besides the traditional\nmachine learning approaches. Here we present a processing pipeline of\nsingle-cell RNA-seq data, survey a total of 25 DL algorithms and their\napplicability for a specific step in the processing pipeline. Specifically, we\nestablish a unified mathematical representation of all variational autoencoder,\nautoencoder, and generative adversarial network models, compare the training\nstrategies and loss functions for these models, and relate the loss functions\nof these models to specific objectives of the data processing step. Such\npresentation will allow readers to choose suitable algorithms for their\nparticular objective at each step in the pipeline. We envision that this survey\nwill serve as an important information portal for learning the application of\nDL for scRNA-seq analysis and inspire innovative use of DL to address a broader\nrange of new challenges in emerging multi-omics and spatial single-cell\nsequencing.", "cat": "q-bio.GN", "authors": ["Mario Flores", "Zhentao Liu", "Ting-He Zhang", "Md Musaddaqui Hasib", "Yu-Chiao Chiu", "Zhenqing Ye", "Karla Paniagua", "Sumin Jo", "Jianqiu Zhang", "Shou-Jiang Gao", "Yu-Fang Jin", "Yidong Chen", "Yufei Huang"]}, "540": {"id": "1803.05447v1", "title": "The Origin of Faint Tidal Features Around Galaxies in the RESOLVE Survey", "url": "http://arxiv.org/pdf/1803.05447v1", "date": "2018-03-14 18:01:02", "abs": "We study tidal features (TFs) around galaxies in the REsolved Spectroscopy of\na Local VolumE (RESOLVE) survey. Our sample consists of 1048 RESOLVE galaxies\nthat overlap with the DECam Legacy Survey, which reaches an r-band 3$\\sigma$\ndepth of $\\sim$27.9 mag arcsec$^{-2}$ for a 100 arcsec$^{2}$ feature. Images\nwere masked, smoothed, and inspected for TFs like streams, shells, or\ntails/arms. We find TFs in 17$^{\\pm 2} \\%$ of our galaxies, setting a lower\nlimit on the true frequency. The frequency of TFs in the gas-poor\n(gas-to-stellar mass ratio $<$ 0.1) subsample is lower than in the gas-rich\nsubsample (13$^{\\pm 3} \\%$ vs. 19$^{\\pm 2} \\%$). Within the gas-poor subsample,\ngalaxies with TFs have higher stellar and halo masses, $\\sim 3\\times$ closer\ndistances to nearest neighbors (in the same group), and possibly fewer group\nmembers at fixed halo mass than galaxies without TFs, but similar specific star\nformation rates. These results suggest TFs in gas-poor galaxies are typically\nstreams/shells from dry mergers or satellite disruption. In contrast, the\npresence of TFs around gas-rich galaxies does not correlate with stellar or\nhalo mass, suggesting these TFs are often tails/arms from resonant\ninteractions. Similar to TFs in gas-poor galaxies, TFs in gas-rich galaxies\nimply 1.7x closer nearest neighbors in the same group; however, TFs in gas-rich\ngalaxies are associated with diskier morphologies, higher star formation rates,\nand higher gas content. In addition to interactions with known neighbors, we\nsuggest that TFs in gas-rich galaxies may arise from accretion of cosmic gas\nand/or gas-rich satellites below the survey limit.", "cat": "astro-ph.GA", "authors": ["Callie E. Hood", "Sheila J. Kannappan", "David V. Stark", "Ian P. Dell'Antonio", "Amanda J. Moffett", "Kathleen D. Eckert", "Mark A. Norris", "David Hendel"]}, "541": {"id": "1705.00622v2", "title": "The bright-star masks for the HSC-SSP survey", "url": "http://arxiv.org/pdf/1705.00622v2", "date": "2017-06-02 14:19:31", "abs": "We present the procedure to build and validate the bright-star masks for the\nHyper-Suprime-Cam Strategic Subaru Proposal (HSC-SSP) survey. To identify and\nmask the saturated stars in the full HSC-SSP footprint, we rely on the Gaia and\nTycho-2 star catalogues. We first assemble a pure star catalogue down to\n$G_{\\rm Gaia} < 18$ after removing $\\sim1.5\\%$ of sources that appear extended\nin the Sloan Digital Sky Survey (SDSS). We perform visual inspection on the\nearly data from the S16A internal release of HSC-SSP, finding that our star\ncatalogue is $99.2\\%$ pure down to $G_{\\rm Gaia} < 18$. Second, we build the\nmask regions in an automated way using stacked detected source measurements\naround bright stars binned per $G_{\\rm Gaia}$ magnitude. Finally, we validate\nthose masks from visual inspection and comparison with the literature of galaxy\nnumber counts and angular two-point correlation functions. This version\n(Arcturus) supersedes the previous version (Sirius) used in the S16A internal\nand DR1 public releases. We publicly release the full masks and tools to flag\nobjects in the entire footprint of the planned HSC-SSP observations at this\naddress: ftp://obsftp.unige.ch/pub/coupon/brightStarMasks/HSC-SSP/.", "cat": "astro-ph.IM", "authors": ["Jean Coupon", "Nicole Czakon", "James Bosch", "Yutaka Komiyama", "Elinor Medezinski", "Satoshi Miyazaki", "Masamune Oguri"]}, "542": {"id": "1801.02201v2", "title": "A survey on software testability", "url": "http://arxiv.org/pdf/1801.02201v2", "date": "2018-12-06 16:29:54", "abs": "Context: Software testability is the degree to which a software system or a\nunit under test supports its own testing. To predict and improve software\ntestability, a large number of techniques and metrics have been proposed by\nboth practitioners and researchers in the last several decades. Reviewing and\ngetting an overview of the entire state-of-the-art and state-of-the-practice in\nthis area is often challenging for a practitioner or a new researcher.\nObjective: Our objective is to summarize the body of knowledge in this area and\nto benefit the readers (both practitioners and researchers) in preparing,\nmeasuring and improving software testability. Method: To address the above\nneed, the authors conducted a survey in the form of a systematic literature\nmapping (classification) to find out what we as a community know about this\ntopic. After compiling an initial pool of 303 papers, and applying a set of\ninclusion/exclusion criteria, our final pool included 208 papers. Results: The\narea of software testability has been comprehensively studied by researchers\nand practitioners. Approaches for measurement of testability and improvement of\ntestability are the most-frequently addressed in the papers. The two most often\nmentioned factors affecting testability are observability and controllability.\nCommon ways to improve testability are testability transformation, improving\nobservability, adding assertions, and improving controllability. Conclusion:\nThis paper serves for both researchers and practitioners as an \"index\" to the\nvast body of knowledge in the area of testability. The results could help\npractitioners measure and improve software testability in their projects.", "cat": "cs.SE", "authors": ["Vahid Garousi", "Michael Felderer", "Feyza Nur Kilicaslan"]}, "543": {"id": "2303.10868v3", "title": "Retrieving Multimodal Information for Augmented Generation: A Survey", "url": "http://arxiv.org/pdf/2303.10868v3", "date": "2023-12-01 02:58:09", "abs": "As Large Language Models (LLMs) become popular, there emerged an important\ntrend of using multimodality to augment the LLMs' generation ability, which\nenables LLMs to better interact with the world. However, there lacks a unified\nperception of at which stage and how to incorporate different modalities. In\nthis survey, we review methods that assist and augment generative models by\nretrieving multimodal knowledge, whose formats range from images, codes,\ntables, graphs, to audio. Such methods offer a promising solution to important\nconcerns such as factuality, reasoning, interpretability, and robustness. By\nproviding an in-depth review, this survey is expected to provide scholars with\na deeper understanding of the methods' applications and encourage them to adapt\nexisting techniques to the fast-growing field of LLMs.", "cat": "cs.CL", "authors": ["Ruochen Zhao", "Hailin Chen", "Weishi Wang", "Fangkai Jiao", "Xuan Long Do", "Chengwei Qin", "Bosheng Ding", "Xiaobao Guo", "Minzhi Li", "Xingxuan Li", "Shafiq Joty"]}, "544": {"id": "1104.0712v1", "title": "Non-Gravitational Contributions to the Clustering of Ly-alpha Selected Galaxies: Implications for Cosmological Surveys", "url": "http://arxiv.org/pdf/1104.0712v1", "date": "2011-04-04 23:53:17", "abs": "We show that the dependence of Ly-alpha absorption on environment leads to\nsignificant non-gravitational features in the redshift space power-spectrum of\nLy-alpha selected galaxies. We derive a physically motivated fitting formula\nthat can be included in clustering analyses, and use this to discuss the\npredicted features in the Ly-alpha galaxy power-spectrum based on detailed\nmodels in which Ly-alpha absorption is influenced by gas infall and/or by\nstrong galactic outflows. We show that power-spectrum measurements could be\nused to study the astrophysics of the galaxy-IGM connection, and to measure the\nproperties of outflows from star-forming galaxies. Applying the modified\nredshift space power-spectrum to a Ly-alpha survey with parameters\ncorresponding to the planned Hobby-Eberly Telescope Dark Energy Experiment\n(HETDEX), we find that the dependence of observed Ly-alpha flux on velocity\ngradient and ionising background may compromise the ability of Ly-alpha\nselected galaxy redshift surveys to constrain cosmology using information from\nthe full power-spectrum. This is because the effects of fluctuating ionizing\nbackground and velocity gradients effect the shape of the observed\npower-spectrum in ways that are similar to the shape of the primordial\npower-spectrum and redshift space distortions respectively. We use the\nAlcock-Paczynski test to show that without prior knowledge of the details of\nLy-alpha absorption in the IGM, the precision of line-of-sight and transverse\ndistance measurements for HETDEX will be ~1.3-1.7%, decreased by a factor of\n~1.5-2 relative to the best case precision of ~0.8% available in a traditional\ngalaxy redshift survey. We specify the precision with which modelling of\nLy-alpha radiative transfer must be understood in order for HETDEX to achieve\ndistance measurements that are better than 1%.", "cat": "astro-ph.CO", "authors": ["Stuart Wyithe", "Mark Dijkstra"]}, "545": {"id": "2407.00783v1", "title": "Diffusion Models and Representation Learning: A Survey", "url": "http://arxiv.org/pdf/2407.00783v1", "date": "2024-06-30 17:59:58", "abs": "Diffusion Models are popular generative modeling methods in various vision\ntasks, attracting significant attention. They can be considered a unique\ninstance of self-supervised learning methods due to their independence from\nlabel annotation. This survey explores the interplay between diffusion models\nand representation learning. It provides an overview of diffusion models'\nessential aspects, including mathematical foundations, popular denoising\nnetwork architectures, and guidance methods. Various approaches related to\ndiffusion models and representation learning are detailed. These include\nframeworks that leverage representations learned from pre-trained diffusion\nmodels for subsequent recognition tasks and methods that utilize advancements\nin representation and self-supervised learning to enhance diffusion models.\nThis survey aims to offer a comprehensive overview of the taxonomy between\ndiffusion models and representation learning, identifying key areas of existing\nconcerns and potential exploration. Github link:\nhttps://github.com/dongzhuoyao/Diffusion-Representation-Learning-Survey-Taxonomy", "cat": "cs.CV", "authors": ["Michael Fuest", "Pingchuan Ma", "Ming Gui", "Johannes S. Fischer", "Vincent Tao Hu", "Bjorn Ommer"]}, "546": {"id": "1810.03360v1", "title": "A Survey on Periocular Biometrics Research", "url": "http://arxiv.org/pdf/1810.03360v1", "date": "2018-10-08 10:15:15", "abs": "Periocular refers to the facial region in the vicinity of the eye, including\neyelids, lashes and eyebrows. While face and irises have been extensively\nstudied, the periocular region has emerged as a promising trait for\nunconstrained biometrics, following demands for increased robustness of face or\niris systems. With a surprisingly high discrimination ability, this region can\nbe easily obtained with existing setups for face and iris, and the requirement\nof user cooperation can be relaxed, thus facilitating the interaction with\nbiometric systems. It is also available over a wide range of distances even\nwhen the iris texture cannot be reliably obtained (low resolution) or under\npartial face occlusion (close distances). Here, we review the state of the art\nin periocular biometrics research. A number of aspects are described,\nincluding: i) existing databases, ii) algorithms for periocular detection\nand/or segmentation, iii) features employed for recognition, iv) identification\nof the most discriminative regions of the periocular area, v) comparison with\niris and face modalities, vi) soft-biometrics (gender/ethnicity\nclassification), and vii) impact of gender transformation and plastic surgery\non the recognition accuracy. This work is expected to provide an insight of the\nmost relevant issues in periocular biometrics, giving a comprehensive coverage\nof the existing literature and current state of the art.", "cat": "cs.CV", "authors": ["Fernando Alonso-Fernandez", "Josef Bigun"]}, "547": {"id": "1607.02291v3", "title": "A Survey of Cellular Automata: Types, Dynamics, Non-uniformity and Applications", "url": "http://arxiv.org/pdf/1607.02291v3", "date": "2018-05-08 12:31:57", "abs": "Cellular automata (CAs) are dynamical systems which exhibit complex global\nbehavior from simple local interaction and computation. Since the inception of\ncellular automaton (CA) by von Neumann in 1950s, it has attracted the attention\nof several researchers over various backgrounds and fields for modelling\ndifferent physical, natural as well as real-life phenomena. Classically, CAs\nare uniform. However, non-uniformity has also been introduced in update\npattern, lattice structure, neighborhood dependency and local rule. In this\nsurvey, we tour to the various types of CAs introduced till date, the different\ncharacterization tools, the global behaviors of CAs, like universality,\nreversibility, dynamics etc. Special attention is given to non-uniformity in\nCAs and especially to non-uniform elementary CAs, which have been very useful\nin solving several real-life problems.", "cat": "cs.FL", "authors": ["Kamalika Bhattacharjee", "Nazma Naskar", "Souvik Roy", "Sukanta Das"]}, "548": {"id": "1507.04096v1", "title": "Studying Young Stars with Large Spectroscopic Surveys", "url": "http://arxiv.org/pdf/1507.04096v1", "date": "2015-07-15 06:22:05", "abs": "Galactic archaeology is the study of the history of star formation and\nchemical evolution in the Milky Way, based on present-day stellar populations.\nStudies of young stars are a key anchor point for Galactic archaeology, since\nquantities like the initial mass function and the star formation rate can be\nstudied directly in young clusters and star forming regions. Conversely,\nmassive spectroscopic Galactic archaeology surveys can be used as a data source\nfor young star studies.", "cat": "astro-ph.SR", "authors": ["Sarah L. Martell"]}, "549": {"id": "2209.01564v2", "title": "MOCCA-Survey Database: Extra Galactic Globular Clusters. III. The population of black holes in Milky Way and Andromeda-like galaxies", "url": "http://arxiv.org/pdf/2209.01564v2", "date": "2023-01-20 10:43:17", "abs": "In this work, we investigate the black hole (BH) population of globular\nclusters (GCs) in Milky Way- (MW) and Andromeda- (M31) like galaxies. We\ncombine the population synthesis code MASinGa and the MOCCA-Survey Database I\nto infer the properties of GCs harbouring a BH subsystem (BHS), an IMBH, or\nneither of those. We find that the typical number of GCs with a BHS, an IMBH,\nor none become comparable in the galactic outskirts, whilst the inner galactic\nregions are dominated by GCs without a significant dark component. Our models\nsuggest that GCs harbouring a BHS are slightly heavier and with larger\nhalf-mass radii compared to the overall population. We retrieve the properties\nof binary BHs (BBHs) that have either merged in the last 3 Gyr or survived in\ntheir parent cluster until present-day. We find that around 80\\% of the merging\nBBHs form due to dynamical interactions while the remaining originate from\nevolution of primordial binaries. We infer a merger rate for BBHs in the local\nUniverse of $1.0-23\\,\\,\\rm{yr^{-1}\\,Gpc^{-3}}$, depending on the adopted\nassumptions. We find around 100-240 BBHs survive until present-day and are\nmostly concentrated in the inner few kpc of the galaxy. We estimate also the\nnumber of BHs transported into the galactic nucleus by infalling star clusters,\nfinding around 1,000-3,000 BHs and 100-200 BBHs are transported over a time\nspan of 12 Gyr. This enables us to constrains the total amount of BHs and BBHs\nbinaries lurking in nuclear star cluster, i.e. $N_{BHs}=(1.4-2.2)\\times10^4$\nand $N_{BBHs}=700-1,100$.", "cat": "astro-ph.GA", "authors": ["A. Leveque", "M. Giersz", "A. Askar", "M. Arca-Sedda", "A. Olejak"]}, "550": {"id": "1002.0636v2", "title": "On the selection effect of radio quasars in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1002.0636v2", "date": "2010-04-19 23:51:15", "abs": "We identified a large sample of radio quasars, including those with complex\nradio morphology, from the Sloan Digital Sky Survey (SDSS) and the Faint Images\nof Radio Sky at Twenty-cm (FIRST). Using this sample, we inspect previous radio\nquasar samples for selection effects resulting from complex radio morphologies\nand adopting positional coincidence between radio and optical sources alone. We\nfind that 13.0% and 8.1% radio quasars do not show a radio core within 1.2 and\n2 arcsecs of their optical position, and thus are missed in such samples. Radio\nflux is under-estimated by a factor of more than 2 for an additional 8.7% radio\nquasars. These missing radio extended quasars are more radio loud with a\ntypical radio-to-optical flux ratio namely radio loudness RL >100, and radio\npower P >10^{25} W/Hz. They account for more than one third of all quasars with\nRL>100. The color of radio extended quasars tends to be bluer than the radio\ncompact quasars. This suggests that radio extended quasars are more radio\npowerful sources, e.g., Fanaroff-Riley type 2 (FR-II) sources, rather than the\ncompact ones viewed at larger inclination angles. By comparison with the radio\ndata from the NRAO VLA Sky Survey (NVSS), we find that for sources with total\nradio flux less than 3 mJy, low surface brightness components tend to be\nunderestimated by FIRST, indicating that lobes in these faint radio sources are\nstill missed.", "cat": "astro-ph.CO", "authors": ["Yu Lu", "Tinggui Wang", "Hongyan Zhou", "Jian Wu"]}, "551": {"id": "1307.8061v2", "title": "Optimising Spectroscopic and Photometric Galaxy Surveys: Efficient Target Selection and Survey Strategy", "url": "http://arxiv.org/pdf/1307.8061v2", "date": "2013-12-31 12:38:02", "abs": "The next generation of spectroscopic surveys will have a wealth of\nphotometric data available for use in target selection. Selecting the best\ntargets is likely to be one of the most important hurdles in making these\nspectroscopic campaigns as successful as possible. Our ability to measure dark\nenergy depends strongly on the types of targets that we are able to select with\na given photometric data set. We show in this paper that we will be able to\nsuccessfully select the targets needed for the next generation of spectroscopic\nsurveys. We also investigate the details of this selection, including\noptimisation of instrument design and survey strategy in order to measure dark\nenergy. We use color-color selection as well as neural networks to select the\nbest possible emission line galaxies and luminous red galaxies for a\ncosmological survey. Using the Fisher matrix formalism we forecast the\nefficiency of each target selection scenario. We show how the dark energy\nfigures of merit change in each target selection regime as a function of target\ntype, survey time, survey density and other survey parameters. We outline the\noptimal target selection scenarios and survey strategy choices which will be\navailable to the next generation of spectroscopic surveys.", "cat": "astro-ph.CO", "authors": ["S. Jouvel", "F. B. Abdalla", "O. Lahav", "D. Kirk", "H. Lin", "J. Annis", "R. Kron", "J. A. Frieman"]}, "552": {"id": "2308.08528v1", "title": "Survey of Bare Active Galactic Nuclei in the local universe (z < 0.2): I. On the origin of Soft-Excess", "url": "http://arxiv.org/pdf/2308.08528v1", "date": "2023-08-16 17:32:46", "abs": "We analyse a sample of 21 `bare' Seyfert~1 Active Galactic Nuclei (AGNs), a\nsub-class of Seyfert~1s, with intrinsic absorption $\\mathrm{N_{H}} \\sim\n10^{20}~ \\mathrm{cm}^{-2}$, in the local universe (z $<$ 0.2) using {\\it\nXMM-Newton} and {\\it Swift}/XRT observations. The luminosities of the primary\ncontinuum, the X-ray emission in the 3 to 10 keV energy range and the\nsoft-excess, the excess emission that appears above the low-energy\nextrapolation of the power-law fit of 3 to 10 keV X-ray spectra, are\ncalculated. Our spectral analysis reveals that the long-term intrinsic\nluminosities of the soft-excess and the primary continuum are tightly\ncorrelated $(L_{PC}\\propto L_{SE}^{1.1\\pm0.04})$. We also found that the\nluminosities are correlated for each source. This result suggests that both the\nprimary continuum and soft excess emissions exhibit a dependency on the\naccretion rate in a similar way.", "cat": "astro-ph.GA", "authors": ["Prantik Nandi", "Arka Chatterjee", "Arghajit Jana", "Sandip K. Chakrabarti", "Sachindra Naik", "Samar Safi-Harb", "Hsiang-Kuang Chang", "Jeremy Heyl"]}, "553": {"id": "2306.07839v1", "title": "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): A forming quadruple system with continuum `ribbons' and intricate outflows", "url": "http://arxiv.org/pdf/2306.07839v1", "date": "2023-06-13 15:18:59", "abs": "One of the most poorly understood aspects of low-mass star formation is how\nmultiple-star systems are formed. Here we present the results of Atacama Large\nMillimeter/submillimeter Array (ALMA) Band-6 observations towards a forming\nquadruple protostellar system, G206.93-16.61E2, in the Orion B molecular cloud.\nALMA 1.3 mm continuum emission reveals four compact objects, of which two are\nClass I young stellar objects (YSOs), and the other two are likely in\nprestellar phase. The 1.3 mm continuum emission also shows three asymmetric\nribbon-like structures that are connected to the four objects, with lengths\nranging from $\\sim$500 au to $\\sim$2200 au. By comparing our data with\nmagneto-hydrodynamic (MHD) simulations, we suggest that these ribbons trace\naccretion flows and also function as gas bridges connecting the member\nprotostars. Additionally, ALMA CO J=2-1 line emission reveals a complicated\nmolecular outflow associated with G206.93-16.61E2 with arc-like structures\nsuggestive of an outflow cavity viewed pole-on.", "cat": "astro-ph.GA", "authors": ["Qiu-yi Luo", "Tie Liu", "Aaron T. Lee", "Stella S. R. Offner", "James di Francesco", "Doug Johnstone", "Mika Juvela", "Paul F. Goldsmith", "Sheng-Li Qin", "Xiaofeng Mai", "Xun-chuan Liu", "Patricio Sanhueza", "Feng-Wei Xu", "Ken'ichi Tatematsu", "Somnath Dutta", "Huei-Ru Vivien Chen", "Shanghuo Li", "Aiyuan Yang", "Sheng-Yuan Liu", "Chin-Fei Lee", "Naomi Hirano", "Chang Won Lee", "Dipen Sahu", "Hsien Shang", "Shih-Ying Hsu", "Leonardo Bronfman", "Woojin Kwon", "M. G. Rawlings", "David Eden", "Xing Lu", "Qi-lao Gu", "Zhiyuan Ren", "D Ward-Thompson", "Zhi-Qiang Shen"]}, "554": {"id": "1709.03989v4", "title": "BAT AGN Spectroscopic Survey - V. X-ray properties of the Swift/BAT 70-month AGN catalog", "url": "http://arxiv.org/pdf/1709.03989v4", "date": "2017-11-28 11:20:51", "abs": "Hard X-ray ($\\geq 10$ keV) observations of Active Galactic Nuclei (AGN) can\nshed light on some of the most obscured episodes of accretion onto supermassive\nblack holes. The 70-month Swift/BAT all-sky survey, which probes the 14-195 keV\nenergy range, has currently detected 838 AGN. We report here on the broad-band\nX-ray (0.3-150 keV) characteristics of these AGN, obtained by combining\nXMM-Newton, Swift/XRT, ASCA, Chandra, and Suzaku observations in the soft X-ray\nband ($\\leq 10$ keV) with 70-month averaged Swift/BAT data. The non-blazar AGN\nof our sample are almost equally divided into unobscured ($N_{\\rm H}<\n10^{22}\\rm cm^{-2}$) and obscured ($N_{\\rm H}\\geq 10^{22}\\rm cm^{-2}$) AGN, and\ntheir Swift/BAT continuum is systematically steeper than the 0.3-10 keV\nemission, which suggests that the presence of a high-energy cutoff is almost\nubiquitous. We discuss the main X-ray spectral parameters obtained, such as the\nphoton index, the reflection parameter, the energy of the cutoff, neutral and\nionized absorbers, and the soft excess for both obscured and unobscured AGN.", "cat": "astro-ph.HE", "authors": ["Claudio Ricci", "Benny Trakhtenbrot", "Michael J. Koss", "Yoshihiro Ueda", "Ivan Delvecchio", "Ezequiel Treister", "Kevin Schawinski", "Stephane Paltani", "Kyuseok Oh", "Isabella Lamperti", "Simon Berney", "Poshak Gandhi", "Kohei Ichikawa", "Franz E. Bauer", "Luis C. Ho", "Daniel Asmus", "Volker Beckmann", "Simona Soldi", "Mislav Balokovic", "Neil Gehrels", "Craig B. Markwardt"]}, "555": {"id": "2005.12085v2", "title": "The Fornax Deep Survey with VST. IX. The catalog of sources in the FDS area, with an example study for globular clusters and background galaxies", "url": "http://arxiv.org/pdf/2005.12085v2", "date": "2020-09-03 14:53:49", "abs": "This paper continues the series of the Fornax Deep Survey (FDS). Following\nthe previous studies dedicated to extended Fornax cluster members, we present\nthe catalogs of compact stellar systems in the Fornax cluster as well as\nextended background sources and point-like sources. We derive ugri photometry\nof ~1.7 million sources over the $\\sim$21 sq. degree area of FDS centered on\nNGC1399. For a wider area, of $\\sim$27 sq. degs extending in the direction of\nNGC1316, we provide gri data for ~3.1 million sources. To improve the\nmorphological characterization of sources we generate multi-band image stacks\nby coadding the best seeing gri-band single exposures with a cut at FWHM<=0.9\narcsec. We use the multi-band stacks as detection frames. The identification of\ncompact sources is obtained from a combination of photometric and morphometric\nselection criteria taking as reference the properties of sources with\nwell-defined classification from the literature. We present a preliminary\nanalysis of globular cluster (GC) distributions in the Fornax area. The study\nconfirms and extends further previous results. We observe the inter-galactic\npopulation of GCs, a population of mainly blue GCs centered on NGC1399, extends\nover $\\sim$0.9Mpc, with an ellipticity $\\sim$0.65. Several sub-structures\nextend over $\\sim$0.5Mpc along various directions. Two of these structures do\nnot cross any bright galaxy; one of them appears to be connected to NGC1404, a\nbright galaxy close to the cluster core and particularly poor of GCs. Using the\ngri catalogs we analyze the GC distribution over the extended FDS area, and do\nnot find any obvious GC sub-structure bridging the two brightest cluster\ngalaxies, NGC1316 and NGC1399. Although NGC1316 is twice brighter of NGC1399 in\noptical bands we estimate a factor of 3-4 richer GC population around NGC1399\ncompared to NGC1316, out to galactocentric distances of 40 arcmin", "cat": "astro-ph.GA", "authors": ["Michele Cantiello", "Aku Venhola", "Aniello Grado", "Maurizio Paolillo", "Raffaele D'Abrusco", "Gabriella Raimondo", "Massimo Quintini", "Michael Hilker", "Steffen Mieske", "Crescenzo Tortora", "Marilena Spavone", "Massimo Capaccioli", "Enrica Iodice", "Reynier Peletier", "Jesus Falcon Barroso", "Luca Limatola", "Nicola Napolitano", "Pietro Schipani", "Glenn van de Ven", "Fabrizio Gentile", "Giovanni Covone"]}, "556": {"id": "1407.5619v1", "title": "The Starfish Diagram: Visualising Data Within the Context of Survey Samples", "url": "http://arxiv.org/pdf/1407.5619v1", "date": "2014-07-21 21:50:40", "abs": "As astronomy becomes increasingly invested in large surveys, the ample\nrepresentation of an individual target becomes a significant challenge.\nTabulations of basic properties can convey the message in an absolute sense,\nbut not within the context of the sample from which the individual is drawn. We\npresent a novel but simple plot that simultaneously visualises the properties\nof the sample and the individual. Numbers and characters are kept at an\nabsolute minimum to enable the stacking of such plots without introducing too\nmuch verbal information. Once the user becomes accustomed to their appearance,\na set of 'starfish diagrams' provide a direct representation of the individual\nwithin a sample, or between various samples. The utility and versatility of the\nplot is demonstrated through its application to astrophysical data and sports\nstatistics. We provide a brief description of the concept and the source code,\nwhich is simple to adapt to any statistical dataset, be it descriptive of\nphysics, demographics, finance, and more.", "cat": "astro-ph.IM", "authors": ["Iraklis S. Konstantopoulos"]}, "557": {"id": "1012.0782v1", "title": "UWISH2 -- The UKIRT Widefield Infrared Survey for H2", "url": "http://arxiv.org/pdf/1012.0782v1", "date": "2010-12-03 16:42:12", "abs": "We present the goals and preliminary results of an unbiased, near-infrared,\nnarrow-band imaging survey of the First Galactic Quadrant (10deg345 km/s) or small (<65 km/s) rotational velocities. Of the\ncandidate runaways, VFTS 358 (classified B0.5: V) has the largest differential\nradial velocity (-106.9 +/- 16.2 km/s), and a preliminary atmospheric analysis\nfinds a significantly enriched nitrogen abundance of 12+log(N/H) > ~8.5.\nCombined with a large rotational velocity (vsini = 345 +/- 22 km/s), this is\nsuggestive of past binary interaction for this star.", "cat": "astro-ph.SR", "authors": ["C. J. Evans", "M. B. Kennedy", "P. L. Dufton", "I. D. Howarth", "N. R. Walborn", "N. Markova", "J. S. Clark", "S. E. de Mink", "A. de Koter", "P. R. Dunstall", "V. H\u00e9nault-Brunet", "J. Ma\u00edz Apell\u00e1niz", "C. M. McEvoy", "H. Sana", "S. Sim\u00f3n-D\u00edaz", "W. D. Taylor", "J. S. Vink"]}, "560": {"id": "0907.4722v3", "title": "The Spitzer Local Volume Legacy: Survey Description and Infrared Photometry", "url": "http://arxiv.org/pdf/0907.4722v3", "date": "2009-08-20 17:31:18", "abs": "The survey description and the near-, mid-, and far-infrared flux properties\nare presented for the 258 galaxies in the Local Volume Legacy (LVL). LVL is a\nSpitzer Space Telescope legacy program that surveys the local universe out to\n11 Mpc, built upon a foundation of ultraviolet, H-alpha, and HST imaging from\n11HUGS (11 Mpc H-alpha and Ultraviolet Galaxy Survey) and ANGST (ACS Nearby\nGalaxy Survey Treasury). LVL covers an unbiased, representative, and\nstatistically robust sample of nearby star-forming galaxies, exploiting the\nhighest extragalactic spatial resolution achievable with Spitzer. As a result\nof its approximately volume-limited nature, LVL augments previous Spitzer\nobservations of present-day galaxies with improved sampling of the\nlow-luminosity galaxy population. The collection of LVL galaxies shows a large\nspread in mid-infrared colors, likely due to the conspicuous deficiency of 8um\nPAH emission from low-metallicity, low-luminosity galaxies. Conversely, the\nfar-infrared emission tightly tracks the total infrared emission, with a\ndispersion in their flux ratio of only 0.1 dex. In terms of the relation\nbetween infrared-to-ultraviolet ratio and ultraviolet spectral slope, the LVL\nsample shows redder colors and/or lower infrared-to-ultraviolet ratios than\nstarburst galaxies, suggesting that reprocessing by dust is less important in\nthe lower mass systems that dominate the LVL sample. Comparisons with\ntheoretical models suggest that the amplitude of deviations from the relation\nfound for starburst galaxies correlates with the age of the stellar populations\nthat dominate the ultraviolet/optical luminosities.", "cat": "astro-ph.CO", "authors": ["D. A. Dale", "S. A. Cohen", "L. C. Johnson", "M. D. Schuster", "D. Calzetti", "C. W. Engelbracht", "A. Gil de Paz", "R. C. Kennicutt", "J. C. Lee", "A. Begum", "M. Block", "J. J. Dalcanton", "J. G. Funes", "K. D. Gordon", "B. D. Johnson", "A. R. Marble", "S. Sakai", "E. D. Skillman", "L. van Zee", "F. Walter", "D. R. Weisz", "B. Williams", "S. -Y. Wu", "Y. Wu"]}, "561": {"id": "0802.0493v1", "title": "An X-ray Survey of Wolf-Rayet Stars in the Magellanic Clouds. II. The ROSAT PSPC and HRI Datasets", "url": "http://arxiv.org/pdf/0802.0493v1", "date": "2008-02-05 08:44:45", "abs": "Wolf-Rayet (WR) stars in the Magellanic Clouds (MCs) are ideal for studying\nthe production of X-ray emission by their strong fast stellar winds. We have\nstarted a systematic survey for X-ray emission from WR stars in the MCs using\narchival Chandra, ROSAT, and XMM-Newton observations. In Paper I, we reported\nthe detection of X-ray emission from 29 WR stars using Chandra ACIS\nobservations of 70 WR stars in the MCs. In this paper, we report the search and\nanalysis of archival ROSAT PSPC and HRI observations of WR stars. While useful\nROSAT observations are available for 117 WR stars in the MCs, X-ray emission is\ndetected from only 7 of them. The detection rate of X-ray emission from MCs WR\nstars in the ROSAT survey is much smaller than in the Chandra ACIS survey,\nillustrating the necessity of high angular resolution and sensitivity. LMC-WR\n101-102 and 116 were detected by both ROSAT and Chandra, but no large long-term\nvariations are evident.", "cat": "astro-ph", "authors": ["Martin A. Guerrero", "You-Hua Chu"]}, "562": {"id": "2402.02015v1", "title": "SkyMapper Southern Survey: Data Release 4", "url": "http://arxiv.org/pdf/2402.02015v1", "date": "2024-02-03 04:10:17", "abs": "We present the fourth data release (DR4) of the SkyMapper Southern Survey\n(SMSS), the last major step in our hemispheric survey with six optical filters:\nu, v, g, r, i, z. SMSS DR4 covers 26,000 sq.deg from over 400,000 images\nacquired by the 1.3m SkyMapper telescope between 2014-03 and 2021-09. The\n6-band sky coverage extends from the South Celestial Pole to Dec = +16deg, with\nsome images reaching Dec ~ +28deg. In contrast to previous DRs, we include all\ngood-quality images from the facility taken during that time span, not only\nthose explicitly taken for the public Survey. From the image dataset, we\nproduce a catalogue of nearly 13 billion detections made from ~700 million\nunique astrophysical objects. The typical 10sigma depths for each field range\nbetween 18.5 and 20.5 mag, depending on the filter, but certain sky regions\ninclude longer exposures that reach as deep as 22 mag in some filters. As with\nprevious SMSS catalogues, we have cross-matched with a host of other imaging\nand spectroscopic datasets to facilitate additional science outcomes. SMSS DR4\nis now available to the worldwide astronomical community.", "cat": "astro-ph.CO", "authors": ["Christopher A. Onken", "Christian Wolf", "Michael S. Bessell", "Seo-Won Chang", "Lance C. Luvaul", "John L. Tonry", "Marc C. White", "Gary S. Da Costa"]}, "563": {"id": "2202.13675v2", "title": "A Survey on Recent Advances and Challenges in Reinforcement Learning Methods for Task-Oriented Dialogue Policy Learning", "url": "http://arxiv.org/pdf/2202.13675v2", "date": "2022-07-11 02:39:34", "abs": "Dialogue Policy Learning is a key component in a task-oriented dialogue\nsystem (TDS) that decides the next action of the system given the dialogue\nstate at each turn. Reinforcement Learning (RL) is commonly chosen to learn the\ndialogue policy, regarding the user as the environment and the system as the\nagent. Many benchmark datasets and algorithms have been created to facilitate\nthe development and evaluation of dialogue policy based on RL. In this paper,\nwe survey recent advances and challenges in dialogue policy from the\nprescriptive of RL. More specifically, we identify the major problems and\nsummarize corresponding solutions for RL-based dialogue policy learning.\nBesides, we provide a comprehensive survey of applying RL to dialogue policy\nlearning by categorizing recent methods into basic elements in RL. We believe\nthis survey can shed a light on future research in dialogue management.", "cat": "cs.CL", "authors": ["Wai-Chung Kwan", "Hongru Wang", "Huimin Wang", "Kam-Fai Wong"]}, "564": {"id": "2206.00427v2", "title": "The GMRT High Resolution Southern Sky Survey for pulsars and transients -- III: searching for long period pulsars", "url": "http://arxiv.org/pdf/2206.00427v2", "date": "2022-06-30 18:37:28", "abs": "Searching for periodic non-accelerated signals in presence of ideal white\nnoise using the fully phase-coherent Fast Folding Algorithm (FFA) is\ntheoretically established as a more sensitive search method than the Fast\nFourier Transform (FFT) search with incoherent harmonic summing. In this paper,\nwe present a comparison of the performance of an FFA search implementation\nusing RIPTIDE and an FFT search implementation using PRESTO, over a range of\nsignal parameters with white noise and with real telescope noise from the GHRSS\nsurvey with the uGMRT. We find that FFA search with appropriate de-reddening of\ntime series, performs better than FFT search with spectral whitening for long\nperiod pulsars in real GHRSS noise conditions. We describe an FFA search\npipeline implemented for the GHRSS survey looking for pulsars over a period\nrange of 0.1 s to 100 s and up to dispersion measure of 500 pc cm$^{-3}$. We\nprocessed GHRSS survey data covering $\\sim$ 1500 degree$^2$ of the sky with\nthis pipeline. We re-detected 43 known pulsars with better signal-to-noise in\nthe FFA search than in the FFT search. We also report discovery of two new\npulsars including a long period pulsar having a short duty-cycle with this FFA\nsearch pipeline. The population of long period pulsars with periods of several\nseconds or higher can help to constrain the pulsar death-line.", "cat": "astro-ph.HE", "authors": ["Shubham Singh", "Jayanta Roy", "Ujjwal Panda", "Bhaswati Bhattacharyya", "Vincent Morello", "Benjamin W. Stappers", "Paul S. Ray", "Maura A. McLaughlin"]}, "565": {"id": "2002.06797v3", "title": "Deep Domain Adaptive Object Detection: a Survey", "url": "http://arxiv.org/pdf/2002.06797v3", "date": "2020-11-11 06:29:01", "abs": "Deep learning (DL) based object detection has achieved great progress. These\nmethods typically assume that large amount of labeled training data is\navailable, and training and test data are drawn from an identical distribution.\nHowever, the two assumptions are not always hold in practice. Deep domain\nadaptive object detection (DDAOD) has emerged as a new learning paradigm to\naddress the above mentioned challenges. This paper aims to review the\nstate-of-the-art progress on deep domain adaptive object detection approaches.\nFirstly, we introduce briefly the basic concepts of deep domain adaptation.\nSecondly, the deep domain adaptive detectors are classified into five\ncategories and detailed descriptions of representative methods in each category\nare provided. Finally, insights for future research trend are presented.", "cat": "cs.CV", "authors": ["Wanyi Li", "Fuyu Li", "Yongkang Luo", "Peng Wang", "Jia sun"]}, "566": {"id": "1707.06565v1", "title": "The Herschel Planetary Nebula Survey (HerPlaNS) - a comprehensive dusty photoionization model of NGC6781", "url": "http://arxiv.org/pdf/1707.06565v1", "date": "2017-07-20 15:18:45", "abs": "We perform a comprehensive analysis of the planetary nebula (PN) NGC6781 to\ninvestigate the physical conditions of each of its ionized, atomic, and\nmolecular gas and dust components and the object's evolution, based on\npanchromatic observational data ranging from UV to radio. Empirical nebular\nelemental abundances, compared with theoretical predictions via nucleosynthesis\nmodels of asymptotic giant branch (AGB) stars, indicate that the progenitor is\na solar-metallicity, 2.25-3.0 Msun initial-mass star. We derive the best-fit\ndistance of 0.46 kpc by fitting the stellar luminosity (as a function of the\ndistance and effective temperature of the central star) with the adopted\npost-AGB evolutionary tracks. Our excitation energy diagram analysis indicate\nhigh excitation temperatures in the photodissociation region (PDR) beyond the\nionized part of the nebula, suggesting extra heating by shock interactions\nbetween the slow AGB wind and the fast PN wind. Through iterative fitting using\nthe Cloudy code with empirically-derived constraints, we find the best-fit\ndusty photoionization model of the object that would inclusively reproduce all\nof the adopted panchromatic observational data. The estimated total gas mass\n(0.41 Msun) corresponds to the mass ejected during the last AGB thermal pulse\nevent predicted for a 2.5 Msun initial-mass star. A significant fraction of the\ntotal mass (about 70 percent) is found to exist in the PDR, demonstrating the\ncritical importance of the PDR in PNe that are generally recognized as the\nhallmark of ionized/H+ regions.", "cat": "astro-ph.SR", "authors": ["Masaaki Otsuka", "Toshiya Ueta", "Peter A. M. van Hoof", "Raghvendra Sahai", "Isabel Aleman", "Albert A. Zijlstra", "You-Hua Chu", "Eva Villaver", "Marcelo L. Leal-Ferreira", "Joel Kastner", "Ryszard Szczerba", "Katrina M. Exter"]}, "567": {"id": "1905.11437v1", "title": "A Survey of Adaptive Resonance Theory Neural Network Models for Engineering Applications", "url": "http://arxiv.org/pdf/1905.11437v1", "date": "2019-05-04 00:54:06", "abs": "This survey samples from the ever-growing family of adaptive resonance theory\n(ART) neural network models used to perform the three primary machine learning\nmodalities, namely, unsupervised, supervised and reinforcement learning. It\ncomprises a representative list from classic to modern ART models, thereby\npainting a general picture of the architectures developed by researchers over\nthe past 30 years. The learning dynamics of these ART models are briefly\ndescribed, and their distinctive characteristics such as code representation,\nlong-term memory and corresponding geometric interpretation are discussed.\nUseful engineering properties of ART (speed, configurability, explainability,\nparallelization and hardware implementation) are examined along with current\nchallenges. Finally, a compilation of online software libraries is provided. It\nis expected that this overview will be helpful to new and seasoned ART\nresearchers.", "cat": "cs.NE", "authors": ["Leonardo Enzo Brito da Silva", "Islam Elnabarawy", "Donald C. Wunsch II"]}, "568": {"id": "1301.1679v1", "title": "The evolution of galaxies resolved in space and time: an inside-out growth view from the CALIFA survey", "url": "http://arxiv.org/pdf/1301.1679v1", "date": "2013-01-08 21:00:00", "abs": "The growth of galaxies is one of the key problems in understanding the\nstructure and evolution of the universe and its constituents. Galaxies can grow\ntheir stellar mass by accretion of halo or intergalactic gas clouds, or by\nmerging with smaller or similar mass galaxies. The gas available translates\ninto a rate of star formation, which controls the generation of metals in the\nuniverse. The spatially resolved history of their stellar mass assembly has not\nbeen obtained so far for any given galaxy beyond the Local Group. Here we\ndemonstrate how massive galaxies grow their stellar mass inside-out. We report\nthe results from the analysis of the first 105 galaxies of the largest to date\nthree-dimensional spectroscopic survey of galaxies in the local universe\n(CALIFA). We apply the fossil record method of stellar population spectral\nsynthesis to recover the spatially and time resolved star formation history of\neach galaxy. We show, for the first time, that the signal of downsizing is\nspatially preserved, with both inner and outer regions growing faster for more\nmassive galaxies. Further, we show that the relative growth rate of the\nspheroidal component, nucleus and inner galaxy, that happened 5-7 Gyr ago,\nshows a maximum at a critical stellar mass ~10^10 Msun. We also find that\ngalaxies less massive than ~10^10 Msun show a transition to outside-in growth,\nthus connecting with results from resolved studies of the growth of low mass\ngalaxies.", "cat": "astro-ph.CO", "authors": ["E. P\u00e9rez", "R. Cid Fernandes", "R. M. Gonz\u00e1lez Delgado", "R. Garc\u00eda-Benito", "S. F. S\u00e1nchez", "B. Husemann", "D. Mast", "J. R. Rod\u00f3n", "D. Kupko", "N. Backsmann", "A. L. de Amorim", "G. van de Ven", "J. Walcher", "L. Wisotzki", "C. Cortijo-Ferrero", "CALIFA Collaboration"]}, "569": {"id": "2307.02012v1", "title": "A Survey Report on Hardware Trojan Detection by Multiple-Parameter Side-Channel Analysis", "url": "http://arxiv.org/pdf/2307.02012v1", "date": "2023-07-05 03:53:58", "abs": "A major security threat to an integrated circuit (IC) design is the Hardware\nTrojan attack which is a malicious modification of the design. Previously\nseveral papers have investigated into side-channel analysis to detect the\npresence of Hardware Trojans. The side channel analysis were prescribed in\nthese papers as an alternative to the conventional logic testing for detecting\nmalicious modification in the design. It has been found that these conventional\nlogic testing are ineffective when it comes to detecting small Trojans due to\ndecrease in the sensitivity due to process variations encountered in the\nmanufacturing techniques. The main paper under consideration in this survey\nreport focuses on proposing a new technique to detect Trojans by using\nmultiple-parameter side-channel analysis. The novel idea will be explained\nthoroughly in this survey report. We also look into several other papers, which\ntalk about single parameter analysis and how they are implemented. We analyzed\nthe short comings of those single parameter analysis techniques and we then\nshow how this multi-parameter analysis technique is better. Finally we will\ntalk about the combined side-channel analysis and logic testing approach in\nwhich there is higher detection coverage for hardware Trojan circuits of\ndifferent types and sizes.", "cat": "cs.CR", "authors": ["Samir R Katte", "Keith E Fernandez"]}, "570": {"id": "1412.4571v1", "title": "Asking gender questions: Results from a survey of gender and question asking among UK Astronomers at NAM2014", "url": "http://arxiv.org/pdf/1412.4571v1", "date": "2014-12-15 13:01:23", "abs": "We report on a survey of astronomers asking questions at the most recent\nNational Astronomy Meeting (NAM2014). The gender balance of both speakers and\nsession chairs at NAM (31% and 29% women respectively) closely matched that of\nattendees (28% female). However, we find that women were under-represented\namong question askers (just 18% female). Women were especially\nunder-represented in asking the first question (only 14% of first questions\nasked by women), but when the Q&A session reached four or more questions, women\nand men were observed to ask roughly equal numbers of questions. We found a\nsmall, but statistically insignificant, increase in the fraction of questions\nfrom women in sessions where the chair was also female. On average $2.2\\pm0.1$\nquestions were asked per talk, with no detectable difference in the number of\nquestions asked of female and male speakers, but on average female chairs\nsolicited slightly fewer questions than male chairs. We compare these results\nto a similar study by Davenport et al. (2014) for the AAS, who also found\nunder-representation of women amongst question askers, but saw more pronounced\ngender effects when a session chair or speaker were female. We conclude with\nsuggestions for improving the balance of questions at future astronomy\nmeetings.", "cat": "astro-ph.IM", "authors": ["Jonathan Pritchard", "Karen Masters", "James Allen", "Filippo Contenta", "Leo Huckvale", "Stephen Wilkins", "Alice Zocchi"]}, "571": {"id": "2307.07207v1", "title": "The Rapid ASKAP Continuum Survey III: Spectra and Polarisation In Cutouts of Extragalactic Sources (SPICE-RACS) First Data Release", "url": "http://arxiv.org/pdf/2307.07207v1", "date": "2023-07-14 07:54:04", "abs": "The Australian SKA Pathfinder (ASKAP) radio telescope has carried out a\nsurvey of the entire Southern Sky at 887.5MHz. The wide area, high angular\nresolution, and broad bandwidth provided by the low-band Rapid ASKAP Continuum\nSurvey (RACS-low) allow the production of a next-generation rotation measure\n(RM) grid across the entire Southern Sky. Here we introduce this project as\nSpectral and Polarisation in Cutouts of Extragalactic sources from RACS\n(SPICE-RACS). In our first data release, we image 30 RACS-low fields in Stokes\n$I$, $Q$, $U$ at 25'' angular resolution, across 744 to 1032MHz with 1MHz\nspectral resolution. Using a bespoke, highly parallelised, software pipeline we\nare able to rapidly process wide-area spectro-polarimetric ASKAP observations.\nNotably, we use 'postage stamp' cutouts to assess the polarisation properties\nof \\ncomponents\\ radio components detected in total intensity. We find that our\nStokes $Q$ and $U$ images have an rms noise of ~80$\\mu$Jy/PSF, and our\ncorrection for instrumental polarisation leakage allows us to characterise\ncomponents with >1% polarisation fraction over most of the field of view. We\nproduce a broadband polarised radio component catalogue that contains \\nrms\\ RM\nmeasurements over an area of ~1300deg^2 with an average error in RM of\n1.6+1.1-1.0rad/m^2, and an average linear polarisation fraction 3.4+3.0-1.6%.\nWe determine this subset of components using the conditions that the polarised\nsignal-to-noise ratio is $>8$, the polarisation fraction is above our estimated\npolarised leakage, and the Stokes $I$ spectrum has a reliable model. Our\ncatalogue provides an areal density of $4\\pm2$ RMs/deg^2; an increase of\n$\\sim4$ times over the previous state-of-the-art (Taylor et al. 2009). Meaning\nthat, having used just 3% of the RACS-low sky area, we have produced the 3rd\nlargest RM catalogue to date. This catalogue has broad applications for\nstudying...", "cat": "astro-ph.GA", "authors": ["Alec J. M. Thomson", "David McConnell", "Emil Lenc", "Timothy J Galvin", "Lawrence Rudnick", "George Heald", "Catherine L. Hale", "Stefan W. Duchesne", "Craig S. Anderson", "Ettore Carretti", "Christoph Federrath", "B. M. Gaensler", "Lisa Harvey-Smith", "Marijke Haverkorn", "Aidan W. Hotan", "Yik Ki Ma", "Tara Murphy", "N. M. McClure-Griffith", "Vanessa A. Moss", "Shane P. O'Sullivan", "Wasim Raja", "Amit Seta", "Cameron L. Van Eck", "Jennifer L. West", "Matthew T. Whiting", "Mark H. Wieringa"]}, "572": {"id": "1608.00636v1", "title": "A survey of sparse matrix-vector multiplication performance on large matrices", "url": "http://arxiv.org/pdf/1608.00636v1", "date": "2016-08-01 22:52:28", "abs": "We contribute a third-party survey of sparse matrix-vector (SpMV) product\nperformance on industrial-strength, large matrices using: (1) The SpMV\nimplementations in Intel MKL, the Trilinos project (Tpetra subpackage), the\nCUSPARSE library, and the CUSP library, each running on modern architectures.\n(2) NVIDIA GPUs and Intel multi-core CPUs (supported by each software package).\n(3) The CSR, BSR, COO, HYB, and ELL matrix formats (supported by each software\npackage).", "cat": "cs.PF", "authors": ["Max Grossman", "Christopher Thiele", "Mauricio Araya-Polo", "Florian Frank", "Faruk O. Alpak", "Vivek Sarkar"]}, "573": {"id": "1806.08545v2", "title": "The PAU Survey: star-galaxy classification with multi narrow-band data", "url": "http://arxiv.org/pdf/1806.08545v2", "date": "2018-11-15 09:38:14", "abs": "Classification of stars and galaxies is a well-known astronomical problem\nthat has been treated using different approaches, most of them relying on\nmorphological information. In this paper, we tackle this issue using the\nlow-resolution spectra from narrow band photometry, provided by the PAUS\n(Physics of the Accelerating Universe) survey. We find that, with the\nphotometric fluxes from the 40 narrow band filters and without including\nmorphological information, it is possible to separate stars and galaxies to\nvery high precision, 98.4% purity with a completeness of 98.8% for objects\nbrighter than I = 22.5. This precision is obtained with a Convolutional Neural\nNetwork as a classification algorithm, applied to the objects' spectra. We have\nalso applied the method to the ALHAMBRA photometric survey and we provide an\nupdated classification for its Gold sample.", "cat": "astro-ph.IM", "authors": ["Laura Cabayol", "Ignacio Sevilla-Noarbe", "Enrique Fern\u00e1ndez", "Jorge Carretero", "Martin Eriksen", "Santiago Serrano", "Alex Alarc\u00f3n", "Adam Amara", "Ricard Casas", "Francisco Javier Castander", "Juan de Vicente", "Martin Folger", "Juan Garc\u00eda-Bellido", "Enrique Gaztanaga", "Henk Hoekstra", "Ramon Miquel", "Cristobal Padilla", "Eusebio S\u00e1nchez", "Lee Stothert", "Pau Tallada", "Luca Tortorelli"]}, "574": {"id": "0805.3319v1", "title": "First results from the ALHAMBRA-Survey", "url": "http://arxiv.org/pdf/0805.3319v1", "date": "2008-05-21 17:37:47", "abs": "We present the first results from the ALHAMBRA survey. ALHAMBRA will cover a\nrelatively wide area (4 square degrees) using a purposely-designed set of 20\nmedium-band filters, down to an homogeneous magnitude limit AB~25 in most of\nthem, adding also deep near-infrared imaging in JHK. To this aim we are using\nthe Calar Alto 3.5m telescope. A small area of the ALHAMBRA survey has already\nbeen observed through our complete filter set, and this allows for the first\ntime to check all the steps of the survey, including the pipelines that have\nbeen designed for the project, the fulfilment of the data quality expectations,\nthe calibration procedures, and the photometric redshift machinery for which\nALHAMBRA has been optimised. We present here the basic results regarding the\nproperties of the galaxy sample selected in a 15x15 square arcmin area of the\nALHAMBRA-8 field, which includes approximately 10000 galaxies with precise\nphotometric redshift measurements. In a first estimate, approximately 500 of\nthem must be galaxies with z>2.", "cat": "astro-ph", "authors": ["A. Fernandez-Soto", "J. A. L. Aguerri", "E. J. Alfaro", "N. Benitez", "T. Broadhurst", "J. Cabrera-Ca\u00f1o", "F. J. Castander", "J. Cepa", "M. Cervi\u00f1o", "D. Cristobal-Hornillos", "A. Fernandez-Soto", "R. M. Gonzalez Delgado", "L. Infante", "I. Marquez", "V. J. Martinez", "J. Masegosa", "A. del Olmo", "J. Perea", "F. Prada", "J. M. Quintana", "S. F. Sanchez"]}, "575": {"id": "2405.00774v2", "title": "The NIRVANDELS Survey: the stellar and gas-phase mass-metallicity relations of star-forming galaxies at z = 3.5", "url": "http://arxiv.org/pdf/2405.00774v2", "date": "2024-07-10 10:34:44", "abs": "We present determinations of the gas-phase and stellar metallicities of a\nsample of 65 star-forming galaxies at $z \\simeq 3.5$ using rest-frame\nfar-ultraviolet (FUV) spectroscopy from the VANDELS survey in combination with\nfollow-up rest-frame optical spectroscopy from VLT/KMOS and Keck/MOSFIRE. We\ninfer gas-phase oxygen abundances ($Z_{\\mathrm{g}}$; tracing O/H) via strong\noptical nebular lines and stellar iron abundances ($Z_{\\star}$; tracing Fe/H)\nfrom full spectral fitting to the FUV continuum. Our sample spans the stellar\nmass range $8.5 < \\mathrm{log}(M_{\\star}/\\mathrm{M}_{\\odot}) < 10.5$ and shows\nclear evidence for both a stellar and gas-phase mass-metallicity relation\n(MZR). We find that our O and Fe abundance estimates both exhibit a similar\nmass-dependence, such that $\\mathrm{Fe/H}\\propto M_{\\star}^{0.30\\pm0.11}$ and\n$\\mathrm{O/H}\\propto M_{\\star}^{0.32\\pm0.09}$. At fixed $M_{\\star}$ we find\nthat, relative to their solar values, O abundances are systematically larger\nthan Fe abundances (i.e., $\\alpha$-enhancement).We estimate an average\nenhancement of $\\mathrm{(O/Fe)} = 2.65 \\pm 0.16 \\times \\mathrm{(O/Fe)_\\odot}$\nwhich appears to be independent of $M_{\\star}$. We employ analytic chemical\nevolution models to place a constraint on the strength of galactic-level\noutflows via the mass-outflow factor ($\\eta$). We show that outflow\nefficiencies that scale as $\\eta \\propto M_{\\star}^{-0.32}$ can simultaneously\nexplain the functional form of of the stellar and gas-phase MZR, as well as the\ndegree of $\\alpha$-enhancement at fixed Fe/H. Our results add further evidence\nto support a picture in which $\\alpha$-enhanced abundance ratios are ubiquitous\nin high-redshift star-forming galaxies, as expected for young systems whose\ninterstellar medium is primarily enriched by core-collapse supernovae.", "cat": "astro-ph.GA", "authors": ["T. M. Stanton", "F. Cullen", "R. J. McLure", "A. E. Shapley", "K. Z. Arellano-C\u00f3rdova", "R. Begley", "R. Amor\u00edn", "L. Barrufet", "A. Calabr\u00f2", "A. C. Carnall", "M. Cirasuolo", "J. S. Dunlop", "C. T. Donnan", "M. L. Hamadouche", "F. -Y. Liu", "D. J. McLeod", "L. Pentericci", "L. Pozzetti", "R. L. Sanders", "D. Scholte", "M. W. Topping"]}, "576": {"id": "2302.03122v3", "title": "State-wise Safe Reinforcement Learning: A Survey", "url": "http://arxiv.org/pdf/2302.03122v3", "date": "2023-06-30 19:12:31", "abs": "Despite the tremendous success of Reinforcement Learning (RL) algorithms in\nsimulation environments, applying RL to real-world applications still faces\nmany challenges. A major concern is safety, in another word, constraint\nsatisfaction. State-wise constraints are one of the most common constraints in\nreal-world applications and one of the most challenging constraints in Safe RL.\nEnforcing state-wise constraints is necessary and essential to many challenging\ntasks such as autonomous driving, robot manipulation. This paper provides a\ncomprehensive review of existing approaches that address state-wise constraints\nin RL. Under the framework of State-wise Constrained Markov Decision Process\n(SCMDP), we will discuss the connections, differences, and trade-offs of\nexisting approaches in terms of (i) safety guarantee and scalability, (ii)\nsafety and reward performance, and (iii) safety after convergence and during\ntraining. We also summarize limitations of current methods and discuss\npotential future directions.", "cat": "cs.LG", "authors": ["Weiye Zhao", "Tairan He", "Rui Chen", "Tianhao Wei", "Changliu Liu"]}, "577": {"id": "1612.02264v1", "title": "Cosmological constraints with weak lensing peak counts and second-order statistics in a large-field survey", "url": "http://arxiv.org/pdf/1612.02264v1", "date": "2016-12-07 14:29:20", "abs": "Peak statistics in weak lensing maps access the non-Gaussian information\ncontained in the large-scale distribution of matter in the Universe. They are\ntherefore a promising complement to two-point and higher-order statistics to\nconstrain our cosmological models. To prepare for the high-precision data of\nnext-generation surveys, we assess the constraining power of peak counts in a\nsimulated Euclid-like survey on the cosmological parameters\n$\\Omega_\\mathrm{m}$, $\\sigma_8$, and $w_0^\\mathrm{de}$. In particular, we study\nhow the Camelus model--a fast stochastic algorithm for predicting peaks--can be\napplied to such large surveys. We measure the peak count abundance in a mock\nshear catalogue of ~5,000 sq. deg. using a multiscale mass map filtering\ntechnique. We then constrain the parameters of the mock survey using Camelus\ncombined with approximate Bayesian computation (ABC). We find that peak\nstatistics yield a tight but significantly biased constraint in the\n$\\sigma_8$-$\\Omega_\\mathrm{m}$ plane, indicating the need to better understand\nand control the model's systematics. We calibrate the model to remove the bias\nand compare results to those from the two-point correlation functions (2PCF)\nmeasured on the same field. In this case, we find the derived parameter\n$\\Sigma_8=\\sigma_8(\\Omega_\\mathrm{m}/0.27)^\\alpha=0.76_{-0.03}^{+0.02}$ with\n$\\alpha=0.65$ for peaks, while for 2PCF the value is\n$\\Sigma_8=0.76_{-0.01}^{+0.02}$ with $\\alpha=0.70$. We therefore see comparable\nconstraining power between the two probes, and the offset of their\n$\\sigma_8$-$\\Omega_\\mathrm{m}$ degeneracy directions suggests that a combined\nanalysis would yield tighter constraints than either measure alone. As\nexpected, $w_0^\\mathrm{de}$ cannot be well constrained without a tomographic\nanalysis, but its degeneracy directions with the other two varied parameters\nare still clear for both peaks and 2PCF. (abridged)", "cat": "astro-ph.CO", "authors": ["Austin Peel", "Chieh-An Lin", "Francois Lanusse", "Adrienne Leonard", "Jean-Luc Starck", "Martin Kilbinger"]}, "578": {"id": "2204.07588v2", "title": "Cosmic evolution of low-excitation radio galaxies in the LOFAR Two-meter Sky Survey Deep Fields", "url": "http://arxiv.org/pdf/2204.07588v2", "date": "2022-04-22 14:03:26", "abs": "Feedback from low-excitation radio galaxies (LERGs) plays a key role in the\nlifecycle of massive galaxies in the local Universe; their evolution, and the\nimpact of these active galactic nuclei on early galaxy evolution, however,\nremain poorly understood. We use a sample of 10481 LERGs from the first data\nrelease of the LOFAR Two-meter Sky Survey Deep Fields, covering $\\sim$ 25\ndeg$^2$, to present the first measurement of the evolution of the radio\nluminosity function (LF) of LERGs out to $z\\sim2.5$; this shows relatively mild\nevolution. We split the LERGs into those hosted by quiescent and star-forming\ngalaxies, finding a new dominant population of LERGs hosted by star-forming\ngalaxies at high redshifts. The incidence of LERGs in quiescent galaxies shows\na steep dependence on stellar-mass out to $z \\sim1.5$, consistent with local\nUniverse measurements of accretion occurring from cooling of hot gas haloes.\nThe quiescent-LERGs dominate the LFs at $z<1$, showing a strong decline in\nspace density with redshift, tracing that of the available host galaxies, while\nthere is an increase in the characteristic luminosity. The star-forming LERG LF\nincreases with redshift, such that this population dominates the space\ndensities at most radio-luminosities by $z \\sim 1$. The incidence of LERGs in\nstar-forming galaxies shows a much weaker stellar-mass dependence, and\nincreases with redshift, suggesting a different fuelling mechanism compared to\ntheir quiescent counterparts, potentially associated with the cold gas supply\npresent in the star-forming galaxies.", "cat": "astro-ph.GA", "authors": ["R. Kondapally", "P. N. Best", "R. K. Cochrane", "J. Sabater", "K. J. Duncan", "M. J. Hardcastle", "P. Haskell", "B. Mingo", "H. J. A. R\u00f6ttgering", "D. J. B. Smith", "W. L. Williams", "M. Bonato", "G. Calistro Rivera", "F. Gao", "C. L. Hale", "K. Ma\u0142ek", "G. K. Miley", "I. Prandoni", "L. Wang"]}, "579": {"id": "1910.13019v2", "title": "Construction of the Supersymmetric Path Integral: A Survey", "url": "http://arxiv.org/pdf/1910.13019v2", "date": "2020-01-31 07:22:03", "abs": "This is a survey based on joint work with Florian Hanisch and Batu G\\\"uneysu\nreporting on a rigorous construction of the supersymmetric path integral\nassociated to compact spin manifolds.", "cat": "math.DG", "authors": ["Matthias Ludewig"]}, "580": {"id": "1304.1233v1", "title": "Shadow Detection: A Survey and Comparative Evaluation of Recent Methods", "url": "http://arxiv.org/pdf/1304.1233v1", "date": "2013-04-04 03:11:38", "abs": "This paper presents a survey and a comparative evaluation of recent\ntechniques for moving cast shadow detection. We identify shadow removal as a\ncritical step for improving object detection and tracking. The survey covers\nmethods published during the last decade, and places them in a feature-based\ntaxonomy comprised of four categories: chromacity, physical, geometry and\ntextures. A selection of prominent methods across the categories is compared in\nterms of quantitative performance measures (shadow detection and discrimination\nrates, colour desaturation) as well as qualitative observations. Furthermore,\nwe propose the use of tracking performance as an unbiased approach for\ndetermining the practical usefulness of shadow detection methods. The\nevaluation indicates that all shadow detection approaches make different\ncontributions and all have individual strength and weaknesses. Out of the\nselected methods, the geometry-based technique has strict assumptions and is\nnot generalisable to various environments, but it is a straightforward choice\nwhen the objects of interest are easy to model and their shadows have different\norientation. The chromacity based method is the fastest to implement and run,\nbut it is sensitive to noise and less effective in low saturated scenes. The\nphysical method improves upon the accuracy of the chromacity method by adapting\nto local shadow models, but fails when the spectral properties of the objects\nare similar to that of the background. The small-region texture based method is\nespecially robust for pixels whose neighbourhood is textured, but may take\nlonger to implement and is the most computationally expensive. The large-region\ntexture based method produces the most accurate results, but has a significant\ncomputational load due to its multiple processing steps.", "cat": "cs.CV", "authors": ["Andres Sanin", "Conrad Sanderson", "Brian C. Lovell"]}, "581": {"id": "1706.04000v1", "title": "The mass--metallicity relation AKARI-FMOS infrared galaxies at $z\\sim0.88$ in the AKARI North Ecliptic Pole Deep Survey Field", "url": "http://arxiv.org/pdf/1706.04000v1", "date": "2017-06-13 11:11:13", "abs": "Mass, metallicity, and star formation rate (SFR) of a galaxy are crucial\nparameters in understanding galaxy formation and evolution. However, the\nrelation among these is still a matter of debate for luminous infrared\ngalaxies, which carry a bulk of SFR budget of the universe at $z\\sim1$. We have\ninvestigated the relation among stellar mass, gas-phase oxygen abundance, and\nSFR of AKARI-detected mid-IR galaxies at $z\\sim0.88$ in the AKARI NEP deep\nfield. We observed about 350 AKARI sources with Subaru/FMOS NIR spectrograph,\nand detected secure and expected H$\\alpha$ emission lines from 25 and 44\ngalaxies, respectively. The SFR of our sample is almost constant ($\\sim\n25M_{\\odot}/yr$) over the stellar mass range of our sample. Compared with\nmain-sequence (MS) galaxies at a similar redshift range, the average SFR of our\ndetected sample is comparable for massive galaxies\n($\\sim10^{10.58}~M_{\\odot}$), while higher by $\\sim$0.6dex for less massive\ngalaxies ($\\sim 10^{10.05}~M_{\\odot}$). We measure metallicities from the\n[NII]/H$\\alpha$ emission line ratio.\n We find that the mass-metallicity relation of our individually measured\nsources agrees with that for optical-selected star-forming galaxies at\n$z\\sim0.1$, while metallicities of stacked spectra agree with that of MS\ngalaxies at $z\\sim0.78$. Considering high SFR of individually measured sources,\nFMR of the IR galaxies is different from that at $z\\sim0.1$. However, on the\nmass-metallicity plane, they are consistent with the MS galaxies, highlighting\nhigher SFR of the IR galaxies. This suggests the evolutionary path of our IR\ngalaxies is different from that of MS galaxies. A possible physical\ninterpretation includes that the star-formation activities of IR galaxies at\n$z\\sim0.88$ in our sample are enhanced by interaction and/or merger of\ngalaxies, but the inflow of metal-poor gas is not yet induced, keeping the\nmetallicity intact.", "cat": "astro-ph.GA", "authors": ["Nagisa Oi", "Tomotsugu Goto", "Matthew Malkan", "Chris Pearson", "Hideo Matsuhara"]}, "582": {"id": "2309.15310v1", "title": "Microlensing Discovery and Characterization Efficiency in the Vera C. Rubin Legacy Survey of Space and Time", "url": "http://arxiv.org/pdf/2309.15310v1", "date": "2023-09-26 23:41:30", "abs": "The Vera C. Rubin Legacy Survey of Space and Time will discover thousands of\nmicrolensing events across the Milky Way Galaxy, allowing for the study of\npopulations of exoplanets, stars, and compact objects. It will reach deeper\nlimiting magnitudes over a wider area than any previous survey. We evaluate\nnumerous survey strategies simulated in the Rubin Operation Simulations\n(OpSims) to assess the discovery and characterization efficiencies of\nmicrolensing events. We have implemented three metrics in the Rubin Metric\nAnalysis Framework: a discovery metric and two characterization metrics, where\none estimates how well the lightcurve is covered and the other quantifies how\nprecisely event parameters can be determined. We also assess the\ncharacterizability of microlensing parallax, critical for detection of\nfree-floating black hole lenses, in a representative bulge and disk field. We\nfind that, given Rubin's baseline cadence, the discovery and characterization\nefficiency will be higher for longer duration and larger parallax events.\nMicrolensing discovery efficiency is dominated by observing footprint, where\nmore time spent looking at regions of high stellar density including the\nGalactic bulge, Galactic plane, and Magellanic clouds, leads to higher\ndiscovery and characterization rates. However, if the observations are\nstretched over too wide an area, including low-priority areas of the Galactic\nplane with fewer stars and higher extinction, event characterization suffers by\n> 10%, which could impact exoplanet, binary star, and compact object events\nalike. We find that some rolling strategies (where Rubin focuses on a fraction\nof the sky in alternating years) in the Galactic bulge can lead to a 15-20%\ndecrease in microlensing parallax characterization, so rolling strategies\nshould be chosen carefully to minimize losses.", "cat": "astro-ph.IM", "authors": ["Natasha S. Abrams", "Markus P. G. Hundertmark", "Somayeh Khakpash", "Rachel A. Street", "R. Lynne Jones", "Jessica R. Lu", "Etienne Bachelet", "Yiannis Tsapras", "Marc Moniez", "Tristan Blaineauu", "Rosanne Di Stefano", "Martin Makler", "Anibal Varela", "Markus Rabus"]}, "583": {"id": "2205.13380v1", "title": "Classification ensembles for multivariate functional data with application to mouse movements in web surveys", "url": "http://arxiv.org/pdf/2205.13380v1", "date": "2022-05-26 14:12:24", "abs": "We propose new ensemble models for multivariate functional data\nclassification as combinations of semi-metric-based weak learners. Our models\nextend current semi-metric-type methods from the univariate to the multivariate\ncase, propose new semi-metrics to compute distances between functions, and\nconsider more flexible options for combining weak learners using stacked\ngeneralisation methods. We apply these ensemble models to identify respondents'\ndifficulty with survey questions, with the aim to improve survey data quality.\nAs predictors of difficulty, we use mouse movement trajectories from the\nrespondents' interaction with a web survey, in which several questions were\nmanipulated to create two scenarios with different levels of difficulty.", "cat": "stat.ME", "authors": ["Amanda Fern\u00e1ndez-Fontelo", "Felix Henninger", "Pascal J. Kieslich", "Frauke Kreuter", "Sonja Greven"]}, "584": {"id": "1612.04042v2", "title": "Non-negative matrix factorization for self-calibration of photometric redshift scatter in weak lensing surveys", "url": "http://arxiv.org/pdf/1612.04042v2", "date": "2017-10-12 01:19:43", "abs": "Photo-z error is one of the major sources of systematics degrading the\naccuracy of weak lensing cosmological inferences. Zhang et al. (2010) proposed\na self-calibration method combining galaxy-galaxy correlations and galaxy-shear\ncorrelations between different photo-z bins. Fisher matrix analysis shows that\nit can determine the rate of photo-z outliers at a level of 0.01-1% merely\nusing photometric data and do not rely on any prior knowledge. In this paper,\nwe develop a new algorithm to implement this method by solving a constrained\nnonlinear optimization problem arising in the self-calibration process. Based\non the techniques of fixed-point iteration and non-negative matrix\nfactorization, the proposed algorithm can efficiently and robustly reconstruct\nthe scattering probabilities between the true-z and photo-z bins. The algorithm\nhas been tested extensively by applying it to mock data from simulated stage IV\nweak lensing projects. We find that the algorithm provides a successful\nrecovery of the scatter rates at the level of 0.01-1%, and the true mean\nredshifts of photo-z bins at the level of 0.001, which may satisfy the\nrequirements in future lensing surveys.", "cat": "astro-ph.CO", "authors": ["Le Zhang", "Yu Yu", "Pengjie Zhang"]}, "585": {"id": "2307.00967v2", "title": "DREAM: III.A helium survey in exoplanets on the edge of the hot Neptune desert with GIANO-B@TNG", "url": "http://arxiv.org/pdf/2307.00967v2", "date": "2023-07-18 07:07:51", "abs": "The population of close-in exoplanets features a desert of hot Neptunes whose\norigin is uncertain. These planets may have lost their atmosphere, eroding into\nmini-Neptunes and super-Earths. Direct observations of evaporating atmospheres\nare essential to derive mass-loss estimates and constrain this scenario. The\nmetastable 1083.3nm HeI triplet represents a powerful diagnostic of atmospheric\nevaporation since it traces the hot gas in extended exoplanet atmospheres, is\nobservable from the ground, and is weakly affected by interstellar medium\nabsorption. We conducted a uniform HeI transmission spectroscopy survey,\nfocusing on 9 planets located at the edges of the Neptunian desert, aiming to\ngain insights into the role of photo-evaporation in its formation. We observed\none transit per planet using the high-resolution, near-infrared spectrograph\nGIANO-B on the Telescopio Nazionale Galileo. We focused our analysis on the HeI\ntriplet by computing high-resolution transmission spectra. We then employed the\np-winds model to interpret the observed transmission spectra. We found no sign\nof planetary absorption in the HeI triplet in any of the investigated targets.\nWe thus provided 3sigma upper-limit estimations on the thermosphere absorption,\ntemperature, and mass loss, and combined them with past measurements to search\nfor correlations with parameters thought to be drivers in the formation of the\nHeI triplet. Our results strengthen the importance of performing homogeneous\nsurveys and analyses to bring clarification in the HeI detection and hence in\nthe Neptunian desert origin. Our findings corroborate the literature\nexpectations that the HeI absorption signal correlates with the stellar mass\nand the received XUV flux. However, these trends seem to disappear in terms of\nmass-loss rates; further studies are essential to shed light on this aspect and\nto understand better the photo-evaporation process.", "cat": "astro-ph.EP", "authors": ["G. Guilluy", "V. Bourrier", "Y. Jaziri", "W. Dethier", "D. Mounzer", "P. Giacobbe", "O. Attia", "R. Allart", "A. S. Bonomo", "L. A. Dos Santos", "M. Rainer", "A. Sozzetti"]}, "586": {"id": "1210.5094v1", "title": "The JCMT Gould Belt Survey: SCUBA-2 observations of radiative feedback in NGC1333", "url": "http://arxiv.org/pdf/1210.5094v1", "date": "2012-10-18 11:20:00", "abs": "We present observations of NGC1333 from SCUBA-2 on JCMT, observed as a JCMT\nGould Belt Survey pilot project during the shared risk campaign when the first\nof four arrays was installed at each of 450 and 850 microns. Temperature maps\nare derived from 450 micron and 850 micron ratios under the assumption of\nconstant dust opacity spectral index beta=1.8. Temperatures indicate that the\ndust in the northern (IRAS 6/8) region of NGC1333 is hot, 20-40 K, due to\nheating by the B star SVS3, other young stars in the IR/optically visible\ncluster, and embedded protostars. Other luminous protostars are also identified\nby temperature rises at the 17\" resolution of the ratio maps (0.02 pc assuming\na distance of 250 pc for Perseus). The extensive heating raises the possibility\nthat the radiative feedback may lead to increased masses for the next\ngeneration of stars.", "cat": "astro-ph.GA", "authors": ["J. Hatchell", "T. Wilson", "E. Drabek", "E. Curtis", "J. Richer", "D. Nutter", "J. Di Francesco", "D. Ward-Thompson"]}, "587": {"id": "1412.5554v1", "title": "The ionised, radical and molecular Milky Way: spectroscopic surveys with the SKA", "url": "http://arxiv.org/pdf/1412.5554v1", "date": "2014-12-17 20:00:07", "abs": "The bandwith, sensitivity and sheer survey speed of the SKA offers unique\npotential for deep spectroscopic surveys of the Milky Way. Within the frequency\nbands available to the SKA lie many transitions that trace the ionised, radical\nand molecular components of the interstellar medium and which will\nrevolutionise our understanding of many physical processes. In this chapter we\ndescribe the impact on our understanding of the Milky Way that can be achieved\nby spectroscopic SKA surveys, including \"out of the box\" early science with\nradio recombination lines, Phase 1 surveys of the molecular ISM using anomalous\nformaldehyde absorption, and full SKA surveys of ammonia inversion lines.", "cat": "astro-ph.GA", "authors": ["Mark Thompson", "Henrik Beuther", "Clive Dickinson", "Joseph C. Mottram", "Pamela Klaassen", "Adam Ginsburg", "Steve Longmore", "Anthony Remijan", "Karl Menten"]}, "588": {"id": "2408.12128v1", "title": "Diffusion-Based Visual Art Creation: A Survey and New Perspectives", "url": "http://arxiv.org/pdf/2408.12128v1", "date": "2024-08-22 04:49:50", "abs": "The integration of generative AI in visual art has revolutionized not only\nhow visual content is created but also how AI interacts with and reflects the\nunderlying domain knowledge. This survey explores the emerging realm of\ndiffusion-based visual art creation, examining its development from both\nartistic and technical perspectives. We structure the survey into three phases,\ndata feature and framework identification, detailed analyses using a structured\ncoding process, and open-ended prospective outlooks. Our findings reveal how\nartistic requirements are transformed into technical challenges and highlight\nthe design and application of diffusion-based methods within visual art\ncreation. We also provide insights into future directions from technical and\nsynergistic perspectives, suggesting that the confluence of generative AI and\nart has shifted the creative paradigm and opened up new possibilities. By\nsummarizing the development and trends of this emerging interdisciplinary area,\nwe aim to shed light on the mechanisms through which AI systems emulate and\npossibly, enhance human capacities in artistic perception and creativity.", "cat": "cs.AI", "authors": ["Bingyuan Wang", "Qifeng Chen", "Zeyu Wang"]}, "589": {"id": "2202.11939v1", "title": "Spectroscopic Study of M33 with LAMOST survey. I. Chemical gradients from nebulae", "url": "http://arxiv.org/pdf/2202.11939v1", "date": "2022-02-24 07:42:02", "abs": "Morphological and chemical structures of M33 are investigated with LAMOST DR7\nsurvey. Physical parameters, extinction, chemical composition of He, N, O, Ne,\nS, Cl, Ar (where available), and radial velocities were determined for 110\nnebulae (95 H\\ii\\ regions and 15 PNe) in M33. Among them, 8 PNe and 55 H\\ii\\\nregions in M33 are newly discovered. We obtained the following O abundance\ngradients: $-$0.199$_{-0.030}^{+0.030}$ dex $R_{25}^{-1}$ (based on 95 H\\ii\\\nregions), $-$0.124$_{-0.036}^{+0.036}$ dex $R_{25}^{-1}$ (based on 93 H\\ii\\\nregions), and $-$0.207$_{-0.174}^{+0.160}$ dex $R_{25}^{-1}$ (based on 21 H\\ii\\\nregion), utilizing abundances from N2 at O3N2 diagnostics and the $T_{\\rm\ne}$-sensitive method, respectively. The He, N, Ne, S, and Ar gradients resulted\nin slopes of $-$0.179$_{-0.146}^{+0.145}$, $-$0.431$_{-0.281}^{+0.282}$,\n$-$0.171$_{-0.239}^{+0.234}$, $-$0.417$_{-0.182}^{+0.174}$,\n$-$0.340$_{-0.157}^{+0.156}$, respectively, utilizing abundances from the\n$T_{\\rm e}$-sensitive method. Our results confirm the existence of negative\naxisymmetric global metallicity distribution that is assumed in the literature.\nWe noticed one new WC star candidate and one transition WR WN/C candidate. The\ngrand-design pattern of spiral structure of M33 is presented.", "cat": "astro-ph.SR", "authors": ["Sofya Alexeeva", "Gang Zhao"]}, "590": {"id": "2108.10066v1", "title": "Dynamic Neural Network Architectural and Topological Adaptation and Related Methods -- A Survey", "url": "http://arxiv.org/pdf/2108.10066v1", "date": "2021-07-28 16:50:29", "abs": "Training and inference in deep neural networks (DNNs) has, due to a steady\nincrease in architectural complexity and data set size, lead to the development\nof strategies for reducing time and space requirements of DNN training and\ninference, which is of particular importance in scenarios where training takes\nplace in resource constrained computation environments or inference is part of\na time critical application. In this survey, we aim to provide a general\noverview and categorization of state-of-the-art (SOTA) of techniques to reduced\nDNN training and inference time and space complexities with a particular focus\non architectural adaptions.", "cat": "cs.LG", "authors": ["Lorenz Kummer"]}, "591": {"id": "2409.02977v1", "title": "Large Language Model-Based Agents for Software Engineering: A Survey", "url": "http://arxiv.org/pdf/2409.02977v1", "date": "2024-09-04 15:59:41", "abs": "The recent advance in Large Language Models (LLMs) has shaped a new paradigm\nof AI agents, i.e., LLM-based agents. Compared to standalone LLMs, LLM-based\nagents substantially extend the versatility and expertise of LLMs by enhancing\nLLMs with the capabilities of perceiving and utilizing external resources and\ntools. To date, LLM-based agents have been applied and shown remarkable\neffectiveness in Software Engineering (SE). The synergy between multiple agents\nand human interaction brings further promise in tackling complex real-world SE\nproblems. In this work, we present a comprehensive and systematic survey on\nLLM-based agents for SE. We collect 106 papers and categorize them from two\nperspectives, i.e., the SE and agent perspectives. In addition, we discuss open\nchallenges and future directions in this critical domain. The repository of\nthis survey is at https://github.com/FudanSELab/Agent4SE-Paper-List.", "cat": "cs.SE", "authors": ["Junwei Liu", "Kaixin Wang", "Yixuan Chen", "Xin Peng", "Zhenpeng Chen", "Lingming Zhang", "Yiling Lou"]}, "592": {"id": "2005.13998v1", "title": "Survey on a quantum stochastic extension of Stone's Theorem", "url": "http://arxiv.org/pdf/2005.13998v1", "date": "2020-05-28 13:47:38", "abs": "From K\\\"ummerer's investigations on stationary Markov processes has emerged\nan operator algebraic definition of white noises which captures many examples\nfrom classical as well as from non-commutative probability. Within\nnon-commutative $L^p$-spaces associated to a white noise, the role of\n(non-)commutative L\\'evy processes is played by additive cocycles for the white\nnoise shift, and moreover, the notion for exponentials of classical L\\'evy\nprocesses is generalized by unitary cocycles. As a main result we report a\nbijective correspondence between additive and unitary cocycles for white noise\nshifts. If the cocycles are required to be differentiable, the presented\ncorrespondence reduces to Stone's theorem (for norm continuous unitary groups).\nThe correspondence needs the development of background results for additive\ncocycles with $L^\\infty$-bounded covariance operators: an operator-valued\nstochastic It\\^o integration, quadratic variations and non-commutative\nmartingale inequalities as well as stochastic differentiation. Related results\nand recent progress towards the case of additive cocycles with unbounded\nvariance operators are reported.", "cat": "math.OA", "authors": ["Claus K\u00f6stler"]}, "593": {"id": "2207.05270v1", "title": "A Survey on Table Question Answering: Recent Advances", "url": "http://arxiv.org/pdf/2207.05270v1", "date": "2022-07-12 02:44:40", "abs": "Table Question Answering (Table QA) refers to providing precise answers from\ntables to answer a user's question. In recent years, there have been a lot of\nworks on table QA, but there is a lack of comprehensive surveys on this\nresearch topic. Hence, we aim to provide an overview of available datasets and\nrepresentative methods in table QA. We classify existing methods for table QA\ninto five categories according to their techniques, which include\nsemantic-parsing-based, generative, extractive, matching-based, and\nretriever-reader-based methods. Moreover, as table QA is still a challenging\ntask for existing methods, we also identify and outline several key challenges\nand discuss the potential future directions of table QA.", "cat": "cs.CL", "authors": ["Nengzheng Jin", "Joanna Siebert", "Dongfang Li", "Qingcai Chen"]}, "594": {"id": "2311.17671v1", "title": "The ALMA-CRISTAL survey: Widespread dust-obscured star formation in typical star-forming galaxies at z=4-6", "url": "http://arxiv.org/pdf/2311.17671v1", "date": "2023-11-29 14:34:43", "abs": "We present the morphological parameters and global properties of\ndust-obscured star formation in typical star-forming galaxies at z=4-6. Among\n26 galaxies composed of 20 galaxies observed by the Cycle-8 ALMA Large Program,\nCRISTAL, and six galaxies from archival data, we have individually detected\nrest-frame 158$\\mu$m dust continuum emission from 19 galaxies, nine of which\nare reported for the first time. The derived far-infrared luminosities are in\nthe range $\\log_{10} L_{\\rm IR}\\,[L_{\\odot}]=$10.9-12.4, an order of magnitude\nlower than previously detected massive dusty star-forming galaxies (DSFGs). The\naverage relationship between the fraction of dust-obscured star formation\n($f_{\\rm obs}$) and the stellar mass is consistent with previous results at\nz=4-6 in a mass range of $\\log_{10} M_{\\ast}\\,[M_{\\odot}]\\sim$9.5-11.0 and show\npotential evolution from z=6-9. The individual $f_{\\rm obs}$ exhibits a\nsignificant diversity, and it shows a correlation with the spatial offset\nbetween the dust and the UV continuum, suggesting the inhomogeneous dust\nreddening may cause the source-to-source scatter in $f_{\\rm obs}$. The\neffective radii of the dust emission are on average $\\sim$1.5 kpc and are\n$\\sim2$ times more extended than the rest-frame UV. The infrared surface\ndensities of these galaxies ($\\Sigma_{\\rm\nIR}\\sim2.0\\times10^{10}\\,L_{\\odot}\\,{\\rm kpc}^{-2}$) are one order of magnitude\nlower than those of DSFGs that host compact central starbursts. On the basis of\nthe comparable contribution of dust-obscured and dust-unobscured star formation\nalong with their similar spatial extent, we suggest that typical star-forming\ngalaxies at z=4-6 form stars throughout the entirety of their disks.", "cat": "astro-ph.GA", "authors": ["Ikki Mitsuhashi", "Ken-ichi Tadaki", "Ryota Ikeda", "Rodrigo Herrera-Camus", "Manuel Aravena", "Ilse De Looze", "Natascha M. F\u00f6rster Schreiber", "Jorge Gonz\u00e1lez-L\u00f3pez", "Justin Spilker", "Roberto J. Assef", "Rychard Bouwens", "Loreto Barcos-Munoz", "Jack Birkin", "Rebecca A. A. Bowler", "Gabriela Calistro Rivera", "Rebecca Davies", "Elisabete Da Cunha", "Tanio D\u00edaz-Santos", "Andrea Ferrara", "Deanne Fisher", "Lilian L. Lee", "Juno Li", "Dieter Lutz", "Monica Rela\u00f1o", "Thorsten Naab", "Marco Palla", "Ana Posses", "Manuel Solimano", "Linda Tacconi", "Hannah \u00dcbler", "Stefan van der Giessen", "Sylvain Veilleux"]}, "595": {"id": "1506.06879v1", "title": "A Probe into Causes of Non-citation Based on Survey Data", "url": "http://arxiv.org/pdf/1506.06879v1", "date": "2015-06-23 07:04:11", "abs": "Empirical analysis results about the possible causes leading to non-citation\nmay help increase the potential of researchers' work to be cited and editorial\nstaffs of journals to identify contributions with potential high quality. In\nthis study, we conduct a survey on the possible causes leading to citation or\nnon-citation based on a questionnaire. We then perform a statistical analysis\nto identify the major causes leading to non-citation in combination with the\nanalysis on the data collected through the survey. Most respondents to our\nquestionnaire identified eight major causes that facilitate easy citation of\none's papers, such as research hotspots and novel topics of content, longer\nintervals after publication, research topics similar to my work, high quality\nof content, reasonable self-citation, highlighted title, prestigious authors,\nacademic tastes and interests similar to mine.They also pointed out that the\nvast difference between their current and former research directions as the\nprimary reason for their previously uncited papers. They feel that text that\nincludes notes, comments, and letters to editors are rarely cited, and the same\nis true for too short or too lengthy papers. In comparison, it is easier for\nreviews, articles, or papers of intermediate length to be cited.", "cat": "cs.DL", "authors": ["Zewen Hu", "Yishan Wu"]}, "596": {"id": "1806.05808v1", "title": "Deep Extragalactic VIsible Legacy Survey (DEVILS): Motivation, Design and Target Catalogue", "url": "http://arxiv.org/pdf/1806.05808v1", "date": "2018-06-15 05:35:48", "abs": "The Deep Extragalactic VIsible Legacy Survey (DEVILS) is a large\nspectroscopic campaign at the Anglo-Australian Telescope (AAT) aimed at\nbridging the near and distant Universe by producing the highest completeness\nsurvey of galaxies and groups at intermediate redshifts ($0.30.1$) are relatively cool with $T_{\\rm eff} < 4500$ K,\nwhich could be a result of having deeper convection zones. Apart from that,\nspot properties show no significant trends with rotation period, infrared\nexcess, or stellar properties. Most notably, we find hot spots in stars that do\nnot show $K-W2$ infrared excess, indicating the possibility of accretion across\nan inner disk cavity or the presence of plage.", "cat": "astro-ph.SR", "authors": ["Carys Herbert", "Dirk Froebrich", "Aleks Scholz"]}, "625": {"id": "2010.03061v1", "title": "A Survey on Recognizing Textual Entailment as an NLP Evaluation", "url": "http://arxiv.org/pdf/2010.03061v1", "date": "2020-10-06 22:23:00", "abs": "Recognizing Textual Entailment (RTE) was proposed as a unified evaluation\nframework to compare semantic understanding of different NLP systems. In this\nsurvey paper, we provide an overview of different approaches for evaluating and\nunderstanding the reasoning capabilities of NLP systems. We then focus our\ndiscussion on RTE by highlighting prominent RTE datasets as well as advances in\nRTE dataset that focus on specific linguistic phenomena that can be used to\nevaluate NLP systems on a fine-grained level. We conclude by arguing that when\nevaluating NLP systems, the community should utilize newly introduced RTE\ndatasets that focus on specific linguistic phenomena.", "cat": "cs.CL", "authors": ["Adam Poliak"]}, "626": {"id": "2405.04870v1", "title": "MOSEL survey: Unwrapping the Epoch of Reionization through mimic galaxies at Cosmic Noon", "url": "http://arxiv.org/pdf/2405.04870v1", "date": "2024-05-08 07:59:26", "abs": "The nature of the first galaxies that reionized the universe during the Epoch\nof Reionization (EoR) remains unclear. Attempts to directly determine spectral\nproperties of these early galaxies are affected by both limited photometric\nconstraints across the spectrum and by the opacity of the intergalactic medium\n(IGM) to the Lyman Continuum (LyC) at high redshift. We approach this by\nanalysing properties of analogous extreme emission line galaxies (EELGs,\n[OIII]+Hbeta EW $>400$ Angstrom) at $2.55.5$ observed with the James Webb\nSpace Telesope (JWST) with self-consistent spectral energy distribution fitting\nmethodology. This work focuses on the comparison of their UV slopes\n($\\beta_P$), ionizing photon production efficiencies $\\xi_{ion}$, star\nformation rates and dust properties to determine the effectiveness of this\nanalogue selection technique. We report the median ionizing photon production\nefficiencies as log$_{10}(\\xi_{ion}/(Hz\\ {\\rm\nerg}^{-1}))=$$25.14^{+0.06}_{-0.04}$,$25.16^{+0.06}_{-0.05}$,$25.16^{+0.04}_{-0.05}$,$25.18^{+0.06}_{-0.07}$\nfor our ZFOURGE control, ZFOURGE EELG, JADES and CEERS samples respectively.\nZFOURGE EELGs are 0.57 dex lower in stellar mass and have half the dust\nextinction, compared to their ZFOURGE control counterparts. They also have a\nsimilar specific star formation rates and $\\beta_P$ to the $z>5.5$ samples. We\nfind that EELGs at low redshift ($2.5=3. Exploiting the red sensitivity of the refurbished\nVIMOS spectrograph, the fundamental aim of the survey is to provide the high\nsignal-to-noise ratio spectra necessary to measure key physical properties such\nas stellar population ages, masses, metallicities and outflow velocities from\ndetailed absorption-line studies. Using integration times calculated to produce\nan approximately constant signal-to-noise ratio (20 < t_int < 80 hours), the\nVANDELS survey targeted: a) bright star-forming galaxies at 2.4 < z < 5.5, b)\nmassive quiescent galaxies at 1.0 < z < 2.5, c) fainter star-forming galaxies\nat 3.0 < z < 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and\nHerschel-detected galaxies. By targeting two extragalactic survey fields with\nsuperb multi-wavelength imaging data, VANDELS will produce a unique legacy data\nset for exploring the physics underpinning high-redshift galaxy evolution. In\nthis paper we provide an overview of the VANDELS survey designed to support the\nscience exploitation of the first ESO public data release, focusing on the\nscientific motivation, survey design and target selection.", "cat": "astro-ph.GA", "authors": ["R. J. McLure", "L. Pentericci", "A. Cimatti", "J. S. Dunlop", "D. Elbaz", "A. Fontana", "K. Nandra", "R. Amorin", "M. Bolzonella", "A. Bongiorno", "A. C. Carnall", "M. Castellano", "M. Cirasuolo", "O. Cucciati", "F. Cullen", "S. De Barros", "S. L. Finkelstein", "F. Fontanot", "P. Franzetti", "M. Fumana", "A. Gargiulo", "B. Garilli", "L. Guaita", "W. G. Hartley", "A. Iovino", "M. J. Jarvis", "S. Juneau", "W. Karman", "D. Maccagni", "F. Marchi", "E. Marmol-Queralto", "E. Pompei", "L. Pozzetti", "M. Scodeggio", "V. Sommariva", "M. Talia", "O. Almaini", "I. Balestra", "S. Bardelli", "E. F. Bell", "N. Bourne", "R. A. A. Bowler", "M. Brusa", "F. Buitrago", "K. I. Caputi", "P. Cassata", "S. Charlot", "A. Citro", "G. Cresci", "S. Cristiani", "E. Curtis-Lake", "M. Dickinson", "G. G. Fazio", "H. C. Ferguson", "F. Fiore", "M. Franco", "J. P. U. Fynbo", "A. Galametz", "A. Georgakakis", "M. Giavalisco", "A. Grazian", "N. P. Hathi", "I. Jung", "S. Kim", "A. M. Koekemoer", "Y. Khusanova", "O. Le Fevre", "J. M. Lotz", "F. Mannucci", "D. T. Maltby", "K. Matsuoka", "D. J. McLeod", "H. Mendez-Hernandez", "J. Mendez-Abreu", "M. Mignoli", "M. Moresco", "A. Mortlock", "M. Nonino", "M. Pannella", "C. Papovich", "P. Popesso", "D. P. Rosario", "M. Salvato", "P. Santini", "D. Schaerer", "C. Schreiber", "D. P. Stark", "L. A. M. Tasca", "R. Thomas", "T. Treu", "E. Vanzella", "V. Wild", "C. C. Williams", "G. Zamorani", "E. Zucca"]}, "630": {"id": "1412.0469v1", "title": "VEGAS-SSS. A VST survey of elliptical galaxies in the southern hemisphere: analysis of small stellar systems. Testing the methodology on the globular cluster system in NGC3115", "url": "http://arxiv.org/pdf/1412.0469v1", "date": "2014-12-01 13:25:52", "abs": "We present a study of globular clusters (GCs) and other small stellar systems\n(SSSs) in the field of NGC3115, observed as part of the VEGAS imaging survey,\ncarried out with the VST telescope. We use deep g and i data of NGC3115, a\nwell-studied lenticular galaxy with excellent scientific literature. This is\nfundamental to test the methodologies, verify the results, and probe the\ncapabilities of the VEGAS-SSS. Leveraging the large field of view of the VST\nallow us to accurately study of the distribution and properties of SSSs as a\nfunction of galactocentric distance Rgc, well beyond ~20 galaxy effective\nradii, in a way not often possible. Our analysis of colors, magnitudes and\nsizes of SSS candidates confirms the results from existing studies, some of\nwhich carried out with 8-10m class telescopes, and further extends them to\nunreached Rgc distances, with similar accuracy. We find a color bimodality for\nthe GC population and a r1/4 profile for the surface density of GCs as for the\ngalaxy light profile. The radial color gradient of blue and red GCs previously\nfound, for instance by the SLUGGS survey, is further extended out to the\nlargest Rgc inspected, ~65 kpc. The surface density profiles of blue and red\nGCs taken separately are well approximated by a r1/4 density profile, with the\nfraction of blue GCs being slightly larger at larger Rgc. We do not find hints\nof a trend for the red GC and for the GC turnover magnitude to vary with\nradius, but we observe a ~0.2 mag difference in the turnover magnitude of the\nblue and red GCs subpopulations. Inspecting SSS sizes and colors we obtained a\nlist of UCDs and GC candidates suitable for future spectroscopic follow-up. In\nconclusion, our study shows the reliability of the methodologies developed to\nstudy SSSs in the field of bright early-type galaxies, and the great potential\nof the VEGAS survey to produce original results on SSSs science.", "cat": "astro-ph.GA", "authors": ["Michele Cantiello", "Massimo Capaccioli", "Nicola Napolitano", "Aniello Grado", "Luca Limatola", "Maurizio Paolillo", "Enrica Iodice", "Aaron J. Romanowsky", "Duncan A. Forbes", "Gabriella Raimondo", "Marilena Spavone", "Francesco La Barbera", "Thomas H. Puzia", "Pietro Schipani"]}, "631": {"id": "2301.05118v1", "title": "QUIJOTE scientific results -- IX. Radio sources in the QUIJOTE-MFI wide survey maps", "url": "http://arxiv.org/pdf/2301.05118v1", "date": "2023-01-12 16:17:37", "abs": "We present the catalogue of Q-U-I JOint TEnerife (QUIJOTE) Wide Survey radio\nsources extracted from the maps of the Multi-Frequency Instrument compiled\nbetween 2012 and 2018. The catalogue contains 786 sources observed in intensity\nand polarization, and is divided into two separate sub-catalogues: one\ncontaining 47 bright sources previously studied by the \\emph{Planck}\ncollaboration and an extended catalogue of 739 sources either selected from the\n\\emph{Planck} Second Catalogue of Compact Sources or found through a blind\nsearch carried out with a Mexican Hat 2 wavelet. A significant fraction of the\nsources in our catalogue (38.7 per cent) are within the $|b| \\leq 20^\\circ$\nregion of the Galactic plane. We determine statistical properties for those\nsources that are likely to be extragalactic. We find that these statistical\nproperties are compatible with currently available models, with a $\\sim$1.8 Jy\ncompleteness limit at 11 GHz. We provide the polarimetric properties of (38,\n33, 31, 23) sources with P detected above the $99.99\\%$ significance level at\n(11, 13, 17, 19) GHz, respectively. Median polarization fractions are in the\n$2.8$-$4.7$\\% range in the 11-19 GHz frequency interval. We do not distinguish\nbetween Galactic and extragalactic sources here. The results presented here are\nconsistent with those reported in the literature for flat- and steep-spectrum\nradio sources.", "cat": "astro-ph.GA", "authors": ["D. Herranz", "M. L\u00f3pez-Caniego", "C. H. L\u00f3pez-Caraballo", "R. T. G\u00e9nova-Santos", "Y. C. Perrott", "J. A. Rubi\u00f1o-Mart\u00edn", "R. Rebolo", "E. Artal", "M. Ashdown", "R. B. Barreiro", "F. J. Casas", "E. de la Hoz", "M. Fern\u00e1ndez-Torreiro", "F. Guidi", "R. J. Hoyland", "A. N. Lasenby", "E. Mart\u00ednez-Gonz\u00e1lez", "M. W. Peel", "L. Piccirillo", "F. Poidevin", "B. Ruiz-Granados", "D. Tramonte", "F. Vansyngel", "P. Vielva", "R. A. Watson"]}, "632": {"id": "2007.08995v2", "title": "The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Baryon acoustic oscillations with Lyman-$\u03b1$ forests", "url": "http://arxiv.org/pdf/2007.08995v2", "date": "2020-10-05 21:33:59", "abs": "We present a measurement of baryonic acoustic oscillations (BAO) from\nLyman-$\\alpha$ (Ly$\\alpha$) absorption and quasars at an effective redshift\n$z=2.33$ using the complete extended Baryonic Oscillation Spectroscopic Survey\n(eBOSS). The sixteenth and final eBOSS data release (SDSS DR16) contains all\ndata from eBOSS and its predecessor, the Baryonic Oscillation Spectroscopic\nSurvey (BOSS), providing $210,005$ quasars with $z_{q}>2.10$ that are used to\nmeasure Ly$\\alpha$ absorption. We measure the BAO scale both in the\nauto-correlation of Ly$\\alpha$ absorption and in its cross correlation with\n$341,468$ quasars with redshift $z_{q}>1.77$. Apart from the statistical gain\nfrom new quasars and deeper observations, the main improvements over previous\nwork come from more accurate modeling of physical and instrumental correlations\nand the use of new sets of mock data. Combining the BAO measurement from the\nauto- and cross-correlation yields the constraints of the two ratios\n$D_{H}(z=2.33)/r_{d} = 8.99 \\pm 0.19$ and $D_{M}(z=2.33)/r_{d} = 37.5 \\pm 1.1$,\nwhere the error bars are statistical. These results are within $1.5\\sigma$ of\nthe prediction of the flat-$\\Lambda$CDM cosmology of Planck~(2016). The\nanalysis code, \\texttt{picca}, the catalog of the flux-transmission field\nmeasurements, and the $\\Delta \\chi^{2}$ surfaces are publicly available.", "cat": "astro-ph.CO", "authors": ["H\u00e9lion du Mas des Bourboux", "James Rich", "Andreu Font-Ribera", "Victoria de Sainte Agathe", "James Farr", "Thomas Etourneau", "Jean-Marc Le Goff", "Andrei Cuceu", "Christophe Balland", "Julian E. Bautista", "Michael Blomqvist", "Jonathan Brinkmann", "Joel R. Brownstein", "Sol\u00e8ne Chabanier", "Edmond Chaussidon", "Kyle Dawson", "Alma X. Gonz\u00e1lez-Morales", "Julien Guy", "Brad W. Lyke", "Axel de la Macorra", "Eva-Maria Mueller", "Adam D. Myers", "Christian Nitschelm", "Andrea Mu\u00f1oz Guti\u00e9rrez", "Nathalie Palanque-Delabrouille", "James Parker", "Will J. Percival", "Ignasi P\u00e9rez-R\u00e0fols", "Patrick Petitjean", "Matthew M. Pieri", "Corentin Ravoux", "Graziano Rossi", "Donald P. Schneider", "Hee-Jong Seo", "An\u017ee Slosar", "Julianna Stermer", "M. Vivek", "Christophe Y\u00e8che", "Samantha Youles"]}, "633": {"id": "2106.15115v1", "title": "Neural Machine Translation for Low-Resource Languages: A Survey", "url": "http://arxiv.org/pdf/2106.15115v1", "date": "2021-06-29 06:31:58", "abs": "Neural Machine Translation (NMT) has seen a tremendous spurt of growth in\nless than ten years, and has already entered a mature phase. While considered\nas the most widely used solution for Machine Translation, its performance on\nlow-resource language pairs still remains sub-optimal compared to the\nhigh-resource counterparts, due to the unavailability of large parallel\ncorpora. Therefore, the implementation of NMT techniques for low-resource\nlanguage pairs has been receiving the spotlight in the recent NMT research\narena, thus leading to a substantial amount of research reported on this topic.\nThis paper presents a detailed survey of research advancements in low-resource\nlanguage NMT (LRL-NMT), along with a quantitative analysis aimed at identifying\nthe most popular solutions. Based on our findings from reviewing previous work,\nthis survey paper provides a set of guidelines to select the possible NMT\ntechnique for a given LRL data setting. It also presents a holistic view of the\nLRL-NMT research landscape and provides a list of recommendations to further\nenhance the research efforts on LRL-NMT.", "cat": "cs.CL", "authors": ["Surangika Ranathunga", "En-Shiun Annie Lee", "Marjana Prifti Skenduli", "Ravi Shekhar", "Mehreen Alam", "Rishemjit Kaur"]}, "634": {"id": "1811.09298v1", "title": "The SAMI Galaxy Survey: Stellar and gas misalignments and the origin of gas in nearby galaxies", "url": "http://arxiv.org/pdf/1811.09298v1", "date": "2018-11-22 20:13:42", "abs": "Misalignment of gas and stellar rotation in galaxies can give clues to the\norigin and processing of accreted gas. Integral field spectroscopic\nobservations of 1213 galaxies from the SAMI Galaxy Survey show that 11% of\ngalaxies with fitted gas and stellar rotation are misaligned by more than 30\ndegrees in both field/group and cluster environments. Using SAMI morphological\nclassifications and Sersic indices, the misalignment fraction is 45+/-6% in\nearly-type galaxies, but only 5+/-1% in late-type galaxies. The distribution of\nposition angle offsets is used to test the physical drivers of this difference.\nSlower dynamical settling time of the gas in elliptical stellar mass\ndistributions accounts for a small increase in misalignment in early-type\ngalaxies. However, gravitational dynamical settling time is insufficient to\nfully explain the observed differences between early- and late-type galaxies in\nthe distributions of the gas/stellar position angle offsets. LTGs have\nprimarily accreted gas close to aligned rather than settled from misaligned\nbased on analysis of the skewed distribution of PA offsets compared to a\ndynamical settling model. Local environment density is less important in\nsetting the misalignment fractions than morphology, suggesting that mergers are\nnot the main source of accreted gas in these disks. Cluster environments are\nfound to have gas misalignment driven primarily by cluster processes not by gas\naccretion.", "cat": "astro-ph.GA", "authors": ["J. J. Bryant", "S. M. Croom", "J. van de Sande", "N. Scott", "L. M. R. Fogarty", "J. Bland-Hawthorn", "J. V. Bloom", "E. N. Taylor", "S. Brough", "A. Robotham", "L. Cortese", "W. Couch", "M. S. Owers", "A. M. Medling", "C. Federrath", "K. Bekki", "S. N. Richards", "J. S. Lawrence", "I. S. Konstantopoulos"]}, "635": {"id": "2312.01058v1", "title": "A Survey of Progress on Cooperative Multi-agent Reinforcement Learning in Open Environment", "url": "http://arxiv.org/pdf/2312.01058v1", "date": "2023-12-02 08:04:31", "abs": "Multi-agent Reinforcement Learning (MARL) has gained wide attention in recent\nyears and has made progress in various fields. Specifically, cooperative MARL\nfocuses on training a team of agents to cooperatively achieve tasks that are\ndifficult for a single agent to handle. It has shown great potential in\napplications such as path planning, autonomous driving, active voltage control,\nand dynamic algorithm configuration. One of the research focuses in the field\nof cooperative MARL is how to improve the coordination efficiency of the\nsystem, while research work has mainly been conducted in simple, static, and\nclosed environment settings. To promote the application of artificial\nintelligence in real-world, some research has begun to explore multi-agent\ncoordination in open environments. These works have made progress in exploring\nand researching the environments where important factors might change. However,\nthe mainstream work still lacks a comprehensive review of the research\ndirection. In this paper, starting from the concept of reinforcement learning,\nwe subsequently introduce multi-agent systems (MAS), cooperative MARL, typical\nmethods, and test environments. Then, we summarize the research work of\ncooperative MARL from closed to open environments, extract multiple research\ndirections, and introduce typical works. Finally, we summarize the strengths\nand weaknesses of the current research, and look forward to the future\ndevelopment direction and research problems in cooperative MARL in open\nenvironments.", "cat": "cs.MA", "authors": ["Lei Yuan", "Ziqian Zhang", "Lihe Li", "Cong Guan", "Yang Yu"]}, "636": {"id": "1207.3460v1", "title": "PS2: Managing the next step in the Pan-STARRS wide field survey system", "url": "http://arxiv.org/pdf/1207.3460v1", "date": "2012-07-14 20:49:06", "abs": "The Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) is\nunique among the existing or planned major ground-based optical survey systems\nas the only \"distributed aperture\" system. The concept of increasing system\n\\'etendue by replicating small telescopes and digital cameras presents both\nmanagement opportunities and challenges. The focus in this paper is on\nmanagement lessons learned from PS1, and how those have been used to form the\nmanagement plan for PS2. The management plan components emphasized here include\ntechnical development, financial and schedule planning, and critical path and\nrisk management. Finally, the status and schedule for PS2 are presented.", "cat": "astro-ph.IM", "authors": ["William S. Burgett"]}, "637": {"id": "1312.3281v1", "title": "The Ultraviolet Sky: An Overview from the GALEX Surveys", "url": "http://arxiv.org/pdf/1312.3281v1", "date": "2013-12-11 19:13:14", "abs": "The Galaxy Evolution Explorer (GALEX) has performed the first surveys of the\nsky in the Ultraviolet (UV). Its legacy is an unprecedented database with more\nthan 200 million source measurements in far-UV (FUV) and near-UV (NUV), as well\nas wide-field imaging of extended objects, filling an important gap in our view\nof the sky across the electromagnetic spectrum. The UV surveys offer unique\nsensitivity for identifying and studying selected classes of astrophysical\nobjects, both stellar and extra-galactic. We examine the overall content and\ndistribution of UV sources over the sky, and with magnitude and color. For this\npurpose, we have constructed final catalogs of UV sources with homogeneous\nquality, eliminating duplicate measurements of the same source. Such catalogs\ncan facilitate a variety of investigations on UV-selected samples, as well as\nplanning of observations with future missions.\n We describe the criteria used to build the catalogs, their coverage and\ncompleteness. We included observations in which both the far-UV and near-UV\ndetectors were exposed; 28,707 fields from the All-Sky Imaging survey (AIS)\ncover a unique area of 22,080 square degrees (after we restrict the catalogs to\nthe central 1-degree diameter of the field), with a typical depth of about\n20/21 mag (FUV/NUV, in the AB mag system), and 3,008 fields from the\nMedium-depth Imaging Survey (MIS) cover a total of 2,251 square degrees at a\ndepth of about 22.7mag. The catalogs contain about 71 and 16.6 million sources\nrespectively. The density of hot stars reflects the Galactic structure, and the\nnumber counts of both Galactic and extra-galactic sources are modulated by the\nMilky Way dust extinction, to which the UV data are very sensitive.", "cat": "astro-ph.GA", "authors": ["Luciana Bianchi", "Alberto Conti", "Bernie Shiao"]}, "638": {"id": "2212.00481v1", "title": "A Survey of Mobile Edge Computing for the Metaverse: Architectures, Applications, and Challenges", "url": "http://arxiv.org/pdf/2212.00481v1", "date": "2022-12-01 13:14:20", "abs": "Metaverse is an emerging virtual universe where humans can have real-time\ninteractions and solid social links like in the physical world, and it opens up\na new era of Internet and interactions. In Metaverse, an immersive and\nphotorealistic environment promotes social activities, including education,\nmeetings, and shopping of digital avatars based on critical technologies,\nincluding 3D rendering, extended reality, digital twins, artificial\nintelligence, and Blockchain. However, the limitations of computation, storage,\nand energy resources restrict the development of Metaverse, and a series of\nsystem issues (e.g., latency, security, and battery-life) continue to arise. As\na result, how to find corresponding measurements to mitigate unsatisfactory\ninfluences becomes the focus. Mobile edge computing (MEC) as a distributed\ncomputing paradigm offloads computation-intensive tasks to the edge of the\nnetwork. It brings the resources as close as possible to the end devices,\naddressing the shortcomings mentioned above. In this paper, we propose a\ncomprehensive survey of the MEC-based Metaverse. Particular emphasis is given\nto the technologies convergence, architectures, and application scenarios,\ne.g., BoundlessXR and CloudXR. Significantly, we introduce the potential future\ndirections for developing Metaverse systems.", "cat": "cs.NI", "authors": ["Yitong Wang", "Jun Zhao"]}, "639": {"id": "1906.05074v1", "title": "Different Approaches for Human Activity Recognition: A Survey", "url": "http://arxiv.org/pdf/1906.05074v1", "date": "2019-06-11 04:12:15", "abs": "Human activity recognition has gained importance in recent years due to its\napplications in various fields such as health, security and surveillance,\nentertainment, and intelligent environments. A significant amount of work has\nbeen done on human activity recognition and researchers have leveraged\ndifferent approaches, such as wearable, object-tagged, and device-free, to\nrecognize human activities. In this article, we present a comprehensive survey\nof the work conducted over the period 2010-2018 in various areas of human\nactivity recognition with main focus on device-free solutions. The device-free\napproach is becoming very popular due to the fact that the subject is not\nrequired to carry anything, instead, the environment is tagged with devices to\ncapture the required information. We propose a new taxonomy for categorizing\nthe research work conducted in the field of activity recognition and divide the\nexisting literature into three sub-areas: action-based, motion-based, and\ninteraction-based. We further divide these areas into ten different sub-topics\nand present the latest research work in these sub-topics. Unlike previous\nsurveys which focus only on one type of activities, to the best of our\nknowledge, we cover all the sub-areas in activity recognition and provide a\ncomparison of the latest research work in these sub-areas. Specifically, we\ndiscuss the key attributes and design approaches for the work presented. Then\nwe provide extensive analysis based on 10 important metrics, to give the\nreader, a complete overview of the state-of-the-art techniques and trends in\ndifferent sub-areas of human activity recognition. In the end, we discuss open\nresearch issues and provide future research directions in the field of human\nactivity recognition.", "cat": "cs.CV", "authors": ["Zawar Hussain", "Michael Sheng", "Wei Emma Zhang"]}, "640": {"id": "2404.01774v2", "title": "MHONGOOSE -- A MeerKAT Nearby Galaxy HI Survey", "url": "http://arxiv.org/pdf/2404.01774v2", "date": "2024-06-06 11:21:43", "abs": "The MHONGOOSE (MeerKAT HI Observations of Nearby Galactic Objects: Observing\nSouthern Emitters) survey maps the distribution and kinematics of the neutral\natomic hydrogen (HI) gas in and around 30 nearby star-forming spiral and dwarf\ngalaxies to extremely low HI column densities. The HI column density\nsensitivity (3 sigma over 16 km/s) ranges from ~ 5 x 10^{17} cm^{-2} at 90''\nresolution to ~4 x 10^{19} cm^{-2} at the highest resolution of 7''. The HI\nmass sensitivity (3 sigma over 50 km/s) is ~5.5 X 10^5 M_sun at a distance of\n10 Mpc (the median distance of the sample galaxies). The velocity resolution of\nthe data is 1.4 km/s. One of the main science goals of the survey is the\ndetection of cold, accreting gas in the outskirts of the sample galaxies. The\nsample was selected to cover a range in HI masses, from 10^7 M_sun to almost\n10^{11} M_sun, to optimally sample possible accretion scenarios and\nenvironments. The distance to the sample galaxies ranges from 3 to 23 Mpc. In\nthis paper, we present the sample selection, survey design, and observation and\nreduction procedures. We compare the integrated HI fluxes based on the MeerKAT\ndata with those derived from single-dish measurement and find good agreement,\nindicating that our MeerKAT observations are recovering all flux. We present HI\nmoment maps of the entire sample based on the first ten percent of the survey\ndata, and find that a comparison of the zeroth- and second-moment values shows\na clear separation between the physical properties of the HI in areas with star\nformation and areas without, related to the formation of a cold neutral medium.\nFinally, we give an overview of the HI-detected companion and satellite\ngalaxies in the 30 fields, five of which have not previously been catalogued.\nWe find a clear relation between the number of companion galaxies and the mass\nof the main target galaxy.", "cat": "astro-ph.GA", "authors": ["W. J. G. de Blok", "J. Healy", "F. M. Maccagni", "D. J. Pisano", "A. Bosma", "J. English", "T. Jarrett", "A. Marasco", "G. R. Meurer", "S. Veronese", "F. Bigiel", "L. Chemin", "F. Fraternali", "B. W. Holwerda", "P. Kamphuis", "H. R. Kl\u00f6ckner", "D. Kleiner", "A. K. Leroy", "M. Mogotsi", "K. A. Oman", "E. Schinnerer", "L. Verdes-Montenegro", "T. Westmeier", "O. I. Wong", "N. Zabel", "P. Amram", "C. Carignan", "F. Combes", "E. Brinks", "R. J. Dettmar", "B. K. Gibson", "G. I. G. Jozsa", "B. S. Koribalski", "S. S. McGaugh", "T. A. Oosterloo", "K. Spekkens", "A. C. Schr\u00f6der", "E. A. K. Adams", "E. Athanassoula", "M. A. Bershady", "R. J. Beswick", "S. Blyth", "E. C. Elson", "B. S. Frank", "G. Heald", "P. A. Henning", "S. Kurapati", "S. I. Loubser", "D. Lucero", "M. Meyer", "B. Namumba", "S. -H. Oh", "A. Sardone", "K. Sheth", "M. W. L. Smith", "A. Sorgho", "F. Walter", "T. Williams", "P. A. Woudt", "A. Zijlstra"]}, "641": {"id": "2108.11411v1", "title": "A case study of ACV variables discovered in the Zwicky Transient Facility survey", "url": "http://arxiv.org/pdf/2108.11411v1", "date": "2021-08-25 18:08:00", "abs": "Magnetic chemically peculiar (mCP) stars exhibit complex atmospheres that\nallow the investigation of the interplay of atomic diffusion, magnetic fields,\nand stellar rotation. A non-uniform surface distribution of chemical elements\nand the non-alignment of the rotational and magnetic axes result in the\nvariability of several observables. Photometrically variable mCP stars are\nreferred to as alpha2 Canum Venaticorum (ACV) variables. The present work\npresents a case study of known variables from the Zwicky Transient Facility\n(ZTF) survey, with the aim of investigating the survey's suitability for the\ndetection and study of new ACV variables. Using suitable selection criteria\nbased on the known characteristics of ACV variables, candidate ACV stars were\nselected from the ZTF Catalog of Periodic Variable Stars. All light curves were\ninspected in detail to select the most promising candidates. Where available,\nlow-resolution spectra from the LAMOST were employed to classify the stars on\nthe MK system and confirm their status as mCP stars. We have identified 86 new\npromising ACV star candidates. 15 of these stars have LAMOST spectra available,\nwhich, in all cases, confirm them as classical mCP stars, which highlights the\nviability of our approach. The sample stars can be sorted into four subgroups\ncharacterized by distinct light curve shapes. Anti-phase variations in\ndifferent photometric passbands, in particular, is a unique characteristic of a\nsubset of ACV stars readily usable for their identification. The availability\nof data in three different passbands (g, r, and i) is a major advantage of the\nZTF survey. On the basis of our experience with other photometric surveys and\nthe analysis of light curves, we conclude that the ZTF is well suited for the\nsearch for, and the analysis of, ACV variables, which, however, are not\nconsidered in the available ZTF variable star catalogues.", "cat": "astro-ph.SR", "authors": ["N. Faltov\u00e1", "K. Kallov\u00e1", "M. Pri\u0161egen", "P. Stan\u011bk", "J. Sup\u00edkov\u00e1", "C. Xia", "K. Bernhard", "S. H\u00fcmmerich", "E. Paunzen"]}, "642": {"id": "0907.2372v1", "title": "Analysis of hydrogen-rich magnetic white dwarfs detected in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/0907.2372v1", "date": "2009-07-14 15:01:05", "abs": "We model the structure of the surface magnetic fields of the hydrogen-rich\nwhite dwarfs in the SDSS. We have calculated a grid of state-of-the-art\ntheoretical optical spectra of hydrogen-rich magnetic white dwarfs with\nmagnetic field strengths between 1 MG and 1200 MG for different angles, and for\neffective temperatures between 7000 K and 50000 K. We used a least-squares\nminimization scheme with an evolutionary algorithm in order to find the\nmagnetic field geometry best fitting the observed data. We used simple centered\ndipoles or dipoles which were shifted along the dipole axis to model the\ncoadded SDSS fiber spectrum of each object. We have analysed the spectra of all\nknown magnetic DAs from the SDSS (97 previously published plus 44 newly\ndiscovered) and also investigated the statistical properties of magnetic field\ngeometries of this sample. The total number of known magnetic white dwarfs\nalready more than tripled by the SDSS and more objects are expected from a more\nsystematic search. The magnetic fields span a range between ~1 and 900 MG. Our\nresults further support the claim that Ap/Bp population is insufficient in\ngenerating the numbers and field strength distributions of the observed MWDs,\nand either another source of progenitor types or binary evolution is needed.\nMoreover clear indications for non-centered dipoles exist in about ~50% of the\nobjects which is consistent with the magnetic field distribution observed in\nAp/Bp stars.", "cat": "astro-ph.SR", "authors": ["B. Kulebi", "S. Jordan", "F. Euchner", "B. Gaensicke", "H. Hirsch"]}, "643": {"id": "2309.01477v1", "title": "Towards Measuring Microlensing Event Rate in the Galactic Center: I. Events Detection from the UKIRT Microlensing Survey Data", "url": "http://arxiv.org/pdf/2309.01477v1", "date": "2023-09-04 09:32:19", "abs": "To overcome the high optical extinction, near-infrared observations are\nneeded for probing the microlensing events toward the Galactic center. The\n2015-2019 UKIRT microlensing survey toward the Galactic center is the first\ndedicated precursor near-infrared (NIR) survey for the Nancy Grace Roman Space\nTelescope. We here analyze the online data from the UKIRT microlensing survey,\nreaching $l=b=0^\\circ$. Using the event-finder algorithm of KMTNet with the\n$\\Delta \\chi^2$ threshold of 250, we find 522 clear events, 436 possible\nevents, and 27 possible anomalous events. We fit a point-source point-lens\n(PSPL) model to all the clear events and derive the PSPL parameters with\nuncertainties using a Markov chain Monte Carlo method. Assuming perfect\ndetection efficiency, we compute the uncorrected event rates, which should\nserve as the lower limits on the true event rate. We find that the uncorrected\nNIR event rates are likely rising toward the Galactic center and higher than\nthe optical event rates.", "cat": "astro-ph.EP", "authors": ["Yongxin Wen", "Weicheng Zang", "Bo Ma"]}, "644": {"id": "0707.3578v1", "title": "The history of star-forming galaxies in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/0707.3578v1", "date": "2007-07-24 15:39:07", "abs": "We study the evolution of 82302 star-forming (SF) galaxies from the SDSS. Our\nmain goals are to explore new ways of handling star formation histories (SFH)\nobtained with our publicly available spectral synthesis code STARLIGHT, and\napply them to investigate how SFHs vary as a function of nebular metallicity\n(Zneb). Our main results are: (1) A conventional correlation analysis shows how\nglobal properties such as luminosity, mass, dust content, mean stellar\nmetallicity and mean stellar age relate to Zneb. (2) We present a simple\nformalism which compresses the results of the synthesis into time-dependent\nstar formation rates (SFR) and mass assembly histories. (3) The current SFR\nderived from the population synthesis and that from H-alpha are shown to agree\nwithin a factor of two. Thus we now have a way to estimate SFR in AGN hosts,\nwhere the H-alpha method cannot be applied. (4) Fully time-dependent SFHs are\nderived for all galaxies and averaged over six Zneb bins spanning the entire SF\nwing in the [OIII]/H-beta X [NII]/H-alpha diagram. (5) We find that SFHs vary\nsystematically along the SF sequence, such that low-Zneb systems evolve slower\nand are currently forming stars at a higher relative rate. (6) At any given\ntime, the distribution of specific SFRs for galaxies within a Zneb-bin is broad\nand roughly log-normal. (7) The same results are found grouping galaxies in\nstellar mass (M*) or surface mass density (S*) bins. (8) The overall pattern of\nSFHs as a function of Zneb, M* or S* is robust against changes in selection\ncriteria, choice of evolutionary synthesis models for the spectral fits, and\ndifferential extinction effects. (Abridged)", "cat": "astro-ph", "authors": ["N. V. Asari", "R. Cid Fernandes", "G. Stasinska", "J. P. Torres-Papaqui", "A. Mateus", "L. Sodre Jr.", "W. Schoenell", "J. M. Gomes"]}, "645": {"id": "2402.01166v2", "title": "A Comprehensive Survey on 3D Content Generation", "url": "http://arxiv.org/pdf/2402.01166v2", "date": "2024-03-19 08:22:42", "abs": "Recent years have witnessed remarkable advances in artificial intelligence\ngenerated content(AIGC), with diverse input modalities, e.g., text, image,\nvideo, audio and 3D. The 3D is the most close visual modality to real-world 3D\nenvironment and carries enormous knowledge. The 3D content generation shows\nboth academic and practical values while also presenting formidable technical\nchallenges. This review aims to consolidate developments within the burgeoning\ndomain of 3D content generation. Specifically, a new taxonomy is proposed that\ncategorizes existing approaches into three types: 3D native generative methods,\n2D prior-based 3D generative methods, and hybrid 3D generative methods. The\nsurvey covers approximately 60 papers spanning the major techniques. Besides,\nwe discuss limitations of current 3D content generation techniques, and point\nout open challenges as well as promising directions for future work.\nAccompanied with this survey, we have established a project website where the\nresources on 3D content generation research are provided. The project page is\navailable at https://github.com/hitcslj/Awesome-AIGC-3D.", "cat": "cs.CV", "authors": ["Jian Liu", "Xiaoshui Huang", "Tianyu Huang", "Lu Chen", "Yuenan Hou", "Shixiang Tang", "Ziwei Liu", "Wanli Ouyang", "Wangmeng Zuo", "Junjun Jiang", "Xianming Liu"]}, "646": {"id": "0711.3199v3", "title": "Analyzing and Modeling Real-World Phenomena with Complex Networks: A Survey of Applications", "url": "http://arxiv.org/pdf/0711.3199v3", "date": "2008-09-16 20:03:59", "abs": "The success of new scientific areas can be assessed by their potential for\ncontributing to new theoretical approaches and in applications to real-world\nproblems. Complex networks have fared extremely well in both of these aspects,\nwith their sound theoretical basis developed over the years and with a variety\nof applications. In this survey, we analyze the applications of complex\nnetworks to real-world problems and data, with emphasis in representation,\nanalysis and modeling, after an introduction to the main concepts and models. A\ndiversity of phenomena are surveyed, which may be classified into no less than\n22 areas, providing a clear indication of the impact of the field of complex\nnetworks.", "cat": "physics.soc-ph", "authors": ["Luciano da F. Costa", "Osvaldo N. Oliveira Jr.", "Gonzalo Travieso", "Francisco A. Rodrigues", "Paulino R. Villas Boas", "Lucas Antiqueira", "Matheus P. Viana", "Luis E. C. da Rocha"]}, "647": {"id": "1605.01215v1", "title": "HELP-ing Extragalactic Surveys : The Herschel Extragalactic Legacy Project and The Coming of Age of Multi-Wavelength Astrophysics", "url": "http://arxiv.org/pdf/1605.01215v1", "date": "2016-05-04 10:47:09", "abs": "How did galaxies form and evolve? This is one of the most challenging\nquestions in astronomy to- day. Answering it requires a careful combination of\nobservational and theoretical work to reliably determine the observed\nproperties of cosmic bodies over large portions of the distant Universe on the\none hand, and accurately model the physical processes driving their evolution\non the other. Most importantly, it requires bringing together disparate\nmulti-wavelength and multi-resolution spectro-photometric datasets in an\nhomogeneous and well-characterized manner so that they are suitable for a\nrigorous statistical analysis. The Herschel Extragalactic Legacy Project (HELP)\nfunded by the EC FP7 SPACE program aims to achieve this goal by combining the\nexpertise of optical, infrared and radio astronomers to provide a\nmulti-wavelength database for the dis- tant Universe as an accessible\nvalue-added resource for the astronomical community. It will do so by bringing\ntogether multi-wavelength datasets covering the 1000 deg2 mapped by Herschel\nextragalactic surveys and thus creating a joint lasting legacy from several\nambitious sky surveys.", "cat": "astro-ph.GA", "authors": ["Mattia Vaccari"]}, "648": {"id": "1505.01945v1", "title": "Composition operators on vector-valued analytic function spaces: a survey", "url": "http://arxiv.org/pdf/1505.01945v1", "date": "2015-05-08 07:28:30", "abs": "We survey recent results about composition operators induced by analytic\nself-maps of the unit disk in the complex plane on various Banach spaces of\nanalytic functions taking values in infinite-dimensional Banach spaces. We\nmostly concentrate on the research line into qualitative properties such as\nweak compactness, initiated by Liu, Saksman and Tylli (1998), and continued in\nseveral other papers. We discuss composition operators on strong, respectively\nweak, spaces of vector-valued analytic functions, as well as between weak and\nstrong spaces. As concrete examples, we review more carefully and present some\nnew observations in the cases of vector-valued Hardy and BMOA spaces, though\nthe study of composition operators has been extended to a wide range of spaces\nof vector-valued analytic functions, including spaces defined on other domains.\nSeveral open problems are stated.", "cat": "math.FA", "authors": ["Jussi Laitila", "Hans-Olav Tylli"]}, "649": {"id": "2210.12062v1", "title": "A survey of open questions in adaptive therapy: bridging mathematics and clinical translation", "url": "http://arxiv.org/pdf/2210.12062v1", "date": "2022-10-18 17:47:15", "abs": "Adaptive therapy is a dynamic cancer treatment protocol that updates (or\n\"adapts\") treatment decisions in anticipation of evolving tumor dynamics. This\nbroad term encompasses many possible dynamic treatment protocols of\npatient-specific dose modulation or dose timing. Adaptive therapy maintains\nhigh levels of tumor burden to benefit from the competitive suppression of\ntreatment-sensitive subpopulations on treatment-resistant subpopulations. This\nevolution-based approach to cancer treatment has been integrated into several\nongoing or planned clinical trials, including treatment of metastatic castrate\nresistant prostate cancer, ovarian cancer, and BRAF-mutant melanoma. In the\nprevious few decades, experimental and clinical investigation of adaptive\ntherapy has progressed synergistically with mathematical and computational\nmodeling. In this work, we discuss 11 open questions in cancer adaptive therapy\nmathematical modeling. The questions are split into three sections: 1) the\nnecessary components of mathematical models of adaptive therapy 2) design and\nvalidation of dosing protocols, and 3) challenges and opportunities in clinical\ntranslation.", "cat": "q-bio.TO", "authors": ["Jeffrey West", "Fred Adler", "Jill Gallaher", "Maximilian Strobl", "Renee Brady-Nicholls", "Joel S. Brown", "Mark Robertson-Tessi", "Eunjung Kim", "Robert Noble", "Yannick Viossat", "David Basanta", "Alexander R. A. Anderson"]}, "650": {"id": "1709.04134v1", "title": "Exploring the expansion dynamics of the universe from galaxy cluster surveys", "url": "http://arxiv.org/pdf/1709.04134v1", "date": "2017-09-13 04:49:46", "abs": "To understand the expansion dynamics of the universe from galaxy cluster\nscales, using the angular diameter distance (ADD) data from two different\ngalaxy cluster surveys, we constrain four cosmological models to explore the\nunderlying value of $H_0$ and employ the model-independent Gaussian Processes\nto investigate the evolution of the equation of state of dark energy. The ADD\ndata in the X-ray bands consists of two samples covering the redshift ranges\n[0.023, 0.784] and [0.14, 0.89], respectively. We find that: (i) For these two\nsamples, the obtained values of $H_0$ are more consistent with the recent local\nobservation by Riess et al. than the global measurement by the Plank\nCollaboration, and the $\\Lambda$CDM model is still preferred utilizing the\ninformation criterions; (ii) For the first sample, there is no evidence of\ndynamical dark energy (DDE) at the $2\\sigma$ confidence level (CL); (iii) For\nthe second one, the reconstructed equation of state of dark energy exhibits a\nphantom-crossing behavior in the relatively low redshift range over the\n$2\\sigma$ CL, which gives a hint that the late-time universe may be actually\ndominated by the DDE from galaxy cluster scales; (iv) By adding a combination\nof Type Ia Supernovae, cosmic chronometers and Planck-2015 shift parameter and\nHII galaxy measurements into both ADD samples, the DDE exists evidently over\nthe $2\\sigma$ CL.", "cat": "astro-ph.CO", "authors": ["Deng Wang", "Xin-He Meng"]}, "651": {"id": "1611.06334v1", "title": "A Survey of Methods for Collective Communication Optimization and Tuning", "url": "http://arxiv.org/pdf/1611.06334v1", "date": "2016-11-19 10:02:40", "abs": "New developments in HPC technology in terms of increasing computing power on\nmulti/many core processors, high-bandwidth memory/IO subsystems and\ncommunication interconnects, pose a direct impact on software and runtime\nsystem development. These advancements have become useful in producing\nhigh-performance collective communication interfaces that integrate efficiently\non a wide variety of platforms and environments. However, number of\noptimization options that shows up with each new technology or software\nframework has resulted in a \\emph{combinatorial explosion} in feature space for\ntuning collective parameters such that finding the optimal set has become a\nnearly impossible task. Applicability of algorithmic choices available for\noptimizing collective communication depends largely on the scalability\nrequirement for a particular usecase. This problem can be further exasperated\nby any requirement to run collective problems at very large scales such as in\nthe case of exascale computing, at which impractical tuning by brute force may\nrequire many months of resources. Therefore application of statistical, data\nmining and artificial Intelligence or more general hybrid learning models seems\nessential in many collectives parameter optimization problems. We hope to\nexplore current and the cutting edge of collective communication optimization\nand tuning methods and culminate with possible future directions towards this\nproblem.", "cat": "cs.DC", "authors": ["Udayanga Wickramasinghe", "Andrew Lumsdaine"]}, "652": {"id": "2211.15588v1", "title": "Internet of Behaviors: A Survey", "url": "http://arxiv.org/pdf/2211.15588v1", "date": "2022-11-28 17:44:32", "abs": "The Internet of Behavior is a research theme that aims to analyze human\nbehavior data on the Internet from the perspective of behavioral psychology,\nobtain insights about human behavior, and better understand the intention\nbehind the behavior. In this way, the Internet of Behavior can predict human\nbehavioral trends in the future and even change human behavior, which can\nprovide more convenience for human life. With the increasing prosperity of the\nInternet of Things, more and more behavior-related data is collected on the\nInternet by connected devices such as sensors. People and behavior are\nconnected through the extension of the Internet of Things -- the Internet of\nBehavior. At present, the Internet of Behavior has gradually been applied to\nour lives, but it is still in its early stages, and many opportunities and\nchallenges are emerging. This paper provides an in-depth overview of the\nfundamental aspects of the Internet of Behavior: (1) We introduce the\ndevelopment process and research status of the Internet of Behavior from the\nperspective of the Internet of Things. (2) We propose the characteristics of\nthe Internet of Behavior and define its development direction in terms of three\naspects: real-time, autonomy, and reliability. (3) We provide a comprehensive\nsummary of the current applications of the Internet of Behavior, including\nspecific discussions in five scenarios that give an overview of the application\nstatus of the Internet of Behavior. (4) We discuss the challenges of the\nInternet of Behavior's development and its future directions, which hopefully\nwill bring some progress to the Internet of Behavior. To the best of our\nknowledge, this is the first survey paper on the Internet of Behavior. We hope\nthat this in-depth review can provide some useful directions for more\nproductive research in related fields.", "cat": "cs.DB", "authors": ["Jiayi Sun", "Wensheng Gan", "Han-Chieh Chao", "Philip S. Yu", "Weiping Ding"]}, "653": {"id": "1904.05409v1", "title": "A survey of the additive dilogarithm", "url": "http://arxiv.org/pdf/1904.05409v1", "date": "2019-04-10 19:49:58", "abs": "Borel's construction of the regulator gives an injective map from the\nalgebraic $K$-groups of a number field to its Deligne-Beilinson cohomology\ngroups. This has many interesting arithmetic and geometric consequences. The\nformula for the regulator is expressed in terms of the classical polyogarithm\nfunctions. In this paper, we give a survey of the additive dilogarithm and the\nseveral different versions of the weight two regulator in the infinitesimal\nsetting. We follow a historical approach which we hope will provide motivation\nfor the definitions and the constructions.", "cat": "math.AG", "authors": ["Sinan Unver"]}, "654": {"id": "2004.13920v1", "title": "HST survey of the Orion Nebula Cluster in the H$_2$O 1.4 $\u03bc$m absorption band: II. The substellar IMF down to planetary masses", "url": "http://arxiv.org/pdf/2004.13920v1", "date": "2020-04-29 02:06:59", "abs": "We exploit the ability of the Hubble Space Telescope to probe near infrared\nwater absorption present in the atmosphere of low-mass stars, brown dwarfs and\nplanetary mass objects to create a very pure sample of Orion Nebula Cluster\n(ONC) members, not affected by contamination from background stars and galaxies\nwhich lack water absorption. Thanks to these data we infer the Initial Mass\nFunction (IMF) of the ONC in the $0.005 - 1.4$M$_{\\odot}$ regime, i.e. down to\nfew Jupiter masses. The young age of the ONC, $\\sim1$ Myr, provides a snapshot\nof the outcome of star formation for the present-day conditions (metallicity,\ntemperature, pressure) of typical Milky Way disk molecular clouds. We\ndemonstrate that the IMF of the ONC is well described by either a log-normal\nfunction or a broken power-law, with parameter values qualitatively in\nagreement with the canonical Chabrier or Kroupa forms for the Milky Way disk\nIMF. This continuity in the mass distribution provides clues to the fact that\nthe same physical processes may be regulating formation of stars, brown dwarfs,\nand planetary mass objects. Both the canonical IMF forms under-predict the\nobserved number of very low mass members (below $0.1$ M$_\\odot$), a regime\nwhere our data allows more precise constraints. Nevertheless, we do not observe\na rise or secondary peak in the brown dwarfs or planetary mass regimes. Our\nstudy thus contradicts findings based on broad-band near infrared ground-based\nphotometry, which predict an extremely high number of free-floating planets,\nbut likely suffer from unaccounted background contamination.", "cat": "astro-ph.SR", "authors": ["Mario Gennaro", "Massimo Robberto"]}, "655": {"id": "2110.01858v1", "title": "KKT Conditions, First-Order and Second-Order Optimization, and Distributed Optimization: Tutorial and Survey", "url": "http://arxiv.org/pdf/2110.01858v1", "date": "2021-10-05 07:50:37", "abs": "This is a tutorial and survey paper on Karush-Kuhn-Tucker (KKT) conditions,\nfirst-order and second-order numerical optimization, and distributed\noptimization. After a brief review of history of optimization, we start with\nsome preliminaries on properties of sets, norms, functions, and concepts of\noptimization. Then, we introduce the optimization problem, standard\noptimization problems (including linear programming, quadratic programming, and\nsemidefinite programming), and convex problems. We also introduce some\ntechniques such as eliminating inequality, equality, and set constraints,\nadding slack variables, and epigraph form. We introduce Lagrangian function,\ndual variables, KKT conditions (including primal feasibility, dual feasibility,\nweak and strong duality, complementary slackness, and stationarity condition),\nand solving optimization by method of Lagrange multipliers. Then, we cover\nfirst-order optimization including gradient descent, line-search, convergence\nof gradient methods, momentum, steepest descent, and backpropagation. Other\nfirst-order methods are explained, such as accelerated gradient method,\nstochastic gradient descent, mini-batch gradient descent, stochastic average\ngradient, stochastic variance reduced gradient, AdaGrad, RMSProp, and Adam\noptimizer, proximal methods (including proximal mapping, proximal point\nalgorithm, and proximal gradient method), and constrained gradient methods\n(including projected gradient method, projection onto convex sets, and\nFrank-Wolfe method). We also cover non-smooth and $\\ell_1$ optimization methods\nincluding lasso regularization, convex conjugate, Huber function,\nsoft-thresholding, coordinate descent, and subgradient methods. Then, we\nexplain second-order methods including Newton's method for unconstrained,\nequality constrained, and inequality constrained problems....", "cat": "math.OC", "authors": ["Benyamin Ghojogh", "Ali Ghodsi", "Fakhri Karray", "Mark Crowley"]}, "656": {"id": "2205.01500v2", "title": "Meta Learning for Natural Language Processing: A Survey", "url": "http://arxiv.org/pdf/2205.01500v2", "date": "2022-07-02 22:37:22", "abs": "Deep learning has been the mainstream technique in natural language\nprocessing (NLP) area. However, the techniques require many labeled data and\nare less generalizable across domains. Meta-learning is an arising field in\nmachine learning studying approaches to learn better learning algorithms.\nApproaches aim at improving algorithms in various aspects, including data\nefficiency and generalizability. Efficacy of approaches has been shown in many\nNLP tasks, but there is no systematic survey of these approaches in NLP, which\nhinders more researchers from joining the field. Our goal with this survey\npaper is to offer researchers pointers to relevant meta-learning works in NLP\nand attract more attention from the NLP community to drive future innovation.\nThis paper first introduces the general concepts of meta-learning and the\ncommon approaches. Then we summarize task construction settings and application\nof meta-learning for various NLP problems and review the development of\nmeta-learning in NLP community.", "cat": "cs.CL", "authors": ["Hung-yi Lee", "Shang-Wen Li", "Ngoc Thang Vu"]}, "657": {"id": "1903.11042v1", "title": "CHANG-ES: XVIII---The CHANG-ES Survey and Selected Results", "url": "http://arxiv.org/pdf/1903.11042v1", "date": "2019-03-26 17:42:45", "abs": "The CHANG-ES (Continuum Halos in Nearby Galaxies) survey of 35 nearby edge-on\ngalaxies is revealing new and sometimes unexpected and startling results in\ntheir radio continuum emission. The observations were in wide bandwidths\ncentered at 1.6 and 6.0 GHz. Unique to this survey is full polarization data\nshowing magnetic field structures in unprecedented detail, resolution and\nsensitivity for such a large sample. A wide range of new results are reported\nhere, some never before seen in any galaxy. We see circular polarization and\nvariability in active galactic nuclei (AGNs), in-disk discrete features,\ndisk-halo structures sometimes only seen in polarization, and broad-scale halos\nwith reversing magnetic fields, among others. This paper summarizes some of the\nCHANG-ES results seen thus far. Released images can be found at\nhttps://www.queensu.ca/changes.", "cat": "astro-ph.GA", "authors": ["Judith Irwin", "Ancor Damas-Segovia", "Marita Krause", "Arpad Miskolczi", "Jiangtao Li", "Yelena Stein", "Jayanne English", "Richard Henriksen", "Rainer Beck", "Theresa Wiegert", "Ralf-Juergen Dettmar"]}, "658": {"id": "2311.00082v1", "title": "UAV Immersive Video Streaming: A Comprehensive Survey, Benchmarking, and Open Challenges", "url": "http://arxiv.org/pdf/2311.00082v1", "date": "2023-10-31 18:45:27", "abs": "Over the past decade, the utilization of UAVs has witnessed significant\ngrowth, owing to their agility, rapid deployment, and maneuverability. In\nparticular, the use of UAV-mounted 360-degree cameras to capture\nomnidirectional videos has enabled truly immersive viewing experiences with up\nto 6DoF. However, achieving this immersive experience necessitates encoding\nomnidirectional videos in high resolution, leading to increased bitrates.\nConsequently, new challenges arise in terms of latency, throughput, perceived\nquality, and energy consumption for real-time streaming of such content. This\npaper presents a comprehensive survey of research efforts in UAV-based\nimmersive video streaming, benchmarks popular video encoding schemes, and\nidentifies open research challenges. Initially, we review the literature on\n360-degree video coding, packaging, and streaming, with a particular focus on\nstandardization efforts to ensure interoperability of immersive video streaming\ndevices and services. Subsequently, we provide a comprehensive review of\nresearch efforts focused on optimizing video streaming for timevarying UAV\nwireless channels. Additionally, we introduce a high resolution 360-degree\nvideo dataset captured from UAVs under different flying conditions. This\ndataset facilitates the evaluation of complexity and coding efficiency of\nsoftware and hardware video encoders based on popular video coding standards\nand formats, including AVC/H.264, HEVC/H.265, VVC/H.266, VP9, and AV1. Our\nresults demonstrate that HEVC achieves the best trade-off between coding\nefficiency and complexity through its hardware implementation, while AV1 format\nexcels in coding efficiency through its software implementation, specifically\nusing the libsvt-av1 encoder. Furthermore, we present a real testbed showcasing\n360-degree video streaming over a UAV, enabling remote control of the drone via\na 5G cellular network.", "cat": "eess.IV", "authors": ["Mohit K. Sharma", "Chen-Feng Liu", "Ibrahim Farhat", "Nassim Sehad", "Wassim Hamidouche", "Merouane Debbah"]}, "659": {"id": "0808.2497v2", "title": "Galaxy density profiles and shapes -- II. selection biases in strong lensing surveys", "url": "http://arxiv.org/pdf/0808.2497v2", "date": "2009-06-18 22:54:42", "abs": "[Abridged] Many current and future astronomical surveys will rely on samples\nof strong gravitational lens systems to draw conclusions about galaxy mass\ndistributions. We use a new strong lensing pipeline (presented in Paper I of\nthis series) to explore selection biases that may cause the population of\nstrong lensing systems to differ from the general galaxy population. Our focus\nis on point-source lensing by early-type galaxies with two mass components\n(stellar and dark matter) that have a variety of density profiles and shapes\nmotivated by observational and theoretical studies of galaxy properties. We\nseek not only to quantify but also to understand the physics behind selection\nbiases related to: galaxy mass, orientation and shape; dark matter profile\nparameters such as inner slope and concentration; and adiabatic contraction. We\nstudy how all of these properties affect the lensing Einstein radius, total\ncross-section, quad/double ratio, and image separation distribution. We find\nsignificant (factors of several) selection biases with mass; orientation, for a\ngiven galaxy shape at fixed mass; cusped dark matter profile inner slope and\nconcentration; concentration of the stellar and dark matter deprojected Sersic\nmodels. Interestingly, the intrinsic shape of a galaxy does not strongly\ninfluence its lensing cross-section when we average over viewing angles. Our\nresults are an important first step towards understanding how strong lens\nsystems relate to the general galaxy population.", "cat": "astro-ph", "authors": ["Rachel Mandelbaum", "Glenn van de Ven", "Charles R. Keeton"]}, "660": {"id": "2203.14538v1", "title": "Zeta-Payne: a fully automated spectrum analysis algorithm for the Milky Way Mapper program of the SDSS-V survey", "url": "http://arxiv.org/pdf/2203.14538v1", "date": "2022-03-28 07:30:16", "abs": "The Sloan Digital Sky Survey has recently initiated its 5th survey generation\n(SDSS-V), with a central focus on stellar spectroscopy. In particular, SDSS-V\nMilky Way Mapper program will deliver multi-epoch optical and near-infrared\nspectra for more than 5 million stars across the entire sky, covering a large\nrange in stellar mass, surface temperature, evolutionary stage, and age. About\n10% of those spectra will be of hot stars of OBAF spectral types, for whose\nanalysis no established survey pipelines exist. Here we present the spectral\nanalysis algorithm, Zeta-Payne, developed specifically to obtain stellar labels\nfrom SDSS-V spectra of stars with these spectral types and drawing on machine\nlearning tools. We provide details of the algorithm training, its test on\nartificial spectra, and its validation on two control samples of real stars.\nAnalysis with Zeta-Payne leads to only modest internal uncertainties in the\nnear-IR with APOGEE (optical with BOSS): 3-10% (1-2%) for Teff, 5-30% (5-25%)\nfor v*sin(i), 1.7-6.3 km/s(0.7-2.2 km/s) for RV, $<0.1$ dex ($<0.05$ dex) for\nlog(g), and 0.4-0.5 dex (0.1 dex) for [M/H] of the star, respectively. We find\na good agreement between atmospheric parameters of OBAF-type stars when\ninferred from their high- and low-resolution optical spectra. For most stellar\nlabels the APOGEE spectra are (far) less informative than the BOSS spectra of\nthese stars, while log(g), v*sin(i), and [M/H] are in most cases too uncertain\nfor meaningful astrophysical interpretation. This makes BOSS low-resolution\noptical spectra better for stellar labels of OBAF-type stars, unless the latter\nare subject to high levels of extinction.", "cat": "astro-ph.IM", "authors": ["Ilya Straumit", "Andrew Tkachenko", "Sarah Gebruers", "Jeroen Audenaert", "Maosheng Xiang", "Eleonora Zari", "Conny Aerts", "Jennifer A. Johnson", "Juna A. Kollmeier", "Hans-Walter Rix", "Rachael L. Beaton", "Jennifer L. Van Saders", "Johanna Teske", "Alexandre Roman-Lopes", "Yuan-Sen Ting", "Carlos G. Rom\u00e1n-Z\u00fa\u00f1iga"]}, "661": {"id": "2209.09914v1", "title": "CLusters in the Uv as EngineS (CLUES): I. Survey presentation \\& FUV spectral analysis of the stellar light", "url": "http://arxiv.org/pdf/2209.09914v1", "date": "2022-09-20 18:00:01", "abs": "The CLusters in the Uv as EngineS (CLUES) survey is a Cosmic Origins\nSpectrograph (COS) campaign aimed at acquiring the 1130 to 1770 {\\AA},\nrestframe spectroscopy of very young (<20 Myr) and massive (>10^4 solar masses)\nstar clusters in galaxies that are part of the Hubble treasury program Legacy\nExtraGalactic Uv Survey (LEGUS). In this first paper of a series, we describe\nthe CLUES sample consisting of 20 young star clusters and report their physical\nproperties as derived by both multi-wavelength photometry and far-UV (FUV)\nspectroscopy with Hubble Space Telescope (HST). Thanks to the synergy of the\ntwo different datasets we build a coherent picture of the diverse stellar\npopulations found in each region (with sizes of 40 to 160 pc). We associate the\nFUV-brightest stellar population to the central targeted star cluster and the\nother modeled population to the diffuse stars that are included in the COS\naperture. We observe better agreement between photometric and spectroscopic\nages for star clusters younger than 5 Myr. For clusters older than 5 Myr,\nphotometry and spectroscopy measurements deviate, with the latter producing\nolder ages, due to the degeneracy of photometric models. FUV spectroscopy\nenables us to better constrain the stellar metallicities, a parameter that\noptical colors are insensitive to. Finally, the derived E(B-V) are quite\nsimilar, with a tendency for FUV spectroscopy to favor solutions with higher\nextinctions. The recovered masses are in agreement within a factor of 2 for all\nthe clusters.", "cat": "astro-ph.GA", "authors": ["M. Sirressi", "A. Adamo", "M. Hayes", "S. Osborne", "S. Hernandez", "J. Chisholm", "M. Messa", "L. J. Smith", "A. Wofford", "A. Fox", "A. Mizener", "C. Usher", "A. Bik", "D. Calzetti", "E. Sabbi", "E. Schinnerer", "G. \u00d6stlin", "K. Grasha", "M. Cignoni", "M. Fumagalli"]}, "662": {"id": "2011.00940v1", "title": "Deep Learning in Computer-Aided Diagnosis and Treatment of Tumors: A Survey", "url": "http://arxiv.org/pdf/2011.00940v1", "date": "2020-11-02 12:42:19", "abs": "Computer-Aided Diagnosis and Treatment of Tumors is a hot topic of deep\nlearning in recent years, which constitutes a series of medical tasks, such as\ndetection of tumor markers, the outline of tumor leisures, subtypes and stages\nof tumors, prediction of therapeutic effect, and drug development. Meanwhile,\nthere are some deep learning models with precise positioning and excellent\nperformance produced in mainstream task scenarios. Thus follow to introduce\ndeep learning methods from task-orient, mainly focus on the improvements for\nmedical tasks. Then to summarize the recent progress in four stages of tumor\ndiagnosis and treatment, which named In-Vitro Diagnosis (IVD), Imaging\nDiagnosis (ID), Pathological Diagnosis (PD), and Treatment Planning (TP).\nAccording to the specific data types and medical tasks of each stage, we\npresent the applications of deep learning in the Computer-Aided Diagnosis and\nTreatment of Tumors and analyzing the excellent works therein. This survey\nconcludes by discussing research issues and suggesting challenges for future\nimprovement.", "cat": "eess.IV", "authors": ["Dan Zhao", "Guizhi Xu", "Zhenghua XU", "Thomas Lukasiewicz", "Minmin Xue", "Zhigang Fu"]}, "663": {"id": "0906.4561v1", "title": "An AzTEC 1.1 mm survey of the GOODS-N field -- II. Multi-wavelength identifications and redshift distribution", "url": "http://arxiv.org/pdf/0906.4561v1", "date": "2009-06-24 20:10:23", "abs": "We present results from a multi-wavelength study of 29 sources (false\ndetection probabilities <5%) from a survey of the Great Observatories Origins\nDeep Survey-North field at 1.1mm using the AzTEC camera. Comparing with\nexisting 850um SCUBA studies in the field, we examine differences in the source\npopulations selected at the two wavelengths. The AzTEC observations uniformly\ncover the entire survey field to a 1-sigma depth of ~1mJy. Searching deep\n1.4GHz VLA, and Spitzer 3--24um catalogues, we identify robust counterparts for\n21 1.1mm sources, and tentative associations for the remaining objects. The\nredshift distribution of AzTEC sources is inferred from available spectroscopic\nand photometric redshifts. We find a median redshift of z=2.7, somewhat higher\nthan z=2.0 for 850um-selected sources in the same field, and our lowest\nredshift identification lies at a spectroscopic redshift z=1.1460. We measure\nthe 850um to 1.1mm colour of our sources and do not find evidence for `850um\ndropouts', which can be explained by the low-SNR of the observations. We also\ncombine these observed colours with spectroscopic redshifts to derive the range\nof dust temperatures T, and dust emissivity indices $\\beta$ for the sample,\nconcluding that existing estimates T~30K and $\\beta$~1.75 are consistent with\nthese new data.", "cat": "astro-ph.CO", "authors": ["E. L. Chapin", "A. Pope", "D. Scott", "I. Aretxaga", "J. E. Austermann", "R-R. Chary", "K. Coppin", "M. Halpern", "D. H. Hughes", "J. D. Lowenthal", "G. E. Morrison", "T. A. Perera", "K. S. Scott", "G. W. Wilson", "M. S. Yun"]}, "664": {"id": "2403.16407v1", "title": "A Survey on Long Video Generation: Challenges, Methods, and Prospects", "url": "http://arxiv.org/pdf/2403.16407v1", "date": "2024-03-25 03:47:53", "abs": "Video generation is a rapidly advancing research area, garnering significant\nattention due to its broad range of applications. One critical aspect of this\nfield is the generation of long-duration videos, which presents unique\nchallenges and opportunities. This paper presents the first survey of recent\nadvancements in long video generation and summarises them into two key\nparadigms: divide and conquer temporal autoregressive.\n We delve into the common models employed in each paradigm, including aspects\nof network design and conditioning techniques. Furthermore, we offer a\ncomprehensive overview and classification of the datasets and evaluation\nmetrics which are crucial for advancing long video generation research.\nConcluding with a summary of existing studies, we also discuss the emerging\nchallenges and future directions in this dynamic field. We hope that this\nsurvey will serve as an essential reference for researchers and practitioners\nin the realm of long video generation.", "cat": "cs.CV", "authors": ["Chengxuan Li", "Di Huang", "Zeyu Lu", "Yang Xiao", "Qingqi Pei", "Lei Bai"]}, "665": {"id": "1605.04607v1", "title": "Nature and statistical properties of quasar associated absorption systems in the XQ-100 Legacy Survey", "url": "http://arxiv.org/pdf/1605.04607v1", "date": "2016-05-15 21:39:48", "abs": "We statistically study the physical properties of a sample of narrow\nabsorption line (NAL) systems looking for empirical evidences to distinguish\nbetween intrinsic and intervening NALs without taking into account any a priori\ndefinition or velocity cut-off. We analyze the spectra of 100 quasars with 3.5\n< z$\\rm_{em}$ < 4.5, observed with X-shooter/VLT in the context of the XQ-100\nLegacy Survey. We detect a $\\sim$ 8 $\\sigma$ excess in the number density of\nabsorbers within 10,000 km/s of the quasar emission redshift with respect to\nthe random occurrence of NALs. This excess does not show a dependence on the\nquasar bolometric luminosity and it is not due to the redshift evolution of\nNALs. It extends far beyond the standard 5000 km/s cut-off traditionally\ndefined for associated absorption lines. We propose to modify this definition,\nextending the threshold to 10,000 km/s when also weak absorbers (equivalent\nwidth < 0.2 \\AA) are considered. We infer NV is the ion that better traces the\neffects of the quasar ionization field, offering the best statistical tool to\nidentify intrinsic systems. Following this criterion we estimate that the\nfraction of quasars in our sample hosting an intrinsic NAL system is 33\npercent. Lastly, we compare the properties of the material along the quasar\nline of sight, derived from our sample, with results based on close quasar\npairs investigating the transverse direction. We find a deficiency of cool gas\n(traced by CII) along the line of sight associated with the quasar host galaxy,\nin contrast with what is observed in the transverse direction.", "cat": "astro-ph.GA", "authors": ["Serena Perrotta", "Valentina D'Odorico", "J. Xavier Prochaska", "Stefano Cristiani", "Guido Cupani", "Sara Ellison", "Sebastian L\u00f2pez", "George D. Becker", "Trystyn A. M. Berg", "Lise Christensen", "Kelly D. Denney", "Frederick Hamann", "Isabelle P\u00e2ris", "Marianne Vestergaard", "G\u00e1bor Worseck"]}, "666": {"id": "2204.09519v1", "title": "A Survey on Neural Abstractive Summarization Methods and Factual Consistency of Summarization", "url": "http://arxiv.org/pdf/2204.09519v1", "date": "2022-04-20 14:56:36", "abs": "Automatic summarization is the process of shortening a set of textual data\ncomputationally, to create a subset (a summary) that represents the most\nimportant pieces of information in the original text. Existing summarization\nmethods can be roughly divided into two types: extractive and abstractive. An\nextractive summarizer explicitly selects text snippets (words, phrases,\nsentences, etc.) from the source document, while an abstractive summarizer\ngenerates novel text snippets to convey the most salient concepts prevalent in\nthe source.", "cat": "cs.CL", "authors": ["Meng Cao"]}, "667": {"id": "1101.3561v1", "title": "Galaxia: a code to generate a synthetic survey of the Milky Way", "url": "http://arxiv.org/pdf/1101.3561v1", "date": "2011-01-18 21:21:17", "abs": "We present here a fast code for creating a synthetic survey of the Milky Way.\nGiven one or more color-magnitude bounds, a survey size and geometry, the code\nreturns a catalog of stars in accordance with a given model of the Milky Way.\nThe model can be specified by a set of density distributions or as an N-body\nrealization. We provide fast and efficient algorithms for sampling both types\nof models. As compared to earlier sampling schemes which generate stars at\nspecified locations along a line of sight, our scheme can generate a continuous\nand smooth distribution of stars over any given volume. The code is quite\ngeneral and flexible and can accept input in the form of a star formation rate,\nage metallicity relation, age velocity dispersion relation and analytic density\ndistribution functions. Theoretical isochrones are then used to generate a\ncatalog of stars and support is available for a wide range of photometric\nbands. As a concrete example we implement the Besancon Milky Way model for the\ndisc. For the stellar halo we employ the simulated stellar halo N-body models\nof Bullock & Johnston (2005). In order to sample N-body models, we present a\nscheme that disperses the stars spawned by an N-body particle, in such a way\nthat the phase space density of the spawned stars is consistent with that of\nthe N-body particles. The code is ideally suited to generating synthetic data\nsets that mimic near future wide area surveys such as GAIA, LSST and HERMES. As\nan application we study the prospect of identifying structures in the stellar\nhalo with a simulated GAIA survey. We plan to make the code publicly available\nat http://galaxia.sourceforge.net.", "cat": "astro-ph.GA", "authors": ["Sanjib Sharma", "Joss Bland-Hawthorn", "Kathryn V. Johnston", "James Binney"]}, "668": {"id": "1012.3711v2", "title": "10C Survey of Radio Sources at 15.7 GHz: I - Observing, mapping and source extraction", "url": "http://arxiv.org/pdf/1012.3711v2", "date": "2011-03-19 04:36:27", "abs": "We have observed an area of approximatley 27 deg^2 to an rms noise level of\nless than 0.2 mJy at 15.7 GHz, using the Arcminute Microkelvin Imager Large\nArray. These observations constitute the most sensitive radio-source survey of\nany extent (greater than approximately 0.2 deg^2) above 1.4 GHz. This paper\npresents the techniques employed for observing, mapping and source extraction.\nWe have used a systematic procedure for extracting information and producing\nsource catalogues, from maps with varying noise and uv-coverage. We have\nperformed simulations to test our mapping and source-extraction procedures, and\ndeveloped methods for identifying extended, overlapping and spurious sources in\nnoisy images. In an accompanying paper, AMI Consortium: Davies et al. 2010, the\nfirst results from the 10C survey, including the deep 15.7-GHz source count,\nare presented.", "cat": "astro-ph.CO", "authors": ["Thomas M. O. Franzen", "Matthew L. Davies", "Elizabeth M. Waldram", "Keith J. B. Grainge", "Michael P. Hobson", "Natasha Hurley-Walker", "Anthony Lasenby", "Malak Olamaie", "Guy G. Pooley", "Carmen Rodriguez-Gonzalvez", "Richard D. E. Saunders", "Anna M. M. Scaife", "Michel P. Schammel", "Paul F. Scott", "Timothy W. Shimwell", "David J. Titterington", "Jonathan T. L. Zwart"]}, "669": {"id": "2207.14566v1", "title": "Forecasting the Cross-Correlation of the CSST galaxy survey with the FAST HI Intensity Map", "url": "http://arxiv.org/pdf/2207.14566v1", "date": "2022-07-29 09:28:33", "abs": "The cross-correlation of optical galaxies with the neutral hydrogen (HI)\nradiation intensity can enhance the signal-to-noise ratio (SNR) of the HI\nintensity measurement. In this paper, we investigate the cross-correlation of\nthe galaxy samples obtained by the spectroscopic survey of the China Space\nStation Telescope (CSST) with the HI Intensity mapping (IM) survey of the\nFive-hundred-meter Aperture Spherical Telescope (FAST). Using the IllusitrisTNG\nsimulation result at redshift $0.2 \\sim 0.3$, we generate mock data of the CSST\nsurvey and a FAST L-band drift scan survey. The CSST spectroscopic survey can\nyield a sample of galaxies with a high comoving number density of $10^{-2}\n(\\unit{Mpc}/h)^{-3}$ at $z \\sim 0.3$. We cross-correlate the foreground-removed\nradio intensity with the CSST galaxies, including both the whole sample, and\nred and blue galaxy sub-samples separately. We find that in all cases the HI\nand optical galaxies are well correlated. The total HI abundance can be\nmeasured with a high precision from this correlation. A relative error of $\\sim\n0.6\\%$ for $\\Omega_{\\rm HI}$ could be achieved at $z\\sim 0.3$ for an\noverlapping survey area of $10000 \\unit{deg}^2$.", "cat": "astro-ph.CO", "authors": ["Furen Deng", "Yan Gong", "Yougang Wang", "Shuting Dong", "Ye Cao", "Xuelei Chen"]}, "670": {"id": "2312.10089v1", "title": "Advancements in Content-Based Image Retrieval: A Comprehensive Survey of Relevance Feedback Techniques", "url": "http://arxiv.org/pdf/2312.10089v1", "date": "2023-12-13 11:07:32", "abs": "Content-based image retrieval (CBIR) systems have emerged as crucial tools in\nthe field of computer vision, allowing for image search based on visual content\nrather than relying solely on metadata. This survey paper presents a\ncomprehensive overview of CBIR, emphasizing its role in object detection and\nits potential to identify and retrieve visually similar images based on content\nfeatures. Challenges faced by CBIR systems, including the semantic gap and\nscalability, are discussed, along with potential solutions. It elaborates on\nthe semantic gap, which arises from the disparity between low-level features\nand high-level semantic concepts, and explores approaches to bridge this gap.\nOne notable solution is the integration of relevance feedback (RF), empowering\nusers to provide feedback on retrieved images and refine search results\niteratively. The survey encompasses long-term and short-term learning\napproaches that leverage RF for enhanced CBIR accuracy and relevance. These\nmethods focus on weight optimization and the utilization of active learning\nalgorithms to select samples for training classifiers. Furthermore, the paper\ninvestigates machine learning techniques and the utilization of deep learning\nand convolutional neural networks to enhance CBIR performance. This survey\npaper plays a significant role in advancing the understanding of CBIR and RF\ntechniques. It guides researchers and practitioners in comprehending existing\nmethodologies, challenges, and potential solutions while fostering knowledge\ndissemination and identifying research gaps. By addressing future research\ndirections, it sets the stage for advancements in CBIR that will enhance\nretrieval accuracy, usability, and effectiveness in various application\ndomains.", "cat": "cs.CV", "authors": ["Hamed Qazanfari", "Mohammad M. AlyanNezhadi", "Zohreh Nozari Khoshdaregi"]}, "671": {"id": "1910.07524v2", "title": "An ALMA survey of the SCUBA-2 CLS UDS field: Physical properties of 707 Sub-millimetre Galaxies", "url": "http://arxiv.org/pdf/1910.07524v2", "date": "2020-10-21 17:05:42", "abs": "We analyse the physical properties of a large, homogeneously selected sample\nof ALMA-located sub-mm galaxies (SMGs). This survey, AS2UDS, identified 707\nSMGs across the ~1 sq.deg. field, including ~17 per cent, which are undetected\nat $K$>~25.7 mag. We interpret their ultraviolet-to-radio data using MAGPHYS\nand determine a median redshift of z=2.61+-0.08 (1$\\sigma$ range of z=1.8-3.4)\nwith just ~6 per cent at z>4. Our survey provides a sample of massive dusty\ngalaxies at z>~1, with median dust and stellar masses of\n$M_d$=(6.8+-0.3)x10$^{8}$M$_\\odot$ (thus, gas masses of ~10$^{11}$M$_\\odot$)\nand $M_\\ast=$(1.26+-0.05)x10$^{11}$M$_\\odot$. We find no evolution in dust\ntemperature at a constant far-infrared luminosity across z~1.5-4. The gas mass\nfunction of our sample increases to z~2-3 and then declines at z>3. The space\ndensity and masses of SMGs suggest that almost all galaxies with\n$M_\\ast$>~3x10$^{11}$M$_\\odot$ have passed through an SMG-like phase. The\nredshift distribution is well fit by a model combining evolution of the gas\nfraction in halos with the growth of halo mass past a threshold of\n$M_h$~6x10$^{12}$M$_\\odot$, thus SMGs may represent the highly efficient\ncollapse of gas-rich massive halos. We show that SMGs are broadly consistent\nwith simple homologous systems in the far-infrared, consistent with a centrally\nilluminated starburst. Our study provides strong support for an evolutionary\nlink between the active, gas-rich SMG population at z>1 and the formation of\nmassive, bulge-dominated galaxies across the history of the Universe.", "cat": "astro-ph.GA", "authors": ["U. Dudzevi\u010di\u016bt\u0117", "Ian Smail", "A. M. Swinbank", "S. M. Stach", "O. Almaini", "E. da Cunha", "Fang Xia An", "V. Arumugam", "J. Birkin", "A. W. Blain", "S. C. Chapman", "C. -C. Chen", "C. J. Conselice", "K. E. K. Coppin", "J. S. Dunlop", "D. Farrah", "J. E. Geach", "B. Gullberg", "W. G. Hartley", "J. A. Hodge", "R. J. Ivison", "D. T. Maltby", "D. Scott", "C. J. Simpson", "J. M. Simpson", "A. P. Thomson", "F. Walter", "J. L. Wardlow", "A. Weiss", "P. van der Werf"]}, "672": {"id": "2302.04270v2", "title": "A Large Population of Faint 8 8$ systems identified using two different photometric redshift codes:\nLePhare and EAZY, combined with other significance criteria. The highest\nredshift object in our sample is at $z=15.57^{+0.39}_{-0.38}$, which has a blue\nbeta slope of $\\beta=-3.25^{+0.41}_{-0.46}$ and a very low inferred stellar\nmass of $M_{*} = 10^{7.39}$ M_0,. We also discover a series of faint, low-mass\ndwarf galaxies with $M_{*} < 10^{8.5}$ M_0 at $z \\sim 9$ that have blue colors\nand UV slopes. The structure of these galaxies is such that they all have very\nflat surface brightness profiles and small sizes $< 1 \\ \\mathrm{kpc}$. We also\ncompare our results to theory, finding no significant disagreement with some\nCDM based models.The discovery of these objects, most of which are low\nluminosity and inferred stellar mass, demonstrates the power of probing\ncontinuously deeper into the Universe, pointing the way to deeper, or similar\ndepth but wider area, surveys and demonstrate the critical need for JWST deep\nfields to explore this aspect of the early Universe.", "cat": "astro-ph.GA", "authors": ["D. Austin", "N. J. Adams", "C. J. Conselice", "T. Harvey", "K. Ormerod", "J. Trussler", "Q. Li", "L. Ferreira", "P. Dayal"]}, "673": {"id": "1610.03492v1", "title": "Galaxy-galaxy and galaxy-cluster lensing with the SDSS and FIRST surveys", "url": "http://arxiv.org/pdf/1610.03492v1", "date": "2016-10-11 20:00:06", "abs": "We perform a galaxy-galaxy lensing study by correlating the shapes of\n$\\sim$2.7 $\\times$ 10$^5$ galaxies selected from the VLA FIRST radio survey\nwith the positions of $\\sim$38.5 million SDSS galaxies, $\\sim$132000 BCGs and\n$\\sim$78000 SDSS galaxies that are also detected in the VLA FIRST survey. The\nmeasurements are conducted on angular scales ${\\theta}$ $\\lesssim$ 1200 arcsec.\nOn scales ${\\theta}$ $\\lesssim$ 200 arcsec we find that the measurements are\ncorrupted by residual systematic effects associated with the instrumental beam\nof the VLA data. Using simulations we show that we can successfully apply a\ncorrection for these effects. Using the three lens samples (the SDSS DR10\nsample, the BCG sample and the SDSS-FIRST matched object sample) we measure a\ntangential shear signal that is inconsistent with zero at the 10${\\sigma}$,\n3.8${\\sigma}$ and 9${\\sigma}$ level respectively. Fitting an NFW model to the\ndetected signals we find that the ensemble mass profile of the BCG sample\nagrees with the values in the literature. However, the mass profiles of the\nSDSS DR10 and the SDSS-FIRST matched object samples are found to be shallower\nand steeper than results in the literature respectively. The best-fitting\nVirial masses for the SDSS DR10, BCG and SDSS-FIRST matched samples, derived\nusing an NFW model and allowing for a varying concentration factor, are\nM$^{SDSS-DR10}_{200}$ = (1.2 $\\pm$ 0.4) $\\times$ 10$^{12}$M$_{\\odot}$,\nM$^{BCG}_{200}$ = (1.4 $\\pm$ 1.3) $\\times$ 10$^{13}$M$_{\\odot}$ and\nM$^{SDSS-FIRST}_{200}$ = 8.0 $\\pm$ 4.2 $\\times$ 10$^{13}$M$_{\\odot}$\nrespectively. These results are in good agreement (within $\\sim$2${\\sigma}$)\nwith values in the literature. Our findings suggest that for galaxies to be\nboth bright in the radio and in the optical they must be embedded in very dense\nenvironment on scales R $\\lesssim$ 1Mpc.", "cat": "astro-ph.GA", "authors": ["Constantinos Demetroullas", "Michael L. Brown"]}, "674": {"id": "2206.08983v3", "title": "BURSTT: Bustling Universe Radio Survey Telescope in Taiwan", "url": "http://arxiv.org/pdf/2206.08983v3", "date": "2022-09-27 01:28:04", "abs": "Fast Radio Bursts (FRBs) are bright millisecond-duration radio transients\nthat appear about 1,000 times per day, all-sky, for a fluence threshold 5 Jy ms\nat 600 MHz. The FRB radio-emission physics and the compact objects involved in\nthese events are subjects of intense active debate. To better constrain source\nmodels, the Bustling Universe Radio Survey Telescope in Taiwan (BURSTT) is\noptimized to discover and localize a large sample of rare, high-fluence, nearby\nFRBs. This is the population most amenable to multi-messenger, multi-wavelength\nfollow-up, allowing deeper understanding of source mechanisms. BURSTT will\nprovide horizon-to-horizon sky coverage with a half power field-of-view (FoV)\nof $\\sim$10$^{4}$ deg$^{2}$, a 400 MHz effective bandwidth between 300-800 MHz,\nand sub-arcsecond localization, made possible using outrigger stations hundreds\nto thousands of km from the main array. Initially, BURSTT will employ 256\nantennas. After tests of various antenna designs and optimization of system\nperformance we plan to expand to 2048 antennas. We estimate that BURSTT-256\nwill detect and localize $\\sim$100 bright ($\\geq$100 Jy ms) FRBs per year.\nAnother advantage of BURSTT's large FoV and continuous operation will be\ngreatly enhanced monitoring of FRBs for repetition. The current lack of\nsensitive all-sky observations likely means that many repeating FRBs are\ncurrently cataloged as single-event FRBs.", "cat": "astro-ph.IM", "authors": ["Hsiu-Hsien Lin", "Kai-yang Lin", "Chao-Te Li", "Yao-Huan Tseng", "Homin Jiang", "Jen-Hung Wang", "Jen-Chieh Cheng", "Ue-Li Pen", "Ming-Tang Chen", "Pisin Chen", "Yaocheng Chen", "Tomotsugu Goto", "Tetsuya Hashimoto", "Yuh-Jing Hwang", "Sun-Kun King", "Derek Kubo", "Chung-Yun Kuo", "Adam Mills", "Jiwoo Nam", "Peter Oshiro", "Chang-Shao Shen", "Hsien-Chun Tseng", "Shih-Hao Wang", "Vigo Feng-Shun Wu", "Geoffrey Bower", "Shu-Hao Chang", "Pai-An Chen", "Ying-Chih Chen", "Yi-Kuan Chiang", "Anatoli Fedynitch", "Nina Gusinskaia", "Simon C. -C. Ho", "Tiger Y. -Y. Hsiao", "Chin-Ping Hu", "Yau De Huang", "Jose Miguel Jauregui Garcia", "Seong Jin Kim", "Cheng-Yu Kuo", "Decmend Fang-Jie Ling", "Alvina Y. L. On", "Jeffrey B. Peterson", "Bjorn Jasper R. Raquel", "Shih-Chieh Su", "Yuri Uno", "Cossas K. -W. Wu", "Shotaro Yamasaki", "Hong-Ming Zhu"]}, "675": {"id": "0711.2517v1", "title": "Deep-Survey Constraints on X-ray Outbursts from Galactic Nuclei", "url": "http://arxiv.org/pdf/0711.2517v1", "date": "2007-11-15 21:20:39", "abs": "Luminous X-ray outbursts with variability amplitudes as high as ~1000 have\nbeen detected from a small number of galactic nuclei. These events are likely\nassociated with transient fueling of nuclear supermassive black holes. In this\npaper, we constrain X-ray outbursts with harder spectra, higher redshifts, and\nlower luminosities than have been studied previously. We performed a systematic\nsurvey of 24668 optical galaxies in the Chandra Deep Fields to search for such\nX-ray outbursts; the median redshift of these galaxies is ~0.8. The survey\nspans 798 days for the Chandra Deep Field-North, and 1828 days for the Chandra\nDeep Field-South. No outbursts were found, and thus we set upper limits on the\nrate of such events in the Universe, which depend upon the adopted outburst\nX-ray luminosity. For an outburst with X-ray luminosity $\\ga 10^{43}$ ergs/s\nand a duration of 6 months, the upper limit on its event rate is ~10^{-4}\n/galaxy/yr, roughly consistent with theoretical predictions. Compared to\nprevious survey results, our harder-band and deeper survey suggests that the\noutburst rate may increase by a maximum factor of 10 when considering both\nobscured X-ray outbursts and redshift evolution from z~0 to z~0.8. Our results\nalso suggest that the X-ray luminosity function for moderate-luminosity active\ngalactic nuclei is not primarily due to stellar tidal disruptions.", "cat": "astro-ph", "authors": ["B. Luo", "W. N. Brandt", "A. T. Steffen", "F. E. Bauer"]}, "676": {"id": "1606.09619v2", "title": "Results of the deepest all-sky survey for continuous gravitational waves on LIGO S6 data running on the Einstein@Home volunteer distributed computing project", "url": "http://arxiv.org/pdf/1606.09619v2", "date": "2016-07-02 19:14:36", "abs": "We report results of a deep all-sky search for periodic gravitational waves\nfrom isolated neutron stars in data from the S6 LIGO science run. The search\nwas possible thanks to the computing power provided by the volunteers of the\nEinstein@Home distributed computing project. We find no significant signal\ncandidate and set the most stringent upper limits to date on the amplitude of\ngravitational wave signals from the target population. At the frequency of best\nstrain sensitivity, between $170.5$ and $171$ Hz we set a 90% confidence upper\nlimit of ${5.5}^{-25}$, while at the high end of our frequency range, around\n505 Hz, we achieve upper limits $\\simeq {10}^{-24}$. At $230$ Hz we can exclude\nsources with ellipticities greater than $10^{-6}$ within 100 pc of Earth with\nfiducial value of the principal moment of inertia of $10^{38} \\textrm{kg m}^2$.\nIf we assume a higher (lower) gravitational wave spindown we constrain farther\n(closer) objects to higher (lower) ellipticities.", "cat": "gr-qc", "authors": ["The LIGO Scientific Collaboration", "The Virgo Collaboration"]}, "677": {"id": "1109.5536v1", "title": "An HI 21-cm line survey of evolved stars", "url": "http://arxiv.org/pdf/1109.5536v1", "date": "2011-09-26 12:22:58", "abs": "The HI line at 21 cm is a tracer of circumstellar matter around AGB stars,\nand especially of the matter located at large distances (0.1-1 pc) from the\ncentral stars. It can give unique information on the kinematics and on the\nphysical conditions in the outer parts of circumstellar shells and in the\nregions where stellar matter is injected into the interstellar medium. However\nthis tracer has not been much used up to now, due to the difficulty of\nseparating the genuine circumstellar emission from the interstellar one.\n With the Nancay Radiotelescope we are carrying out a survey of the HI\nemission in a large sample of evolved stars. We report on recent progresses of\nthis long term programme, with emphasis on S-type stars.", "cat": "astro-ph.SR", "authors": ["E. Gerard", "T. Le Bertre", "Y. Libert"]}, "678": {"id": "0803.3891v1", "title": "Accounting for self-protective responses in randomized response data from a social security survey using the zero-inflated Poisson model", "url": "http://arxiv.org/pdf/0803.3891v1", "date": "2008-03-27 11:12:38", "abs": "In 2004 the Dutch Department of Social Affairs conducted a survey to assess\nthe extent of noncompliance with social security regulations. The survey was\nconducted among 870 recipients of social security benefits and included a\nseries of sensitive questions about regulatory noncompliance. Due to the\nsensitive nature of the questions the randomized response design was used.\nAlthough randomized response protects the privacy of the respondent, it is\nunlikely that all respondents followed the design. In this paper we introduce a\nmodel that allows for respondents displaying self-protective response behavior\nby consistently giving the nonincriminating response, irrespective of the\noutcome of the randomizing device. The dependent variable denoting the total\nnumber of incriminating responses is assumed to be generated by the application\nof randomized response to a latent Poisson variable denoting the true number of\nrule violations. Since self-protective responses result in an excess of\nobserved zeros in relation to the Poisson randomized response distribution,\nthese are modeled as observed zero-inflation. The model includes predictors of\nthe Poisson parameters, as well as predictors of the probability of\nself-protective response behavior.", "cat": "stat.AP", "authors": ["Maarten J. L. F. Cruyff", "Ulf B\u00f6ckenholt", "Ardo van den Hout", "Peter G. M. van der Heijden"]}, "679": {"id": "1802.01724v1", "title": "Massive stars in the SDSS-IV/APOGEE SURVEY. I- OB stars", "url": "http://arxiv.org/pdf/1802.01724v1", "date": "2018-02-05 23:05:28", "abs": "In this work we make use of DR14 APOGEE spectroscopic data to study a sample\nof 92 known OB stars. We developed a near-infrared semi-empirical spectral\nclassification method that was successfully used in case of four new exemplars,\npreviously classified as later B-type stars. Our results agree well with those\ndetermined independently from ECHELLE optical spectra, being in line with the\nspectral types derived from the \"canonical\" MK blue optical system. This\nconfirms that the APOGEE spectrograph can also be used as a powerful tool in\nsurveys aiming to unveil and study large number of moderately and highly\nobscured OB stars still hidden in the Galaxy.", "cat": "astro-ph.GA", "authors": ["A. Roman-Lopes", "C. Rom\u00c1n-Z\u00da\u00d1iga", "Mauricio Tapia", "Drew Chojnowski", "Y. G\u00d3mez Maqueo Chew", "D. A. Garc\u00cda-Hern\u00c1ndez", "Jura Borissova", "Dante Minniti", "Kevin R. Covey", "Pen\u00c9lope Longa-Pe\u00d1a", "J. G. Fernandez-Trincado", "Olga Zamora", "Christian Nitschelm"]}, "680": {"id": "0810.4011v1", "title": "Cool White Dwarfs Identified in the Second Data Release of the UKIRT Infrared Deep Sky Survey", "url": "http://arxiv.org/pdf/0810.4011v1", "date": "2008-10-22 08:47:28", "abs": "We have paired the Second Data Release of the Large Area Survey of the UKIRT\nInfrared Deep Sky Survey with the Fifth Data Release of the Sloan Digital Sky\nSurvey to identify ten cool white dwarf candidates, from their photometry and\nastrometry. Of these ten, one was previously known to be a very cool white\ndwarf. We have obtained optical spectroscopy for seven of the candidates using\nthe GMOS-N spectrograph on Gemini North, and have confirmed all seven as white\ndwarfs. Our photometry and astrometry indicates that the remaining two objects\nare also white dwarfs. Model analysis of the photometry and available\nspectroscopy shows that the seven confirmed new white dwarfs, and the two new\nlikely white dwarfs, have effective temperatures in the range Teff = 5400-6600\nK. Our analysis of the previously known white dwarf confirms that it is cool,\nwith Teff = 3800 K. The cooling age for this dwarf is 8.7 Gyr, while that of\nthe nine ~6000 K white dwarfs is 1.8-3.6 Gyr. We are unable to determine the\nmasses of the white dwarfs from the existing data, and therefore we cannot\nconstrain the total ages of the white dwarfs. The large cooling age for the\ncoolest white dwarf in the sample, combined with its low estimated tangential\nvelocity, suggests that it is an old member of the thin disk, or a member of\nthe thick disk of the Galaxy, with an age 10-11 Gyr. The warmer white dwarfs\nappear to have velocities typical of the thick disk or even halo; these may be\nvery old remnants of low-mass stars, or they may be relatively young thin disk\nobjects with unusually high space motion.", "cat": "astro-ph", "authors": ["N. Lodieu", "S. K. Leggett", "P. Bergeron", "A. Nitta"]}, "681": {"id": "1611.09871v1", "title": "Characterizing the properties of cluster precursors in the MALT90 survey", "url": "http://arxiv.org/pdf/1611.09871v1", "date": "2016-11-29 21:01:52", "abs": "In the Milky Way there are thousands of stellar clusters each harboring from\na hundred to a million stars. Although clusters are common, the initial\nconditions of cluster formation are still not well understood. To determine the\nprocesses involved in the formation and evolution of clusters it is key to\ndetermine the global properties of cluster-forming clumps in their earliest\nstages of evolution. Here, we present the physical properties of 1,244 clumps\nidentified from the MALT90 survey. Using the dust temperature of the clumps as\na proxy for evolution we determined how the clump properties change at\ndifferent evolutionary stages. We find that less-evolved clumps exhibiting dust\ntemperatures lower than 20 K have higher densities and are more gravitationally\nbound than more-evolved clumps with higher dust temperatures. We also\nidentified a sample of clumps in a very early stage of evolution, thus\npotential candidates for high-mass star-forming clumps. Only one clump in our\nsample has physical properties consistent with a young massive cluster\nprogenitor, reinforcing the fact that massive proto-clusters are very rare in\nthe Galaxy.", "cat": "astro-ph.GA", "authors": ["Yanett Contreras", "Jill M. Rathborne", "Andres Guzman", "James Jackson", "Scott Whitaker", "Patricio Sanhueza", "Jonathan Foster"]}, "682": {"id": "2210.16484v3", "title": "A Systematic Survey of Chemical Pre-trained Models", "url": "http://arxiv.org/pdf/2210.16484v3", "date": "2023-04-27 03:30:37", "abs": "Deep learning has achieved remarkable success in learning representations for\nmolecules, which is crucial for various biochemical applications, ranging from\nproperty prediction to drug design. However, training Deep Neural Networks\n(DNNs) from scratch often requires abundant labeled molecules, which are\nexpensive to acquire in the real world. To alleviate this issue, tremendous\nefforts have been devoted to Molecular Pre-trained Models (CPMs), where DNNs\nare pre-trained using large-scale unlabeled molecular databases and then\nfine-tuned over specific downstream tasks. Despite the prosperity, there lacks\na systematic review of this fast-growing field. In this paper, we present the\nfirst survey that summarizes the current progress of CPMs. We first highlight\nthe limitations of training molecular representation models from scratch to\nmotivate CPM studies. Next, we systematically review recent advances on this\ntopic from several key perspectives, including molecular descriptors, encoder\narchitectures, pre-training strategies, and applications. We also highlight the\nchallenges and promising avenues for future research, providing a useful\nresource for both machine learning and scientific communities.", "cat": "cs.LG", "authors": ["Jun Xia", "Yanqiao Zhu", "Yuanqi Du", "Stan Z. Li"]}, "683": {"id": "1806.10761v1", "title": "Survey of multifidelity methods in uncertainty propagation, inference, and optimization", "url": "http://arxiv.org/pdf/1806.10761v1", "date": "2018-06-28 04:06:17", "abs": "In many situations across computational science and engineering, multiple\ncomputational models are available that describe a system of interest. These\ndifferent models have varying evaluation costs and varying fidelities.\nTypically, a computationally expensive high-fidelity model describes the system\nwith the accuracy required by the current application at hand, while\nlower-fidelity models are less accurate but computationally cheaper than the\nhigh-fidelity model. Outer-loop applications, such as optimization, inference,\nand uncertainty quantification, require multiple model evaluations at many\ndifferent inputs, which often leads to computational demands that exceed\navailable resources if only the high-fidelity model is used. This work surveys\nmultifidelity methods that accelerate the solution of outer-loop applications\nby combining high-fidelity and low-fidelity model evaluations, where the\nlow-fidelity evaluations arise from an explicit low-fidelity model (e.g., a\nsimplified physics approximation, a reduced model, a data-fit surrogate, etc.)\nthat approximates the same output quantity as the high-fidelity model. The\noverall premise of these multifidelity methods is that low-fidelity models are\nleveraged for speedup while the high-fidelity model is kept in the loop to\nestablish accuracy and/or convergence guarantees. We categorize multifidelity\nmethods according to three classes of strategies: adaptation, fusion, and\nfiltering. The paper reviews multifidelity methods in the outer-loop contexts\nof uncertainty propagation, inference, and optimization.", "cat": "math.NA", "authors": ["Benjamin Peherstorfer", "Karen Willcox", "Max Gunzburger"]}, "684": {"id": "0812.0926v2", "title": "A Surprisingly High Pair Fraction for Extremely Massive Galaxies at z ~ 3 in the GOODS NICMOS Survey", "url": "http://arxiv.org/pdf/0812.0926v2", "date": "2008-12-05 14:08:11", "abs": "We calculate the major pair fraction and derive the major merger fraction and\nrate for 82 massive ($M_{*}>10^{11}M_{\\odot}$) galaxies at $1.7 < z < 3.0$\nutilising deep HST NICMOS data taken in the GOODS North and South fields. For\nthe first time, our NICMOS data provides imaging with sufficient angular\nresolution and depth to collate a sufficiently large sample of massive galaxies\nat z $>$ 1.5 to reliably measure their pair fraction history. We find strong\nevidence that the pair fraction of massive galaxies evolves with redshift. We\ncalculate a pair fraction of $f_{m}$ = 0.29 +/- 0.06 for our whole sample at\n$1.7 < z < 3.0$. Specifically, we fit a power law function of the form\n$f_{m}=f_{0}(1+z)^{m}$ to a combined sample of low redshift data from Conselice\net al. (2007) and recently acquired high redshift data from the GOODS NICMOS\nSurvey. We find a best fit to the free parameters of $f_{0}$ = 0.008 +/- 0.003\nand $m$ = 3.0 +/- 0.4. We go on to fit a theoretically motivated\nPress-Schechter curve to this data. This Press-Schechter fit, and the data,\nshow no sign of levelling off or turning over, implying that the merger\nfraction of massive galaxies continues to rise with redshift out to z $\\sim$ 3.\nSince previous work has established that the merger fraction for lower mass\ngalaxies turns over at z $\\sim$ 1.5 - 2.0, this is evidence that higher mass\ngalaxies experience more mergers earlier than their lower mass counterparts,\ni.e. a galaxy assembly downsizing. Finally, we calculate a merger rate at z =\n2.6 of $\\Re$ $<$ 5 $\\times$ 10$^{5}$ Gpc$^{-3}$ Gyr$^{-1}$, which experiences\nno significant change to $\\Re$ $<$ 1.2 $\\times$ 10$^{5}$ Gpc$^{-3}$ Gyr$^{-1}$\nat z = 0.5. This corresponds to an average $M_{*}>10^{11}M_{\\odot}$ galaxy\nexperiencing 1.7 +/- 0.5 mergers between z = 3 and z = 0.", "cat": "astro-ph", "authors": ["Asa F. L. Bluck", "Christopher J. Conselice", "Rychard J. Bouwens", "Emanuele Daddi", "Mark Dickinson", "Casey Papovich", "Haojing Yan"]}, "685": {"id": "1306.4376v1", "title": "Full Spectral Survey of Active Galactic Nuclei in the Rossi X-ray Timing Explorer Archive", "url": "http://arxiv.org/pdf/1306.4376v1", "date": "2013-06-18 22:19:17", "abs": "We have analyzed spectra for all active galactic nuclei in the Rossi X-ray\nTiming Explorer (RXTE) archive. We present long-term average values of\nabsorption, Fe line equivalent width, Compton reflection and photon index, as\nwell as calculating fluxes and luminosities in the 2-10 keV band for 100 AGN\nwith sufficient brightness and overall observation time to yield high quality\nspectral results. We compare these parameters across the different\nclassifications of Seyferts and blazars. Our distributions of photon indices\nfor Seyfert 1's and 2's are consistent with the idea that Seyferts share a\ncommon central engine, however our distributions of Compton reflection hump\nstrengths do not support the classical picture of absorption by a torus and\nreflection off a Compton-thick disk with type depending only on inclination\nangle. We conclude that a more complex reflecting geometry such as a combined\ndisk and torus or clumpy torus is likely a more accurate picture of the\nCompton-thick material. We find that Compton reflection is present in ~85% of\nSeyferts and by comparing Fe line EW's to Compton reflection hump strengths we\nhave found that on average 40% of the Fe line arises in Compton thick material,\nhowever this ratio was not consistent from object to object and did not seem to\nbe dependent on optical classification.", "cat": "astro-ph.HE", "authors": ["Elizabeth Rivers", "Alex Markowitz", "Richard Rothschild"]}, "686": {"id": "1210.0547v1", "title": "Resolved Debris Discs Around A Stars in the Herschel DEBRIS Survey", "url": "http://arxiv.org/pdf/1210.0547v1", "date": "2012-10-01 20:01:26", "abs": "The majority of debris discs discovered so far have only been detected\nthrough infrared excess emission above stellar photospheres. While disc\nproperties can be inferred from unresolved photometry alone under various\nassumptions for the physical properties of dust grains, there is a degeneracy\nbetween disc radius and dust temperature that depends on the grain size\ndistribution and optical properties. By resolving the disc we can measure the\nactual location of the dust. The launch of Herschel, with an angular resolution\nsuperior to previous far-infrared telescopes, allows us to spatially resolve\nmore discs and locate the dust directly. Here we present the nine resolved\ndiscs around A stars between 20 and 40 pc observed by the DEBRIS survey. We use\nthese data to investigate the disc radii by fitting narrow ring models to\nimages at 70, 100 and 160 {\\mu}m and by fitting blackbodies to full spectral\nenergy distributions. We do this with the aim of finding an improved way of\nestimating disc radii for unresolved systems. The ratio between the resolved\nand blackbody radii varies between 1 and 2.5. This ratio is inversely\ncorrelated with luminosity and any remaining discrepancies are most likely\nexplained by differences to the minimum size of grain in the size distribution\nor differences in composition. We find that three of the systems are well fit\nby a narrow ring, two systems are borderline cases and the other four likely\nrequire wider or multiple rings to fully explain the observations, reflecting\nthe diversity of planetary systems.", "cat": "astro-ph.EP", "authors": ["Mark Booth", "Grant Kennedy", "Bruce Sibthorpe", "Brenda C. Matthews", "Mark C. Wyatt", "Gaspard Duch\u00eane", "J. J. Kavelaars", "David Rodriguez", "Jane S. Greaves", "Alice Koning", "Laura Vican", "George H. Rieke", "Kate Y. L. Su", "Amaya Moro-Mart\u00edn", "Paul Kalas"]}, "687": {"id": "1501.06416v1", "title": "A brief survey on local holomorphic dynamics in higher dimensions", "url": "http://arxiv.org/pdf/1501.06416v1", "date": "2015-01-26 14:45:35", "abs": "We give a brief survey on local holomorphic dynamics in higher dimensions.\nThe main novelty of this note is that we will organize the material by the\n\"level\" of local invariants rather than the type of maps.", "cat": "math.CV", "authors": ["Feng Rong"]}, "688": {"id": "1405.0580v1", "title": "Web Content Classification: A Survey", "url": "http://arxiv.org/pdf/1405.0580v1", "date": "2014-05-03 12:57:50", "abs": "As the information contained within the web is increasing day by day,\norganizing this information could be a necessary requirement.The data mining\nprocess is to extract information from a data set and transform it into an\nunderstandable structure for further use. Classification of web page content is\nessential to many tasks in web information retrieval such as maintaining web\ndirectories and focused crawling.The uncontrolled type of nature of web content\npresents additional challenges to web page classification as compared to the\ntraditional text classification, but the interconnected nature of hypertext\nalso provides features that can assist the process. In this paper the web\nclassification is discussed in detail and its importance in field of data\nmining is explored.", "cat": "cs.IR", "authors": ["Prabhjot Kaur"]}, "689": {"id": "1202.6333v2", "title": "Initial data release of the Kepler-INT Survey", "url": "http://arxiv.org/pdf/1202.6333v2", "date": "2012-05-14 10:41:24", "abs": "This paper describes the first data release of the Kepler-INT Survey (KIS),\nthat covers a 116 deg2 region of the Cygnus and Lyra constellations. The Kepler\nfield is the target of the most intensive search for transiting planets to\ndate. Despite the fact that the Kepler mission provides superior time series\nphotometry, with an enormous impact on all areas of stellar variability, its\nfield lacks optical photometry complete to the confusion limit of the Kepler\ninstrument necessary for selecting various classes of targets. For this reason,\nwe follow the observing strategy and data reduction method used in the IPHAS\nand UVEX galactic plane surveys in order to produce a deep optical survey of\nthe Kepler field. This initial release concerns data taken between May and\nAugust 2011, using the Isaac Newton Telescope on the island of La Palma. Four\nbroadband filters were used, U, g, r, i, as well as one narrowband one, Halpha,\nreaching down to a 10-sigma limit of around 20th mag in the Vega system.\nObservations covering around 50 deg2, thus about half of the field, passed our\nquality control thresholds and constitute this first data release. We derive a\nglobal photometric calibration by placing the KIS magnitudes as close as\npossible to the Kepler Input Catalog (KIC) photometry. The initial data release\ncatalogue containing around 6 million sources from all the good photometric\nfields is available for download from the KIS webpage, as well as via MAST.", "cat": "astro-ph.GA", "authors": ["S. Greiss", "D. Steeghs", "B. T. G\u00e4nsicke", "E. L. Mart\u00edn", "P. J. Groot", "M. J. Irwin", "E. Gonz\u00e1lez-Solares", "R. Greimel", "C. Knigge", "R. H. \u00d8stensen", "K. Verbeek", "J. E. Drew", "J. Drake", "P. G. Jonker", "V. Ripepi", "S. Scaringi", "J. Southworth", "M. Still", "N. J. Wright", "H. Farnhill", "L. van Haaften", "S. Shah"]}, "690": {"id": "2007.12795v2", "title": "Photo-z outlier self-calibration in weak lensing surveys", "url": "http://arxiv.org/pdf/2007.12795v2", "date": "2021-06-18 18:00:00", "abs": "Calibrating photometric redshift errors in weak lensing surveys with external\ndata is extremely challenging. We show that both Gaussian and outlier photo-z\nparameters can be self-calibrated from the data alone. This comes at no cost\nfor the neutrino masses, curvature and dark energy equation of state $w_0$, but\nwith a 65% degradation when both $w_0$ and $w_a$ are varied. We perform a\nrealistic forecast for the Vera Rubin Observatory (VRO) Legacy Survey of Space\nand Time (LSST) 3x2 analysis, combining cosmic shear, projected galaxy\nclustering and galaxy - galaxy lensing. We confirm the importance of\nmarginalizing over photo-z outliers. We examine a subset of internal\ncross-correlations, dubbed \"null correlations\", which are usually ignored in\n3x2 analyses. Despite contributing only $\\sim$ 10% of the total\nsignal-to-noise, these null correlations improve the constraints on photo-z\nparameters by up to an order of magnitude. Using the same galaxy sample as\nsources and lenses dramatically improves the photo-z uncertainties too.\nTogether, these methods add robustness to any claim of detected new Physics,\nand reduce the statistical errors on cosmology by 15% and 10% respectively.\nFinally, including CMB lensing from an experiment like Simons Observatory or\nCMB-S4 improves the cosmological and photo-z posterior constraints by about\n10%, and further improves the robustness to systematics. To give intuition on\nthe Fisher forecasts, we examine in detail several toy models that explain the\norigin of the photo-z self-calibration. Our Fisher code LaSSI (Large-Scale\nStructure Information), which includes the effect of Gaussian and outlier\nphoto-z, shear multiplicative bias, linear galaxy bias, and extensions to\n$\\Lambda$CDM, is publicly available at https://github.com/EmmanuelSchaan/LaSSI .", "cat": "astro-ph.CO", "authors": ["Emmanuel Schaan", "Simone Ferraro", "Uro\u0161 Seljak"]}, "691": {"id": "2201.13327v1", "title": "Survey on effective separability", "url": "http://arxiv.org/pdf/2201.13327v1", "date": "2022-01-31 16:24:45", "abs": "Separability for groups refers to the question which subsets of a group can\nbe detected in its finite quotients. Classically, separability is studied in\nterms of which classes have a certain separability property, and this question\nis related to algorithmic problems in groups such as the word problem. A more\nrecent perspective tries to study the order of the smallest finite quotient in\nwhich one detects the subset under consideration depending on its complexity,\nmeasured using the word norm on a finitely generated group. In this survey, we\npresent what is currently known in the field of effective separability and give\nan overview of the open questions for several classes of groups.", "cat": "math.GR", "authors": ["Jonas Der\u00e9", "Michal Ferov", "Mark Pengitore"]}, "692": {"id": "1007.5396v1", "title": "The bright end of the z ~ 7 UV Luminosity Function from a wide and deep HAWK-I survey", "url": "http://arxiv.org/pdf/1007.5396v1", "date": "2010-07-30 09:42:44", "abs": "(Abridged) We present here the second half of an ESO Large Programme, which\nexploits the unique combination of area and sensitivity provided in the near-IR\nby the camera Hawk-I at the VLT. We have obtained - 30 observing hours with\nHawk-I in the Y-band of two high galactic latitude fields. We combined the\nY-band data with deep J and K Hawk-I observations, and with FORS1/FORS2 U, B,\nV, R, I, and Z observations to select z-drop galaxies having Z - Y > 1, no\noptical detection and flat Y - J and Y - K colour terms. We detect 8\nhigh-quality candidates in the magnitude range Y = 25.5 - 26.5 that we add to\nthe z-drop candidates selected in two Hawk-I pointings over the GOODS-South\nfield. We use this full sample of 15 objects found in -161 arcmin^2 of our\nsurvey to constrain the average physical properties and the evolution of the\nnumber density of z ~ 7 LBGs. A stacking analysis yields a best-fit SED with\nphotometric redshift z= 6.85 +0.20 -0.15 and an E(B-V)=0.05 +0.15 -0.05. We\ncompute a binned estimate of the z ~ 7 LF and explore the effects of\nphotometric scatter and model uncertainties on the statistical constraints.\nAfter accounting for the expected incompleteness through MonteCarlo\nsimulations, we strengthen our previous finding that a Schechter luminosity\nfunction constant from z=6 to z=7 is ruled out at a >99% confidence level, even\nincluding the effects of cosmic variance. For galaxies brighter than M_1500=\n-19.0, we derive a luminosity density rho_UV = 1.5^{+2.1}{-0.8} x 10^25\nerg/s/Hz/Mpc^3, implying a decrease by a factor 3.5 from z=6 to z=6.8. We find\nthat, under standard assumptions, the emission rate of ionizing photons coming\nfrom UV bright galaxies is lower by at least a factor of two than the value\nrequired for reionization. Finally, we exploit deep Hawk-I J and K band\nobservations to derive an upper limit on the number density of M1500<~ -22.0\nLBGs at z-8 (Y-dropouts).", "cat": "astro-ph.CO", "authors": ["M. Castellano", "A. Fontana", "D. Paris", "A. Grazian", "L. Pentericci", "K. Boutsia", "P. Santini", "V. Testa", "M. Dickinson", "M. Giavalisco", "R. Bouwens", "J. -G. Cuby", "F. Mannucci", "B. Cl\u00e9ment", "S. Cristiani", "F. Fiore", "S. Gallozzi", "E. Giallongo", "R. Maiolino", "N. Menci", "A. Moorwood", "M. Nonino", "A. Renzini", "P. Rosati", "S. Salimbeni", "E. Vanzella"]}, "693": {"id": "2304.13051v1", "title": "MIGHTEE-HI: The first MeerKAT HI mass function from an untargeted interferometric survey", "url": "http://arxiv.org/pdf/2304.13051v1", "date": "2023-04-25 18:00:01", "abs": "We present the first measurement of the HI mass function (HIMF) using data\nfrom MeerKAT, based on 276 direct detections from the MIGHTEE Survey Early\nScience data covering a period of approximately a billion years ($0 \\leq z \\leq\n0.084 $). This is the first HIMF measured using interferometric data over\nnon-group or cluster field, i.e. a deep blank field. We constrain the\nparameters of the Schechter function which describes the HIMF with two\ndifferent methods: $1/\\rm V_{\\rm max}$ and Modified Maximum Likelihood (MML).\nWe find a low-mass slope $\\alpha=-1.29^{+0.37}_{-0.26}$, `knee' mass\n$\\log_{10}(M_{*}/{\\rm M_{\\odot}}) = 10.07^{+0.24}_{-0.24}$ and normalisation\n$\\log_{10}(\\phi_{*}/\\rm Mpc^{-3})=-2.34^{+0.32}_{-0.36}$ ($H_0 = 67.4$\nkms$^{-1}$ Mpc$^{-1}$) for $1/\\rm V_{\\rm max}$ and\n$\\alpha=-1.44^{+0.13}_{-0.10}$, `knee' mass $\\log_{10}(M_{*}/{\\rm M_{\\odot}}) =\n10.22^{+0.10}_{-0.13}$ and normalisation $\\log_{10}(\\phi_{*}/\\rm\nMpc^{-3})=-2.52^{+0.19}_{-0.14}$ for MML. When using $1/\\rm V_{\\rm max}$ we\nfind both the low-mass slope and `knee' mass to be consistent within $1\\sigma$\nwith previous studies based on single-dish surveys. The cosmological mass\ndensity of HI is found to be slightly larger than previously reported:\n$\\Omega_{\\rm HI}=5.46^{+0.94}_{-0.99} \\times 10^{-4}h^{-1}_{67.4}$ from $1/\\rm\nV_{\\rm max}$ and $\\Omega_{\\rm HI}=6.31^{+0.31}_{-0.31} \\times\n10^{-4}h^{-1}_{67.4}$ from MML but consistent within the uncertainties. We find\nno evidence for evolution of the HIMF over the last billion years.", "cat": "astro-ph.GA", "authors": ["Anastasia A. Ponomareva", "Matt J. Jarvis", "Hengxing Pan", "Natasha Maddox", "Michael G. Jones", "Bradley S. Frank", "Sambatriniaina H. A. Rajohnson", "Wanga Mulaudzi", "Martin Meyer", "Elizabeth A. K. Adams", "Maarten Baes", "Kelley M. Hess", "Sushma Kurapati", "Isabella Prandoni", "Francesco Sinigaglia", "Kristine Spekkens", "Madalina Tudorache", "Ian Heywood", "Jordan D. Collier", "Srikrishna Sekhar"]}, "694": {"id": "2301.13434v1", "title": "DESI and DECaLS (D&D): galaxy-galaxy lensing measurements with 1% survey and its forecast", "url": "http://arxiv.org/pdf/2301.13434v1", "date": "2023-01-31 06:10:46", "abs": "The shear measurement from DECaLS (Dark Energy Camera Legacy Survey) provides\nan excellent opportunity for galaxy-galaxy lensing study with DESI (Dark Energy\nSpectroscopic Instrument) galaxies, given the large ($\\sim 9000$ deg$^2$) sky\noverlap. We explore this potential by combining the DESI 1\\% survey and DECaLS\nDR8. With $\\sim 106$ deg$^2$ sky overlap, we achieve significant detection of\ngalaxy-galaxy lensing for BGS and LRG as lenses. Scaled to the full BGS sample,\nwe expect the statistical errors to improve from $18(12)\\%$ to a promising\nlevel of $2(1.3)\\%$ at $\\theta>8^{'}(<8^{'})$. This brings stronger\nrequirements for future systematics control. To fully realize such potential,\nwe need to control the residual multiplicative shear bias $|m|<0.01$ and the\nbias in the mean redshift $|\\Delta z|<0.015$. We also expect significant\ndetection of galaxy-galaxy lensing with DESI LRG/ELG full samples as lenses,\nand cosmic magnification of ELG through cross-correlation with low-redshift\nDECaLS shear. {If such systematical error control can be achieved,} we find the\nadvantages of DECaLS, comparing with KiDS (Kilo Degree Survey) and HSC\n(Hyper-Suprime Cam), are at low redshift, large-scale, and in measuring the\nshear-ratio (to $\\sigma_R\\sim 0.04$) and cosmic magnification.", "cat": "astro-ph.CO", "authors": ["Ji Yao", "Huanyuan Shan", "Pengjie Zhang", "Eric Jullo", "Jean-Paul Kneib", "Yu Yu", "Ying Zu", "David Brooks", "Axel de la Macorra", "Peter Doel", "Andreu Font-Ribera", "Satya Gontcho A Gontcho", "Theodore Kisner", "Martin Landriau", "Aaron Meisner", "Ramon Miquel", "Jundan Nie", "Claire Poppett", "Francisco Prada", "Michael Schubnell", "Mariana Vargas Magana", "Zhimin Zhou"]}, "695": {"id": "1809.01206v1", "title": "MAGNUM survey: A MUSE-Chandra resolved view on ionized outflows and photoionization in the Seyfert galaxy NGC 1365", "url": "http://arxiv.org/pdf/1809.01206v1", "date": "2018-09-04 19:09:42", "abs": "Ionized outflows, revealed by broad asymmetric wings of the [OIII] line, are\ncommonly observed in AGN but the low intrinsic spatial resolution of\nobservations has generally prevented a detailed characterization of their\nproperties. The MAGNUM survey aims at overcoming these limitations by focusing\non the nearest AGN, including NGC 1365, a nearby Seyfert galaxy (D~17 Mpc),\nhosting a low-luminosity AGN (Lbol ~ 2x10^43 erg/s). We want to obtain a\ndetailed picture of the ionized gas in the central ~5 kpc of NGC 1365 in terms\nof physical properties, kinematics, and ionization mechanisms. We also aim to\ncharacterize the warm ionized outflow as a function of distance from the\nnucleus and its relation with the nuclear X-ray wind. We employed VLT/MUSE\noptical integral field spectroscopic observations to investigate the warm\nionized gas and Chandra ACIS-S X-ray data for the hot highly-ionized phase. We\nobtained flux, kinematic, and diagnostic maps of the optical emission lines,\nwhich we used to disentangle outflows from disk motions and measure the gas\nproperties down to a spatial resolution of ~70 pc. [OIII] emission mostly\ntraces an AGN-ionized kpc-scale biconical outflow with velocities up to ~200\nkm/s. H{\\alpha} emission traces instead star formation in a circumnuclear ring\nand along the bar, where we detect non-circular motions. Soft X-rays are mostly\ndue to thermal emission from the star-forming regions, but we could isolate the\nAGN photoionized component which matches the [OIII] emission. The mass outflow\nrate of the extended ionized outflow matches that of the nuclear X-ray wind and\nthen decreases with radius. However, the hard X-ray emission from the\ncircumnuclear ring suggests that star formation might contribute to the\noutflow. The integrated mass outflow rate, kinetic energy rate, and outflow\nvelocity are broadly consistent with the typical relations observed in more\nluminous AGN.", "cat": "astro-ph.GA", "authors": ["G. Venturi", "E. Nardini", "A. Marconi", "S. Carniani", "M. Mingozzi", "G. Cresci", "F. Mannucci", "G. Risaliti", "R. Maiolino", "B. Balmaverde", "A. Bongiorno", "M. Brusa", "A. Capetti", "C. Cicone", "S. Ciroi", "C. Feruglio", "F. Fiore", "A. Gallazzi", "F. La Franca", "V. Mainieri", "K. Matsuoka", "T. Nagao", "M. Perna", "E. Piconcelli", "E. Sani", "P. Tozzi", "S. Zibetti"]}, "696": {"id": "2012.09830v7", "title": "Autotelic Agents with Intrinsically Motivated Goal-Conditioned Reinforcement Learning: a Short Survey", "url": "http://arxiv.org/pdf/2012.09830v7", "date": "2022-07-12 08:48:32", "abs": "Building autonomous machines that can explore open-ended environments,\ndiscover possible interactions and build repertoires of skills is a general\nobjective of artificial intelligence. Developmental approaches argue that this\ncan only be achieved by $autotelic$ $agents$: intrinsically motivated learning\nagents that can learn to represent, generate, select and solve their own\nproblems. In recent years, the convergence of developmental approaches with\ndeep reinforcement learning (RL) methods has been leading to the emergence of a\nnew field: $developmental$ $reinforcement$ $learning$. Developmental RL is\nconcerned with the use of deep RL algorithms to tackle a developmental problem\n-- the $intrinsically$ $motivated$ $acquisition$ $of$ $open$-$ended$\n$repertoires$ $of$ $skills$. The self-generation of goals requires the learning\nof compact goal encodings as well as their associated goal-achievement\nfunctions. This raises new challenges compared to standard RL algorithms\noriginally designed to tackle pre-defined sets of goals using external reward\nsignals. The present paper introduces developmental RL and proposes a\ncomputational framework based on goal-conditioned RL to tackle the\nintrinsically motivated skills acquisition problem. It proceeds to present a\ntypology of the various goal representations used in the literature, before\nreviewing existing methods to learn to represent and prioritize goals in\nautonomous systems. We finally close the paper by discussing some open\nchallenges in the quest of intrinsically motivated skills acquisition.", "cat": "cs.LG", "authors": ["C\u00e9dric Colas", "Tristan Karch", "Olivier Sigaud", "Pierre-Yves Oudeyer"]}, "697": {"id": "0912.1462v2", "title": "Eight New Quasar Lenses from the Sloan Digital Sky Survey Quasar Lens Search", "url": "http://arxiv.org/pdf/0912.1462v2", "date": "2010-03-15 13:15:44", "abs": "We report the discovery and confirmation of eight new two-image lensed\nquasars by the Sloan Digital Sky Survey (SDSS) Quasar Lens Search. The lenses\nare\n SDSSJ0904+1512 (image separation \\theta=1\"13, source redshift z_s=1.826),\n SDSSJ1054+2733 (\\theta=1\"27, z_s=1.452),\n SDSSJ1055+4628 (\\theta=1\"15, z_s=1.249),\n SDSSJ1131+1915 (\\theta=1\"46, z_s=2.915),\n SDSSJ1304+2001 (\\theta=1\"87, z_s=2.175),\n SDSSJ1349+1227 (\\theta=3\"00, z_s=1.722),\n SDSSJ1455+1447 (\\theta=1\"73, z_s=1.424), and\n SDSSJ1620+1203 (\\theta=2\"77, z_s=1.158).\n Three of them, SDSSJ1055+4628, SDSSJ1455+1447, and SDSSJ1620+1203, satisfy\nthe criteria for constructing our statistical sample for studying the\ncosmological model. Based on galactic absorption lines of the lens galaxies, we\nalso derive lens redshifts of z_l=0.398 and z_l=0.513 for SDSSJ1620+1203 and\nthe previously discovered lens SDSSJ0746+4403, respectively.", "cat": "astro-ph.CO", "authors": ["Issha Kayo", "Naohisa Inada", "Masamune Oguri", "Tomoki Morokuma", "Patrick B. Hall", "Christopher S. Kochanek", "Donald P. Schneider"]}, "698": {"id": "1703.01930v1", "title": "The SCUBA-2 Ambitious Sky Survey: a catalogue of beam-sized sources in the Galactic longitude range 120 to 140", "url": "http://arxiv.org/pdf/1703.01930v1", "date": "2017-03-06 15:43:21", "abs": "The SCUBA-2 Ambitious Sky Survey (SASSy) is composed of shallow 850-$\\umu$m\nimaging using the Sub-millimetre Common-User Bolometer Array 2 (SCUBA-2) on the\nJames Clerk Maxwell Telescope. Here we describe the extraction of a catalogue\nof beam-sized sources from a roughly $120\\,{\\rm deg}^2$ region of the Galactic\nplane mapped uniformly (to an rms level of about 40\\,mJy), covering longitude\n120\\degr\\,$<$\\,\\textit{l}\\,$<$\\,140\\degr\\ and latitude\n$\\abs{\\textit{b}}$\\,$<$\\,2.9\\degr. We used a matched-filtering approach to\nincrease the signal-to-noise (S/N) ratio in these noisy maps and tested the\nefficiency of our extraction procedure through estimates of the false discovery\nrate, as well as by adding artificial sources to the real images. The primary\ncatalogue contains a total of 189 sources at 850\\,$\\umu$m, down to a S/N\nthreshold of approximately 4.6. Additionally, we list 136 sources detected down\nto ${\\rm S/N}=4.3$, but recognise that as we go lower in S/N, the reliability\nof the catalogue rapidly diminishes. We perform follow-up observations of some\nof our lower significance sources through small targeted SCUBA-2 images, and\nlist 265 sources detected in these maps down to ${\\rm S/N}=5$. This illustrates\nthe real power of SASSy: inspecting the shallow maps for regions of 850-$\\umu$m\nemission and then using deeper targeted images to efficiently find fainter\nsources. We also perform a comparison of the SASSy sources with the Planck\nCatalogue of Compact Sources and the \\textit{IRAS} Point Source Catalogue, to\ndetermine which sources discovered in this field might be new, and hence\npotentially cold regions at an early stage of star formation.", "cat": "astro-ph.GA", "authors": ["Will Nettke", "Douglas Scott", "Andy Gibb", "Mark Thompson", "Antonio Chrysostomou", "A. Evans", "Tracey Hill", "Tim Jenness", "Gilles Joncas", "Toby Moore", "Stephen Serjeant", "James Urquhart", "Mattia Vaccari", "Bernd Weferling", "Glenn White", "Ming Zhu"]}, "699": {"id": "1904.02743v2", "title": "How should my chatbot interact? A survey on human-chatbot interaction design", "url": "http://arxiv.org/pdf/1904.02743v2", "date": "2020-10-22 22:00:31", "abs": "Chatbots' growing popularity has brought new challenges to HCI, having\nchanged the patterns of human interactions with computers. The increasing need\nto approximate conversational interaction styles raises expectations for\nchatbots to present social behaviors that are habitual in human-human\ncommunication. In this survey, we argue that chatbots should be enriched with\nsocial characteristics that cohere with users' expectations, ultimately\navoiding frustration and dissatisfaction. We bring together the literature on\ndisembodied, text-based chatbots to derive a conceptual model of social\ncharacteristics for chatbots. We analyzed 56 papers from various domains to\nunderstand how social characteristics can benefit human-chatbot interactions\nand identify the challenges and strategies to designing them. Additionally, we\ndiscussed how characteristics may influence one another. Our results provide\nrelevant opportunities to both researchers and designers to advance\nhuman-chatbot interactions.", "cat": "cs.HC", "authors": ["Ana Paula Chaves", "Marco Aurelio Gerosa"]}, "700": {"id": "1307.2919v1", "title": "Neutrinos and dark energy constraints from future galaxy surveys and CMB lensing information", "url": "http://arxiv.org/pdf/1307.2919v1", "date": "2013-07-10 21:00:02", "abs": "We explore the possibility of obtaining better constraints from future\nastronomical data by means of the Fisher information matrix formalism. In\nparticular, we consider how cosmic microwave background (CMB) lensing\ninformation can improve our parameter error estimation. We consider a massive\nneutrino scenario and a time-evolving dark energy equation of state in the\n$\\Lambda$CDM framework. We use Planck satellite experimental specifications\ntogether with the future galaxy survey Euclid in our forecast. We found\nimprovements in almost all studied parameters considering Planck alone when CMB\nlensing information is used. In this case, the improvement with respect to the\nconstraints found without using CMB lensing is of 93% around the fiducial value\nfor the neutrino parameter. The improvement on one of the dark energy parameter\nreaches 4.4%. When Euclid information is included in the analysis, the\nimprovements on the neutrino parameter constraint is of approximately 128%\naround its fiducial value. The addition of Euclid information provides smaller\nerrors on the dark energy parameters as well. For Euclid alone, the FoM is a\nfactor of $\\sim$ 29 higher than that from Planck alone even considering CMB\nlensing. Finally, the consideration of a nearly perfect CMB experiment showed\nthat CMB lensing cannot be neglected specially in more precise future CMB\nexperiments since it provided in our case a 6 times better FoM in respect to\nthe unlensed CMB analysis .", "cat": "astro-ph.CO", "authors": ["Larissa Santos", "Paolo Cabella", "Amedeo Balbi", "Nicola Vittorio"]}, "701": {"id": "2107.10856v1", "title": "The ALPINE-ALMA [CII] survey: The contribution of major mergers to the galaxy mass assembly at z~5", "url": "http://arxiv.org/pdf/2107.10856v1", "date": "2021-07-22 18:00:02", "abs": "Galaxy mergers are thought to be one of the main mechanisms of the mass\nassembly of galaxies. Recently, many works have suggested a possible increase\nin the fraction of major mergers in the early Universe, reviving the debate on\nwhich processes (e.g., cold accretion, star formation, mergers) most contribute\nto the mass build-up of galaxies through cosmic time. To estimate the\nimportance of major mergers in this context, we make use of the new data\ncollected by the ALMA Large Program to INvestigate [CII] at Early times\n(ALPINE), which observed the [CII] 158 $\\mu$m emission line from a sample of 75\nmain-sequence star-forming galaxies at 4.4 < z < 5.9. We used, for the first\ntime, the morpho-kinematic information provided by the [CII] emission to obtain\nthe fraction of major mergers ($f_{MM}$) at z~5. By adopting different\nprescriptions for the merger timescales ($T_{MM}$), we converted this fraction\ninto the merger rate per galaxy ($R_{MM}$) and per volume ($\\Gamma_{MM}$). We\nthen combined our results with those at lower redshifts from the literature,\ncomputing the cosmic evolution of the merger fraction. This is described by a\nrapid increase from z~0 to higher redshifts, a peak at z~3, and a slow decrease\ntowards earlier epochs. Depending on the timescale prescription used, this\nfraction translates into a merger rate ranging between ~0.1 and ~4.0 Gyr$^{-1}$\nat z~5. Finally, we compare the specific star formation and star-formation rate\ndensity with the analogous quantities from major mergers. Our new ALPINE data\nreveal the presence of a significant merging activity in the early Universe.\nHowever, whether this population of mergers can provide a relevant contribution\nto the galaxy mass assembly at these redshifts and through the cosmic epochs is\nstrongly dependent on the assumption of the merger timescale.", "cat": "astro-ph.GA", "authors": ["M. Romano", "P. Cassata", "L. Morselli", "G. C. Jones", "M. Ginolfi", "A. Zanella", "M. B\u00e9thermin", "P. Capak", "A. Faisst", "O. Le F\u00e8vre", "D. Schaerer", "J. D. Silverman", "L. Yan", "S. Bardelli", "M. Boquien", "A. Cimatti", "M. Dessauges-Zavadsky", "A. Enia", "S. Fujimoto", "C. Gruppioni", "N. P. Hathi", "E. Ibar", "A. M. Koekemoer", "B. C. Lemaux", "G. Rodighiero", "D. Vergani", "G. Zamorani", "E. Zucca"]}, "702": {"id": "2206.13650v1", "title": "The Open Cluster Chemical Abundances and Mapping Survey: VI. Galactic Chemical Gradient Analysis from APOGEE DR17", "url": "http://arxiv.org/pdf/2206.13650v1", "date": "2022-06-27 22:14:12", "abs": "The goal of the Open Cluster Chemical Abundances and Mapping (OCCAM) survey\nis to constrain key Galactic dynamic and chemical evolution parameters by the\nconstruction and analysis of a large, comprehensive, uniform data set of\ninfrared spectra for stars in hundreds of open clusters. This sixth\ncontribution from the OCCAM survey presents analysis of SDSS/APOGEE Data\nRelease 17 (DR17) results for a sample of stars in 150 open clusters, 94 of\nwhich we designate to be \"high quality'' based on the appearance of their\ncolor-magnitude diagram. We find the APOGEE DR17-derived [Fe/H] values to be in\ngood agreement with those from previous high resolution spectroscopic open\ncluster abundance studies. Using a subset of the high quality sample, the\nGalactic abundance gradients were measured for 16 chemical elements, including\n[Fe/H], for both Galactocentric radius ($R_{GC}$) and guiding center radius\n($R_{Guide}$). We find an overall Galactic [Fe/H] vs $R_{GC}$ gradient of\n$-0.073 \\pm 0.002$ dex/kpc over the range of $6 < R_{GC} < 11.5$ kpc, and a\nsimilar gradient is found for [Fe/H] versus $R_{Guide}$. Significant Galactic\nabundance gradients are also noted for O, Mg, S, Ca, Mn, Na, Al, K and Ce. Our\nlarge sample additionally allows us to explore the evolution of the gradients\nin four age bins for the remaining 15 elements.", "cat": "astro-ph.GA", "authors": ["Natalie Myers", "John Donor", "Taylor Spoo", "Peter M. Frinchaboy", "Katia Cunha", "Adrian M. Price-Whelan", "Steven R. Majewski", "Rachael L. Beaton", "Gail Zasowski", "Julia O'Connell", "Amy E. Ray", "Dmitry Bizyaev", "Cristina Chiappini", "D. A. Garc\u00eda-Hern\u00e1ndez", "Doug Geisler", "Henrik J\u00f6nsson", "Richard R. Lane", "Pen\u00e9lope Longa-Pe\u00f1a", "Ivan Minchev", "Dante Minniti", "Christian Nitschelm", "A. Roman-Lopes"]}, "703": {"id": "2008.07267v1", "title": "A Survey of Active Learning for Text Classification using Deep Neural Networks", "url": "http://arxiv.org/pdf/2008.07267v1", "date": "2020-08-17 12:53:20", "abs": "Natural language processing (NLP) and neural networks (NNs) have both\nundergone significant changes in recent years. For active learning (AL)\npurposes, NNs are, however, less commonly used -- despite their current\npopularity. By using the superior text classification performance of NNs for\nAL, we can either increase a model's performance using the same amount of data\nor reduce the data and therefore the required annotation efforts while keeping\nthe same performance. We review AL for text classification using deep neural\nnetworks (DNNs) and elaborate on two main causes which used to hinder the\nadoption: (a) the inability of NNs to provide reliable uncertainty estimates,\non which the most commonly used query strategies rely, and (b) the challenge of\ntraining DNNs on small data. To investigate the former, we construct a taxonomy\nof query strategies, which distinguishes between data-based, model-based, and\nprediction-based instance selection, and investigate the prevalence of these\nclasses in recent research. Moreover, we review recent NN-based advances in NLP\nlike word embeddings or language models in the context of (D)NNs, survey the\ncurrent state-of-the-art at the intersection of AL, text classification, and\nDNNs and relate recent advances in NLP to AL. Finally, we analyze recent work\nin AL for text classification, connect the respective query strategies to the\ntaxonomy, and outline commonalities and shortcomings. As a result, we highlight\ngaps in current research and present open research questions.", "cat": "cs.CL", "authors": ["Christopher Schr\u00f6der", "Andreas Niekler"]}, "704": {"id": "1705.03768v2", "title": "Defining and Surveying Wireless Link Virtualization and Wireless Network Virtualization", "url": "http://arxiv.org/pdf/1705.03768v2", "date": "2018-07-04 16:44:41", "abs": "Virtualization is a topic of great interest in the area of mobile and\nwireless communication systems. However the term virtualization is used in an\ninexact manner which makes it difficult to compare and contrast work that has\nbeen carried out to date. The purpose of this paper is twofold. In the first\nplace, the paper develops a formal theory for defining virtualization. In the\nsecond instance, this theory is used as a way of surveying a body of work in\nthe field of wireless link virtualization, a subspace of wireless network\nvirtualization. The formal theory provides a means for distinguishing work that\nshould be classed as resource allocation as distinct from virtualization. It\nalso facilitates a further classification of the representation level at which\nthe virtualization occurs, which makes comparison of work more meaningful. The\npaper provides a comprehensive survey and highlights gaps in the research that\nmake for fruitful future work.", "cat": "cs.NI", "authors": ["Jonathan van de Belt", "Hamed Ahmadi", "Linda E. Doyle"]}, "705": {"id": "2406.09062v1", "title": "State-Space Modeling in Long Sequence Processing: A Survey on Recurrence in the Transformer Era", "url": "http://arxiv.org/pdf/2406.09062v1", "date": "2024-06-13 12:51:22", "abs": "Effectively learning from sequential data is a longstanding goal of\nArtificial Intelligence, especially in the case of long sequences. From the\ndawn of Machine Learning, several researchers engaged in the search of\nalgorithms and architectures capable of processing sequences of patterns,\nretaining information about the past inputs while still leveraging the upcoming\ndata, without losing precious long-term dependencies and correlations. While\nsuch an ultimate goal is inspired by the human hallmark of continuous real-time\nprocessing of sensory information, several solutions simplified the learning\nparadigm by artificially limiting the processed context or dealing with\nsequences of limited length, given in advance. These solutions were further\nemphasized by the large ubiquity of Transformers, that have initially shaded\nthe role of Recurrent Neural Nets. However, recurrent networks are facing a\nstrong recent revival due to the growing popularity of (deep) State-Space\nmodels and novel instances of large-context Transformers, which are both based\non recurrent computations to go beyond several limits of currently ubiquitous\ntechnologies. In fact, the fast development of Large Language Models enhanced\nthe interest in efficient solutions to process data over time. This survey\nprovides an in-depth summary of the latest approaches that are based on\nrecurrent models for sequential data processing. A complete taxonomy over the\nlatest trends in architectural and algorithmic solutions is reported and\ndiscussed, guiding researchers in this appealing research field. The emerging\npicture suggests that there is room for thinking of novel routes, constituted\nby learning algorithms which depart from the standard Backpropagation Through\nTime, towards a more realistic scenario where patterns are effectively\nprocessed online, leveraging local-forward computations, opening to further\nresearch on this topic.", "cat": "cs.LG", "authors": ["Matteo Tiezzi", "Michele Casoni", "Alessandro Betti", "Marco Gori", "Stefano Melacci"]}, "706": {"id": "2308.10407v2", "title": "Federated Learning for Connected and Automated Vehicles: A Survey of Existing Approaches and Challenges", "url": "http://arxiv.org/pdf/2308.10407v2", "date": "2023-11-11 21:51:17", "abs": "Machine learning (ML) is widely used for key tasks in Connected and Automated\nVehicles (CAV), including perception, planning, and control. However, its\nreliance on vehicular data for model training presents significant challenges\nrelated to in-vehicle user privacy and communication overhead generated by\nmassive data volumes. Federated learning (FL) is a decentralized ML approach\nthat enables multiple vehicles to collaboratively develop models, broadening\nlearning from various driving environments, enhancing overall performance, and\nsimultaneously securing local vehicle data privacy and security. This survey\npaper presents a review of the advancements made in the application of FL for\nCAV (FL4CAV). First, centralized and decentralized frameworks of FL are\nanalyzed, highlighting their key characteristics and methodologies. Second,\ndiverse data sources, models, and data security techniques relevant to FL in\nCAVs are reviewed, emphasizing their significance in ensuring privacy and\nconfidentiality. Third, specific applications of FL are explored, providing\ninsight into the base models and datasets employed for each application.\nFinally, existing challenges for FL4CAV are listed and potential directions for\nfuture investigation to further enhance the effectiveness and efficiency of FL\nin the context of CAV are discussed.", "cat": "cs.LG", "authors": ["Vishnu Pandi Chellapandi", "Liangqi Yuan", "Christopher G. Brinton", "Stanislaw H Zak", "Ziran Wang"]}, "707": {"id": "0707.2118v1", "title": "A formula for a quartic integral: a survey of old proofs and some new ones", "url": "http://arxiv.org/pdf/0707.2118v1", "date": "2007-07-14 03:03:31", "abs": "We discuss several existing proofs of the value of a quartic integral and\npresent a new proof that evolved from rational Landen transformations.", "cat": "math.CA", "authors": ["Tewodros Amdeberhan", "Victor H. Moll"]}, "708": {"id": "1804.07362v1", "title": "Survey of Face Detection on Low-quality Images", "url": "http://arxiv.org/pdf/1804.07362v1", "date": "2018-04-19 20:13:36", "abs": "Face detection is a well-explored problem. Many challenges on face detectors\nlike extreme pose, illumination, low resolution and small scales are studied in\nthe previous work. However, previous proposed models are mostly trained and\ntested on good-quality images which are not always the case for practical\napplications like surveillance systems. In this paper, we first review the\ncurrent state-of-the-art face detectors and their performance on benchmark\ndataset FDDB, and compare the design protocols of the algorithms. Secondly, we\ninvestigate their performance degradation while testing on low-quality images\nwith different levels of blur, noise, and contrast. Our results demonstrate\nthat both hand-crafted and deep-learning based face detectors are not robust\nenough for low-quality images. It inspires researchers to produce more robust\ndesign for face detection in the wild.", "cat": "cs.CV", "authors": ["Yuqian Zhou", "Ding Liu", "Thomas Huang"]}, "709": {"id": "1209.1405v1", "title": "Deep slitless infrared spectroscopic surveys with HST/WFC3", "url": "http://arxiv.org/pdf/1209.1405v1", "date": "2012-09-06 20:33:48", "abs": "HST is commonly thought of as an optical-IR imaging or UV-spectroscopy\nobservatory. However, the advent of WFC3-IR made it possible to do slitless\ninfrared spectroscopic surveys over an area significant for galaxy evolution\nstudies (~0.15 deg^2). Slitless infrared spectroscopy is uniquely possible from\nspace due to the reduced background. Redshift surveys with WFC3-IR offer probes\nof the astrophysics of the galaxy population at z=1-3 from line features, and\nthe true redshift and spatial distribution of galaxies, that cannot be done\nwith photometric surveys alone. While HST slitless spectroscopy is low spectral\nresolution, its high multiplex advantage makes it competitive with future\nground based IR spectrographs, its flux calibration is stable, and its high\nspatial resolution allows measuring the spatial extent of emission lines, which\nonly HST can do currently for large numbers of objects. A deeper slitless IR\nspectroscopic survey over hundreds of arcmin^2 (eg one or more GOODS fields) is\none of the remaining niches for large galaxy evolution studies with HST, and\nwould produce a sample of thousands of spectroscopically confirmed galaxies at\n1 0.05 \\AA{} in 855 AGN spectra (out of 3702 objects with\nredshifts in the accessible range for OVI detection). This sample is further\nsubdivided into 3 groups according to the likelihood of being real and the\npotential for follow-up observation of the candidate. The group with the\ncleanest and most secure candidates is comprised of 145 candidates. 69 of these\nreside at a velocity separation > 5000 km/s from the QSO, and can therefore be\nclassified tentatively as intervening absorbers. Most of these absorbers have\nnot been picked up by earlier, automated QSO absorption line detection\nalgorithms. This sample increases the number of known OVI absorbers at\nredshifts beyond z$_{abs} > 2.7 substantially.", "cat": "astro-ph", "authors": ["S. Frank", "S. Mathur", "M. Pieri", "D. G. York"]}, "717": {"id": "1310.0008v2", "title": "MOA-2011-BLG-322Lb: a \"second generation survey\" microlensing planet", "url": "http://arxiv.org/pdf/1310.0008v2", "date": "2013-12-26 08:03:43", "abs": "Global \"second-generation\" microlensing surveys aim to discover and\ncharacterize extrasolar planets and their frequency, by means of\nround-the-clock high-cadence monitoring of a large area of the Galactic bulge,\nin a controlled experiment. We report the discovery of a giant planet in\nmicrolensing event MOA-2011-BLG-322. This moderate-magnification event, which\ndisplays a clear anomaly induced by a second lensing mass, was inside the\nfootprint of our second-generation microlensing survey, involving MOA, OGLE and\nthe Wise Observatory. The event was observed by the survey groups, without\nprompting alerts that could have led to dedicated follow-up observations.\nFitting a microlensing model to the data, we find that the timescale of the\nevent was t_E=23.2 +/-0.8 days, and the mass ratio between the lens star and\nits companion is q=0.028 +/-0.001. Finite-source effects are marginally\ndetected, and upper limits on them help break some of the degeneracy in the\nsystem parameters. Using a Bayesian analysis that incorporates a Galactic\nstructure model, we estimate the mass of the lens at 0.39 +0.45/-0.19 M_sun, at\na distance of 7.56 +/-0.91 kpc. Thus, the companion is likely a planet of mass\n11.6 +13.4/-5.6 M_J, at a projected separation of 4.3 +1.5/-1.2 AU, rather far\nbeyond the snow line. This is the first pure-survey planet reported from a\nsecond-generation microlensing survey, and shows that survey data alone can be\nsufficient to characterize a planetary model. With the detection of additional\nsurvey-only planets, we will be able to constrain the frequency of extrasolar\nplanets near their systems' snow lines.", "cat": "astro-ph.EP", "authors": ["Y. Shvartzvald", "D. Maoz", "S. Kaspi", "T. Sumi", "A. Udalski", "A. Gould", "D. P. Bennett", "C. Han", "F. Abe", "I. A. Bond", "C. S. Botzler", "M. Freeman", "A. Fukui", "D. Fukunaga", "Y. Itow", "N. Koshimoto", "C. H. Ling", "K. Masuda", "Y. Matsubara", "Y. Muraki", "S. Namba", "K. Ohnishi", "N. J. Rattenbury", "To. Saito", "D. J. Sullivan", "W. L. Sweatman", "D. Suzuki", "P. J. Tristram", "K. Wada", "P. C. M. Yock", "J. Skowron", "S. Koz\u0142owski", "M. K. Szyma\u0144ski", "M. Kubiak", "G. Pietrzy\u0144ski", "I. Soszy\u0144ski", "K. Ulaczyk", "\u0141. Wyrzykowski", "R. Poleski", "P. Pietrukowicz"]}, "718": {"id": "1501.01330v1", "title": "The Gaia-ESO Survey: Discovery of a spatially extended low-mass population in the Vela OB2 association", "url": "http://arxiv.org/pdf/1501.01330v1", "date": "2015-01-06 22:45:57", "abs": "The nearby (distance~350-400 pc), rich Vela OB2 association, includes\n$\\gamma^2$ Velorum, one of the most massive binaries in the solar neighbourhood\nand an excellent laboratory for investigating the formation and early evolution\nof young clusters. Recent Gaia-ESO survey observations have led to the\ndiscovery of two kinematically distinct populations in the young (10-15 Myr)\ncluster immediately surrounding $\\gamma^2$ Velorum. Here we analyse the results\nof Gaia-ESO survey observations of NGC 2547, a 35 Myr cluster located two\ndegrees south of $\\gamma^2$ Velorum. The radial velocity distribution of\nlithium-rich pre-main sequence stars shows a secondary population that is\nkinematically distinct from and younger than NGC 2547. The radial velocities,\nlithium absorption lines, and the positions in a colour-magnitude diagram of\nthis secondary population are consistent with those of one of the components\ndiscovered around $\\gamma^2$ Velorum. This result shows that there is a young,\nlow-mass stellar population spread over at least several square degrees in the\nVela OB2 association. This population could have originally been part of a\ncluster around $\\gamma^2$ Velorum that expanded after gas expulsion or formed\nin a less dense environment that is spread over the whole Vela OB2 region.", "cat": "astro-ph.SR", "authors": ["G. G. Sacco", "R. D. Jeffries", "S. Randich", "E. Franciosini", "R. J. Jackson", "M. Cottaar", "L. Spina", "F. Palla", "M. Mapelli", "E. J. Alfaro", "R. Bonito", "F. Damiani", "A. Frasca", "A. Klutsch", "A. Lanzafame", "A. Bayo", "D. Barrado", "F. Jimenez-Esteban", "G. Gilmore", "G. Micela", "A. Vallenari", "C. Allende Prieto", "E. Flaccomio", "G. Carraro", "M. T. Costado", "P. Jofre", "C. Lardo", "L. Magrini", "L. Morbidelli", "L. Prisinzano", "L. Sbordone"]}, "719": {"id": "1701.05234v1", "title": "Survey of Promising Technologies for 5G Networks", "url": "http://arxiv.org/pdf/1701.05234v1", "date": "2016-12-21 17:57:30", "abs": "As an enhancement of cellular networks, the future-generation 5G network can\nbe considered an ultra-high-speed technology. The proposed 5G network might\ninclude all types of advanced dominant technologies to provide remarkable\nservices. Consequently, new architectures and service management schemes for\ndifferent applications of the emerging technologies need to be recommended to\nsolve issues related to data traffic capacity, high data rate, and reliability\nfor ensuring QoS. Cloud computing, Internet of things (IoT), and\nsoftware-defined networking (SDN) have become some of the core technologies for\nthe 5G network. Cloud-based services provide flexible and efficient solutions\nfor information and communications technology by reducing the cost of investing\nin and managing information technology infrastructure. In terms of\nfunctionality, SDN is a promising architecture that decouples control planes\nand data planes to support programmability, adaptability, and flexibility in\never-changing network architectures. However, IoT combines cloud computing and\nSDN to achieve greater productivity for evolving technologies in 5G by\nfacilitating interaction between the physical and human world. The major\nobjective of this study provides a lawless vision on comprehensive works\nrelated to enabling technologies for the next generation of mobile systems and\nnetworks, mainly focusing on 5G mobile communications.", "cat": "cs.NI", "authors": ["Nam Tuan Le", "Mohammad Arif Hossain", "Amirul Islam", "Do-yun Kim", "Young-June Choi", "Yeong Min Jang"]}, "720": {"id": "1610.09962v3", "title": "An Experimental Survey on Big Data Frameworks", "url": "http://arxiv.org/pdf/1610.09962v3", "date": "2018-06-06 15:34:57", "abs": "Recently, increasingly large amounts of data are generated from a variety of\nsources. Existing data processing technologies are not suitable to cope with\nthe huge amounts of generated data. Yet, many research works focus on Big Data,\na buzzword referring to the processing of massive volumes of (unstructured)\ndata. Recently proposed frameworks for Big Data applications help to store,\nanalyze and process the data. In this paper, we discuss the challenges of Big\nData and we survey existing Big Data frameworks. We also present an\nexperimental evaluation and a comparative study of the most popular Big Data\nframeworks. This survey is concluded with a presentation of best practices\nrelated to the use of the studied frameworks in several application domains\nsuch as machine learning, graph processing and real-world applications.", "cat": "cs.DC", "authors": ["Wissem Inoubli", "Sabeur Aridhi", "Haithem Mezni", "Mondher Maddouri", "Engelbert Mephu Nguifo"]}, "721": {"id": "1111.4243v3", "title": "SED fitting with MCMC: methodology and application to large galaxy surveys", "url": "http://arxiv.org/pdf/1111.4243v3", "date": "2012-01-17 00:06:54", "abs": "We present GalMC (Acquaviva et al 2011), our publicly available Markov Chain\nMonte Carlo algorithm for SED fitting, show the results obtained for a stacked\nsample of Lyman Alpha Emitting galaxies at z ~ 3, and discuss the dependence of\nthe inferred SED parameters on the assumptions made in modeling the stellar\npopulations. We also introduce SpeedyMC, a version of GalMC based on\ninterpolation of pre-computed template libraries. While the flexibility and\nnumber of SED fitting parameters is reduced with respect to GalMC, the average\nrunning time decreases by a factor of 20,000, enabling SED fitting of each\ngalaxy in about one second on a 2.2GHz MacBook Pro laptop, and making SpeedyMC\nthe ideal instrument to analyze data from large photometric galaxy surveys.", "cat": "astro-ph.CO", "authors": ["Viviana Acquaviva", "Eric Gawiser", "Lucia Guaita"]}, "722": {"id": "2310.06501v1", "title": "A sensitive, high-resolution, wide-field IRAM NOEMA CO(1-0) survey of the very nearby spiral galaxy IC 342", "url": "http://arxiv.org/pdf/2310.06501v1", "date": "2023-10-10 10:18:20", "abs": "We present a new wide-field 10.75 x 10.75 arcmin^2 (~11x11 kpc^2),\nhigh-resolution (theta = 3.6\" ~ 60 pc) NOEMA CO(1-0) survey of the very nearby\n(d=3.45 Mpc) spiral galaxy IC 342. The survey spans out to about 1.5 effective\nradii and covers most of the region where molecular gas dominates the cold\ninterstellar medium. We resolved the CO emission into >600 individual giant\nmolecular clouds and associations. We assessed their properties and found that\noverall the clouds show approximate virial balance, with typical virial\nparameters of alpha_vir=1-2. The typical surface density and line width of\nmolecular gas increase from the inter-arm region to the arm and bar region, and\nthey reach their highest values in the inner kiloparsec of the galaxy (median\nSigma_mol~80, 140, 160, and 1100 M_sun/pc^2, sigma_CO~6.6, 7.6, 9.7, and 18.4\nkm/s for inter-arm, arm, bar, and center clouds, respectively). Clouds in the\ncentral part of the galaxy show an enhanced line width relative to their\nsurface densities and evidence of additional sources of dynamical broadening.\nAll of these results agree well with studies of clouds in more distant galaxies\nat a similar physical resolution. Leveraging our measurements to estimate the\ndensity and gravitational free-fall time at 90 pc resolution, averaged on 1.5\nkpc hexagonal apertures, we estimate a typical star formation efficiency per\nfree-fall time of 0.45% with a 16-84% variation of 0.33-0.71% among such 1.5\nkpc regions. We speculate that bar-driven gas inflow could explain the large\ngas concentration in the central kiloparsec and the buildup of the massive\nnuclear star cluster. This wide-area CO map of the closest face-on massive\nspiral galaxy demonstrates the current mapping power of NOEMA and has many\npotential applications. The data and products are publicly available.", "cat": "astro-ph.GA", "authors": ["M. Querejeta", "J. Pety", "A. Schruba", "A. K. Leroy", "C. N. Herrera", "I-D. Chiang", "S. E. Meidt", "E. Rosolowsky", "E. Schinnerer", "K. Schuster", "J. Sun", "K. A. Herrmann", "A. T. Barnes", "I. Beslic", "F. Bigiel", "Y. Cao", "M. Chevance", "C. Eibensteiner", "E. Emsellem", "C. M. Faesi", "A. Hughes", "J. Kim", "R. S. Klessen", "K. Kreckel", "J. M. D. Kruijssen", "D. Liu", "N. Neumayer", "H. -A. Pan", "T. Saito", "K. Sandstrom", "Y. -S. Teng", "A. Usero", "T. G. Williams", "A. Zakardjian"]}, "723": {"id": "2308.00393v1", "title": "A Survey of Time Series Anomaly Detection Methods in the AIOps Domain", "url": "http://arxiv.org/pdf/2308.00393v1", "date": "2023-08-01 09:13:57", "abs": "Internet-based services have seen remarkable success, generating vast amounts\nof monitored key performance indicators (KPIs) as univariate or multivariate\ntime series. Monitoring and analyzing these time series are crucial for\nresearchers, service operators, and on-call engineers to detect outliers or\nanomalies indicating service failures or significant events. Numerous advanced\nanomaly detection methods have emerged to address availability and performance\nissues. This review offers a comprehensive overview of time series anomaly\ndetection in Artificial Intelligence for IT operations (AIOps), which uses AI\ncapabilities to automate and optimize operational workflows. Additionally, it\nexplores future directions for real-world and next-generation time-series\nanomaly detection based on recent advancements.", "cat": "cs.LG", "authors": ["Zhenyu Zhong", "Qiliang Fan", "Jiacheng Zhang", "Minghua Ma", "Shenglin Zhang", "Yongqian Sun", "Qingwei Lin", "Yuzhi Zhang", "Dan Pei"]}, "724": {"id": "2107.02823v5", "title": "Deep Learning for Micro-expression Recognition: A Survey", "url": "http://arxiv.org/pdf/2107.02823v5", "date": "2022-10-10 11:20:14", "abs": "Micro-expressions (MEs) are involuntary facial movements revealing people's\nhidden feelings in high-stake situations and have practical importance in\nmedical treatment, national security, interrogations and many human-computer\ninteraction systems. Early methods for MER mainly based on traditional\nappearance and geometry features. Recently, with the success of deep learning\n(DL) in various fields, neural networks have received increasing interests in\nMER. Different from macro-expressions, MEs are spontaneous, subtle, and rapid\nfacial movements, leading to difficult data collection, thus have small-scale\ndatasets. DL based MER becomes challenging due to above ME characters. To date,\nvarious DL approaches have been proposed to solve the ME issues and improve MER\nperformance. In this survey, we provide a comprehensive review of deep\nmicro-expression recognition (MER), including datasets, deep MER pipeline, and\nthe bench-marking of most influential methods. This survey defines a new\ntaxonomy for the field, encompassing all aspects of MER based on DL. For each\naspect, the basic approaches and advanced developments are summarized and\ndiscussed. In addition, we conclude the remaining challenges and and potential\ndirections for the design of robust deep MER systems. To the best of our\nknowledge, this is the first survey of deep MER methods, and this survey can\nserve as a reference point for future MER research.", "cat": "cs.CV", "authors": ["Yante Li", "Jinsheng Wei", "Yang Liu", "Janne Kauttonen", "Guoying Zhao"]}, "725": {"id": "1601.05111v1", "title": "Direct and Inverse Variational Problems on Time Scales: A Survey", "url": "http://arxiv.org/pdf/1601.05111v1", "date": "2016-01-19 21:43:39", "abs": "We deal with direct and inverse problems of the calculus of variations on\narbitrary time scales. Firstly, using the Euler-Lagrange equation and the\nstrengthened Legendre condition, we give a general form for a variational\nfunctional to attain a local minimum at a given point of the vector space.\nFurthermore, we provide a necessary condition for a dynamic\nintegro-differential equation to be an Euler-Lagrange equation (Helmholtz's\nproblem of the calculus of variations on time scales). New and interesting\nresults for the discrete and quantum settings are obtained as particular cases.\nFinally, we consider very general problems of the calculus of variations given\nby the composition of a certain scalar function with delta and nabla integrals\nof a vector valued field.", "cat": "math.OC", "authors": ["Monika Dryl", "Delfim F. M. Torres"]}, "726": {"id": "1505.08064v1", "title": "The LAMOST Survey of Background Quasars in the Vicinity Fields of the M 31 and M 33 - III. Results from the 2013 Regular Survey", "url": "http://arxiv.org/pdf/1505.08064v1", "date": "2015-05-29 14:36:14", "abs": "In this work, we report new quasars discovered in the vicinity fields of the\nAndromeda (M31) and Triangulum (M33) galaxies with the LAMOST (Large Sky Area\nMulti-Object Fiber Spectroscopic Telescope, also named Guoshoujing Telescope)\nduring the 2013 observational season, the second year of Regular Survey. In\ntotal, 1330 new quasars are discovered in an area of $\\sim$133 deg$^2$ around\nM31 and M33. With $i$ magnitudes ranging from 14.79 to 20.0, redshifts from\n0.08 to 4.85, the 1330 new quasars represent a significant increase of the\nnumber of identified quasars in the vicinity fields of M31 and M33. Up to the\nmoment, there are in total 1870 quasars discovered by LAMOST in this area (see\nalso Huo et al. 2010, 2013). The much enlarged sample of known quasars in this\narea can potentially be utilized to construct a precise astrometric reference\nframe for the measurement of the minute proper motions of M31, M33 and the\nassociated substructures, vital for the understanding of the formation and\nevolution of M31, M33 and the Local Group of galaxies.Meanwhile, amongst the\nsample, there are in total 45, 98 and 225 quasars with $i$ magnitudes brighter\nthan 17.0, 17.5 and 18.0 respectively. In the aforementioned brightness bins,\n15, 35 and 84 quasars are reported here for the first time, 6, 21 and 81 are\nreported in Huo et al. (2010, 2013), while 0, 1 and 6 are from the Sloan\nDigital Sky Survey, and 24, 41 and 54 are from the NED database. These bright\nquasars provide an invaluable sample for the kinematics and chemistry study of\nthe interstellar/intergalactic medium of the Local Group.", "cat": "astro-ph.GA", "authors": ["Zhi-Ying Huo", "Xiao-Wei Liu", "Mao-Sheng Xiang", "Jian-Rong Shi", "Hai-Bo Yuan", "Yang Huang", "Yong Zhang", "Yong-Hui Hou", "Yue-Fei Wang", "Ming Yang"]}, "727": {"id": "2303.01368v1", "title": "A survey of path planning and feedrate interpolation in computer numerical control", "url": "http://arxiv.org/pdf/2303.01368v1", "date": "2023-02-28 08:25:32", "abs": "This paper presents a brief survey (in Chinese) on path planning and feedrate\ninterpolation. Numerical control technology is widely employed in the modern\nmanufacturing industry, and related research has been emphasized by academia\nand industry. The traditional process of numerical control technology is mainly\ncomposed of tool path planning and feedrate interpolation. To attain the\nmachining of high speed and precision, several problems in tool path planning\nand feedrate interpolation are usually transformed into mathematical\noptimization models. To better undertake the research on the integrated design\nand optimization idea of tool path planning and feedrate interpolation, it is\nnecessary to systematically review and drawn on the existing representative\nworks. We will introduce the relevant methods and technical progress of tool\npath planning and feedrate interpolation in CNC machining successively,\nincluding tool path planning based on end milling, tool orientation\noptimization, G-code processing and corner transition, feedrate planning of\nparameter curves, and some new machining optimization methods proposed\nrecently.", "cat": "math.OC", "authors": ["Hong-yu Ma", "Li-yong Shen", "Xin Jiang", "Qiang Zou", "Chun-ming Yuan"]}, "728": {"id": "2101.06303v1", "title": "Hypergeometric Functions over Finite Fields and Modular Forms: A Survey and New Conjectures", "url": "http://arxiv.org/pdf/2101.06303v1", "date": "2021-01-15 21:22:44", "abs": "Hypergeometric functions over finite fields were introduced by Greene in the\n1980s as a finite field analogue of classical hypergeometric series. These\nfunctions, and their generalizations, naturally lend themselves to, and have\nbeen widely used in, character sum evaluations and counting points on algebraic\nvarieties. More interestingly, perhaps, are their links to Fourier coefficients\nof modular forms. In this paper, we outline the main results in this area and\nalso conjecture 13 new relations.", "cat": "math.NT", "authors": ["Madeline Locus Dawsey", "Dermot McCarthy"]}, "729": {"id": "1701.04290v1", "title": "Machine Translation Approaches and Survey for Indian Languages", "url": "http://arxiv.org/pdf/1701.04290v1", "date": "2017-01-16 13:55:01", "abs": "In this study, we present an analysis regarding the performance of the\nstate-of-art Phrase-based Statistical Machine Translation (SMT) on multiple\nIndian languages. We report baseline systems on several language pairs. The\nmotivation of this study is to promote the development of SMT and linguistic\nresources for these language pairs, as the current state-of-the-art is quite\nbleak due to sparse data resources. The success of an SMT system is contingent\non the availability of a large parallel corpus. Such data is necessary to\nreliably estimate translation probabilities. We report the performance of\nbaseline systems translating from Indian languages (Bengali, Guajarati, Hindi,\nMalayalam, Punjabi, Tamil, Telugu and Urdu) into English with average 10%\naccurate results for all the language pairs.", "cat": "cs.CL", "authors": ["Nadeem Jadoon Khan", "Waqas Anwar", "Nadir Durrani"]}, "730": {"id": "1012.0816v1", "title": "The Westerbork Hydrogen Accretion in Local Galaxies (HALOGAS) Survey I. Survey Description and Pilot Observations", "url": "http://arxiv.org/pdf/1012.0816v1", "date": "2010-12-03 19:01:30", "abs": "We introduce a new, very deep neutral hydrogen (HI) survey being performed\nwith the Westerbork Synthesis Radio Telescope (WSRT). The Westerbork Hydrogen\nAccretion in LOcal GAlaxieS (HALOGAS) Survey is producing an archive of some of\nthe most sensitive HI observations available, on the angular scales which are\nmost useful for studying faint, diffuse gas in and around nearby galaxies. The\nsurvey data are being used to perform careful modeling of the galaxies,\ncharacterizing their gas content, morphology, and kinematics, with the primary\ngoal of revealing the global characteristics of cold gas accretion onto spiral\ngalaxies in the local Universe. In this paper, we describe the survey sample\nselection, the data acquisition, reduction, and analysis, and present the data\nproducts obtained during our pilot program, which consists of UGC 2082, NGC\n672, NGC 925, and NGC 4565. The observations reveal a first glimpse of the\npicture that the full HALOGAS project aims to illuminate: the properties of\naccreting HI in different types of spirals, and across a range of galactic\nenvironments. None of the pilot survey galaxies hosts an HI halo of the scale\nof NGC 891, but all show varying indications of halo gas features. We compare\nthe properties of detected features in the pilot survey galaxies with their\nglobal characteristics, and discuss similarities and differences with NGC 891\nand NGC 2403.", "cat": "astro-ph.CO", "authors": ["George Heald", "Gyula Jozsa", "Paolo Serra", "Laura Zschaechner", "Richard Rand", "Filippo Fraternali", "Tom Oosterloo", "Rene Walterbos", "Eva Juette", "Gianfranco Gentile"]}, "731": {"id": "2111.14203v1", "title": "How Deep Are the Fakes? Focusing on Audio Deepfake: A Survey", "url": "http://arxiv.org/pdf/2111.14203v1", "date": "2021-11-28 18:28:30", "abs": "Deepfake is content or material that is synthetically generated or\nmanipulated using artificial intelligence (AI) methods, to be passed off as\nreal and can include audio, video, image, and text synthesis. This survey has\nbeen conducted with a different perspective compared to existing survey papers,\nthat mostly focus on just video and image deepfakes. This survey not only\nevaluates generation and detection methods in the different deepfake\ncategories, but mainly focuses on audio deepfakes that are overlooked in most\nof the existing surveys. This paper critically analyzes and provides a unique\nsource of audio deepfake research, mostly ranging from 2016 to 2020. To the\nbest of our knowledge, this is the first survey focusing on audio deepfakes in\nEnglish. This survey provides readers with a summary of 1) different deepfake\ncategories 2) how they could be created and detected 3) the most recent trends\nin this domain and shortcomings in detection methods 4) audio deepfakes, how\nthey are created and detected in more detail which is the main focus of this\npaper. We found that Generative Adversarial Networks(GAN), Convolutional Neural\nNetworks (CNN), and Deep Neural Networks (DNN) are common ways of creating and\ndetecting deepfakes. In our evaluation of over 140 methods we found that the\nmajority of the focus is on video deepfakes and in particular in the generation\nof video deepfakes. We found that for text deepfakes there are more generation\nmethods but very few robust methods for detection, including fake news\ndetection, which has become a controversial area of research because of the\npotential of heavy overlaps with human generation of fake content. This paper\nis an abbreviated version of the full survey and reveals a clear need to\nresearch audio deepfakes and particularly detection of audio deepfakes.", "cat": "cs.SD", "authors": ["Zahra Khanjani", "Gabrielle Watson", "Vandana P. Janeja"]}, "732": {"id": "2004.13818v1", "title": "A Survey of Document Grounded Dialogue Systems (DGDS)", "url": "http://arxiv.org/pdf/2004.13818v1", "date": "2020-04-17 03:22:28", "abs": "Dialogue system (DS) attracts great attention from industry and academia\nbecause of its wide application prospects. Researchers usually divide the DS\naccording to the function. However, many conversations require the DS to switch\nbetween different functions. For example, movie discussion can change from\nchit-chat to QA, the conversational recommendation can transform from chit-chat\nto recommendation, etc. Therefore, classification according to functions may\nnot be enough to help us appreciate the current development trend. We classify\nthe DS based on background knowledge. Specifically, study the latest DS based\non the unstructured document(s). We define Document Grounded Dialogue System\n(DGDS) as the DS that the dialogues are centering on the given document(s). The\nDGDS can be used in scenarios such as talking over merchandise against product\nManual, commenting on news reports, etc. We believe that extracting\nunstructured document(s) information is the future trend of the DS because a\ngreat amount of human knowledge lies in these document(s). The research of the\nDGDS not only possesses a broad application prospect but also facilitates AI to\nbetter understand human knowledge and natural language. We analyze the\nclassification, architecture, datasets, models, and future development trends\nof the DGDS, hoping to help researchers in this field.", "cat": "cs.CL", "authors": ["Longxuan Ma", "Wei-Nan Zhang", "Mingda Li", "Ting Liu"]}, "733": {"id": "1707.07435v7", "title": "Deep Learning based Recommender System: A Survey and New Perspectives", "url": "http://arxiv.org/pdf/1707.07435v7", "date": "2019-07-10 01:26:36", "abs": "With the ever-growing volume of online information, recommender systems have\nbeen an effective strategy to overcome such information overload. The utility\nof recommender systems cannot be overstated, given its widespread adoption in\nmany web applications, along with its potential impact to ameliorate many\nproblems related to over-choice. In recent years, deep learning has garnered\nconsiderable interest in many research fields such as computer vision and\nnatural language processing, owing not only to stellar performance but also the\nattractive property of learning feature representations from scratch. The\ninfluence of deep learning is also pervasive, recently demonstrating its\neffectiveness when applied to information retrieval and recommender systems\nresearch. Evidently, the field of deep learning in recommender system is\nflourishing. This article aims to provide a comprehensive review of recent\nresearch efforts on deep learning based recommender systems. More concretely,\nwe provide and devise a taxonomy of deep learning based recommendation models,\nalong with providing a comprehensive summary of the state-of-the-art. Finally,\nwe expand on current trends and provide new perspectives pertaining to this new\nexciting development of the field.", "cat": "cs.IR", "authors": ["Shuai Zhang", "Lina Yao", "Aixin Sun", "Yi Tay"]}, "734": {"id": "1309.2660v2", "title": "Data-Driven Grasp Synthesis - A Survey", "url": "http://arxiv.org/pdf/1309.2660v2", "date": "2016-04-14 05:59:17", "abs": "We review the work on data-driven grasp synthesis and the methodologies for\nsampling and ranking candidate grasps. We divide the approaches into three\ngroups based on whether they synthesize grasps for known, familiar or unknown\nobjects. This structure allows us to identify common object representations and\nperceptual processes that facilitate the employed data-driven grasp synthesis\ntechnique. In the case of known objects, we concentrate on the approaches that\nare based on object recognition and pose estimation. In the case of familiar\nobjects, the techniques use some form of a similarity matching to a set of\npreviously encountered objects. Finally for the approaches dealing with unknown\nobjects, the core part is the extraction of specific features that are\nindicative of good grasps. Our survey provides an overview of the different\nmethodologies and discusses open problems in the area of robot grasping. We\nalso draw a parallel to the classical approaches that rely on analytic\nformulations.", "cat": "cs.RO", "authors": ["Jeannette Bohg", "Antonio Morales", "Tamim Asfour", "Danica Kragic"]}, "735": {"id": "1201.2587v2", "title": "Identification of known objects in solar system surveys", "url": "http://arxiv.org/pdf/1201.2587v2", "date": "2012-03-29 10:02:25", "abs": "The discovery of new objects in modern wide-field asteroid and comet surveys\ncan be enhanced by first identifying observations belonging to known solar\nsystem objects. The assignation of new observations to a known object is an\nattribution problem that occurs when a least squares orbit already exists for\nthe object but a separate fit is not possible to just the set of new\nobservations. In this work we explore the strongly asymmetric attribution\nproblem in which the existing least squares orbit is very well constrained and\nthe new data are sparse. We describe an attribution algorithm that introduces\nnew quality control metrics in the presence of strong biases in the astrometric\nresiduals. The main biases arise from the stellar catalogs used in the\nreduction of asteroid observations and we show that a simple debiasing with\nmeasured regional catalog biases significantly improves the results. We tested\nthe attribution algorithm using data from the PS1 survey that used the 2MASS\nstar catalog for the astrometric reduction. We found small but statistically\nsignificant biases in the data of up to 0.1 arcsec that are relevant only when\nthe observations reach the level of accuracy made possible by instruments like\nPS1. The false attribution rate was measured to be < 1/1,000 with a simple\nadditional condition that can reduce it to zero while the attribution\nefficiency is consistent with 100%.", "cat": "astro-ph.EP", "authors": ["Andrea Milani", "Zoran Knezevic", "Davide Farnocchia", "Fabrizio Bernardi", "Robert Jedicke", "Larry Denneau", "Richard J. Wainscoat", "William Burgett", "Tommy Grav", "Nick Kaiser", "Eugene Magnier", "Paul A. Price"]}, "736": {"id": "2202.09120v1", "title": "Analysis of Dual Band and Survey Photometry of Two Low Mass Ratio Contact Binary Systems", "url": "http://arxiv.org/pdf/2202.09120v1", "date": "2022-02-18 10:50:08", "abs": "The study presents photometric analysis of the completely eclipsing contact\nbinary systems TYC 8351-1081-1 and ASAS J210406-0522.3. TYC 8351-1081-1 is an\nextremely low mass ratio (q=0.086) system with high degree of contact (f=0.66)\nwhile ASAS J210406-0522.3 is found to be in marginal contact (f=0.08) with a\nrelatively low mass ratio of 0.272. There is good thermal contact in both\nsystems with only a small difference in the temperature of the components. The\nsystems have been observed by a number sky surveys over the past 20 years. We\ncompare the light curve solutions from up to three of these surveys and find\nthat survey photometric data manually analysed is robust and yields results\ncomparable to dedicated ground based photometry. There is evidence of\nsignificant luminosity transfer from the primary to the secondary, on the order\nof 0.5LJ for TYC 8351-1081-1 and 0.06LJ for ASAS J210406-0522.3. There appears\nto be no change in period of either system over the past 20 years and\ntheoretical angular momentum loss is below current measurement threshold in\nboth cases. We also show that the mass ratio and separation are well above the\ntheoretical values for orbital instability in both cases. As would be expected,\nthe density of the secondary components is significantly higher relative to the\nprimary.", "cat": "astro-ph.SR", "authors": ["Surjit S. Wadhwa", "Ain Y. De Horta", "Miroslav D. Filipovic", "Nick F. H. Tothill"]}, "737": {"id": "1809.10745v2", "title": "A Short Survey of Topological Data Analysis in Time Series and Systems Analysis", "url": "http://arxiv.org/pdf/1809.10745v2", "date": "2018-10-20 17:40:31", "abs": "Topological Data Analysis (TDA) is the collection of mathematical tools that\ncapture the structure of shapes in data. Despite computational topology and\ncomputational geometry, the utilization of TDA in time series and signal\nprocessing is relatively new. In some recent contributions, TDA has been\nutilized as an alternative to the conventional signal processing methods.\nSpecifically, TDA is been considered to deal with noisy signals and time\nseries. In these applications, TDA is used to find the shapes in data as the\nmain properties, while the other properties are assumed much less informative.\nIn this paper, we will review recent developments and contributions where\ntopological data analysis especially persistent homology has been applied to\ntime series analysis, dynamical systems and signal processing. We will cover\nproblem statements such as stability determination, risk analysis, systems\nbehaviour, and predicting critical transitions in financial markets.", "cat": "cs.IR", "authors": ["Shafie Gholizadeh", "Wlodek Zadrozny"]}, "738": {"id": "2005.07359v1", "title": "A Survey on Security and Privacy Issues in Modern Healthcare Systems: Attacks and Defenses", "url": "http://arxiv.org/pdf/2005.07359v1", "date": "2020-05-15 05:10:07", "abs": "The recent advancements in computing systems and wireless communications have\nmade healthcare systems more efficient than before. Modern healthcare devices\ncan monitor and manage different health conditions of the patients\nautomatically without any manual intervention from medical professionals.\nAdditionally, the use of implantable medical devices (IMDs), body area networks\n(BANs), and Internet of Things (IoT) technologies in healthcare systems improve\nthe overall patient monitoring and treatment process. However, these systems\nare complex in software and hardware, and optimizing between security, privacy,\nand treatment is crucial for healthcare systems as any security or privacy\nviolation can lead to severe effects on patients' treatments and overall health\nconditions. Indeed, the healthcare domain is increasingly facing security\nchallenges and threats due to numerous design flaws and the lack of proper\nsecurity measures in healthcare devices and applications. In this paper, we\nexplore various security and privacy threats to healthcare systems and discuss\nthe consequences of these threats. We present a detailed survey of different\npotential attacks and discuss their impacts. Furthermore, we review the\nexisting security measures proposed for healthcare systems and discuss their\nlimitations. Finally, we conclude the paper with future research directions\ntoward securing healthcare systems against common vulnerabilities.", "cat": "cs.CR", "authors": ["AKM Iqridar Newaz", "Amit Kumar Sikder", "Mohammad Ashiqur Rahman", "A. Selcuk Uluagac"]}, "739": {"id": "2012.03960v2", "title": "The Pristine survey -- XII: Gemini-GRACES chemo-dynamical study of newly discovered extremely metal-poor stars in the Galaxy", "url": "http://arxiv.org/pdf/2012.03960v2", "date": "2021-06-12 18:17:41", "abs": "High-resolution optical spectra of 30 metal-poor stars selected from the\n\\Pristine\\ survey are presented, based on observations taken with the Gemini\nObservatory GRACES spectrograph. Stellar parameters \\teff and \\logg are\ndetermined using a Gaia DR2 colour-temperature calibration and surface gravity\nfrom the Stefan-Boltzmann equation. GRACES spectra are used to determine\nchemical abundances (or upper-limits) for 20 elements (Li, O, Na, Mg, K, Ca,\nTi, Sc, Cr, Mn, Fe, Ni, Cu, Zn, Y, Zr, Ba, La, Nd, Eu). These stars are\nconfirmed to be metal-poor ([Fe/H]$<-2.5$), with higher precision than from\nearlier medium-resolution analyses. The chemistry for most targets is similar\nto other extremely metal-poor stars in the Galactic halo. Three stars near\n[Fe/H]$=-3.0$ have unusually low Ca and high Mg, suggestive of contributions\nfrom few SN~II where alpha-element formation through hydrostatic\nnucleosynthesis was more efficient. Three new carbon-enhanced metal-poor stars\nare also identified (two CEMP-s and one potential CEMP-no star) when our\nchemical abundances are combined with carbon from previous medium-resolution\nanalyses. The GRACES spectra also provide precision radial velocities\n($\\sigma_{\\rm RV}\\le0.2$km\\,s$^{-1}$) for dynamical orbit calculations with the\nGaia DR2 proper motions. Most of our targets are dynamically associated with\nthe Galactic halo; however, five stars with [Fe/H]$<-3$ have planar-like\norbits, including one retrograde star. Another five stars are dynamically\nconsistent with the Gaia-Sequoia accretion event; three have typical halo\n[$\\alpha$/Fe] ratios for their metallicities, whereas two are\n[Mg/Fe]-deficient, and one is a new CEMP-s candidate. These results are\ndiscussed in terms of the formation and early chemical evolution of the Galaxy.", "cat": "astro-ph.GA", "authors": ["Collin L. Kielty", "Kim A. Venn", "Federico Sestito", "Else Starkenburg", "Nicolas F. Martin", "David S. Aguado", "Anke Arentsen", "S\u00e9bastien Fabbro", "Jonay I. Gonz\u00e1lez Hern\u00e1ndez", "Vanessa Hill", "Pascale Jablonka", "Carmela Lardo", "Lyudmila I. Mashonkina", "Julio F. Navarro", "Chris Sneden", "Guillaume F. Thomas", "Kris Youakim", "Spencer Bialek", "Rub\u00e9n S\u00e1nchez-Janssen"]}, "740": {"id": "1708.09704v1", "title": "IVOA Recommendation: HiPS - Hierarchical Progressive Survey", "url": "http://arxiv.org/pdf/1708.09704v1", "date": "2017-08-31 13:38:21", "abs": "This document presents HiPS, a hierarchical scheme for the description,\nstorage and access of sky survey data. The system is based on hierarchical\ntiling of sky regions at finer and finer spatial resolution which facilitates a\nprogressive view of a survey, and supports multi-resolution zooming and\npanning. HiPS uses the HEALPix tessellation of the sky as the basis for the\nscheme and is implemented as a simple file structure with a direct indexing\nscheme that leads to practical implementations.", "cat": "astro-ph.IM", "authors": ["Pierre Fernique", "Mark Allen", "Thomas Boch", "Tom Donaldson", "Daniel Durand", "Ken Ebisawa", "Laurent Michel", "Jesus Salgado", "Felix Stoehr"]}, "741": {"id": "1412.5326v1", "title": "The XMM deep survey in the CDF-S VIII. X-ray properties of the two brightest sources", "url": "http://arxiv.org/pdf/1412.5326v1", "date": "2014-12-17 10:39:26", "abs": "We present results from the deep XMM-Newton observations of the two brightest\nX-ray sources in the Chandra Deep Field South (CDFS), PID 203 (z=0.544) and PID\n319 (z=0.742). The long exposure of 2.5 Ms over a 10 year period (net 4 yr with\na 6 yr gap) makes it possible to obtain high quality X-ray spectra of these two\nType I AGN with X-ray luminosity of 10^44 erg/s, typical luminosity for\nlow-redshift PG quasars, track their X-ray variability both in flux and\nspectral shape. Both sources showed X-ray flux variability of ~10-20 per cent\nin rms which is similar in the soft (0.5-2 keV) and hard (2-7 keV) bands. PID\n203, which has evidence for optical extinction, shows modest amount of\nabsorption (nH~1e21cm^-2) in the X-ray spectrum. Fe K emission is strongly\ndetected in both objects with EW~0.2 keV. The lines in both objects are\nmoderately broad and exhibit marginal evidence for variability in shape and\nflux, indicating that the bulk of the line emission come from their accretion\ndisks rather than distant tori.", "cat": "astro-ph.HE", "authors": ["K. Iwasawa", "C. Vignali", "A. Comastri", "R. Gilli", "F. Vito", "W. N. Brandt", "F. J. Carrera", "G. Lanzuisi", "S. Falocco", "F. Vagnetti"]}, "742": {"id": "2212.01352v1", "title": "The SDSS-HET Survey of Kepler Eclipsing Binaries. A Sample of Four Benchmark Binaries", "url": "http://arxiv.org/pdf/2212.01352v1", "date": "2022-12-02 18:18:37", "abs": "The purpose of this work is to extend a sample of accurately modeled,\nbenchmark-grade eclipsing binaries with accurately determined masses and radii.\nWe select four \"well-behaved\" Kepler binaries, KIC2306740, KIC4076952,\nKIC5193386 and KIC5288543, each with at least 8 double-lined spectra from the\napogee instrument that is part of the Sloan Digital Sky Surveys III and IV, and\nfrom the Hobby-Eberly High Resolution Spectrograph. We obtain masses and radii\nwith uncertainties of 2.5% or less for all four systems. Three of these systems\nhave orbital periods longer than 9 days, and thus populate an under-sampled\nregion of the parameter space for extremely well-characterized detached\neclipsing binaries. We compare the derived masses and radii against MESA MIST\nisochrones to determine the ages of the systems. All systems were found to be\ncoeval, showing that the results are consistent across MESA MIST and PHOEBE.", "cat": "astro-ph.SR", "authors": ["Kelly Hambleton", "Andrej Prsa", "Scott W. Fleming", "Suvrath Mahadevan", "Chad F. Bender"]}, "743": {"id": "2011.05979v2", "title": "Probing episodic accretion with chemistry: CALYPSO observations of IRAM 04191+1522. Results from the CALYPSO IRAM-PdBI survey", "url": "http://arxiv.org/pdf/2011.05979v2", "date": "2020-11-12 08:35:50", "abs": "Context. The process of mass accretion in the earliest phases of star\nformation is still not fully understood: Does the accretion rate smoothly\ndecline with the age of the protostar or are there short, intermittent\naccretion bursts? Aims. We aim to explore whether or not the observed C$^{18}$O\nand N$_2$H$^+$ emission pattern towards the VeLLO IRAM 04191+1522 can be\nunderstood in the framework of a scenario where the emission is chemically\ntracing a past accretion burst. Methods.We used high-angular-resolution Plateau\nde Bure Interferometer (PdBI) observations of C$^{18}$O and N$_2$H$^+$ towards\nIRAM 04191+1522 that were obtained as part of the CALYPSO IRAM Large Program.\nWe model these observations using a chemical code with a time-dependent\nphysical structure coupled with a radiative transfer module, where we allow for\nvariations in the source luminosity. Results. We find that the N$_2$H$^+$ line\nemission shows a central hole, while the C$^{18}$O emission is compact. The\nmorphology of these two lines cannot be reproduced with a constant luminosity\nmodel based on the present-day internal luminosity (0.08 L$_{sun}$). However,\nthe N$_2$H$^+$ peaks are consistent with a constant-luminosity model of 12\nL$_{sun}$. Using a model with time-dependent temperature and density profiles,\nwe show that the observed N$_2$H$^+$ peak emission could indeed be caused by a\npast accretion burst. Such a burst should have occurred a couple of hundred\nyears ago. Conclusions. We suggest that an accretion burst occurred in IRAM\n04191+1522 in the recent past. If such bursts are common and sufficiently long\nin VeLLOs, they could lead to higher accretion onto the central object than\ntheir luminosity suggests. For IRAM 04191 in particular, our results yield an\nestimated final mass of 0.2 - 0.25 M$_{sun}$ by the end of the Class 0 phase,\nwhich would make this object a low-mass star rather than a brown dwarf.", "cat": "astro-ph.SR", "authors": ["S. Anderl", "S. Maret", "S. Cabrit", "A. J. Maury", "A. Belloche", "Ph. Andr\u00e9", "A. Bacmann", "C. Codella", "L. Podio", "F. Gueth"]}, "744": {"id": "2310.00010v1", "title": "Artificial Empathy Classification: A Survey of Deep Learning Techniques, Datasets, and Evaluation Scales", "url": "http://arxiv.org/pdf/2310.00010v1", "date": "2023-09-04 16:02:59", "abs": "From the last decade, researchers in the field of machine learning (ML) and\nassistive developmental robotics (ADR) have taken an interest in artificial\nempathy (AE) as a possible future paradigm for human-robot interaction (HRI).\nHumans learn empathy since birth, therefore, it is challenging to instill this\nsense in robots and intelligent machines. Nevertheless, by training over a vast\namount of data and time, imitating empathy, to a certain extent, can be\npossible for robots. Training techniques for AE, along with findings from the\nfield of empathetic AI research, are ever-evolving. The standard workflow for\nartificial empathy consists of three stages: 1) Emotion Recognition (ER) using\nthe retrieved features from video or textual data, 2) analyzing the perceived\nemotion or degree of empathy to choose the best course of action, and 3)\ncarrying out a response action. Recent studies that show AE being used with\nvirtual agents or robots often include Deep Learning (DL) techniques. For\ninstance, models like VGGFace are used to conduct ER. Semi-supervised models\nlike Autoencoders generate the corresponding emotional states and behavioral\nresponses. However, there has not been any study that presents an independent\napproach for evaluating AE, or the degree to which a reaction was empathetic.\nThis paper aims to investigate and evaluate existing works for measuring and\nevaluating empathy, as well as the datasets that have been collected and used\nso far. Our goal is to highlight and facilitate the use of state-of-the-art\nmethods in the area of AE by comparing their performance. This will aid\nresearchers in the area of AE in selecting their approaches with precision.", "cat": "cs.RO", "authors": ["Sharjeel Tahir", "Syed Afaq Shah", "Jumana Abu-Khalaf"]}, "745": {"id": "2204.12731v1", "title": "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from their SiO Knots", "url": "http://arxiv.org/pdf/2204.12731v1", "date": "2022-04-27 06:58:40", "abs": "We have selected six sources (G209.55-19.68S2, G205.46-14.56S1$_{-}$A,\nG203.21-11.20W2, G191.90-11.21S, G205.46-14.56S3, and G206.93-16.61W2) from the\nAtacama Large Millimeter/submillimeter Array Survey of Orion Planck Galactic\nCold Clumps (ALMASOP), in which these sources have been mapped in the CO\n(J=2-1), SiO (J=5-4), and C$^{18}$O (J=2-1) lines. These sources have\nhigh-velocity SiO jets surrounded by low-velocity CO outflows. The SiO jets\nconsist of a chain of knots. These knots have been thought to be produced by\nsemi-periodical variations in jet velocity. Therefore, we adopt a shock-forming\nmodel, which uses such variations to estimate the inclination angle and\nvelocity of the jets. We also derive the inclination angle of the CO outflows\nusing the wide-angle wind-driven shell model, and find it to be broadly\nconsistent with that of the associated SiO jets. In addition, we apply this\nshock-forming model to another three protostellar sources with SiO jets in the\nliterature -- HH 211, HH 212, and L1448C(N) -- and find that their inclination\nangle and jet velocity are consistent with those previously estimated from\nproper motion and radial velocity studies.", "cat": "astro-ph.GA", "authors": ["Kai-Syun Jhan", "Chin-Fei Lee", "Doug Johnstone", "Tie Liu", "Sheng-Yuan Liu", "Naomi Hirano", "Kenichi Tatematsu", "Somnath Dutta", "Anthony Moraghan", "Hsien Shang", "Jeong-Eun Lee", "Shanghuo Li", "Chun-Fan Liu", "Shih-Ying Hsu", "Woojin Kwon", "Dipen Sahu", "Xun-Chuan Liu", "Kee-Tae Kim", "Qiuyi Luo", "Sheng-Li Qin", "Patricio Sanhueza", "Leonardo Bronfman", "Zhang Qizhou", "David Eden", "Alessio Traficante", "Chang Won Lee"]}, "746": {"id": "2401.16386v2", "title": "Continual Learning with Pre-Trained Models: A Survey", "url": "http://arxiv.org/pdf/2401.16386v2", "date": "2024-04-23 10:44:01", "abs": "Nowadays, real-world applications often face streaming data, which requires\nthe learning system to absorb new knowledge as data evolves. Continual Learning\n(CL) aims to achieve this goal and meanwhile overcome the catastrophic\nforgetting of former knowledge when learning new ones. Typical CL methods build\nthe model from scratch to grow with incoming data. However, the advent of the\npre-trained model (PTM) era has sparked immense research interest, particularly\nin leveraging PTMs' robust representational capabilities. This paper presents a\ncomprehensive survey of the latest advancements in PTM-based CL. We categorize\nexisting methodologies into three distinct groups, providing a comparative\nanalysis of their similarities, differences, and respective advantages and\ndisadvantages. Additionally, we offer an empirical study contrasting various\nstate-of-the-art methods to highlight concerns regarding fairness in\ncomparisons. The source code to reproduce these evaluations is available at:\nhttps://github.com/sun-hailong/LAMDA-PILOT", "cat": "cs.LG", "authors": ["Da-Wei Zhou", "Hai-Long Sun", "Jingyi Ning", "Han-Jia Ye", "De-Chuan Zhan"]}, "747": {"id": "1201.2896v1", "title": "The Future of X-ray Time Domain Surveys", "url": "http://arxiv.org/pdf/1201.2896v1", "date": "2012-01-13 17:06:53", "abs": "Modern X-ray observatories yield unique insight into the astrophysical time\ndomain. Each X-ray photon can be assigned an arrival time, an energy and a sky\nposition, yielding sensitive, energy-dependent light curves and enabling\ntime-resolved spectra down to millisecond time-scales. Combining those with\nmultiple views of the same patch of sky (e.g., in the Chandra and XMM-Newton\ndeep fields) so as to extend variability studies over longer baselines, the\nspectral timing capacity of X-ray observatories then stretch over 10 orders of\nmagnitude at spatial resolutions of arcseconds, and 13 orders of magnitude at\nspatial resolutions of a degree. A wealth of high-energy time-domain data\nalready exists, and indicates variability on timescales ranging from\nmicroseconds to years in a wide variety of objects, including numerous classes\nof AGN, high-energy phenomena at the Galactic centre, Galactic and\nextra-Galactic X-ray binaries, supernovae, gamma-ray bursts, stellar flares,\ntidal disruption flares, and as-yet unknown X-ray variables. This workshop\nexplored the potential of strategic X-ray surveys to probe a broad range of\nastrophysical sources and phenomena. Here we present the highlights, with an\nemphasis on the science topics and mission designs that will drive future\ndiscovery in the X-ray time domain.", "cat": "astro-ph.HE", "authors": ["Daryl Haggard", "Gregory R. Sivakoff"]}, "748": {"id": "2110.10477v1", "title": "The Gaia-ESO Survey: Membership probabilities for stars in 63 open and 7 globular clusters from 3D kinematics", "url": "http://arxiv.org/pdf/2110.10477v1", "date": "2021-10-20 10:31:44", "abs": "Spectroscopy from the final internal data release of the Gaia-ESO Survey\n(GES) has been combined with Gaia EDR3 to assign membership probabilities to\ntargets observed towards 63 Galactic open clusters and 7 globular clusters. The\nmembership probabilities are based chiefly on maximum likelihood modelling of\nthe 3D kinematics of the targets, separating them into cluster and field\npopulations. From 43211 observed targets, 13985 are identified as highly\nprobable cluster members ($P>0.9$), with an average membership probability of\n0.993. The addition of GES radial velocities successfully drives down the\nfraction of false positives and we achieve better levels of discrimination in\nmost clusters over the use of astrometric data alone, especially those at\nlarger distances. Since the membership selection is almost purely kinematic,\nthe union of this catalogue with GES and Gaia is ideal for investigating the\nphotometric and chemical properties of clusters as a function of stellar mass,\nage and Galactic position.", "cat": "astro-ph.SR", "authors": ["R. J. Jackson", "R. D. Jeffries", "N. J. Wright", "S. Randich", "G. Sacco", "A. Bragaglia", "A. Hourihane", "E. Tognelli", "S. Degl'Innocenti", "P. G. Prada Moroni", "G. Gilmore", "T. Bensby", "E. Pancino", "R. Smiljanic", "M. Bergemann", "G. Carraro", "E. Franciosini", "A. Gonneau", "P. Jofr\u00e9", "J. Lewis", "L. Magrini", "L. Morbidelli", "L. Prisinzano", "C. Worley", "S. Zaggia", "G. Tautvai\u0161iene", "M. L. Guti\u00e9rrez Albarr\u00e1n", "D. Montes", "F. Jim\u00e9nez-Esteban"]}, "749": {"id": "1709.06182v2", "title": "A Survey of Machine Learning for Big Code and Naturalness", "url": "http://arxiv.org/pdf/1709.06182v2", "date": "2018-05-05 02:38:45", "abs": "Research at the intersection of machine learning, programming languages, and\nsoftware engineering has recently taken important steps in proposing learnable\nprobabilistic models of source code that exploit code's abundance of patterns.\nIn this article, we survey this work. We contrast programming languages against\nnatural languages and discuss how these similarities and differences drive the\ndesign of probabilistic models. We present a taxonomy based on the underlying\ndesign principles of each model and use it to navigate the literature. Then, we\nreview how researchers have adapted these models to application areas and\ndiscuss cross-cutting and application-specific challenges and opportunities.", "cat": "cs.SE", "authors": ["Miltiadis Allamanis", "Earl T. Barr", "Premkumar Devanbu", "Charles Sutton"]}, "750": {"id": "1504.02053v1", "title": "OMEGA -- OSIRIS Mapping of Emission-line Galaxies in A901/2: I.-- Survey description, data analysis, and star formation and AGN activity in the highest density regions", "url": "http://arxiv.org/pdf/1504.02053v1", "date": "2015-04-08 17:51:56", "abs": "We present an overview of and first results from the OMEGA survey: the OSIRIS\nMapping of Emission-line Galaxies in the multi-cluster system A901/2. The\nultimate goal of this project is to study star formation and AGN activity\nacross a broad range of environments at a single redshift. Using the\ntuneable-filter mode of the OSIRIS instrument on GTC, we target Halpha and\n[NII] emission lines over a ~0.5 X 0.5 deg2 region containing the z~0.167\nmulti-cluster system A901/2. In this paper we describe the design of the\nsurvey, the observations and the data analysis techniques developed. We then\npresent early results from two OSIRIS pointings centred on the cores of the\nA901a and A902 clusters. AGN and star-forming (SF) objects are identified using\nthe [NII]/Halpha vs. W_Halpha (WHAN) diagnostic diagram. The AGN hosts are\nbrighter, more massive, and possess earlier-type morphologies than SF galaxies.\nBoth populations tend to be located towards the outskirts of the high density\nregions we study. The typical Halpha luminosity of these sources is\nsignificantly lower than that of field galaxies at similar redshifts, but\ngreater than that found for A1689, a rich cluster at z~0.2. The Halpha\nluminosities of our objects translate into star-formation rates (SFRs) between\n~0.02 and 6 Msun/yr. Comparing the relationship between stellar mass and\nHalpha-derived SFR with that found in the field indicates a suppression of star\nformation in the cores of the clusters. These findings agree with previous\ninvestigations of this multi-cluster structure, based on other star formation\nindicators, and demonstrate the power of tuneable filters for this kind of\nstudy.", "cat": "astro-ph.GA", "authors": ["Ana L. Chies-Santos", "Bruno Rodr\u00edguez del Pino", "Alfonso Arag\u00f3n-Salamanca", "Steven P. Bamford", "Meghan E. Gray", "Christian Wolf", "Asmus B\u00f6hm", "David T. Maltby", "Irene Pintos-Castro", "Miguel S\u00e1nchez-Portal", "Tim Weinzirl"]}, "751": {"id": "1709.04165v2", "title": "The kinematic dipole in galaxy redshift surveys", "url": "http://arxiv.org/pdf/1709.04165v2", "date": "2017-12-11 11:13:36", "abs": "In the concordance model of the Universe, the matter distribution - as\nobserved in galaxy number counts or the intensity of line emission (such as the\n21cm line of neutral hydrogen) - should have a kinematic dipole due to the\nSun's motion relative to the CMB rest-frame. This dipole should be aligned with\nthe kinematic dipole in the CMB temperature. Accurate measurement of the\ndirection of the matter dipole will become possible with future galaxy surveys,\nand this will be a critical test of the foundations of the concordance model.\nThe amplitude of the matter dipole is also a potential cosmological probe. We\nderive formulas for the amplitude of the kinematic dipole in galaxy redshift\nand intensity mapping surveys, taking into account the Doppler, aberration and\nother relativistic effects. The amplitude of the matter dipole can be\nsignificantly larger than that of the CMB dipole. Its redshift dependence\nencodes information on the evolution of the Universe and on the tracers, and we\ndiscuss possible ways to determine the amplitude.", "cat": "astro-ph.CO", "authors": ["Roy Maartens", "Chris Clarkson", "Song Chen"]}, "752": {"id": "2109.00486v3", "title": "Survey of Low-Resource Machine Translation", "url": "http://arxiv.org/pdf/2109.00486v3", "date": "2022-02-07 15:50:14", "abs": "We present a survey covering the state of the art in low-resource machine\ntranslation research. There are currently around 7000 languages spoken in the\nworld and almost all language pairs lack significant resources for training\nmachine translation models. There has been increasing interest in research\naddressing the challenge of producing useful translation models when very\nlittle translated training data is available. We present a summary of this\ntopical research field and provide a description of the techniques evaluated by\nresearchers in several recent shared tasks in low-resource MT.", "cat": "cs.CL", "authors": ["Barry Haddow", "Rachel Bawden", "Antonio Valerio Miceli Barone", "Jind\u0159ich Helcl", "Alexandra Birch"]}, "753": {"id": "2112.09715v2", "title": "Reconciling the Results of the z~2 MOSDEF and KBSS-MOSFIRE Surveys", "url": "http://arxiv.org/pdf/2112.09715v2", "date": "2022-06-09 06:24:08", "abs": "The combination of the MOSDEF and KBSS-MOSFIRE surveys represents the largest\njoint investment of Keck/MOSFIRE time to date, with ~3000 galaxies at\n1.4<=z<=3.8, roughly half of which are at z~2. MOSDEF is photometric- and\nspectroscopic-redshift selected with a rest-optical magnitude limit, while\nKBSS-MOSFIRE is primarily selected based on rest-UV colors and a rest-UV\nmagnitude limit. Analyzing both surveys in a uniform manner with consistent\nspectral-energy-distribution (SED) models, we find that the MOSDEF z~2 targeted\nsample has a higher median M_* and redder rest U-V color than the KBSS-MOSFIRE\nz~2 targeted sample, and a smaller median SED-based SFR and sSFR (SFR(SED) and\nsSFR(SED)). Specifically, MOSDEF targeted a larger population of red galaxies\nwith U-V and V-J >=1.25, while KBSS-MOSFIRE contains more young galaxies with\nintense star formation. Despite these differences in the z~2 targeted samples,\nthe subsets of the surveys with multiple emission lines detected and analyzed\nin previously published work are much more similar. All median host-galaxy\nproperties with the exception of stellar population age -- i.e., M_*, SFR(SED),\nsSFR(SED), A_V, and UVJ colors -- agree within the uncertainties. Additionally,\nwhen uniform emission-line fitting and stellar Balmer absorption correction\ntechniques are applied, there is no significant offset between the two samples\nin the [OIII]$\\lambda$5008/H$\\beta$ vs. [NII]$\\lambda$6585/H$\\alpha$ diagnostic\ndiagram, in contrast to previously-reported discrepancies. We can now combine\nthe MOSDEF and KBSS-MOSFIRE surveys to form the largest z~2 sample with\nmoderate-resolution rest-optical spectra and construct the fundamental scaling\nrelations of star-forming galaxies during this important epoch.", "cat": "astro-ph.GA", "authors": ["Jordan N. Runco", "Naveen A. Reddy", "Alice E. Shapley", "Charles C. Steidel", "Ryan L. Sanders", "Allison L. Strom", "Alison L. Coil", "Mariska Kriek", "Bahram Mobasher", "Max Pettini", "Gwen C. Rudie", "Brian Siana", "Michael W. Topping", "Ryan F. Trainor", "William R. Freeman", "Irene Shivaei", "Mojegan Azadi", "Sedona H. Price", "Gene C. K. Leung", "Tara Fetherolf", "Laura de Groot", "Tom Zick", "Francesca M. Fornasini", "Guillermo Barro"]}, "754": {"id": "2205.05173v5", "title": "Self-Supervised Anomaly Detection in Computer Vision and Beyond: A Survey and Outlook", "url": "http://arxiv.org/pdf/2205.05173v5", "date": "2024-01-23 06:25:31", "abs": "Anomaly detection (AD) plays a crucial role in various domains, including\ncybersecurity, finance, and healthcare, by identifying patterns or events that\ndeviate from normal behaviour. In recent years, significant progress has been\nmade in this field due to the remarkable growth of deep learning models.\nNotably, the advent of self-supervised learning has sparked the development of\nnovel AD algorithms that outperform the existing state-of-the-art approaches by\na considerable margin. This paper aims to provide a comprehensive review of the\ncurrent methodologies in self-supervised anomaly detection. We present\ntechnical details of the standard methods and discuss their strengths and\ndrawbacks. We also compare the performance of these models against each other\nand other state-of-the-art anomaly detection models. Finally, the paper\nconcludes with a discussion of future directions for self-supervised anomaly\ndetection, including the development of more effective and efficient algorithms\nand the integration of these techniques with other related fields, such as\nmulti-modal learning.", "cat": "cs.LG", "authors": ["Hadi Hojjati", "Thi Kieu Khanh Ho", "Narges Armanfard"]}, "755": {"id": "1303.5948v1", "title": "Perfectoid Spaces: A survey", "url": "http://arxiv.org/pdf/1303.5948v1", "date": "2013-03-24 13:42:41", "abs": "This paper, written in relation to the Current Developments in Mathematics\n2012 Conference, discusses the recent papers on perfectoid spaces. Apart from\ngiving an introduction to their content, it includes some open questions, as\nwell as complements to the results of the previous papers.", "cat": "math.AG", "authors": ["Peter Scholze"]}, "756": {"id": "1801.02546v1", "title": "Quality Control in Crowdsourcing: A Survey of Quality Attributes, Assessment Techniques and Assurance Actions", "url": "http://arxiv.org/pdf/1801.02546v1", "date": "2018-01-08 16:42:17", "abs": "Crowdsourcing enables one to leverage on the intelligence and wisdom of\npotentially large groups of individuals toward solving problems. Common\nproblems approached with crowdsourcing are labeling images, translating or\ntranscribing text, providing opinions or ideas, and similar - all tasks that\ncomputers are not good at or where they may even fail altogether. The\nintroduction of humans into computations and/or everyday work, however, also\nposes critical, novel challenges in terms of quality control, as the crowd is\ntypically composed of people with unknown and very diverse abilities, skills,\ninterests, personal objectives and technological resources. This survey studies\nquality in the context of crowdsourcing along several dimensions, so as to\ndefine and characterize it and to understand the current state of the art.\nSpecifically, this survey derives a quality model for crowdsourcing tasks,\nidentifies the methods and techniques that can be used to assess the attributes\nof the model, and the actions and strategies that help prevent and mitigate\nquality problems. An analysis of how these features are supported by the state\nof the art further identifies open issues and informs an outlook on hot future\nresearch directions.", "cat": "cs.HC", "authors": ["Florian Daniel", "Pavel Kucherbaev", "Cinzia Cappiello", "Boualem Benatallah", "Mohammad Allahbakhsh"]}, "757": {"id": "2206.04132v1", "title": "Forecasting AI Progress: Evidence from a Survey of Machine Learning Researchers", "url": "http://arxiv.org/pdf/2206.04132v1", "date": "2022-06-08 19:05:12", "abs": "Advances in artificial intelligence (AI) are shaping modern life, from\ntransportation, health care, science, finance, to national defense. Forecasts\nof AI development could help improve policy- and decision-making. We report the\nresults from a large survey of AI and machine learning (ML) researchers on\ntheir beliefs about progress in AI. The survey, fielded in late 2019, elicited\nforecasts for near-term AI development milestones and high- or human-level\nmachine intelligence, defined as when machines are able to accomplish every or\nalmost every task humans are able to do currently. As part of this study, we\nre-contacted respondents from a highly-cited study by Grace et al. (2018), in\nwhich AI/ML researchers gave forecasts about high-level machine intelligence\nand near-term milestones in AI development. Results from our 2019 survey show\nthat, in aggregate, AI/ML researchers surveyed placed a 50% likelihood of\nhuman-level machine intelligence being achieved by 2060. The results show\nresearchers newly contacted in 2019 expressed similar beliefs about the\nprogress of advanced AI as respondents in the Grace et al. (2018) survey. For\nthe recontacted participants from the Grace et al. (2018) study, the aggregate\nforecast for a 50% likelihood of high-level machine intelligence shifted from\n2062 to 2076, although this change is not statistically significant, likely due\nto the small size of our panel sample. Forecasts of several near-term AI\nmilestones have reduced in time, suggesting more optimism about AI progress.\nFinally, AI/ML researchers also exhibited significant optimism about how\nhuman-level machine intelligence will impact society.", "cat": "cs.CY", "authors": ["Baobao Zhang", "Noemi Dreksler", "Markus Anderljung", "Lauren Kahn", "Charlie Giattino", "Allan Dafoe", "Michael C. Horowitz"]}, "758": {"id": "1806.10140v1", "title": "The Stripe 82 1-2 GHz Very Large Array Snapshot Survey: Multiwavelength Counterparts", "url": "http://arxiv.org/pdf/1806.10140v1", "date": "2018-06-26 18:00:01", "abs": "We have combined spectrosopic and photometric data from the Sloan Digital Sky\nSurvey (SDSS) with $1.4$ GHz radio observations, conducted as part of the\nStripe 82 $1-2$ GHz Snapshot Survey using the Karl G. Jansky Very Large Array\n(VLA), which covers $\\sim100$ sq degrees, to a flux limit of 88 $\\mu$Jy rms.\nCross-matching the $11\\,768$ radio source components with optical data via\nvisual inspection results in a final sample of $4\\,795$ cross-matched objects,\nof which $1\\,996$ have spectroscopic redshifts and $2\\,799$ objects have\nphotometric redshifts. Three previously undiscovered Giant Radio Galaxies\n(GRGs) were found during the cross-matching process, which would have been\nmissed using automated techniques. For the objects with spectroscopy we\nseparate radio-loud Active Galactic Nuclei (AGN) and star-forming galaxies\n(SFGs) using three diagnostics and then further divide our radio-loud AGN into\nthe HERG and LERG populations. A control matched sample of HERGs and LERGs,\nmatched on stellar mass, redshift and radio luminosity, reveals that the host\ngalaxies of LERGs are redder and more concentrated than HERGs. By combining\nwith near-infrared data, we demonstrate that LERGs also follow a tight $K-z$\nrelationship. These results imply the LERG population are hosted by population\nof massive, passively evolving early-type galaxies. We go on to show that\nHERGs, LERGs, QSOs and star-forming galaxies in our sample all reside in\ndifferent regions of a WISE colour-colour diagram. This cross-matched sample\nbridges the gap between previous `wide but shallow' and `deep but narrow'\nsamples and will be useful for a number of future investigations.", "cat": "astro-ph.GA", "authors": ["Matthew Prescott", "I. H. Whittam", "M. J. Jarvis", "K. McAlpine", "L. L. Richter", "S. Fine", "T. Mauch", "I. Heywood", "M. Vaccari"]}, "759": {"id": "1901.03450v2", "title": "Ubiquitous Acoustic Sensing on Commodity IoT Devices: A Survey", "url": "http://arxiv.org/pdf/1901.03450v2", "date": "2021-08-12 04:30:13", "abs": "With the proliferation of Internet-of-Things devices, acoustic sensing\nattracts much attention in recent years. It exploits acoustic transceivers such\nas microphones and speakers beyond their primary functions, namely recording\nand playing, to enable novel applications and new user experiences. In this\npaper, we present the first systematic survey of recent advances in active\nacoustic sensing using commodity hardware with a frequency range below\n24~\\!kHz. We propose a general framework that categorizes main building blocks\nof acoustic sensing systems. This framework encompasses three layers, i.e.,\nphysical layer, core technique layer, and application layer. The physical layer\nincludes basic hardware components, acoustic platforms as well as the air-borne\nand structure-borne channel characteristics. The core technique layer\nencompasses key mechanisms to generate acoustic signals (waveforms) and to\nextract useful temporal, spatial and spectral information from received\nsignals. The application layer builds upon the functions offered by the core\ntechniques to realize different acoustic sensing applications. We highlight\nunique challenges due to the limitations of physical devices and acoustic\nchannels and how they are mitigated or overcame by core processing techniques\nand application-specific solutions. Finally, research opportunities and future\ndirections are discussed to spawn further in-depth investigation on acoustic\nsensing.", "cat": "cs.SD", "authors": ["Chao Cai", "Rong Zheng", "Jun Luo"]}, "760": {"id": "1502.01296v1", "title": "(Almost) Dark HI Sources in the ALFALFA Survey: The Intriguing Case of HI1232+20", "url": "http://arxiv.org/pdf/1502.01296v1", "date": "2015-02-04 19:22:46", "abs": "We report the discovery and follow-up observations of a system of three\nobjects identified by the ALFALFA extragalactic HI survey, cataloged as\n(almost) dark extragalactic sources, i.e., extragalactic HI detections with no\ndiscernible counterpart in publicly available, wide-field, imaging surveys. We\nhave obtained deep optical imaging with WIYN pODI and HI synthesis maps with\nWSRT of the HI1232+20 system. The source with the highest HI flux has a newly\ndiscovered ultra-low surface brightness (LSB) optical counterpart associated\nwith it, while the other two sources have no detected optical counterparts in\nour images. Our optical observations show that the detected LSB optical\ncounterpart has a peak surface brightness of ~26.4 mag/arcsec^2 in g', which is\nexceptionally faint. This source (AGC 229385) has the largest accurately\nmeasured HI mass-to-light ratio of an isolated object: MHI/Lg'=46 Msun/Lsun,\nand has an HI mass of 7.2*10^8 Msun. The other two HI sources (with HI masses\n2.0*10^8 and 1.2*10^8 Msun) without optical counterparts have upper limit\nsurface brightnesses of 27.9 and 27.8 mag/arcsec^2 in g', and lower limits on\ntheir gas mass-to-light ratio of MHI/Lg'>57 and >31 Msun/Lsun. This system lies\nrelatively close in projection to the Virgo Cluster, but velocity flow models\nindicate that it is located at ~25 Mpc, substantially beyond Virgo. The system\nappears to be quite isolated, with no known object closer than 500 kpc. These\nHI sources may represent both sides of the threshold between \"dark\" star-less\ngalaxies and galaxies with stellar populations. We discuss a variety of\npossible formation scenarios for the HI1232+20 system.", "cat": "astro-ph.GA", "authors": ["Steven Janowiecki", "Lukas Leisman", "Gyula Jozsa", "John J. Salzer", "Martha P. Haynes", "Riccardo Giovanelli", "Katherine L. Rhode", "John M. Cannon", "Elizabeth A. K. Adams", "William F. Janesh"]}, "761": {"id": "2306.07194v1", "title": "The Rapid ASKAP Continuum Survey IV: continuum imaging at 1367.5 MHz and the first data release of RACS-mid", "url": "http://arxiv.org/pdf/2306.07194v1", "date": "2023-06-12 15:50:13", "abs": "The Australian SKA Pathfinder (ASKAP) is being used to undertake a campaign\nto rapidly survey the sky in three frequency bands across its operational\nspectral range. The first pass of the Rapid ASKAP Continuum Survey (RACS) at\n887.5 MHz in the low band has already been completed, with images, visibility\ndatasets, and catalogues made available to the wider astronomical community\nthrough the CSIRO ASKAP Science Data Archive (CASDA). This work presents\ndetails of the second observing pass in the mid band at 1367.5 MHz, RACS-mid,\nand associated data release comprising images and visibility datasets covering\nthe whole sky south of declination $+$49$^\\circ$. This data release\nincorporates selective peeling to reduce artefacts around bright sources, as\nwell as accurately modelled primary beam responses. The Stokes I images reach a\nmedian noise of 198 $\\mu$Jy PSF$^{-1}$ with a declination-dependent angular\nresolution of 8.1 to 47.5 arcsec that fills a niche in the existing ecosystem\nof large-area astronomical surveys. We also supply Stokes V images after\napplication of a widefield leakage correction, with a median noise of 165\n$\\mu$Jy PSF$^{-1}$. We find the residual leakage of Stokes I into V to be\n$\\lesssim$ 0.9 to 2.4 % over the survey. This initial RACS-mid data release\nwill be complemented by a future release comprising catalogues of the survey\nregion. As with other RACS data releases, data products from this release will\nbe made available through CASDA.", "cat": "astro-ph.IM", "authors": ["S. W. Duchesne", "A. J. M. Thomson", "J. Pritchard", "E. Lenc", "V. A. Moss", "D. McConnell", "M. H. Wieringa", "M. T. Whiting", "Z. Wang", "Y. Wang", "K. Rose", "W. Raja", "Tara Murphy", "J. K. Leung", "M. T. Huynh", "A. W. Hotan", "T. Hodgson", "G. H. Heald"]}, "762": {"id": "2402.15231v1", "title": "Which Model to Transfer? A Survey on Transferability Estimation", "url": "http://arxiv.org/pdf/2402.15231v1", "date": "2024-02-23 09:47:27", "abs": "Transfer learning methods endeavor to leverage relevant knowledge from\nexisting source pre-trained models or datasets to solve downstream target\ntasks. With the increase in the scale and quantity of available pre-trained\nmodels nowadays, it becomes critical to assess in advance whether they are\nsuitable for a specific target task. Model transferability estimation is an\nemerging and growing area of interest, aiming to propose a metric to quantify\nthis suitability without training them individually, which is computationally\nprohibitive. Despite extensive recent advances already devoted to this area,\nthey have custom terminological definitions and experimental settings. In this\nsurvey, we present the first review of existing advances in this area and\ncategorize them into two separate realms: source-free model transferability\nestimation and source-dependent model transferability estimation. Each category\nis systematically defined, accompanied by a comprehensive taxonomy. Besides, we\naddress challenges and outline future research directions, intending to provide\na comprehensive guide to aid researchers and practitioners.", "cat": "cs.LG", "authors": ["Yuhe Ding", "Bo Jiang", "Aijing Yu", "Aihua Zheng", "Jian Liang"]}, "763": {"id": "1908.09221v1", "title": "A tale of two test setups: The effect of randomizing a popular conceptual survey in electricity and magnetism", "url": "http://arxiv.org/pdf/1908.09221v1", "date": "2019-08-24 22:10:49", "abs": "We describe a retrospective study of the responses to the Brief Electricity\nand Magnetism Assessment (BEMA) collected from a large population of 3480\nstudents at a large public university. Two different online testing setups were\nemployed for administering the BEMA. Our tale focuses on the interpretation of\nthe data collected from these two testing setups. Our study brings new insight\nand awareness to the effect of the randomization on the BEMA test results.\nStarting from an a priori common sense model, we show simple methods to detect\nand separate guessing from the genuinely thought responses. In addition, we\nshow that the group of responses with low scores (7 or less out of 30) had\ndifferent answer choice strategies than the groups with average or high scores,\nand that the time-in-testing is an essential parameter to be reported. Our\nresults suggest that the data should be cleaned to insure that only valid\ntimes-in-testing are included before reporting and comparing statistics. We\nanalyze in detail the effect of the answer-options randomization and the effect\nof the shuffling of the questions order. Our study did not detect any\nsignificant effect of the option randomization alone on the BEMA scores, for\nvalid times-in-testing. We found clear evidence that shuffling the order of the\nindependent questions does not affect the scores of the BEMA test, while\nshuffling the order of the dependent questions does.", "cat": "physics.ed-ph", "authors": ["Emanuela Ene", "Robert C. Webb"]}, "764": {"id": "1509.06384v2", "title": "The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Effect of smoothing of density field on reconstruction and anisotropic BAO analysis", "url": "http://arxiv.org/pdf/1509.06384v2", "date": "2016-12-08 14:34:57", "abs": "The reconstruction algorithm introduced by \\cite{Eis07}, which is widely used\nin clustering analysis, is based on the inference of the first order Lagrangian\ndisplacement field from the Gaussian smoothed galaxy density field in redshift\nspace. The \\modif2{smoothing scale} applied to the density field affects the\ninferred displacement field that is used to move {the galaxies}, and partially\n\\modif2{erases} the nonlinear evolution {of the density field}.\n In this article, we explore this crucial step \\modif2{in} the reconstruction\nalgorithm. We study the performance of the reconstruction technique using two\nmetrics: first, we study the performance using the anisotropic clustering,\nextending previous studies focused on isotropic clustering; second, we study\nits effect on the displacement field. We find that smoothing has a strong\neffect in the quadrupole of the correlation function and affects the accuracy\nand precision \\modif2{with} which we can measure $D_A (z)$ and $H(z)$. We find\nthat the optimal smoothing scale to use in the reconstruction algorithm applied\nto BOSS-CMASS is between 5-10 $h^{-1}$Mpc. Varying from the \"usual\"\n15$h^{-1}$Mpc to $5 h^{-1}$Mpc \\modif2{shows} $\\sim$ 0.3\\% variations in\n$D_A(z)$ and $\\sim$ 0.4\\% $H(z)$ and uncertainties are also reduced by 40\\% and\n30\\% respectively. We also find that the accuracy of velocity field\nreconstruction depends strongly on the smoothing scale used for the density\nfield. We measure the bias and uncertainties associated with different choices\nof smoothing length.", "cat": "astro-ph.CO", "authors": ["M. Vargas-Maga\u00f1a", "S. Ho", "S. Fromenteau", "A. J. Cuesta"]}, "765": {"id": "1108.0402v1", "title": "The relationship between star formation rates, local density and stellar mass up to z ~ 3 in the GOODS NICMOS Survey", "url": "http://arxiv.org/pdf/1108.0402v1", "date": "2011-08-01 19:39:48", "abs": "We investigate the relation between star formation rates and local galaxy\nenvironment for a stellar mass selected galaxy sample in the redshift range 1.5\n< z < 3. We use near-infra-red imaging from an extremely deep Hubble Space\nTelescope survey, the GOODS-NICMOS Survey (GNS) to measure local galaxy\ndensities based on the nearest neighbour approach, while star-formation rates\nare estimated from rest-frame UV-fluxes. Due to our imaging depth we can\nexamine galaxies down to a colour-independent stellar mass completeness limit\nof log M\\ast = 9.5 M\\odot at z ~ 3. We find a strong dependence of star\nformation activity on galaxy stellar mass over the whole redshift range, which\ndoes not depend on local environment. The average star formation rates are\nlargely independent of local environment apart from in the highest relative\nover-densities. Galaxies in over-densities of a factor of > 5 have on average\nlower star formation rates by a factor of 2 - 3, but only up to redshifts of z\n~ 2. We do not see any evidence for AGN activity influencing these relations.\nWe also investigate the influence of the very local environment on\nstar-formation activity by counting neighbours within 30 kpc radius. This shows\nthat galaxies with two or more close neighbours have on average significantly\nlower star formation rates as well as lower specific star formation rates up to\nz ~ 2.5. We suggest that this might be due to star formation quenching induced\nby galaxy merging processes.", "cat": "astro-ph.CO", "authors": ["R. Gruetzbauch", "C. J. Conselice", "A. E. Bauer", "A. F. L. Bluck", "R. W. Chuter", "F. Buitrago", "A. Mortlock", "T. Weinzirl", "S. Jogee"]}, "766": {"id": "1307.7905v1", "title": "A Population of Teraelectronvolt Pulsar Wind Nebulae in the H.E.S.S. Galactic Plane Survey", "url": "http://arxiv.org/pdf/1307.7905v1", "date": "2013-07-30 11:04:41", "abs": "The most numerous source class that emerged from the H.E.S.S. Galactic Plane\nSurvey are Pulsar Wind Nebulae (PWNe). The 2013 reanalysis of this survey,\nundertaken after almost 10 years of observations, provides us with the most\nsensitive and most complete census of gamma-ray PWNe to date. In addition to a\nuniform analysis of spectral and morphological parameters, for the first time\nalso flux upper limits for energetic young pulsars were extracted from the\ndata. We present a discussion of the correlation between energetic pulsars and\nTeV objects, and their respective properties. We will put the results in\ncontext with the current theoretical understanding of PWNe and evaluate the\nplausibility of previously non-established PWN candidates.", "cat": "astro-ph.HE", "authors": ["S. Klepser", "S. Carrigan", "E. de O\u00f1a Wilhelmi", "C. Deil", "A. F\u00f6rster", "V. Marandon", "M. Mayer", "K. Stycz", "K. Valerius"]}, "767": {"id": "2407.13278v1", "title": "Deep Time Series Models: A Comprehensive Survey and Benchmark", "url": "http://arxiv.org/pdf/2407.13278v1", "date": "2024-07-18 08:31:55", "abs": "Time series, characterized by a sequence of data points arranged in a\ndiscrete-time order, are ubiquitous in real-world applications. Different from\nother modalities, time series present unique challenges due to their complex\nand dynamic nature, including the entanglement of nonlinear patterns and\ntime-variant trends. Analyzing time series data is of great significance in\nreal-world scenarios and has been widely studied over centuries. Recent years\nhave witnessed remarkable breakthroughs in the time series community, with\ntechniques shifting from traditional statistical methods to advanced deep\nlearning models. In this paper, we delve into the design of deep time series\nmodels across various analysis tasks and review the existing literature from\ntwo perspectives: basic modules and model architectures. Further, we develop\nand release Time Series Library (TSLib) as a fair benchmark of deep time series\nmodels for diverse analysis tasks, which implements 24 mainstream models,\ncovers 30 datasets from different domains, and supports five prevalent analysis\ntasks. Based on TSLib, we thoroughly evaluate 12 advanced deep time series\nmodels on different tasks. Empirical results indicate that models with specific\nstructures are well-suited for distinct analytical tasks, which offers insights\nfor research and adoption of deep time series models. Code is available at\nhttps://github.com/thuml/Time-Series-Library.", "cat": "cs.LG", "authors": ["Yuxuan Wang", "Haixu Wu", "Jiaxiang Dong", "Yong Liu", "Mingsheng Long", "Jianmin Wang"]}, "768": {"id": "1010.1147v1", "title": "XML Query Processing and Query Languges: A Survey", "url": "http://arxiv.org/pdf/1010.1147v1", "date": "2010-10-06 13:03:18", "abs": "Today's database is associated with interoperability between different\ndomains and applications. This consequently results in the importance of data\nportability in database. XML format fits the requirements and it has been\nincreasingly used for serving applications across different domains and\npurposes. However, querying XML document effectively and efficiently is still a\nchallenging issue. This paper discusses query processing issues on XML and\nreviews proposed solutions for querying XML databases by various authors.", "cat": "cs.DB", "authors": ["Mikael Fernandus Simalango"]}, "769": {"id": "2009.09075v1", "title": "A Survey on Smart Metering Systems using Blockchain for E-Mobility", "url": "http://arxiv.org/pdf/2009.09075v1", "date": "2020-09-06 22:55:25", "abs": "Electricity is an essential comfort to support our daily activities. With the\ncompetitive increase and energy costs by the industry, new values and\nopportunities for delivering electricity to customers are produced. One of\nthese new opportunities is electric vehicles. With the arrival of electric\nvehicles, various challenges and opportunities are being presented in the\nelectric power system worldwide. For example, under the traditional electric\npower billing scheme, electric power has to be consumed where it is needed so\nthat end-users could not charge their electric vehicles at different points\n(e.g. a relative's house) if this the correct user is not billed (this due to\nthe high consumption of electrical energy that makes it expensive). To achieve\nelectric mobility, they must solve new challenges, such as the smart metering\nof energy consumption and the cybersecurity of these measurements. The present\nwork shows a study of the different smart metering technologies that use\nblockchain and other security mechanisms to achieve e-mobility.", "cat": "cs.CY", "authors": ["Juan C. Olivares-Rojas", "Enrique Reyes-Archundia", "Jos\u00e9 A. Guti\u00e9rrez-Gnecchi", "Ismael Molina-Moreno"]}, "770": {"id": "2206.06373v1", "title": "COSMOS2020: Manifold Learning to Estimate Physical Parameters in Large Galaxy Surveys", "url": "http://arxiv.org/pdf/2206.06373v1", "date": "2022-06-13 18:00:00", "abs": "We present a novel method to estimate galaxy physical properties from\nspectral energy distributions (SEDs), alternate to template fitting techniques\nand based on self-organizing maps (SOM) to learn the high-dimensional manifold\nof a photometric galaxy catalog. The method has been previously tested with\nhydrodynamical simulations in Davidzon et al. (2019) while here is applied to\nreal data for the first time. It is crucial for its implementation to build the\nSOM with a high quality, panchromatic data set, which we elect to be the\n\"COSMOS2020\" galaxy catalog. After the training and calibration steps with\nCOSMOS2020, other galaxies can be processed through SOM to obtain an estimate\nof their stellar mass and star formation rate (SFR). Both quantities result to\nbe in good agreement with independent measurements derived from more extended\nphotometric baseline, and also their combination (i.e., the SFR vs. stellar\nmass diagram) shows a main sequence of star forming galaxies consistent with\nprevious studies. We discuss the advantages of this method compared to\ntraditional SED fitting, highlighting the impact of having, instead of the\nusual synthetic templates, a collection of empirical SEDs built by the SOM in a\n\"data-driven\" way. Such an approach also allows, even for extremely large data\nsets, an efficient visual inspection to identify photometric errors or peculiar\ngalaxy types. Considering in addition the computational speed of this new\nestimator, we argue that it will play a valuable role in the analysis of\noncoming large-area surveys like Euclid or the Legacy Survey of Space and Time\nat the Vera Cooper Rubin Telescope.", "cat": "astro-ph.GA", "authors": ["I. Davidzon", "K. Jegatheesan", "O. Ilbert", "S. de la Torre", "S. K. Leslie", "C. Laigle", "S. Hemmati", "D. C. Masters", "D. Blanquez-Sese", "O. B. Kauffmann", "G. E. Magdis", "K. Ma\u0142ek", "H. J. McCracken", "B. Mobasher", "A. Moneti", "D. B. Sanders", "M. Shuntov", "S. Toft", "J. R. Weaver"]}, "771": {"id": "0809.1394v2", "title": "First Results from the Catalina Real-time Transient Survey", "url": "http://arxiv.org/pdf/0809.1394v2", "date": "2008-09-08 22:28:24", "abs": "We report on the results from the first six months of the Catalina Real-time\nTransient Survey (CRTS). In order to search for optical transients with\ntimescales of minutes to years, the CRTS analyses data from the Catalina Sky\nSurvey which repeatedly covers twenty six thousand of square degrees on the\nsky. The CRTS provides a public stream of transients that are bright enough to\nbe followed up using small telescopes. Since the beginning of the survey, all\nCRTS transients have been made available to astronomers around the world in\nreal-time using HTML tables, RSS feeds and VOEvents. As part of our public\noutreach program the detections are now also available in KML through Google\nSky.\n The initial discoveries include over 350 unique optical transients rising\nmore than two magnitudes from past measurements. Sixty two of these are\nclassified as supernovae, based on light curves, prior deep imaging and\nspectroscopic data. Seventy seven are due to cataclysmic variables (only 13\npreviously known), while an additional 100 transients were too infrequently\nsampled to distinguish between faint CVs and SNe. The remaining optical\ntransients include AGN, Blazars, high proper motions stars, highly variable\nstars (such as UV Ceti stars) and transients of an unknown nature. Our results\nsuggest that there is a large population of SNe missed by many current\nsupernova surveys because of selection biases. These objects appear to be\nassociated with faint host galaxies. We also discuss the unexpected discovery\nof white dwarf binary systems through dramatic eclipses.", "cat": "astro-ph", "authors": ["A. J. Drake", "S. G. Djorgovski", "A. Mahabal", "E. Beshore", "S. Larson", "M. J. Graham", "R. Williams", "E. Christensen", "M. Catelan", "A. Boattini", "A. Gibbs", "R. Hill", "R. Kowalski"]}, "772": {"id": "2111.10382v1", "title": "The Dark Energy Survey Supernova Program: Cosmological biases from supernova photometric classification", "url": "http://arxiv.org/pdf/2111.10382v1", "date": "2021-11-19 19:00:01", "abs": "Cosmological analyses of samples of photometrically-identified Type Ia\nsupernovae (SNe Ia) depend on understanding the effects of 'contamination' from\ncore-collapse and peculiar SN Ia events. We employ a rigorous analysis on\nstate-of-the-art simulations of photometrically identified SN Ia samples and\ndetermine cosmological biases due to such 'non-Ia' contamination in the Dark\nEnergy Survey (DES) 5-year SN sample. As part of the analysis, we test on our\nDES simulations the performance of SuperNNova, a photometric SN classifier\nbased on recurrent neural networks. Depending on the choice of non-Ia SN models\nin both the simulated data sample and training sample, contamination ranges\nfrom 0.8-3.5 %, with the efficiency of the classification from 97.7-99.5 %.\nUsing the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and\nits extension 'BEAMS with Bias Correction' (BBC), we produce a redshift-binned\nHubble diagram marginalised over contamination and corrected for selection\neffects and we use it to constrain the dark energy equation-of-state, $w$.\nAssuming a flat universe with Gaussian $\\Omega_M$ prior of $0.311\\pm0.010$, we\nshow that biases on $w$ are $<0.008$ when using SuperNNova and accounting for a\nwide range of non-Ia SN models in the simulations. Systematic uncertainties\nassociated with contamination are estimated to be at most $\\sigma_{w,\n\\mathrm{syst}}=0.004$. This compares to an expected statistical uncertainty of\n$\\sigma_{w,\\mathrm{stat}}=0.039$ for the DES-SN sample, thus showing that\ncontamination is not a limiting uncertainty in our analysis. We also measure\nbiases due to contamination on $w_0$ and $w_a$ (assuming a flat universe), and\nfind these to be $<$0.009 in $w_0$ and $<$0.108 in $w_a$, hence 5 to 10 times\nsmaller than the statistical uncertainties expected from the DES-SN sample.", "cat": "astro-ph.CO", "authors": ["M. Vincenzi", "M. Sullivan", "A. M\u00f6ller", "P. Armstrong", "B. A. Bassett", "D. Brout", "D. Carollo", "A. Carr", "T. M. Davis", "C. Frohmaier", "L. Galbany", "K. Glazebrook", "O. Graur", "L. Kelsey", "R. Kessler", "E. Kovacs", "G. F. Lewis", "C. Lidman", "U. Malik", "R. C. Nichol", "B. Popovic", "M. Sako", "D. Scolnic", "M. Smith", "G. Taylor", "B. E. Tucker", "P. Wiseman", "M. Aguena", "S. Allam", "J. Annis", "J. Asorey", "D. Bacon", "E. Bertin", "D. Brooks", "D. L. Burke", "A. Carnero Rosell", "J. Carretero", "F. J. Castander", "M. Costanzi", "L. N. da Costa", "M. E. S. Pereira", "J. De Vicente", "S. Desai", "H. T. Diehl", "P. Doel", "S. Everett", "I. Ferrero", "B. Flaugher", "P. Fosalba", "J. Frieman", "J. Garc\u00eda-Bellido", "D. W. Gerdes", "D. Gruen", "G. Gutierrez", "S. R. Hinton", "D. L. Hollowood", "K. Honscheid", "D. J. James", "K. Kuehn", "N. Kuropatkin", "O. Lahav", "T. S. Li", "M. Lima", "M. A. G. Maia", "J. L. Marshall", "R. Miquel", "R. Morgan", "R. L. C. Ogando", "A. Palmese", "F. Paz-Chinch\u00f3n", "A. Pieres", "A. A. Plazas Malag\u00f3n", "K. Reil", "A. Roodman", "E. Sanchez", "M. Schubnell", "S. Serrano", "I. Sevilla-Noarbe", "E. Suchyta", "G. Tarle", "C. To", "T. N. Varga", "J. Weller", "R. D. Wilkinson"]}, "773": {"id": "1101.5260v2", "title": "Highlights from the SOAP project survey. What Scientists Think about Open Access Publishing", "url": "http://arxiv.org/pdf/1101.5260v2", "date": "2011-01-28 17:43:01", "abs": "The SOAP (Study of Open Access Publishing) project has run a large-scale\nsurvey of the attitudes of researchers on, and the experiences with, open\naccess publishing. Around forty thousands answers were collected across\ndisciplines and around the world, showing an overwhelming support for the idea\nof open access, while highlighting funding and (perceived) quality as the main\nbarriers to publishing in open access journals. This article serves as an\nintroduction to the survey and presents this and other highlights from a\npreliminary analysis of the survey responses. To allow a maximal re-use of the\ninformation collected by this survey, the data are hereby released under a CC0\nwaiver, so to allow libraries, publishers, funding agencies and academics to\nfurther analyse risks and opportunities, drivers and barriers, in the\ntransition to open access publishing.", "cat": "cs.DL", "authors": ["Suenje Dallmeier-Tiessen", "Robert Darby", "Bettina Goerner", "Jenni Hyppoelae", "Peter Igo-Kemenes", "Deborah Kahn", "Simon Lambert", "Anja Lengenfelder", "Chris Leonard", "Salvatore Mele", "Malgorzata Nowicka", "Panayiota Polydoratou", "David Ross", "Sergio Ruiz-Perez", "Ralf Schimmer", "Mark Swaisland", "Wim van der Stelt"]}, "774": {"id": "1909.02591v1", "title": "Dust Polarization Toward Embedded Protostars in Ophiuchus with ALMA. III. Survey Overview", "url": "http://arxiv.org/pdf/1909.02591v1", "date": "2019-09-05 18:30:07", "abs": "We present 0.25 arcsec resolution (35 au) ALMA 1.3 mm dust polarization\nobservations for 37 young stellar objects (YSOs) in the Ophiuchus cloud. These\ndata encompass all the embedded protostars in the cloud and several Flat and\nClass II objects to produce the largest, homogeneous study of dust polarization\non disk scales to date. The goal of this study is to study dust polarization\ndown to disk scales. We find that 14/37 (38%) of the YSOs are detected in\npolarization. Nine of these sources have uniform polarization angles and four\nsources have azimuthal polarization. The sources with uniform polarization tend\nto have steeper inclinations (> 60 degree) than those with azimuthal\npolarization (< 60 degree). The majority (9/14) of the detected sources have\npolarization morphologies and disk properties consistent with dust\nself-scattering in optically thick disks. The remaining sources may be instead\ntracing magnetic fields. Their inferred field directions from rotating the\npolarization vectors by 90 degree are mainly poloidal or hourglass shaped. We\nfind no evidence of a strong toroidal field component toward any of our disks.\nFor the 23 YSOs that are undetected in polarization, roughly half of them have\n3-sigma upper limits of < 2%. These sources also tend to have inclinations < 60\ndegree and they are generally compact. Since lower inclination sources tend to\nhave azimuthal polarization, these YSOs may be undetected in polarization due\nto unresolved polarization structure within our beam. We propose that disks\nwith inclinations > 60 degree are the best candidates for future polarization\nstudies of dust self-scattering as these systems will generally show uniform\npolarization vectors that do not require very high resolution to resolve. We\nrelease the continuum and polarization images for all the sources with this\npublication. Data from the entire survey can be obtained from Dataverse.", "cat": "astro-ph.SR", "authors": ["Sarah I. Sadavoy", "Ian W. Stephens", "Philip C. Myers", "Leslie Looney", "John Tobin", "Woojin Kwon", "Benoit Commercon", "Dominique Segura-Cox", "Thomas Henning", "Patrick Hennebelle"]}, "775": {"id": "0710.5012v1", "title": "Comment: Struggles with Survey Weighting and Regression Modeling", "url": "http://arxiv.org/pdf/0710.5012v1", "date": "2007-10-26 07:35:28", "abs": "Comment: Struggles with Survey Weighting and Regression Modeling\n[arXiv:0710.5005]", "cat": "stat.ME", "authors": ["F. Jay Breidt", "Jean D. Opsomer"]}, "776": {"id": "2204.12824v2", "title": "Maritime Communications: A Survey on Enabling Technologies, Opportunities, and Challenges", "url": "http://arxiv.org/pdf/2204.12824v2", "date": "2022-09-14 07:56:42", "abs": "Water covers 71% of the Earth's surface, where the steady increase in oceanic\nactivities has promoted the need for reliable maritime communication\ntechnologies. The existing maritime communication systems involve terrestrial,\naerial, and satellite networks. This paper presents a holistic overview of the\ndifferent forms of maritime communications and provides the latest advances in\nvarious marine technologies. The paper first introduces the different\ntechniques used for maritime communications over the RF and optical bands.\nThen, we present the channel models for RF and optical bands, modulation and\ncoding schemes, coverage and capacity, and radio resource management in\nmaritime communications. After that, the paper presents some emerging use cases\nof maritime networks, such as the Internet of Ships (IoS) and the\nship-to-underwater Internet of things (IoT). Finally, we highlight a few\nexciting open challenges and identify a set of future research directions for\nmaritime communication, including bringing broadband connectivity to the deep\nsea, using THz and visible light signals for on-board applications, and\ndata-driven modeling for radio and optical marine propagation.", "cat": "cs.ET", "authors": ["Fahad S. Alqurashi", "Abderrahmen Trichili", "Nasir Saeed", "Boon S. Ooi", "Mohamed-Slim Alouini"]}, "777": {"id": "2106.12135v1", "title": "Deep Gaussian Processes: A Survey", "url": "http://arxiv.org/pdf/2106.12135v1", "date": "2021-06-21 13:59:47", "abs": "Gaussian processes are one of the dominant approaches in Bayesian learning.\nAlthough the approach has been applied to numerous problems with great success,\nit has a few fundamental limitations. Multiple methods in literature have\naddressed these limitations. However, there has not been a comprehensive survey\nof the topics as of yet. Most existing surveys focus on only one particular\nvariant of Gaussian processes and their derivatives. This survey details the\ncore motivations for using Gaussian processes, their mathematical formulations,\nlimitations, and research themes that have flourished over the years to address\nsaid limitations. Furthermore, one particular research area is Deep Gaussian\nProcesses (DGPs), it has improved substantially in the past decade. The\nsignificant publications that advanced the forefront of this research area are\noutlined in their survey. Finally, a brief discussion on open problems and\nresearch directions for future work is presented at the end.", "cat": "cs.LG", "authors": ["Kalvik Jakkala"]}, "778": {"id": "2401.15607v1", "title": "Survey of Distributed Algorithms for Resource Allocation over Multi-Agent Systems", "url": "http://arxiv.org/pdf/2401.15607v1", "date": "2024-01-28 09:17:36", "abs": "Resource allocation and scheduling in multi-agent systems present challenges\ndue to complex interactions and decentralization. This survey paper provides a\ncomprehensive analysis of distributed algorithms for addressing the distributed\nresource allocation (DRA) problem over multi-agent systems. It covers a\nsignificant area of research at the intersection of optimization, multi-agent\nsystems, and distributed consensus-based computing. The paper begins by\npresenting a mathematical formulation of the DRA problem, establishing a solid\nfoundation for further exploration. Real-world applications of DRA in various\ndomains are examined to underscore the importance of efficient resource\nallocation, and relevant distributed optimization formulations are presented.\nThe survey then delves into existing solutions for DRA, encompassing linear,\nnonlinear, primal-based, and dual-formulation-based approaches. Furthermore,\nthis paper evaluates the features and properties of DRA algorithms, addressing\nkey aspects such as feasibility, convergence rate, and network reliability. The\nanalysis of mathematical foundations, diverse applications, existing solutions,\nand algorithmic properties contributes to a broader comprehension of the\nchallenges and potential solutions for this domain.", "cat": "eess.SY", "authors": ["Mohammadreza Doostmohammadian", "Alireza Aghasi", "Mohammad Pirani", "Ehsan Nekouei", "Houman Zarrabi", "Reza Keypour", "Apostolos I. Rikos", "Karl H. Johansson"]}, "779": {"id": "1211.1386v1", "title": "SNe Ia host galaxy properties from Sloan Digital Sky Survey-II spectroscopy", "url": "http://arxiv.org/pdf/1211.1386v1", "date": "2012-11-06 21:00:04", "abs": "We study the stellar populations of SNe Ia host galaxies using SDSS-II\nspectroscopy. We focus on the relationships of SNe Ia properties with stellar\nvelocity dispersion and the stellar population parameters age, metallicity and\nelement abundance ratios derived by fitting absorption line indices to stellar\npopulation models. We concentrate on a sub-sample of 84 SNe Ia from the SDSS-II\nSupernova Survey. In agreement with previous findings, we find that SALT2\nstretch factor values show the strongest dependence on stellar population age.\nHence, SNe Ia peak-luminosity is closely related to the age of the stellar\nprogenitor systems, where more luminous SNe Ia appear in younger stellar\npopulations. We find no statistically significant trends in the Hubble residual\nwith any of the stellar population parameters studied, including age and\nmetallicity contrary to the literature, as well as with stellar velocity\ndispersion. Moreover, we find that the method of stellar mass derivation is\naffecting the Hubble residual-mass relationship when lower number statistics\nare used. We extend the sample to also include SNe Ia with available SDSS host\ngalaxy photometry only. For this larger sample (247 objects) the reported\nHubble residual-mass relation is strongly dependent on the stellar mass range\nstudied and behaves as a step function. In the high mass regime, probed by our\nhost spectroscopy sample, the relation between Hubble residual and stellar mass\nis flat. Below a stellar mass of ~2x10^10 Msun, i.e. close to the evolutionary\ntransition mass of low-redshift galaxies reported in the literature, the trend\nchanges dramatically such that lower mass galaxies possess lower luminosity SNe\nIa after light-curve corrections. This non-linear behaviour of the Hubble\nresidual-mass relationship should be accounted for when using stellar mass as a\nfurther parameter for minimising the Hubble residuals.", "cat": "astro-ph.CO", "authors": ["Jonas Johansson", "Daniel Thomas", "Janine Pforr", "Claudia Maraston", "Robert C. Nichol", "Mathew Smith", "Hubert Lampeitl", "Alessandra Beifiori", "Ravi R. Gupta", "Donald P. Schneider"]}, "780": {"id": "1909.13329v1", "title": "The ALMA-PILS survey: propyne (CH$_3$CCH) in IRAS 16293$-$2422", "url": "http://arxiv.org/pdf/1909.13329v1", "date": "2019-09-29 17:50:17", "abs": "Context. Propyne (CH$_3$CCH) has been detected in a variety of environments,\nfrom Galactic star-forming regions to extragalactic sources. Such molecules are\nexcellent tracers of the physical conditions in star-forming regions.\n Aims. This study explores the emission of CH$_3$CCH in the low-mass\nprotostellar binary, IRAS 16293$-$2422, examining the spatial scales traced by\nthis molecule, as well as its formation and destruction pathways.\n Methods. ALMA observations from the Protostellar Interferometric Line Survey\n(PILS) are used to determine the abundances and excitation temperatures of\nCH$_3$CCH towards both protostars, exploring spatial scales from 70 to 2400 au.\nThe three-phase chemical kinetics model MAGICKAL is also used, to explore the\nchemical reactions of this molecule.\n Results. CH$_3$CCH is detected towards both IRAS 16293A and IRAS 16293B and\nis found to trace the hot corino component around each source in the PILS\ndataset. Eighteen transitions above 3$\\sigma$ are detected, enabling robust\nexcitation temperatures and column densities to be determined in each source.\nIn IRAS 16293A, an excitation temperature of 90 K and a column density of\n7.8$\\times$10$^{15}$ cm$^{-2}$ best fits the spectra. In IRAS 16293B, an\nexcitation temperature of 100 K and 6.8$\\times$10$^{15}$ cm$^{-2}$ best fits\nthe spectra. The chemical modelling finds that in order to reproduce the\nobserved abundances, both gas-phase and grain-surface reactions are needed.\n Conclusions. CH$_3$CCH is a molecule whose brightness and abundance in many\ndifferent regions can be utilised to provide a benchmark of molecular variation\nwith the physical properties of star-forming regions. It is essential when\nmaking such comparisons, that the abundances are determined with a good\nunderstanding of the spatial scale of the emitting region, to ensure that\naccurate abundances are derived.", "cat": "astro-ph.SR", "authors": ["H. Calcutt", "E. R. Willis", "J. K. J\u00f8rgensen", "P. Bjerkeli", "N. F. W. Ligterink", "A. Coutens", "H. S. P. M\u00fcller", "R. T. Garrod", "S. F. Wampfler", "M. N. Drozdovskaya"]}, "781": {"id": "0709.0506v1", "title": "The Mass Of The Coma Cluster From Weak Lensing In The Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/0709.0506v1", "date": "2007-09-04 19:08:10", "abs": "We present a weak lensing analysis of the Coma Cluster using the Sloan\nDigital Sky Survey (SDSS) Data Release Five. Complete imaging of a ~ 200 square\ndegree region is used to measure the tangential shear of this cluster. The\nshear is fit to an NFW model and we find a virial radius of\nr_{200}=1.99_{-0.22}^{+0.21}h^{-1}Mpc which corresponds to a virial mass of\nM_{200}=1.88_{-0.56}^{+0.65}\\times10^{15}h^{-1}M_{\\odot}. We additionally\ncompare our weak lensing measurement to the virial mass derived using dynamical\ntechniques, and find they are in agreement. This is the lowest redshift,\nlargest angle weak lensing measurement of an individual cluster to date.", "cat": "astro-ph", "authors": ["Jeffrey M. Kubo", "Albert Stebbins", "James Annis", "Ian P. Dell'Antonio", "Huan Lin", "Hossein Khiabanian", "Joshua A. Frieman"]}, "782": {"id": "2006.04284v2", "title": "The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: The nature of the faintest dusty star-forming galaxies", "url": "http://arxiv.org/pdf/2006.04284v2", "date": "2020-09-23 00:39:17", "abs": "We present a characterization of the physical properties of a sample of 35\nsecurely-detected, dusty galaxies in the deep ALMA 1.2-mm image obtained as\npart of the ALMA Spectroscopic Survey in the {\\it Hubble} Ultra Deep Field\n(ASPECS) Large Program. This sample is complemented by 26 additional sources\nidentified via an optical/infrared source positional prior. Using their\nwell-characterized spectral energy distributions, we derive median stellar\nmasses and star formation rates (SFR) of $4.8\\times10^{10}~M_\\odot$ and 30\n$M_\\odot$ yr$^{-1}$, and interquartile ranges of\n$(2.4-11.7)\\times10^{10}~M_\\odot$ and $20-50~M_\\odot$ yr$^{-1}$, respectively.\nWe derive a median spectroscopic redshift of 1.8 with an interquartile range\n$1.1-2.6$, significantly lower than submillimeter galaxies detected in\nshallower, wide-field surveys. We find that 59\\%$\\pm$13\\%, 6\\%$\\pm$4\\%, and\n34\\%$\\pm$9\\% of our sources are within, above and below $\\pm0.4$ dex from the\nSFR-stellar mass relation or main-sequence (MS), respectively. The ASPECS\ngalaxies closely follow the SFR-molecular gas mass relation and other\npreviously established scaling relations, confirming a factor of five increase\nof the gas-to-stellar mass ratio from $z=0.5$ to $z=2.5$ and a mild evolution\nof the gas depletion timescales with a typical value of 0.7 Gyr at $z=1-3$.\nASPECS galaxies located significantly below the MS, a poorly exploited\nparameter space, have low gas-to-stellar-mass ratios of $\\sim0.1-0.2$ and long\ndepletion timescales $>1$ Gyr. Galaxies along the MS dominate the cosmic\ndensity of molecular gas at all redshifts. Systems above the main sequence have\nan increasing contribution to the total gas reservoirs from $z<1$ to $z=2.5$,\nwhile the opposite is found for galaxies below the MS.", "cat": "astro-ph.GA", "authors": ["Manuel Aravena", "Leindert Boogaard", "Jorge G\u00f3nzalez-L\u00f3pez", "Roberto Decarli", "Fabian Walter", "Chris L. Carilli", "Ian Smail", "Axel Weiss", "Roberto J. Assef", "Franz Erik Bauer", "Rychard J. Bouwens", "Paulo C. Cortes", "Pierre Cox", "Elisabete da Cunha", "Emanuele Daddi", "Tanio D\u00edaz-Santos", "Hanae Inami", "Rob Ivison", "Mladen Novak", "Gerg\u007f\u00f6 Popping", "Dominik Riechers", "Paul van der Werf", "Jeff Wagg"]}, "783": {"id": "1707.09183v2", "title": "A Survey of Learning in Multiagent Environments: Dealing with Non-Stationarity", "url": "http://arxiv.org/pdf/1707.09183v2", "date": "2019-03-11 20:17:29", "abs": "The key challenge in multiagent learning is learning a best response to the\nbehaviour of other agents, which may be non-stationary: if the other agents\nadapt their strategy as well, the learning target moves. Disparate streams of\nresearch have approached non-stationarity from several angles, which make a\nvariety of implicit assumptions that make it hard to keep an overview of the\nstate of the art and to validate the innovation and significance of new works.\nThis survey presents a coherent overview of work that addresses\nopponent-induced non-stationarity with tools from game theory, reinforcement\nlearning and multi-armed bandits. Further, we reflect on the principle\napproaches how algorithms model and cope with this non-stationarity, arriving\nat a new framework and five categories (in increasing order of sophistication):\nignore, forget, respond to target models, learn models, and theory of mind. A\nwide range of state-of-the-art algorithms is classified into a taxonomy, using\nthese categories and key characteristics of the environment (e.g.,\nobservability) and adaptation behaviour of the opponents (e.g., smooth,\nabrupt). To clarify even further we present illustrative variations of one\ndomain, contrasting the strengths and limitations of each category. Finally, we\ndiscuss in which environments the different approaches yield most merit, and\npoint to promising avenues of future research.", "cat": "cs.MA", "authors": ["Pablo Hernandez-Leal", "Michael Kaisers", "Tim Baarslag", "Enrique Munoz de Cote"]}, "784": {"id": "0802.4190v1", "title": "Bayesian Estimation of Inequalities with Non-Rectangular Censored Survey Data", "url": "http://arxiv.org/pdf/0802.4190v1", "date": "2008-02-28 12:35:02", "abs": "Synthetic indices are used in Economics to measure various aspects of\nmonetary inequalities. These scalar indices take as input the distribution over\na finite population, for example the population of a specific country. In this\narticle we consider the case of the French 2004 Wealth survey. We have at hand\na partial measurement on the distribution of interest consisting of bracketed\nand sometimes missing data, over a subsample of the population of interest. We\npresent in this article the statistical methodology used to obtain point and\ninterval estimates taking into account the various uncertainties. The\ninequality indices being nonlinear in the input distribution, we rely on a\nsimulation based approach where the model for the wealth per household is\nmultivariate. Using the survey data as well as matched auxiliary tax\ndeclarations data, we have at hand a quite intricate non-rectangle\nmultidimensional censoring. For practical issues we use a Bayesian approach.\nInference using Monte-Carlo approximations relies on a Monte-Carlo Markov chain\nalgorithm namely the Gibbs sampler. The quantities interesting to the decision\nmaker are taken to be the various inequality indices for the French population.\nTheir distribution conditional on the data of the subsample are assumed to be\nnormal centered on the design-based estimates with variance computed through\nlinearization and taking into account the sample design and total nonresponse.\nExogeneous selection of the subsample, in particular the nonresponse mechanism,\nis assumed and we condition on the adequate covariates.", "cat": "stat.AP", "authors": ["Eric Gautier"]}, "785": {"id": "1003.4509v1", "title": "A Far-UV Variability Survey of the Globular Cluster M80", "url": "http://arxiv.org/pdf/1003.4509v1", "date": "2010-03-23 20:00:03", "abs": "We have searched for variable sources in the core region of M80, using far\nultra-violet data taken with the Advanced Camera for Surveys on board the\nHubble Space Telescope. We found three sources that exhibit strong signs of\nvariability in our data. Among these is source TDK1, which we believe to be an\nRR Lyrae star that reached maximum brightness during our observations. The\nlight curve shows a >3 mag FUV brightening over the course of ~5 hours, with an\nestimated peak brightness of ~16.7 mag, followed by a decrease to ~20 mag.\nArchival optical data obtained with WFPC2 confirm that TDK1 is variable in all\nwavebands. TDK1's SED is reasonably fit by a star with temperature T(eff)=6700K\nand radius R=4.2R(sun), consistent with the suggestion that it is an RR Lyrae.\nBased on the photometric and variability characteristics of the other two\nvariables, we suggest that TDK2 is likely to be an SX Phoenicis star with ~55\nminutes period, and TDK3 is likely another RR Lyrae. Finally, we briefly\ndiscuss the FUV counterparts to two previously known variables in M80, the\nclassical nova T Sco and the dwarf nova DN1.", "cat": "astro-ph.SR", "authors": ["Grace S Thomson", "Andrea Dieball", "Christian Knigge", "Knox S Long", "David R Zurek"]}, "786": {"id": "1111.6399v1", "title": "A GPU-based survey for millisecond radio transients using ARTEMIS", "url": "http://arxiv.org/pdf/1111.6399v1", "date": "2011-11-28 10:41:22", "abs": "Astrophysical radio transients are excellent probes of extreme physical\nprocesses originating from compact sources within our Galaxy and beyond. Radio\nfrequency signals emitted from these objects provide a means to study the\nintervening medium through which they travel. Next generation radio telescopes\nare designed to explore the vast unexplored parameter space of high time\nresolution astronomy, but require High Performance Computing (HPC) solutions to\nprocess the enormous volumes of data that are produced by these telescopes. We\nhave developed a combined software /hardware solution (code named ARTEMIS) for\nreal-time searches for millisecond radio transients, which uses GPU technology\nto remove interstellar dispersion and detect millisecond radio bursts from\nastronomical sources in real-time. Here we present an introduction to ARTEMIS.\nWe give a brief overview of the software pipeline, then focus specifically on\nthe intricacies of performing incoherent de-dispersion. We present results from\ntwo brute-force algorithms. The first is a GPU based algorithm, designed to\nexploit the L1 cache of the NVIDIA Fermi GPU. Our second algorithm is CPU based\nand exploits the new AVX units in Intel Sandy Bridge CPUs.", "cat": "astro-ph.IM", "authors": ["W. Armour", "A. Karastergiou", "M. Giles", "C. Williams", "A. Magro", "K. Zagkouris", "S. Roberts", "S. Salvini", "F. Dulwich", "B. Mort"]}, "787": {"id": "1901.03407v2", "title": "Deep Learning for Anomaly Detection: A Survey", "url": "http://arxiv.org/pdf/1901.03407v2", "date": "2019-01-23 06:26:15", "abs": "Anomaly detection is an important problem that has been well-studied within\ndiverse research areas and application domains. The aim of this survey is\ntwo-fold, firstly we present a structured and comprehensive overview of\nresearch methods in deep learning-based anomaly detection. Furthermore, we\nreview the adoption of these methods for anomaly across various application\ndomains and assess their effectiveness. We have grouped state-of-the-art\nresearch techniques into different categories based on the underlying\nassumptions and approach adopted. Within each category we outline the basic\nanomaly detection technique, along with its variants and present key\nassumptions, to differentiate between normal and anomalous behavior. For each\ncategory, we present we also present the advantages and limitations and discuss\nthe computational complexity of the techniques in real application domains.\nFinally, we outline open issues in research and challenges faced while adopting\nthese techniques.", "cat": "cs.LG", "authors": ["Raghavendra Chalapathy", "Sanjay Chawla"]}, "788": {"id": "2302.04978v1", "title": "The bulk flow motion and the Hubble-Lema\u00eetre law in the Local Universe with the ALFALFA survey", "url": "http://arxiv.org/pdf/2302.04978v1", "date": "2023-02-09 23:37:46", "abs": "The knowledge of the main features of the bulk flow in the Local Universe is\nimportant for a better determination of the relative motions there, an\ninformation that would contribute to a precise calculation of the\nHubble-Lema\\^{\\i}tre law at very low redshifts. We study how to obtain the\nHubble-Lema\\^{\\i}tre law in two sky regions using the catalog of HI sources of\nthe ALFALFA survey, with data $cz_{\\odot} < 6000$ km/s. Our methodology aims to\ncompute $H_0$ in two regions -- located in opposite galactic hemispheres --\nmapped by the ALFALFA survey, and look for dependence with distance, direction,\nand also test for reference frame changes. We calculate the Hubble constant, in\nthe Cosmic Microwave Background reference frame, in opposite galactic\nhemispheres: $H_0^N = 70.87 \\pm 2.38$ and $H_0^S = 66.07 \\pm 3.02$, which\nallows us to measure the bulk flow velocity $V_{BF} = 401.06 \\pm 150.55$ km/s\nat the effective distance $31.3 \\pm 6.26$ Mpc, a novel result found analysing\nthe ALFALFA data at low redshift. We confirm the influence of the bulk flow on\nthe structures of the Local Universe which manifests through a dipolar behavior\nof the Hubble constant in opposite hemispheres.", "cat": "astro-ph.CO", "authors": ["Felipe Avila", "Jezebel Oliveira", "Mariana L. S. Dias", "Armando Bernui"]}, "789": {"id": "1405.7559v1", "title": "A Herschel PACS survey of brown dwarfs in IC 2391: Limits on primordial and debris disk fractions", "url": "http://arxiv.org/pdf/1405.7559v1", "date": "2014-05-29 14:14:03", "abs": "We present results from a Herschel PACS survey of 8 brown dwarfs in the IC\n2391 cluster. Our aim was to determine the brown dwarf disk fraction at ages of\n~40-50 Myr. None of the 8 brown dwarfs observed were detected in the PACS 70 or\n160mu bands. We have determined the detection limits of our survey using the\n1-sigma flux upper limits in the PACS far-infrared and the WISE mid-infrared\nbands. The sensitivity of our observations would only allow for the detection\nof debris disks with exceptionally large fractional luminosities (>1%).\nConsidering that only the most extreme and rare debris disks have such high\nfractional luminosities, it can be hypothesized that Vega-like debris disks, as\nobserved around ~30% of low-mass stars at similar ages, could exist around the\ntargeted IC 2391 brown dwarfs. Most primordial disks similar to the ones\nobserved for the younger 1-10 Myr brown dwarfs would be within the detection\nsensitivities of our survey, and could have been detected. The non-detection\nfor all targets then suggests that brown dwarf disks have transitioned to the\ndebris phase by ~40-50 Myr ages. We also present the sensitivity limits for\ndetecting brown dwarf disks with future SPICA observations.", "cat": "astro-ph.SR", "authors": ["B. Riaz", "G. M. Kennedy"]}, "790": {"id": "2204.09591v1", "title": "A Survey on Bias and Fairness in Natural Language Processing", "url": "http://arxiv.org/pdf/2204.09591v1", "date": "2022-03-06 18:12:30", "abs": "As NLP models become more integrated with the everyday lives of people, it\nbecomes important to examine the social effect that the usage of these systems\nhas. While these models understand language and have increased accuracy on\ndifficult downstream tasks, there is evidence that these models amplify gender,\nracial and cultural stereotypes and lead to a vicious cycle in many settings.\nIn this survey, we analyze the origins of biases, the definitions of fairness,\nand how different subfields of NLP mitigate bias. We finally discuss how future\nstudies can work towards eradicating pernicious biases from NLP algorithms.", "cat": "cs.CL", "authors": ["Rajas Bansal"]}, "791": {"id": "2009.12950v1", "title": "Human-Object Interaction Detection:A Quick Survey and Examination of Methods", "url": "http://arxiv.org/pdf/2009.12950v1", "date": "2020-09-27 20:58:39", "abs": "Human-object interaction detection is a relatively new task in the world of\ncomputer vision and visual semantic information extraction. With the goal of\nmachines identifying interactions that humans perform on objects, there are\nmany real-world use cases for the research in this field. To our knowledge,\nthis is the first general survey of the state-of-the-art and milestone works in\nthis field. We provide a basic survey of the developments in the field of\nhuman-object interaction detection. Many works in this field use multi-stream\nconvolutional neural network architectures, which combine features from\nmultiple sources in the input image. Most commonly these are the humans and\nobjects in question, as well as the spatial quality of the two. As far as we\nare aware, there have not been in-depth studies performed that look into the\nperformance of each component individually. In order to provide insight to\nfuture researchers, we perform an individualized study that examines the\nperformance of each component of a multi-stream convolutional neural network\narchitecture for human-object interaction detection. Specifically, we examine\nthe HORCNN architecture as it is a foundational work in the field. In addition,\nwe provide an in-depth look at the HICO-DET dataset, a popular benchmark in the\nfield of human-object interaction detection. Code and papers can be found at\nhttps://github.com/SHI-Labs/Human-Object-Interaction-Detection.", "cat": "cs.CV", "authors": ["Trevor Bergstrom", "Humphrey Shi"]}, "792": {"id": "1101.3549v1", "title": "The Sloan Digital Sky Survey DR7 Spectroscopic M Dwarf Catalog II: Statistical Parallax Analysis", "url": "http://arxiv.org/pdf/1101.3549v1", "date": "2011-01-18 21:00:00", "abs": "We present a statistical parallax analysis of low-mass dwarfs from the Sloan\nDigital Sky Survey (SDSS). We calculate absolute r-band magnitudes (M_r) as a\nfunction of color and spectral type, and investigate changes in M_r with\nlocation in the Milky Way. We find that magnetically active M dwarfs are\nintrinsically brighter in M_r than their inactive counterparts at the same\ncolor or spectral type. Metallicity, as traced by the proxy zeta, also affects\nM_r, with metal poor stars having fainter absolute magnitudes than higher\nmetallicity M dwarfs at the same color or spectral type. Additionally, we\nmeasure the velocity ellipsoid and solar reflex motion for each subsample of M\ndwarfs. We find good agreement between our measured solar peculiar motion and\nprevious results for similar populations, as well as some evidence for\ndiffering motions of early and late M type populations in U and W velocities\nthat cannot be attributed to asymmetric drift. The reflex solar motion and the\nvelocity dispersions both show that younger populations, as traced by magnetic\nactivity and location near the Galactic plane, have experienced less dynamical\nheating. We introduce a new parameter, the independent position altitude (IPA),\nto investigate populations as a function of vertical height from the Galactic\nplane. M dwarfs at all types exhibit an increase in velocity dispersion when\nanalyzed in comparable IPA subgroups.", "cat": "astro-ph.SR", "authors": ["John J. Bochanski", "Suzanne L. Hawley", "Andrew A. West"]}, "793": {"id": "1102.1619v1", "title": "The B3-VLA CSS sample. VIII: New optical identifications from the Sloan Digital Sky Survey. The ultraviolet-optical spectral energy distribution of the young radio sources", "url": "http://arxiv.org/pdf/1102.1619v1", "date": "2011-02-08 14:55:14", "abs": "Compact steep-spectrum radio sources and giga-hertz peaked spectrum radio\nsources (CSS/GPS) are generally considered to be mostly young radio sources. In\nrecent years we studied at many wavelengths a sample of these objects selected\nfrom the B3-VLA catalog: the B3-VLA CSS sample. Only ~ 60 % of the sources were\noptically identified. We aim to increase the number of optical identifications\nand study the properties of the host galaxies of young radio sources. We\ncross-correlated the CSS B3-VLA sample with the Sloan Digital Sky Survey\n(SDSS), DR7, and complemented the SDSS photometry with available GALEX (DR 4/5\nand 6) and near-IR data from UKIRT and 2MASS. We obtained new identifications\nand photometric redshifts for eight faint galaxies and for one quasar and two\nquasar candidates. Overall we have 27 galaxies with SDSS photometry in five\nbands, for which we derived the ultraviolet-optical spectral energy\ndistribution (UV-O-SED). We extended our investigation to additional CSS/GPS\nselected from the literature. Most of the galaxies show an excess of\nultra-violet (UV) radiation compared with the UV-O-SED of local radio-quiet\nellipticals. We found a strong dependence of the UV excess on redshift and\nanalyzed it assuming that it is generated either from the nucleus (hidden\nquasar) or from a young stellar population (YSP). We also compare the UV-O-SEDs\nof our CSS/GPS sources with those of a selection of large size (LSO) powerful\nradio sources from the literature. If the major process of the UV excess is\ncaused by a YSP, our conclusion is that it is the result of the merger process\nthat also triggered the onset of the radio source with some time delay. We do\nnot see evidence for a major contribution from a YSP triggered by the radio\nsources itself.", "cat": "astro-ph.CO", "authors": ["C. Fanti", "R. Fanti", "A. Zanichelli", "D. Dallacasa", "C. Stanghellini"]}, "794": {"id": "0910.1994v1", "title": "A survey on Weyl calculus for representations of nilpotent Lie groups", "url": "http://arxiv.org/pdf/0910.1994v1", "date": "2009-10-11 11:10:29", "abs": "We survey some aspects of the pseudo-differential Weyl calculus for\nirreducible unitary representations of nilpotent Lie groups, ranging from the\nclassical ideas to recently obtained results. The classical Weyl-H\\\"ormander\ncalculus is recovered for the Schr\\\"odinger representation of the Heisenberg\ngroup. Our discussion concerns various extensions of this classical situation\nto arbitrary nilpotent Lie groups and to some infinite-dimensional Lie groups\nthat allow us to handle the magnetic pseudo-differential calculus.", "cat": "math.AP", "authors": ["Ingrid Beltita", "Daniel Beltita"]}, "795": {"id": "2409.01743v1", "title": "A survey of equivariant operations on quantum cohomology for symplectic manifolds", "url": "http://arxiv.org/pdf/2409.01743v1", "date": "2024-09-03 09:36:31", "abs": "In this survey paper, we will collate various different ideas and thoughts\nregarding equivariant operations on quantum cohomology (and some in more\ngeneral Floer theory) for a symplectic manifold. We will discuss a general\nnotion of equivariant quantum operations associated to finite groups, in\naddition to their properties, examples, and calculations. We will provide a\nbrief connection to Floer theoretic invariants. We then provide abridged\ndescriptions (as per the author's understanding) of work by other authors in\nthe field, along with their major results. Finally we discuss the first step to\ncompact groups, specifically $S^1$-equivariant operations. Contained within\nthis survey are also a sketch of the idea of mod-$p$ pseudocycles, and an\nin-depth appendix detailing the author's understanding of when one can define\nthese equivariant operations in an additive way.", "cat": "math.SG", "authors": ["Nicholas Wilkins"]}, "796": {"id": "1208.0163v1", "title": "Spatial and Spatio-Temporal Multidimensional Data Modelling: A Survey", "url": "http://arxiv.org/pdf/1208.0163v1", "date": "2012-08-01 10:21:55", "abs": "Data warehouse store and provide access to large volume of historical data\nsupporting the strategic decisions of organisations. Data warehouse is based on\na multidimensional model which allow to express user's needs for supporting the\ndecision making process. Since it is estimated that 80% of data used for\ndecision making has a spatial or location component [1, 2], spatial data have\nbeen widely integrated in Data Warehouses and in OLAP systems. Extending a\nmultidimensional data model by the inclusion of spatial data provides a concise\nand organised spatial datawarehouse representation. This paper aims to provide\na comprehensive review of litterature on developed and suggested spatial and\nspatio-temporel multidimensional models. A benchmarking study of the proposed\nmodels is presented. Several evaluation criterias are used to identify the\nexistence of trends as well as potential needs for further investigations.", "cat": "cs.DB", "authors": ["Saida Aissi", "Mohamed Salah Gouider"]}, "797": {"id": "1401.2274v1", "title": "Discovery of Four Doubly Imaged Quasar Lenses from the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1401.2274v1", "date": "2014-01-10 10:00:23", "abs": "We report the discovery of four doubly imaged quasar lenses. All the four\nsystems are selected as lensed quasar candidates from the Sloan Digital Sky\nSurvey data. We confirm their lensing hypothesis with additional imaging and\nspectroscopic follow-up observations. The discovered lenses are SDSS J0743+2457\nwith the source redshift z_s=2.165, the lens redshift z_l=0.381, and the image\nseparation theta=1.034\", SDSS J1128+2402 with z_s=1.608 and theta=0.844\", SDSS\nJ1405+0959 with z_s=1.810, z_l~0.66, and theta=1.978\", and SDSS J1515+1511 with\nz_s=2.054, z_l=0.742, and theta=1.989\". It is difficult to estimate the lens\nredshift of SDSS J1128+2402 from the current data. Two of the four systems\n(SDSS J1405+0959 and SDSS J1515+1511) are included in our final statistical\nlens sample to derive constraints on dark energy and the evolution of massive\ngalaxies.", "cat": "astro-ph.CO", "authors": ["Naohisa Inada", "Masamune Oguri", "Cristian E. Rusu", "Issha Kayo", "Tomoki Morokuma"]}, "798": {"id": "1706.01246v2", "title": "The Taipan Galaxy Survey: Scientific Goals and Observing Strategy", "url": "http://arxiv.org/pdf/1706.01246v2", "date": "2018-03-19 05:49:58", "abs": "Taipan is a multi-object spectroscopic galaxy survey starting in 2017 that\nwill cover 2pi steradians over the southern sky, and obtain optical spectra for\nabout two million galaxies out to z<0.4. Taipan will use the newly-refurbished\n1.2m UK Schmidt Telescope at Siding Spring Observatory with the new TAIPAN\ninstrument, which includes an innovative 'Starbugs' positioning system capable\nof rapidly and simultaneously deploying up to 150 spectroscopic fibres (and up\nto 300 with a proposed upgrade) over the 6-deg diameter focal plane, and a\npurpose-built spectrograph operating from 370 to 870nm with resolving power\nR>2000. The main scientific goals of Taipan are: (i) to measure the distance\nscale of the Universe (primarily governed by the local expansion rate, H_0) to\n1% precision, and the structure growth rate of structure to 5%; (ii) to make\nthe most extensive map yet constructed of the mass distribution and motions in\nthe local Universe, using peculiar velocities based on improved Fundamental\nPlane distances, which will enable sensitive tests of gravitational physics;\nand (iii) to deliver a legacy sample of low-redshift galaxies as a unique\nlaboratory for studying galaxy evolution as a function of mass and environment.\nThe final survey, which will be completed within 5 years, will consist of a\ncomplete magnitude-limited sample (i<17) of about 1.2x10^6 galaxies,\nsupplemented by an extension to higher redshifts and fainter magnitudes\n(i<18.1) of a luminous red galaxy sample of about 0.8x10^6 galaxies.\nObservations and data processing will be carried out remotely and in a\nfully-automated way, using a purpose-built automated 'virtual observer'\nsoftware and an automated data reduction pipeline. The Taipan survey is\ndeliberately designed to maximise its legacy value, by complementing and\nenhancing current and planned surveys of the southern sky at wavelengths from\nthe optical to the radio.", "cat": "astro-ph.GA", "authors": ["Elisabete da Cunha", "Andrew M. Hopkins", "Matthew Colless", "Edward N. Taylor", "Chris Blake", "Cullan Howlett", "Christina Magoulas", "John R. Lucey", "Claudia Lagos", "Kyler Kuehn", "Yjan Gordon", "Dilyar Barat", "Fuyan Bian", "Christian Wolf", "Michael J. Cowley", "Marc White", "Ixandra Achitouv", "Maciej Bilicki", "Joss Bland-Hawthorn", "Krzysztof Bolejko", "Michael J. I. Brown", "Rebecca Brown", "Julia Bryant", "Scott Croom", "Tamara M. Davis", "Simon P. Driver", "Miroslav D. Filipovic", "Samuel R. Hinton", "Melanie Johnston-Hollitt", "D. Heath Jones", "Baerbel Koribalski", "Dane Kleiner", "Jon Lawrence", "Nuria Lorente", "Jeremy Mould", "Matt S. Owers", "Kevin Pimbblet", "C. G. Tinney", "Nicholas F. H. Tothill", "Fred Watson"]}, "799": {"id": "0802.0149v1", "title": "Spectroscopy of clusters in the ESO distant cluster survey (EDisCS).II. Redshifts, velocity dispersions, and substructure for clusters in the last 15 fields", "url": "http://arxiv.org/pdf/0802.0149v1", "date": "2008-02-01 15:37:33", "abs": "AIMS. We present spectroscopic observations of galaxies in 15 survey fields\nas part of the ESO Distant Cluster Survey (EDisCS). We determine the redshifts\nand velocity dispersions of the galaxy clusters located in these fields, and we\ntest for possible substructure in the clusters.\n METHODS. We obtained multi-object mask spectroscopy using the FORS2\ninstrument at the VLT. We reduced the data with particular attention to the sky\nsubtraction. We implemented the method of Kelson for performing sky subtraction\nprior to any rebinning/interpolation of the data. From the measured galaxy\nredshifts, we determine cluster velocity dispersions using the biweight\nestimator and test for possible substructure in the clusters using the\nDressler-Shectman test.\n RESULTS. The method of subtracting the sky prior to any\nrebinning/interpolation of the data delivers photon-noise-limited results,\nwhereas the traditional method of subtracting the sky after the data have been\nrebinned/interpolated results in substantially larger noise for spectra from\ntilted slits. Redshifts for individual galaxies are presented and redshifts and\nvelocity dispersions are presented for 21 galaxy clusters. For the 9 clusters\nwith at least 20 spectroscopically confirmed members, we present the\nstatistical significance of the presence of substructure obtained from the\nDressler-Shectman test, and substructure is detected in two of the clusters.\n CONCLUSIONS. Together with data from our previous paper, spectroscopy and\nspectroscopic velocity dispersions are now available for 26 EDisCS clusters\nwith redshifts in the range 0.40-0.96 and velocity dispersions in the range\n166-1080 km/s.", "cat": "astro-ph", "authors": ["Bo Milvang-Jensen", "Stefan Noll", "Claire Halliday", "Bianca M. Poggianti", "Pascale Jablonka", "Alfonso Aragon-Salamanca", "Roberto P. Saglia", "Nina Nowak", "Anja von der Linden", "Gabriella De Lucia", "Roser Pello", "John Moustakas", "Sebastien Poirier", "Steven P. Bamford", "Douglas I. Clowe", "Julianne J. Dalcanton", "Gregory H. Rudnick", "Luc Simard", "Simon D. M. White", "Dennis Zaritsky"]}, "800": {"id": "1301.4521v1", "title": "The ACS Nearby Galaxy Survey Treasury XI. The Remarkably Undisturbed NGC 2403 Disk", "url": "http://arxiv.org/pdf/1301.4521v1", "date": "2013-01-18 23:18:35", "abs": "We present detailed analysis of color-magnitude diagrams of NGC2403, obtained\nfrom a deep (m<28) Hubble Space Telescope (HST) Wide Field Planetary Camera 2\nobservation of the outer disk of NGC2403, supplemented by several shallow\n(m<26) HST Advanced Camera for Surveys fields. We derive the spatially resolved\nstar formation history of NGC2403 out to 11 disk scale lengths. In the inner\nportions of the galaxy, we compare the recent star formation rates (SFRs) we\nderive from the resolved stars with those measured using GALEX FUV + Spitzer\n24-micron fluxes, finding excellent agreement between the methods. Our\nmeasurements also show that the radial gradient in recent SFR mirror s the disk\nexponential profile to 11 scale lengths with no break, extending to SFR\ndensities a factor of 100 lower than those that can be measured with GALEX and\nSpitzer (2x10^{-6} M_{\\sun} yr^{-1} kpc^{-2}). Furthermore, we find that the\ncumulative stellar mass of the disk was formed at similar times at all radii.\nWe compare these characteristics of NGC2403 to those of its \"morphological\ntwins,\" NGC300 and M33, showing that the structure and age distributions of the\nNGC2403 disk are more similar to those of the relatively isolated system NGC300\nthan to those of the Local Group analog M33. We also discuss the environments\nand HI morphologies of these three nearby galaxies, comparing them to\nintegrated light studies of larger samples of more distant galaxy disks. Taken\ntogether, the physical properties and evolutionary history of NGC2403 suggest\nthat the galaxy has had no close encounters with other M81 group members and\nmay be falling into the group for the first time.", "cat": "astro-ph.CO", "authors": ["Benjamin F. Williams", "Julianne J. Dalcanton", "Adrienne Stilp", "Andrew Dolphin", "Evan D. Skillman", "David Radburn-Smith"]}, "801": {"id": "2408.02479v1", "title": "From LLMs to LLM-based Agents for Software Engineering: A Survey of Current, Challenges and Future", "url": "http://arxiv.org/pdf/2408.02479v1", "date": "2024-08-05 14:01:15", "abs": "With the rise of large language models (LLMs), researchers are increasingly\nexploring their applications in var ious vertical domains, such as software\nengineering. LLMs have achieved remarkable success in areas including code\ngeneration and vulnerability detection. However, they also exhibit numerous\nlimitations and shortcomings. LLM-based agents, a novel tech nology with the\npotential for Artificial General Intelligence (AGI), combine LLMs as the core\nfor decision-making and action-taking, addressing some of the inherent\nlimitations of LLMs such as lack of autonomy and self-improvement. Despite\nnumerous studies and surveys exploring the possibility of using LLMs in\nsoftware engineering, it lacks a clear distinction between LLMs and LLM based\nagents. It is still in its early stage for a unified standard and benchmarking\nto qualify an LLM solution as an LLM-based agent in its domain. In this survey,\nwe broadly investigate the current practice and solutions for LLMs and\nLLM-based agents for software engineering. In particular we summarise six key\ntopics: requirement engineering, code generation, autonomous decision-making,\nsoftware design, test generation, and software maintenance. We review and\ndifferentiate the work of LLMs and LLM-based agents from these six topics,\nexamining their differences and similarities in tasks, benchmarks, and\nevaluation metrics. Finally, we discuss the models and benchmarks used,\nproviding a comprehensive analysis of their applications and effectiveness in\nsoftware engineering. We anticipate this work will shed some lights on pushing\nthe boundaries of LLM-based agents in software engineering for future research.", "cat": "cs.SE", "authors": ["Haolin Jin", "Linghan Huang", "Haipeng Cai", "Jun Yan", "Bo Li", "Huaming Chen"]}, "802": {"id": "2007.02963v2", "title": "The Sloan Digital Sky Survey Reverberation Mapping Project: Estimating Masses of Black Holes in Quasars with Single-Epoch Spectroscopy", "url": "http://arxiv.org/pdf/2007.02963v2", "date": "2020-09-27 12:38:00", "abs": "It is well known that reverberation mapping of active galactic nuclei (AGN)\nreveals a relationship between AGN luminosity and the size of the broad-line\nregion, and that use of this relationship, combined with the Doppler width of\nthe broad emission line, enables an estimate of the mass of the black hole at\nthe center of the active nucleus based on a single spectrum. An unresolved key\nissue is the choice of parameter used to characterize the line width, either\nFWHM or line dispersion (the square root of the second moment of the line\nprofile). We argue here that use of FWHM introduces a bias, stretching the mass\nscale such that high masses are overestimated and low masses are\nunderestimated. Here we investigate estimation of black hole masses in AGNs\nbased on individual or \"single epoch\" observations, with a particular emphasis\nin comparing mass estimates based on line dispersion and FWHM. We confirm the\nrecent findings that, in addition to luminosity and line width, a third\nparameter is required to obtain accurate masses and that parameter seems to be\nEddington ratio. We present simplified empirical formulae for estimating black\nhole masses from the Hbeta 4861 A and C IV 1549 A emission lines. While the AGN\ncontinuum luminosity at 5100 A is usually used to predict the Hbeta\nreverberation lag, we show that the luminosity of the Hbeta broad component can\nbe used instead without any loss of precision, thus eliminating the difficulty\nof accurately accounting for the host-galaxy contribution to the observed\nluminosity.", "cat": "astro-ph.GA", "authors": ["Elena Dalla Bonta`", "Bradley M. Peterson", "Misty C. Bentz", "W. N. Brandt", "Stefano Ciroi", "Gisella De Rosa", "Gloria Fonseca Alvarez", "Catherine J. Grier", "P. B. Hall", "Juan V. Hernandez Santisteban", "Luis C. Ho", "Y. Homayouni", "Keith Horne", "C. S. Kochanek", "Jennifer I-Hsiu Li", "Lorenzo Morelli", "Alessandro Pizzella", "R. W. Pogge", "D. P. Schneider", "Yue Shen", "J. R. Trump", "Marianne Vestergaard"]}, "803": {"id": "1409.5036v1", "title": "An extensive survey of the estimation of uncertainties from missing higher orders in perturbative calculations", "url": "http://arxiv.org/pdf/1409.5036v1", "date": "2014-09-17 15:43:04", "abs": "We consider two approaches to estimate and characterise the theoretical\nuncertainties stemming from the missing higher orders in perturbative\ncalculations in Quantum Chromodynamics: the traditional one based on\nrenormalisation and factorisation scale variation, and the Bayesian framework\nproposed by Cacciari and Houdeau. We estimate uncertainties with these two\nmethods for a comprehensive set of more than thirty different observables\ncomputed in perturbative Quantum Chromodynamics, and we discuss their\nperformance in properly estimating the size of the higher order terms that are\nknown. We find that scale variation with the conventional choice of varying\nscales within a factor of two of a central scale gives uncertainty intervals\nthat tend to be somewhat too small to be interpretable as 68%\nconfidence-level-heuristic ones. We propose a modified version of the Bayesian\napproach of Cacciari and Houdeau which performs well for non-hadronic\nobservables and, after an appropriate choice of the relevant expansion\nparameter for the perturbative series, for hadronic ones too.", "cat": "hep-ph", "authors": ["Emanuele Bagnaschi", "Matteo Cacciari", "Alberto Guffanti", "Laura Jenniches"]}, "804": {"id": "1704.08531v1", "title": "A Survey of Neural Network Techniques for Feature Extraction from Text", "url": "http://arxiv.org/pdf/1704.08531v1", "date": "2017-04-27 12:27:25", "abs": "This paper aims to catalyze the discussions about text feature extraction\ntechniques using neural network architectures. The research questions discussed\nin the paper focus on the state-of-the-art neural network techniques that have\nproven to be useful tools for language processing, language generation, text\nclassification and other computational linguistics tasks.", "cat": "cs.CL", "authors": ["Vineet John"]}, "805": {"id": "2309.10187v2", "title": "Automated Interviewer or Augmented Survey? Collecting Social Data with Large Language Models", "url": "http://arxiv.org/pdf/2309.10187v2", "date": "2023-10-10 21:45:04", "abs": "Qualitative methods like interviews produce richer data in comparison with\nquantitative surveys, but are difficult to scale. Switching from web-based\nquestionnaires to interactive chatbots offers a compromise, improving user\nengagement and response quality. Uptake remains limited, however, because of\ndifferences in users' expectations versus the capabilities of natural language\nprocessing methods. In this study, we evaluate the potential of large language\nmodels (LLMs) to support an information elicitation chatbot that narrows this\n\"gulf of expectations\" (Luger & Sellen 2016). We conduct a user study in which\nparticipants (N = 399) were randomly assigned to interact with a rule-based\nchatbot versus one of two LLM-augmented chatbots. We observe limited evidence\nof differences in user engagement or response richness between conditions.\nHowever, the addition of LLM-based dynamic probing skills produces significant\nimprovements in both quantitative and qualitative measures of user experience,\nconsistent with a narrowing of the expectations gulf.", "cat": "cs.HC", "authors": ["Alejandro Cuevas Villalba", "Eva M. Brown", "Jennifer V. Scurrell", "Jason Entenmann", "Madeleine I. G. Daepp"]}, "806": {"id": "2308.16238v1", "title": "The High-Redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs using LOFAR", "url": "http://arxiv.org/pdf/2308.16238v1", "date": "2023-08-30 18:00:10", "abs": "Bent radio AGN morphology depends on the density of the surrounding gas.\nHowever, bent sources are found inside and outside clusters, raising the\nquestion of how environment impacts bent AGN morphology. We analyze new\nLOw-Frequency Array Two-metre Sky Survey (LoTSS) Data Release II observations\nof 20 bent AGNs in clusters and 15 not in clusters from the high-$z$ Clusters\nOccupied by Bent Radio AGN (COBRA) survey (0.35 $<$ $z$ $<$ 2.35). We measure\nthe impact of environment on size, lobe symmetry, and radio luminosity. We find\nthat the most asymmetric radio lobes lie outside of clusters and we uncover a\ntentative correlation between the total projected physical area and cluster\noverdensity. Additionally, we, for the first time, present spectral index\nmeasurements of a large sample of high-$z$ bent sources using LoTSS and Very\nLarge Array Faint Images of the Radio Sky at Twenty-centimeters (VLA FIRST)\nobservations. We find that the median spectral index for the cluster sample is\n-0.76 $\\pm$ 0.01, while the median spectral index for the non-cluster sample\nmedian is -0.81 $\\pm$ 0.02. Furthermore, 13 of 20 cluster bent AGNs have flat\ncores ($\\alpha$ $\\geq$ -0.6) compared to 4 of 15 of non-clusters, indicating a\nkey environmental signature. Beyond core spectral index, bent AGNs inside and\noutside clusters are remarkably similar. We conclude that the non-cluster\nsample may be more representative of bent AGNs at large offsets from the\ncluster center ($>$ 1.2Mpc) or bent AGNs in weaker groups rather than the\nfield.", "cat": "astro-ph.GA", "authors": ["Emmet Golden-Marx", "Emily Moravec", "Lu Shen", "Zheng Cai", "Elizabeth Blanton", "Marie-Lou Gendron-Marsolais", "Huub Rottgering", "Reinout van Weeren", "Victorine Buiten", "Richard Grumitt", "Jesse Golden-Marx", "Siddhant Pinjarkar", "Honming Tang"]}, "807": {"id": "1208.5020v2", "title": "MASSIV: Mass Assembly Survey with SINFONI in VVDS. V. The major merger rate of star-forming galaxies at 0.9 < z < 1.8 from IFS-based close pairs", "url": "http://arxiv.org/pdf/1208.5020v2", "date": "2013-05-13 15:36:10", "abs": "We aim to measure the major merger rate of star-forming galaxies at 0.9 < z\n<1.8, using close pairs identified from integral field spectroscopy (IFS). We\nuse the velocity field maps obtained with SINFONI/VLT on the MASSIV sample,\nselected from the star-forming population in the VVDS. We identify physical\npairs of galaxies from the measurement of the relative velocity and the\nprojected separation (r_p) of the galaxies in the pair. Using the well\nconstrained selection function of the MASSIV sample we derive the gas-rich\nmajor merger fraction (luminosity ratio mu = L_2/L_1 >= 1/4), and, using merger\ntime scales from cosmological simulations, the gas-rich major merger rate at a\nmean redshift up to z = 1.54. We find a high gas-rich major merger fraction of\n20.8+15.2-6.8 %, 20.1+8.0-5.1 % and 22.0+13.7-7.3 % for close pairs with r_p <=\n20h^-1 kpc in redshift ranges z = [0.94, 1.06], [1.2, 1.5) and [1.5, 1.8),\nrespectively. This translates into a gas-rich major merger rate of\n0.116+0.084-0.038 Gyr^-1, 0.147+0.058-0.037 Gyr^-1 and 0.127+0.079-0.042 Gyr^-1\nat z = 1.03, 1.32 and 1.54, respectively. Combining our results with previous\nstudies at z < 1, the gas-rich major merger rate evolves as (1+z)^n, with n =\n3.95 +- 0.12, up to z = 1.5. From these results we infer that ~35% of the\nstar-forming galaxies with stellar masses M = 10^10 - 10^10.5 M_Sun have\nundergone a major merger since z ~ 1.5. We develop a simple model which shows\nthat, assuming that all gas-rich major mergers lead to early-type galaxies, the\ncombined effect of gas-rich and dry mergers is able to explain most of the\nevolution in the number density of massive early-type galaxies since z ~ 1.5,\nwith our measured gas-rich merger rate accounting for about two-thirds of this\nevolution.", "cat": "astro-ph.CO", "authors": ["C. L\u00f3pez-Sanjuan", "O. Le F\u00e8vre", "L. A. M. Tasca", "B. Epinat", "P. Amram", "T. Contini", "B. Garilli", "M. Kissler-Patig", "J. Moultaka", "L. Paioro", "V. Perret", "J. Queyrel", "L. Tresse", "D. Vergani", "C. Divoy"]}, "808": {"id": "2406.19664v1", "title": "Recent Advances in Deep Learning for Channel Coding: A Survey", "url": "http://arxiv.org/pdf/2406.19664v1", "date": "2024-06-28 05:15:51", "abs": "This paper provides a comprehensive survey on recent advances in deep\nlearning (DL) techniques for the channel coding problems. Inspired by the\nrecent successes of DL in a variety of research domains, its applications to\nthe physical layer technologies have been extensively studied in recent years,\nand are expected to be a potential breakthrough in supporting the emerging use\ncases of the next generation wireless communication systems such as 6G. In this\npaper, we focus exclusively on the channel coding problems and review existing\napproaches that incorporate advanced DL techniques into code design and channel\ndecoding. After briefly introducing the background of recent DL techniques, we\ncategorize and summarize a variety of approaches, including model-free and\nmode-based DL, for the design and decoding of modern error-correcting codes,\nsuch as low-density parity check (LDPC) codes and polar codes, to highlight\ntheir potential advantages and challenges. Finally, the paper concludes with a\ndiscussion of open issues and future research directions in channel coding.", "cat": "cs.IT", "authors": ["Toshiki Matsumine", "Hideki Ochiai"]}, "809": {"id": "1408.5765v1", "title": "Ionized gas kinematics of galaxies in the CALIFA survey I: Velocity fields, kinematic parameters of the dominant component, and presence of kinematically distinct gaseous systems", "url": "http://arxiv.org/pdf/1408.5765v1", "date": "2014-08-25 14:08:24", "abs": "This work provides an overall characterization of the kinematic behavior of\nthe ionized gas of the galaxies included in the Calar Alto Legacy Integral\nfield Area (CALIFA), offering kinematic clues to potential users of this survey\nfor including kinematical criteria for specific studies. From the first 200\ngalaxies observed by CALIFA, we present the 2D kinematic view of the 177\ngalaxies satisfying a gas detection threshold. After removing the stellar\ncontribution, we used the cross-correlation technique to obtain the radial\nvelocity of the dominant gaseous component. The main kinematic parameters were\ndirectly derived from the radial velocities with no assumptions on the internal\nmotions. Evidence of the presence of several gaseous components with different\nkinematics were detected by using [OIII] profiles. Most objects in the sample\nshow regular velocity fields, although the ionized-gas kinematics are rarely\nconsistent with simple coplanar circular motions. 35% of the objects present\nevidence of a displacement between the photometric and kinematic centers larger\nthan the original spaxel radii. Only 17% of the objects in the sample exhibit\nkinematic lopsidedness when comparing receding and approaching sides of the\nvelocity fields, but most of them are interacting galaxies exhibiting nuclear\nactivity. Early-type galaxies in the sample present clear photometric-kinematic\nmisaligments. There is evidence of asymmetries in the emission line profiles\nsuggesting the presence of kinematically distinct gaseous components at\ndifferent distances from the nucleus. This work constitutes the first\ndetermination of the ionized gas kinematics of the galaxies observed in the\nCALIFA survey. The derived velocity fields, the reported kinematic\npeculiarities and the identification of the presence of several gaseous\ncomponents might be used as additional criteria for selecting galaxies for\nspecific studies.", "cat": "astro-ph.GA", "authors": ["B. Garcia-Lorenzo", "I. Marquez", "J. K. Barrera-Ballesteros", "J. Masegosa", "B. Husemann", "J. Falc\u00f3n-Barroso", "M. Lyubenova", "S. F. Sanchez", "J. Walcher", "D. Mast", "R. Garcia-Benito", "J. Mendez-Abreu", "G. van de Ven", "K. Spekkens", "L. Holmes", "A. Monreal-Ibero", "A. del Olmo", "B. Ziegler", "J. Bland-Hawthorn", "P. Sanchez-Blazquez", "J. Iglesias-Paramo", "J. A. L. Aguerri", "P. Papaderos", "J. M. Gomes", "R. A. Marino", "R. M. Gonzalez Delgado", "C. Cortijo-Ferrero", "A. R. Lopez-Sanchez", "S. Bekeraite", "L. Wisotzki", "D. Bomans", "the CALIFA team"]}, "810": {"id": "2403.03859v1", "title": "Cosmological forecasts from the combination of Stage-IV photometric galaxy surveys and the magnification from forthcoming GW observatories", "url": "http://arxiv.org/pdf/2403.03859v1", "date": "2024-03-06 17:10:05", "abs": "In this work we have investigated the synergy between Stage-IV galaxy surveys\nand future GW observatories for constraining the underlying cosmological model\nof the Universe, focussing on photometric galaxy clustering, cosmic shear and\nGW magnification as cosmological probes. We have implemented a Fisher matrix\napproach for the evaluation of the full $6\\times2$pt statistics composed by the\nangular power spectra of the single probes together with their combination. For\nour analysis, we have in particular considered dynamical dark energy and\nmassive neutrino scenarios. We have found that the improvement to galaxy survey\nperformance is below 1\\%, in the case $\\ell^{\\rm GW}_{\\rm max}=100$ and a\nluminosity distance error of $\\sigma_{d_L}/d_L=10\\%$. However, when extending\nthe analysis to $\\ell^{\\rm GW}_{\\rm max}=1000$, we find that the GW\nmagnification improves the galaxy survey performance on all the cosmological\nparameters, reducing their errors by $3\\%$-$5\\%$, when $\\sigma_{d_L}/d_L=10\\%$,\nand by $10\\%$-$18\\%$ when $\\sigma_{d_L}/d_L=1\\%$, especially for $M_\\nu$, $w_0$\nand $w_a$. However, here our analysis is unavoidably optimistic: a much more\ndetailed and realistic approach will be needed, especially by including\nsystematic effects. But we can conclude that, in the case of future\ngravitational wave observatories the inclusion of the gravitational wave\nmagnification can improve Stage-IV galaxy surveys performance on constraining\nthe underlying cosmological model of the Universe.", "cat": "astro-ph.CO", "authors": ["Matteo Beltrame", "Marco Bonici", "Carmelita Carbone"]}, "811": {"id": "2306.04542v3", "title": "On the Design Fundamentals of Diffusion Models: A Survey", "url": "http://arxiv.org/pdf/2306.04542v3", "date": "2023-10-19 12:28:12", "abs": "Diffusion models are generative models, which gradually add and remove noise\nto learn the underlying distribution of training data for data generation. The\ncomponents of diffusion models have gained significant attention with many\ndesign choices proposed. Existing reviews have primarily focused on\nhigher-level solutions, thereby covering less on the design fundamentals of\ncomponents. This study seeks to address this gap by providing a comprehensive\nand coherent review on component-wise design choices in diffusion models.\nSpecifically, we organize this review according to their three key components,\nnamely the forward process, the reverse process, and the sampling procedure.\nThis allows us to provide a fine-grained perspective of diffusion models,\nbenefiting future studies in the analysis of individual components, the\napplicability of design choices, and the implementation of diffusion models.", "cat": "cs.LG", "authors": ["Ziyi Chang", "George Alex Koulieris", "Hubert P. H. Shum"]}, "812": {"id": "1505.00442v1", "title": "The VIMOS Public Extragalactic Redshift Survey (VIPERS): On the correct recovery of the count-in-cell probability distribution function", "url": "http://arxiv.org/pdf/1505.00442v1", "date": "2015-05-03 15:42:30", "abs": "We compare three methods to measure the count-in-cell probability density\nfunction of galaxies in a spectroscopic redshift survey. From this comparison\nwe found that when the sampling is low (the average number of object per cell\nis around unity) it is necessary to use a parametric method to model the galaxy\ndistribution. We used a set of mock catalogues of VIPERS, in order to verify if\nwe were able to reconstruct the cell-count probability distribution once the\nobservational strategy is applied. We find that in the simulated catalogues,\nthe probability distribution of galaxies is better represented by a Gamma\nexpansion than a Skewed Log-Normal. Finally, we correct the cell-count\nprobability distribution function from the angular selection effect of the\nVIMOS instrument and study the redshift and absolute magnitude dependency of\nthe underlying galaxy density function in VIPERS from redshift $0.5$ to $1.1$.\nWe found very weak evolution of the probability density distribution function\nand that it is well approximated, independently from the chosen tracers, by a\nGamma distribution.", "cat": "astro-ph.CO", "authors": ["J. Bel", "E. Branchini", "C. Di Porto", "O. Cucciati", "B. R. Granett", "A. Iovino", "S. de la Torre", "C. Marinoni", "L. Guzzo", "L. Moscardini", "A. Cappi", "U. Abbas", "C. Adami", "S. Arnouts", "M. Bolzonella", "D. Bottini", "J. Coupon", "I. Davidzon", "G. De Lucia", "A. Fritz", "P. Franzetti", "M. Fumana", "B. Garilli", "O. Ilbert", "J. Krywult", "V. Le Brun", "O. Le F\u00e8vre", "D. Maccagni", "K. Ma\u0142ek", "F. Marulli", "H. J. McCracken", "L. Paioro", "M. Polletta", "A. Pollo", "H. Schlagenhaufer", "M. Scodeggio", "L. A. M. Tasca", "R. Tojeiro", "D. Vergani", "A. Zanichelli", "A. Burden", "A. Marchetti", "Y. Mellier", "R. C. Nichol", "J. A. Peacock", "W. J. Percival", "S. Phleps", "M. Wolk"]}, "813": {"id": "2309.09937v1", "title": "TransientViT: A novel CNN - Vision Transformer hybrid real/bogus transient classifier for the Kilodegree Automatic Transient Survey", "url": "http://arxiv.org/pdf/2309.09937v1", "date": "2023-09-18 16:55:41", "abs": "The detection and analysis of transient astronomical sources is of great\nimportance to understand their time evolution. Traditional pipelines identify\ntransient sources from difference (D) images derived by subtracting\nprior-observed reference images (R) from new science images (N), a process that\ninvolves extensive manual inspection. In this study, we present TransientViT, a\nhybrid convolutional neural network (CNN) - vision transformer (ViT) model to\ndifferentiate between transients and image artifacts for the Kilodegree\nAutomatic Transient Survey (KATS). TransientViT utilizes CNNs to reduce the\nimage resolution and a hierarchical attention mechanism to model features\nglobally. We propose a novel KATS-T 200K dataset that combines the difference\nimages with both long- and short-term images, providing a temporally\ncontinuous, multidimensional dataset. Using this dataset as the input,\nTransientViT achieved a superior performance in comparison to other\ntransformer- and CNN-based models, with an overall area under the curve (AUC)\nof 0.97 and an accuracy of 99.44%. Ablation studies demonstrated the impact of\ndifferent input channels, multi-input fusion methods, and cross-inference\nstrategies on the model performance. As a final step, a voting-based ensemble\nto combine the inference results of three NRD images further improved the\nmodel's prediction reliability and robustness. This hybrid model will act as a\ncrucial reference for future studies on real/bogus transient classification.", "cat": "astro-ph.IM", "authors": ["Zhuoyang Chen", "Wenjie Zhou", "Guoyou Sun", "Mi Zhang", "Jiangao Ruan", "Jingyuan Zhao"]}, "814": {"id": "1403.0947v2", "title": "The COS-Halos Survey: Physical Conditions and Baryonic Mass in the Low-Redshift Circumgalactic Medium", "url": "http://arxiv.org/pdf/1403.0947v2", "date": "2014-08-07 21:19:19", "abs": "We analyze the physical conditions of the cool, photoionized (T $\\sim 10^4$\nK) circumgalactic medium (CGM) using the COS-Halos suite of gas column density\nmeasurements for 44 gaseous halos within 160 kpc of $L \\sim L^*$ galaxies at $z\n\\sim 0.2$. These data are well described by simple photoionization models, with\nthe gas highly ionized (n$_{\\rm HII}$/n$_{\\rm H} \\gtrsim 99\\%$) by the\nextragalactic ultraviolet background (EUVB). Scaling by estimates for the\nvirial radius, R$_{\\rm vir}$, we show that the ionization state (tracked by the\ndimensionless ionization parameter, U) increases with distance from the host\ngalaxy. The ionization parameters imply a decreasing volume density profile\nn$_{\\rm H}$ = (10$^{-4.2 \\pm 0.25}$)(R/R$_{\\rm vir})^{-0.8\\pm0.3}$. Our derived\ngas volume densities are several orders of magnitude lower than predictions\nfrom standard two-phase models with a cool medium in pressure equilibrium with\na hot, coronal medium expected in virialized halos at this mass scale. Applying\nthe ionization corrections to the HI column densities, we estimate a lower\nlimit to the cool gas mass M$_{\\rm CGM}^{\\rm cool} > 6.5 \\times 10^{10}$\nM$_{\\odot}$ for the volume within R $<$ R$_{\\rm vir}$. Allowing for an\nadditional warm-hot, OVI-traced phase, the CGM accounts for at least half of\nthe baryons purported to be missing from dark matter halos at the 10$^{12}$\nM$_{\\odot}$ scale.", "cat": "astro-ph.CO", "authors": ["Jessica K. Werk", "J. Xavier Prochaska", "Jason Tumlinson", "Molly S. Peeples", "Todd M. Tripp", "Andrew J. Fox", "Nicolas Lehner", "Christopher Thom", "John M. O'Meara", "Amanda Brady Ford", "Rongmon Bordoloi", "Neal Katz", "Nicolas Tejos", "Benjamin D. Oppenheimer", "Romeel Dav\u00e9", "David H. Weinberg"]}, "815": {"id": "1306.3060v2", "title": "A spectroscopic and proper motion search of Sloan digital Sky Survey: red subdwarfs in binary systems", "url": "http://arxiv.org/pdf/1306.3060v2", "date": "2013-07-18 08:24:27", "abs": "Red subdwarfs in binary systems are crucial for both model calibration and\nspectral classification. We search for red subdwarfs in binary systems from a\nsample of high proper motion objects with Sloan digital Sky Survey\nspectroscopy. We present here discoveries from this search, as well as\nhighlight several additional objects of interest. We find 30 red subdwarfs in\nwide binary systems including: two with spectral type of esdM5.5, 6 companions\nto white dwarfs and 3 carbon enhanced red subdwarfs with normal red subdwarf\ncompanions. 15 red subdwarfs in our sample are partially resolved close binary\nsystems. With this binary sample, we estimate the low limit of the red subdwarf\nbinary fraction of ~ 10%. We find that the binary fraction goes down with\ndecreasing masses and metallicities of red subdwarfs. A spectroscopic esdK7\nsubdwarf + white dwarf binary candidate is also reported. 30 new M subdwarfs\nhave spectral type of >= M6 in our sample. We also derive relationships between\nspectral types and absolute magnitudes in the optical and near-infrared for M\nand L subdwarfs, and we present an M subdwarf sample with measured U, V, W\nspace velocities.", "cat": "astro-ph.GA", "authors": ["Z. H. Zhang", "D. J. Pinfield", "B. Burningham", "H. R. A. Jones", "M. C. Galvez-Ortiz", "S. Catalan", "R. L. Smart", "S. Lepine", "J. R. A. Clarke", "Ya. V. Pavlenko", "D. N. Murray", "M. K. Kuznetsov", "A. C. Day-Jones", "J. Gomes", "F. Marocco", "B. Sipocz"]}, "816": {"id": "0803.2236v2", "title": "Next Generation Redshift Surveys and the Origin of Cosmic Acceleration", "url": "http://arxiv.org/pdf/0803.2236v2", "date": "2008-07-09 20:11:20", "abs": "Cosmologists are exploring two possible sets of explanations for the\nremarkable observation of cosmic acceleration: dark energy fills space or\ngeneral relativity fails on cosmological scales. We define a null test\nparameter $\\epsilon(k,a) \\equiv\\Omega_m^{- \\gamma} d \\ln D / d \\ln a - 1$,\nwhere $a$ is the scale factor, $D$ is the growth rate of structure,\n$\\Omega_m(a)$ is the matter density parameter, and $\\gamma$ is a simple\nfunction of redshift.\n We show that it can be expressed entirely in terms of the bias factor,\n$b(a)$, (measured from cross-correlations with CMB lensing) and the amplitude\nof redshift space distortions, $\\beta(k,a)$. Measurements of the CMB power\nspectrum determine $\\Omega_{m 0} H_0^2$. If dark energy within GR is the\nsolution to the cosmic acceleration problem, then the logarithmic growth rate\nof structure $d \\ln D / d \\ln a = \\Omega_m^\\gamma$. Thus, $\\epsilon(k,a) =0$ on\nlinear scales to better than 1%. We show that in the class of Modified Gravity\nmodels known as $f(R)$, the growth rate has a different dependence on scale and\nredshift.\n By combining measurements of the amplitude of $\\beta$ and of the bias, $b$,\nredshift surveys will be able to determine the logarithmic growth rate as a\nfunction of scale and redshift. We estimate the predicted sensitivity of the\nproposed SDSS III (BOSS) survey and the proposed ADEPT mission and find that\nthey will test structure growth in General Relativity to the percent level.", "cat": "astro-ph", "authors": ["Viviana Acquaviva", "Amir Hajian", "David N. Spergel", "Sudeep Das"]}, "817": {"id": "2408.07335v1", "title": "Newly Discovered Changing-look Active Galactic Nuclei from SDSS and LAMOST Surveys", "url": "http://arxiv.org/pdf/2408.07335v1", "date": "2024-08-14 07:17:41", "abs": "Changing-look Active Galactic Nuclei (CL AGN) exhibit drastic variations in\nbroad emission lines (BELs), the mechanism of which remains unclear. Expanding\nthe sample of CL AGN is helpful to reveal the mechanism. This study aims to\nidentify more CL AGNs by cross-matching spectroscopic data from the Sloan\nDigital Sky Survey (SDSS) and the Large Sky Area Multi-Object Fiber\nSpectroscopic Telescope (LAMOST). Our approach to identify CL AGN candidates is\nbased on the automatic spectral fitting, followed by detailed visual\ninspections. Through this method, we present a sample of 88 CL AGNs, in which\n77 sources being newly discovered. Within this sample, 59 CL AGNs primarily\nshow the variability of the H$\\beta$ line, 22 exhibit changes in both the\nH$\\beta$ and H$\\alpha$ lines, and 7 mainly display variations in the H$\\alpha$\nline. Our findings reveal that the sequence of appearance and disappearance of\nthe BELs aligns with the known CL sequence. We estimate the black hole mass and\nEddington ratio for these CL AGNs, which range from $2.5\\times 10^6$ to\n$8.0\\times 10^8 M_\\odot$ and from 0.001 to 0.13, respectively. The Eddington\nratio is lower than that of most typical AGNs, and is consistent with the\nresults of previous studies on CL AGN. Our results support the hypothesis that\nthe CL behavior is driven by the state transitions of the accretion disk.", "cat": "astro-ph.GA", "authors": ["Qian Dong", "Zhi-Xiang Zhang", "Wei-Min Gu", "Mouyuan Sun", "Yong-Gang Zheng"]}, "818": {"id": "2408.12224v1", "title": "The MAGPI Survey: the evolution and drivers of gas turbulence in intermediate-redshift galaxies", "url": "http://arxiv.org/pdf/2408.12224v1", "date": "2024-08-22 08:50:01", "abs": "We measure the ionised gas velocity dispersions of star-forming galaxies in\nthe MAGPI survey ($z\\sim0.3$) and compare them with galaxies in the SAMI\n($z\\sim0.05$) and KROSS ($z\\sim1$) surveys to investigate how the ionised gas\nvelocity dispersion evolves. For the first time, we use a consistent method\nthat forward models galaxy kinematics from $z=0$ to $z=1$. This method accounts\nfor spatial substructure in emission line flux and beam smearing. We\ninvestigate the correlation between gas velocity dispersion and galaxy\nproperties to understand the mechanisms that drive gas turbulence. We find that\nin both MAGPI and SAMI galaxies, the gas velocity dispersion more strongly\ncorrelates with the star-formation rate surface density ($\\Sigma_{\\rm SFR}$)\nthan with a variety of other physical properties, and the average gas velocity\ndispersion is similar, at the same $\\Sigma_{\\rm SFR}$, for SAMI, MAGPI and\nKROSS galaxies. The results indicate that mechanisms related to $\\Sigma_{\\rm\nSFR}$ could be the dominant driver of gas turbulence from $z\\sim1$ to $z\\sim0$,\nfor example, stellar feedback and/or gravitational instability. The gas\nvelocity dispersion of MAGPI galaxies is also correlated with the\nnon-rotational motion of the gas, illustrating that in addition to\nstar-formation feedback, gas transportation and accretion may also contribute\nto the gas velocity dispersion for galaxies at $z\\sim 0.3$. KROSS galaxies only\nhave a moderate correlation between gas velocity dispersion and $\\Sigma_{\\rm\nSFR}$ and a higher scatter of gas velocity dispersion with respect to\n$\\Sigma_{\\rm SFR}$, in agreement with the suggestion that other mechanisms,\nsuch as gas transportation and accretion, are relatively more important at\nhigher redshift galaxies.", "cat": "astro-ph.GA", "authors": ["Yifan Mai", "Scott M. Croom", "Emily Wisnioski", "Sam P. Vaughan", "Mathew R. Varidel", "Andrew J. Battisti", "J. Trevor Mendel", "Marcie Mun", "Takafumi Tsukui", "Caroline Foster", "Katherine E. Harborne", "Claudia D. P. Lagos", "Di Wang", "Sabine Bellstedt", "Joss Bland-Hawthorn", "Matthew Colless", "Francesco D'Eugenio", "Kathryn Grasha", "Yingjie Peng", "Giulia Santucci", "Sarah M. Sweet", "Sabine Thater", "Lucas M. Valenzuela", "Bodo Ziegler"]}, "819": {"id": "0705.1520v1", "title": "Deconstructing dwarf galaxies: a Suprime-Cam survey of Andromeda II", "url": "http://arxiv.org/pdf/0705.1520v1", "date": "2007-05-10 17:26:12", "abs": "(Abridged) We present deep, sub-horizontal branch, multi-colour photometry of\nthe Andromeda II dwarf spheroidal (And II dSph) taken with Subaru Suprime-Cam.\nWe identify a red clump population in this galaxy, the first time this feature\nhas been detected in a M31 dSph, which are normally characterized as having no\nsignificant intermediate age populations. We construct radial profiles for the\nvarious stellar populations and show that the horizontal branch has a nearly\nconstant density spatial distribution out to large radius, whereas the reddest\nred giant branch stars are centrally concentrated in an exponential profile. We\nargue that these populations trace two distinct structural components in And II\nand show that this assumption provides a good match to the overall radial\nprofile of this galaxy. The extended component dominates the stellar\npopulations at large radius, whereas the exponential component dominates the\ninner few arcminutes. We show that the two components have very different\nstellar populations; the exponential component has an average age of $\\sim 7 -\n10$ Gyrs old, is relatively metal-rich ([Fe/H] $\\sim -1$) but with a\nsignificant tail to low metallicities, and possesses a red clump. The extended\ncomponent, on the other hand, is ancient ($\\sim 13$ Gyrs), metal-poor ([Fe/H]\n$\\sim -1.5$) with a narrower dispersion $\\sigma_{\\rm [Fe/H]} \\simeq 0.28$, and\nhas a well developed blue horizontal branch. The extended component contains\napproximately three-quarters of the light of And II and its unusual density\nprofile is unique in Local Group dwarf galaxies. This suggests that its\nformation and/or evolution may have been quite different to other dwarf\ngalaxies.", "cat": "astro-ph", "authors": ["Alan McConnachie", "Nobuo Arimoto", "Mike Irwin"]}, "820": {"id": "2001.06379v1", "title": "A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).VI. Environmental quenching on HII region scales", "url": "http://arxiv.org/pdf/2001.06379v1", "date": "2020-01-17 15:36:43", "abs": "The Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) is a\nblind narrow-band Halpha+[NII] imaging survey of the Virgo cluster carried out\nwith MegaCam at the Canada-French-Hawaii telescope (CFHT). We use a new set of\ndata extracted from VESTIGE to study the impact of the hostile cluster\nenvironment on the star formation process down to the scale of HII regions (~\n50 pc). HII regions are identified and their parameters measured using the\nHIIphot code on a sample of 114 late-type galaxies spanning a wide range in\nmorphological type (Sa-Sd, Im, BCD), stellar mass (10^6.5 <= M_star <= 10^11\nMo), and star formation activity (10^-3 <= SFR <= 10 Mo yr^-1). Owing to the\nexquisite average resolution of the VESTIGE data (0.65 arcsec), we detect 11302\nHII regions with an Halpha luminosity L(Halpha) >= 10^37 erg s^-1. We show that\nthe typical number of HII regions in gas-stripped objects is significantly\nlower than in healthy late-types of similar stellar mass. We also show that in\nthese gas-stripped galaxies the number of HII regions significantly drops\noutside the effective radius, suggesting that the quenching process occurs\noutside-in, in agreement with other multifrequency observations. These new\nresults consistently confirm that the main mechanism responsible for the\ndecrease of the star formation activity observed in cluster galaxies is ram\npressure, allowing us to discard other milder processes such as starvation or\nstrangulation unable to reproduce the observed radially truncated profiles.", "cat": "astro-ph.GA", "authors": ["A. Boselli", "M. Fossati", "A. Longobardi", "S. Boissier", "M. Boquien", "J. Braine", "P. Cote", "J. C. Cuillandre", "B. Epinat", "L. Ferrarese", "G. Gavazzi", "S. Gwyn", "G. Hensler", "H. Plana", "Y. Roehlly", "C. Schimd", "M. Sun", "G. Trinchieri"]}, "821": {"id": "1504.02778v1", "title": "Calibrated Ultra Fast Image Simulations for the Dark Energy Survey", "url": "http://arxiv.org/pdf/1504.02778v1", "date": "2015-04-10 20:00:39", "abs": "Weak lensing by large-scale structure is a powerful technique to probe the\ndark components of the universe. To understand the measurement process of weak\nlensing and the associated systematic effects, image simulations are becoming\nincreasingly important. For this purpose we present a first implementation of\nthe $\\textit{Monte Carlo Control Loops}$ ($\\textit{MCCL}$; Refregier & Amara\n2014), a coherent framework for studying systematic effects in weak lensing. It\nallows us to model and calibrate the shear measurement process using image\nsimulations from the Ultra Fast Image Generator (UFig; Berge et al. 2013). We\napply this framework to a subset of the data taken during the Science\nVerification period (SV) of the Dark Energy Survey (DES). We calibrate the UFig\nsimulations to be statistically consistent with DES images. We then perform\ntolerance analyses by perturbing the simulation parameters and study their\nimpact on the shear measurement at the one-point level. This allows us to\ndetermine the relative importance of different input parameters to the\nsimulations. For spatially constant systematic errors and six simulation\nparameters, the calibration of the simulation reaches the weak lensing\nprecision needed for the DES SV survey area. Furthermore, we find a sensitivity\nof the shear measurement to the intrinsic ellipticity distribution, and an\ninterplay between the magnitude-size and the pixel value diagnostics in\nconstraining the noise model. This work is the first application of the\n$\\textit{MCCL}$ framework to data and shows how it can be used to methodically\nstudy the impact of systematics on the cosmic shear measurement.", "cat": "astro-ph.CO", "authors": ["Claudio Bruderer", "Chihway Chang", "Alexandre Refregier", "Adam Amara", "Joel Berge", "Lukas Gamper"]}, "822": {"id": "1506.07882v1", "title": "The SLUGGS Survey: Globular cluster kinematics in a \"double sigma\" galaxy - NGC 4473", "url": "http://arxiv.org/pdf/1506.07882v1", "date": "2015-06-25 20:01:40", "abs": "NGC 4473 is a so--called double sigma (2$\\sigma$) galaxy, i.e. a galaxy with\nrare, double peaks in its 2D stellar velocity dispersion. Here, we present the\nglobular cluster (GC) kinematics in NGC 4473 out to $\\sim10\\,R_e$ (effective\nradii) using data from combined HST/ACS and Subaru/Suprime--Cam imaging and\nKeck/DEIMOS spectroscopy. We find that the 2$\\sigma$ nature of NGC 4473\npersists up to 3 $R_e$, though it becomes misaligned to the photometric major\naxis. We also observe a significant offset between the stellar and GC rotation\namplitudes. This offset can be understood as a co--addition of\ncounter--rotating stars producing little net stellar rotation. We identify a\nsharp radial transition in the GC kinematics at $\\sim4\\,R_e$ suggesting a well\ndefined kinematically distinct halo. In the inner region ($<4\\,R_e$), the blue\nGCs rotate along the photometric major axis, but in an opposite direction to\nthe galaxy stars and red GCs. In the outer region ($>4\\,R_e$), the red GCs\nrotate in an opposite direction compared to the inner region red GCs, along the\nphotometric major axis, while the blue GCs rotate along an axis intermediate\nbetween the major and minor photometric axes. We also find a kinematically\ndistinct population of very red GCs in the inner region with elevated rotation\namplitude and velocity dispersion. The multiple kinematic components in NGC\n4473 highlight the complex formation and evolutionary history of this 2$\\sigma$\ngalaxy, as well as a distinct transition between the inner and outer\ncomponents.", "cat": "astro-ph.GA", "authors": ["Adebusola B. Alabi", "Caroline Foster", "Duncan A. Forbes", "Aaron J. Romanowsky", "Nicola Pastorello", "Jean P. Brodie", "Lee R. Spitler", "Jay Strader", "Christopher Usher"]}, "823": {"id": "2407.11046v3", "title": "A Survey on LoRA of Large Language Models", "url": "http://arxiv.org/pdf/2407.11046v3", "date": "2024-08-12 12:41:57", "abs": "Low-Rank Adaptation~(LoRA), which updates the dense neural network layers\nwith pluggable low-rank matrices, is one of the best performed parameter\nefficient fine-tuning paradigms. Furthermore, it has significant advantages in\ncross-task generalization and privacy-preserving. Hence, LoRA has gained much\nattention recently, and the number of related literature demonstrates\nexponential growth. It is necessary to conduct a comprehensive overview of the\ncurrent progress on LoRA. This survey categorizes and reviews the progress from\nthe perspectives of (1) downstream adaptation improving variants that improve\nLoRA's performance on downstream tasks; (2) cross-task generalization methods\nthat mix multiple LoRA plugins to achieve cross-task generalization; (3)\nefficiency-improving methods that boost the computation-efficiency of LoRA; (4)\ndata privacy-preserving methods that use LoRA in federated learning; (5)\napplication. Besides, this survey also discusses the future directions in this\nfield. At last, we provide a Github\npage~\\footnote{\\href{https://github.com/ZJU-LLMs/Awesome-LoRAs.git}{https://github.com/ZJU-LLMs/Awesome-LoRAs.git}}\nfor readers to check the updates and initiate discussions on this survey paper.", "cat": "cs.LG", "authors": ["Yuren Mao", "Yuhang Ge", "Yijiang Fan", "Wenyi Xu", "Yu Mi", "Zhonghao Hu", "Yunjun Gao"]}, "824": {"id": "2311.10754v2", "title": "A Recent Survey of the Advancements in Deep Learning Techniques for Monkeypox Disease Detection", "url": "http://arxiv.org/pdf/2311.10754v2", "date": "2023-11-23 20:08:49", "abs": "Monkeypox (MPox) is a zoonotic infectious disease induced by the MPox Virus,\npart of the poxviridae orthopoxvirus group initially discovered in Africa and\ngained global attention in mid-2022 with cases reported outside endemic areas.\nSymptoms include headaches, chills, fever, smallpox, measles, and\nchickenpox-like skin manifestations and the WHO officially announced MPox as a\nglobal public health pandemic, in July 2022.Traditionally, PCR testing of skin\nlesions is considered a benchmark for the primary diagnosis by WHO, with\nsymptom management as the primary treatment and antiviral drugs like\ntecovirimat for severe cases. However, manual analysis within hospitals poses a\nsubstantial challenge including the substantial burden on healthcare\nprofessionals, limited facilities, availability and fatigue among doctors, and\nhuman error during public health emergencies. Therefore, this survey paper\nprovides an extensive and efficient analysis of deep learning (DL) methods for\nthe automatic detection of MPox in skin lesion images. These DL techniques are\nbroadly grouped into categories, including deep CNN, Deep CNNs ensemble, deep\nhybrid learning, the newly developed, and Vision transformer for diagnosing\nMPox. Moreover, this study offers a systematic exploration of the evolutionary\nprogression of DL techniques and identifies, and addresses limitations in\nprevious methods while highlighting the valuable contributions and innovation.\nAdditionally, the paper addresses benchmark datasets and their collection from\nvarious authentic sources, pre-processing techniques, and evaluation metrics.\nThe survey also briefly delves into emerging concepts, identifies research\ngaps, limitations, and applications, and outlines challenges in the diagnosis\nprocess. This survey furnishes valuable insights into the prospective areas of\nDL innovative ideas and is anticipated to serve as a path for researchers.", "cat": "eess.IV", "authors": ["Saddam Hussain Khan", "Rashid Iqbal", "Saeeda Naz"]}, "825": {"id": "2404.03853v1", "title": "A survey of ultra-compact rotating boson star spacetimes", "url": "http://arxiv.org/pdf/2404.03853v1", "date": "2024-04-05 01:10:53", "abs": "Solitonic boson stars (SBS) are compact shell-like objects with an inside\nhaving a nearly constant value of scalar field bounded by a thin shell where\nthe scalar field rapidly changes. While the spherically symmetric SBS can be\ndescribed by an analytical approximation that works well in the thin-shell\ncase, no such approximation exists for rotating SBS and the investigation of\nsuch stars poses a numerical challenge. We numerically investigate rotating SBS\nin case if the relative thickness of the shell is small. We compute\nGerosh-Hansen multipole moments to study the structure of SBS spacetime in the\noutside region and the closeness of SBS to the rotating black hole metric.", "cat": "gr-qc", "authors": ["Nikolay Sukhov"]}, "826": {"id": "1908.07918v1", "title": "Mining Association Rules in Various Computing Environments: A Survey", "url": "http://arxiv.org/pdf/1908.07918v1", "date": "2019-06-30 11:13:50", "abs": "Association Rule Mining (ARM) is one of the well know and most researched\ntechnique of data mining. There are so many ARM algorithms have been designed\nthat their counting is a large number. In this paper we have surveyed the\nvarious ARM algorithms in four computing environments. The considered computing\nenvironments are sequential computing, parallel and distributed computing, grid\ncomputing and cloud computing. With the emergence of new computing paradigm,\nARM algorithms have been designed by many researchers to improve the efficiency\nby utilizing the new paradigm. This paper represents the journey of ARM\nalgorithms started from sequential algorithms, and through parallel and\ndistributed, and grid based algorithms to the current state-of-the-art, along\nwith the motives for adopting new machinery.", "cat": "cs.DC", "authors": ["Sudhakar Singh", "Pankaj Singh", "Rakhi Garg", "P. K. Mishra"]}, "827": {"id": "1004.1257v1", "title": "A Survey on Preprocessing Methods for Web Usage Data", "url": "http://arxiv.org/pdf/1004.1257v1", "date": "2010-04-08 07:07:16", "abs": "World Wide Web is a huge repository of web pages and links. It provides\nabundance of information for the Internet users. The growth of web is\ntremendous as approximately one million pages are added daily. Users' accesses\nare recorded in web logs. Because of the tremendous usage of web, the web log\nfiles are growing at a faster rate and the size is becoming huge. Web data\nmining is the application of data mining techniques in web data. Web Usage\nMining applies mining techniques in log data to extract the behavior of users\nwhich is used in various applications like personalized services, adaptive web\nsites, customer profiling, prefetching, creating attractive web sites etc., Web\nusage mining consists of three phases preprocessing, pattern discovery and\npattern analysis. Web log data is usually noisy and ambiguous and preprocessing\nis an important process before mining. For discovering patterns sessions are to\nbe constructed efficiently. This paper reviews existing work done in the\npreprocessing stage. A brief overview of various data mining techniques for\ndiscovering patterns, and pattern analysis are discussed. Finally a glimpse of\nvarious applications of web usage mining is also presented.", "cat": "cs.IR", "authors": ["V. Chitraa", "Dr. Antony Selvdoss Davamani"]}, "828": {"id": "1010.1533v2", "title": "The PN.S Elliptical Galaxy Survey: a standard LCDM halo around NGC 4374?", "url": "http://arxiv.org/pdf/1010.1533v2", "date": "2010-10-11 18:06:17", "abs": "As part of our current programme to test LCDM predictions for dark matter\n(DM) haloes using extended kinematical observations of early-type galaxies, we\npresent a dynamical analysis of the bright elliptical galaxy NGC 4374 (M84)\nbased on ~450 Planetary Nebulae (PNe) velocities from the PN.Spectrograph,\nalong with extended long-slit stellar kinematics. This is the first such\nanalysis of a galaxy from our survey with a radially constant velocity\ndispersion profile. We find that the spatial and kinematical distributions of\nthe PNe agree with the field stars in the region of overlap. The velocity\nkurtosis is consistent with zero at almost all radii. We construct a series of\nJeans models, fitting both velocity dispersion and kurtosis to help break the\nmass-anisotropy degeneracy. Our mass models include DM halos either with\nshallow cores or with central cusps as predicted by cosmological simulations -\nalong with the novel introduction in this context of adiabatic halo contraction\nfrom baryon infall. Both classes of models confirm a very massive dark halo\naround NGC 4374, demonstrating that PN kinematics data are well able to detect\nsuch haloes when present. Considering the default cosmological mass model, we\nconfirm earlier suggestions that bright galaxies tend to have halo\nconcentrations higher than LCDM predictions, but this is found to be solved if\neither a Salpeter IMF or adiabatic contraction with a Kroupa IMF is assumed.\nThus for the first time a case is found where the PN dynamics may well be\nconsistent with a standard dark matter halo. A cored halo can also fit the\ndata, and prefers a stellar mass consistent with a Salpeter IMF. The less\ndramatic dark matter content found in lower-luminosity \"ordinary\" ellipticals\nsuggests a bimodality in the halo properties which may be produced by divergent\nbaryonic effects during their assembly histories.", "cat": "astro-ph.CO", "authors": ["N. R. Napolitano", "A. J. Romanowsky", "M. Capaccioli", "N. G. Douglas", "M. Arnaboldi", "L. Coccato", "O. Gerhard", "K. Kuijken", "M. R. Merrifield", "S. P. Bamford", "A. Cortesi", "P. Das", "K. C. Freeman"]}, "829": {"id": "2008.08196v1", "title": "Survey of 360$^{\\circ}$ domain walls in magnetic heterostructures: topology, chirality and current-driven dynamics", "url": "http://arxiv.org/pdf/2008.08196v1", "date": "2020-08-18 23:45:18", "abs": "Chirality and current-driven dynamics of topologically nontrivial\n360$^{\\circ}$ domain walls (360DWs) in magnetic heterostructures (MHs) are\nsystematically investigated. For MHs with normal substrates, the static 360DWs\nare N\\'{e}el-type with no chirality. While for those with heavy-metal\nsubstrates, the interfacial Dzyaloshinskii-Moriya interaction (iDMI) therein\nmakes 360DWs prefer specific chirality. Under in-plane driving charge currents,\nas the direct result of \"full-circle\" topology a certain 360DW does not undergo\nthe \"Walker breakdown\"-type process like a well-studied 180$^{\\circ}$ domain\nwall as the current density increases. Alternatively, it keeps a fixed\npropagating mode (either steady-flow or precessional-flow, depending on the\neffective damping constant of the MH) until it collapses or changes to other\ntypes of solition when the current density becomes too high. Similarly, the\nfield-like spin-orbit torque (SOT) has no effects on the dynamics of 360DWs,\nwhile the anti-damping SOT has. For both modes, modifications to the mobility\nof 360DWs by iDMI and anti-damping SOT are provided.", "cat": "cond-mat.mes-hall", "authors": ["Mei Li", "Jie Lu"]}, "830": {"id": "1706.01472v3", "title": "Full-sky Gravitational Lensing Simulation for Large-area Galaxy Surveys and Cosmic Microwave Background Experiments", "url": "http://arxiv.org/pdf/1706.01472v3", "date": "2017-11-24 10:51:49", "abs": "We present 108 full-sky gravitational lensing simulation data sets generated\nby performing multiple-lens plane ray-tracing through high-resolution\ncosmological $N$-body simulations. The data sets include full-sky convergence\nand shear maps from redshifts $z=0.05$ to $5.3$ at intervals of $150 \\,\nh^{-1}{\\rm Mpc}$ comoving radial distance (corresponding to a redshift interval\nof $\\Delta z \\simeq 0.05$ at the nearby universe), enabling the construction of\na mock shear catalog for an arbitrary source distribution up to $z=5.3$. The\ndark matter halos are identified from the same $N$-body simulations with enough\nmass resolution to resolve the host halos of the Sloan Digital Sky Survey\n(SDSS) CMASS and Luminous Red Galaxies (LRGs). Angular positions and redshifts\nof the halos are provided by a ray-tracing calculation, enabling the creation\nof a mock halo catalog to be used for galaxy-galaxy and cluster-galaxy lensing.\nThe simulation also yields maps of gravitational lensing deflections for a\nsource redshift at the last scattering surface, and we provide 108 realizations\nof lensed cosmic microwave background (CMB) maps in which the post-Born\ncorrections caused by multiple light scattering are included. We present basic\nstatistics of the simulation data, including the angular power spectra of\ncosmic shear, CMB temperature and polarization anisotropies, galaxy-galaxy\nlensing signals for halos, and their covariances. The angular power spectra of\nthe cosmic shear and CMB anisotropies agree with theoretical predictions within\n$5\\%$ up to $\\ell = 3000$ (or at an angular scale $\\theta > 0.5$ arcsin). The\nsimulation data sets are generated primarily for the ongoing Subaru Hyper\nSuprime-Cam survey but are freely available for download at\nhttp://cosmo.phys.hirosaki-u.ac.jp/takahasi/allsky_raytracing.", "cat": "astro-ph.CO", "authors": ["Ryuichi Takahashi", "Takashi Hamana", "Masato Shirasaki", "Toshiya Namikawa", "Takahiro Nishimichi", "Ken Osato", "Kosei Shiroyama"]}, "831": {"id": "1705.02506v1", "title": "AngularJS Performance: A Survey Study", "url": "http://arxiv.org/pdf/1705.02506v1", "date": "2017-05-06 17:01:14", "abs": "AngularJS is a popular JavaScript MVC-based framework to construct\nsingle-page web applications. In this paper, we report the results of a survey\nwith 95 professional developers about performance issues of AngularJS\napplications. We report common practices followed by developers to avoid\nperformance problems (e.g., use of third-party or custom components), the\ngeneral causes of performance problems in AngularJS applications (e.g.,\ninadequate architecture decisions taken by AngularJS users), and the technical\nand specific causes of performance problems (e.g., unnecessary processing\nincluded in the digest cycle, which is the internal computation that\nautomatically updates the view with changes detected in the model).", "cat": "cs.SE", "authors": ["Miguel Ramos", "Marco Tulio Valente", "Ricardo Terra"]}, "832": {"id": "1607.06235v1", "title": "Haze Visibility Enhancement: A Survey and Quantitative Benchmarking", "url": "http://arxiv.org/pdf/1607.06235v1", "date": "2016-07-21 08:57:13", "abs": "This paper provides a comprehensive survey of methods dealing with visibility\nenhancement of images taken in hazy or foggy scenes. The survey begins with\ndiscussing the optical models of atmospheric scattering media and image\nformation. This is followed by a survey of existing methods, which are grouped\nto multiple image methods, polarizing filters based methods, methods with known\ndepth, and single-image methods. We also provide a benchmark of a number of\nwell known single-image methods, based on a recent dataset provided by Fattal\nand our newly generated scattering media dataset that contains ground truth\nimages for quantitative evaluation. To our knowledge, this is the first\nbenchmark using numerical metrics to evaluate dehazing techniques. This\nbenchmark allows us to objectively compare the results of existing methods and\nto better identify the strengths and limitations of each method.", "cat": "cs.CV", "authors": ["Yu Li", "Shaodi You", "Michael S. Brown", "Robby T. Tan"]}, "833": {"id": "2306.01929v1", "title": "Recent Advances of Local Mechanisms in Computer Vision: A Survey and Outlook of Recent Work", "url": "http://arxiv.org/pdf/2306.01929v1", "date": "2023-06-02 22:05:52", "abs": "Inspired by the fact that human brains can emphasize discriminative parts of\nthe input and suppress irrelevant ones, substantial local mechanisms have been\ndesigned to boost the development of computer vision. They can not only focus\non target parts to learn discriminative local representations, but also process\ninformation selectively to improve the efficiency. In terms of application\nscenarios and paradigms, local mechanisms have different characteristics. In\nthis survey, we provide a systematic review of local mechanisms for various\ncomputer vision tasks and approaches, including fine-grained visual\nrecognition, person re-identification, few-/zero-shot learning, multi-modal\nlearning, self-supervised learning, Vision Transformers, and so on.\nCategorization of local mechanisms in each field is summarized. Then,\nadvantages and disadvantages for every category are analyzed deeply, leaving\nroom for exploration. Finally, future research directions about local\nmechanisms have also been discussed that may benefit future works. To the best\nour knowledge, this is the first survey about local mechanisms on computer\nvision. We hope that this survey can shed light on future research in the\ncomputer vision field.", "cat": "cs.CV", "authors": ["Qiangchang Wang", "Yilong Yin"]}, "834": {"id": "1712.05191v1", "title": "Relation Extraction : A Survey", "url": "http://arxiv.org/pdf/1712.05191v1", "date": "2017-12-14 12:04:10", "abs": "With the advent of the Internet, large amount of digital text is generated\neveryday in the form of news articles, research publications, blogs, question\nanswering forums and social media. It is important to develop techniques for\nextracting information automatically from these documents, as lot of important\ninformation is hidden within them. This extracted information can be used to\nimprove access and management of knowledge hidden in large text corpora.\nSeveral applications such as Question Answering, Information Retrieval would\nbenefit from this information. Entities like persons and organizations, form\nthe most basic unit of the information. Occurrences of entities in a sentence\nare often linked through well-defined relations; e.g., occurrences of person\nand organization in a sentence may be linked through relations such as employed\nat. The task of Relation Extraction (RE) is to identify such relations\nautomatically. In this paper, we survey several important supervised,\nsemi-supervised and unsupervised RE techniques. We also cover the paradigms of\nOpen Information Extraction (OIE) and Distant Supervision. Finally, we describe\nsome of the recent trends in the RE techniques and possible future research\ndirections. This survey would be useful for three kinds of readers - i)\nNewcomers in the field who want to quickly learn about RE; ii) Researchers who\nwant to know how the various RE techniques evolved over time and what are\npossible future research directions and iii) Practitioners who just need to\nknow which RE technique works best in various settings.", "cat": "cs.CL", "authors": ["Sachin Pawar", "Girish K. Palshikar", "Pushpak Bhattacharyya"]}, "835": {"id": "2103.09245v2", "title": "The MOSDEF Survey: The Mass-Metallicity relationship and the existence of the FMR at z~1.5", "url": "http://arxiv.org/pdf/2103.09245v2", "date": "2021-06-23 14:48:34", "abs": "We analyze the rest-optical emission-line ratios of z~1.5 galaxies drawn from\nthe MOSFIRE Deep Evolution Field (MOSDEF) survey. Using composite spectra we\ninvestigate the mass-metallicity relation (MZR) at z~1.5 and measure its\nevolution to z=0. When using gas-phase metallicities based on the N2 line\nratio, we find that the MZR evolution from z~1.5 to z=0 depends on stellar\nmass, evolving by $\\Delta\\rm log(\\rm O/H)\\sim0.25$ dex at\n$M_*<10^{9.75}M_{\\odot}$ down to $\\Delta\\rm log(\\rm O/H)\\sim0.05$ at\n$M_*>10^{10.5}M_{\\odot}$. In contrast, the O3N2-based MZR shows a constant\noffset of $\\Delta\\rm log(\\rm O/H)\\sim0.30$ across all masses, consistent with\nprevious MOSDEF results based on independent metallicity indicators, and\nsuggesting that O3N2 provides a more robust metallicity calibration for our\nz~1.5 sample. We investigated the secondary dependence of the MZR on SFR by\nmeasuring correlated scatter about the mean $M_*$-specific SFR and\n$M_*-\\log(\\rm O3N2)$ relations. We find an anti-correlation between $\\log(\\rm\nO/H)$ and sSFR offsets, indicating the presence of a $M_*$-SFR-Z relation,\nthough with limited significance. Additionally, we find that our z~1.5 stacks\nlie along the z=0 metallicity sequence at fixed\n$\\mu=\\log(M_*/M_{\\odot})-0.6\\times\\log(\\rm SFR / M_{\\odot} yr^{-1})$ suggesting\nthat the z~1.5 stacks can be described by the z=0 fundamental metallicity\nrelation (FMR). However, using different calibrations can shift the calculated\nmetallicities off of the local FMR, indicating that appropriate calibrations\nare essential for understanding metallicity evolution with redshift. Finally,\nunderstanding how [NII]/H$\\alpha$ scales with galaxy properties is crucial to\naccurately describe the effects of blended [NII] and H$\\alpha$ on redshift and\nH$\\alpha$ flux measurements in future large surveys utilizing low-resolution\nspectra such as with Euclid and the Roman Space Telescope.", "cat": "astro-ph.GA", "authors": ["Michael W. Topping", "Alice E. Shapley", "Ryan L. Sanders", "Mariska Kriek", "Naveen A. Reddy", "Alison L. Coil", "Bahram Mobasher", "Brian Siana", "William R. Freeman", "Irene Shivaei", "Mojegan Azadi", "Sedona H. Price", "Gene C. K. Leung", "Tara Fetherolf", "Laura de Groot", "Tom Zick", "Francesca M. Fornasini", "Guillermo Barro", "Jordan N. Runco"]}, "836": {"id": "2406.10877v2", "title": "WALLABY Pilot Survey: the Tully-Fisher relation in the NGC 4808, Vela and NGC 5044 fields", "url": "http://arxiv.org/pdf/2406.10877v2", "date": "2024-06-20 03:53:56", "abs": "The Tully-Fisher Relation (TFR) is a well-known empirical relationship\nbetween the luminosity of a spiral galaxy and its circular velocity, allowing\nus to estimate redshift independent distances. Here we use high signal-to-noise\nHI 21-cm integrated spectra from the second pilot data release (PDR2, 180 deg2)\nof the Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY). In order\nto prepare for the full WALLABY survey, we have investigated the TFR in phase 2\nof the pilot survey with a further three fields. The data were obtained with\nwide-field Phased Array Feeds on the Australian Square Kilometre Array\nPathfinder (ASKAP) and have an angular resolution of 30 arcsec and a velocity\nresolution of ~4 km/s. Galaxy luminosities have been measured from the\nWide-field Infrared Survey Explorer (WISE), and optical galaxy inclinations\nfrom the Dark Energy Camera Legacy Survey. We present TFRs for wavelengths from\n0.8-3.4{\\mu}m. We examine sources of galaxy inclination data and investigate\nmagnitudes from the DECam Local Volume Exploration Survey (DELVE) and DENIS\ncatalogues and the 4HS target catalogue based on the VISTA Hemisphere Survey\n(VHS). We consider the baryonic TFR. These are all of interest for TFR using\nthe full WALLABY survey of 200,000 galaxies. We demonstrate that WALLABY TFR\ndistances can take their place among state of the art studies of the local\nvelocity field.", "cat": "astro-ph.GA", "authors": ["Jeremy Mould", "T. H. Jarrett", "H\u00e9l\u00e8ne Courtois", "Albert Bosma", "Nathan Deg", "Alexandra Dupuy", "Lister Staveley-Smith", "E. N. Taylor", "Jayanne English", "S. H. A. Rajohnson", "Ren\u00e9e Kraan-Korteweg", "Duncan Forbes", "Helga D\u00e9nes", "Karen Lee-Waddell", "Austin Shen", "O. I. Wong", "Benne Holwerda", "B\u00e4rbel Koribalski", "Denis Leahy", "Pavel Mancera Pi\u00f1a", "Niankun Yu"]}, "837": {"id": "2204.01781v1", "title": "Constraints on Multi-Field Inflation from the BOSS Galaxy Survey", "url": "http://arxiv.org/pdf/2204.01781v1", "date": "2022-04-04 18:23:51", "abs": "We use redshift-space galaxy clustering data from the BOSS survey to\nconstrain local primordial non-Gaussianity (LPNG). This is of particular\nimportance due to the consistency relations, which imply that a detection of\nLPNG would rule out all single-field inflationary models. Our constraints are\nbased on the consistently analyzed redshift-space galaxy power spectra and\nbispectra, extracted from the public BOSS data with optimal window-free\nestimators. We use a complete perturbation theory model including all one-loop\npower spectrum corrections generated by LPNG. Our constraint on the amplitude\nof the local non-Gaussian shape is $f_{\\rm NL}^{\\rm local}=-33\\pm 28$ at\n68\\%\\,CL, yielding no evidence for primordial non-Gaussianity. The addition of\nthe bispectrum tightens the $f_{\\rm NL}^{\\rm local}$ constraints from BOSS by\n$20\\%$, and allows breaking of degeneracies with non-Gaussian galaxy bias.\nThese results set the stage for the analysis of future surveys, whose larger\nvolumes will yield significantly tighter constraints on LPNG.", "cat": "astro-ph.CO", "authors": ["Giovanni Cabass", "Mikhail M. Ivanov", "Oliver H. E. Philcox", "Marko Simonovi\u0107", "Matias Zaldarriaga"]}, "838": {"id": "1809.04865v1", "title": "MIRIS Pa\u03b1 Galactic Plane Survey. I. Comparison with IPHAS H\u03b1 in l = 96\u00b0-116\u00b0", "url": "http://arxiv.org/pdf/1809.04865v1", "date": "2018-09-13 10:03:42", "abs": "The Multipurpose InfraRed Imaging System (MIRIS) performed the MIRIS\nPa{\\alpha} Galactic Plane Survey (MIPAPS), which covers the entire Galactic\nplane within the latitude range of -3{\\deg} < b < +3{\\deg} at Pa{\\alpha} (1.87\num). We present the first result of the MIPAPS data extracted from the\nlongitude range of l = 96.5{\\deg}-116.3{\\deg}, and demonstrate the data quality\nand scientific potential of the data by comparing them with H{\\alpha} maps\nobtained from the INT Photometric H{\\alpha} Survey (IPHAS) data. We newly\nidentify 90 H II region candidates in the WISE H II region catalog as definite\nH II regions by detecting the Pa{\\alpha} and/or H{\\alpha} recombination lines,\nout of which 53 H II regions are detected at Pa{\\alpha}. We also report the\ndetection of additional 29 extended and 18 point-like sources at Pa{\\alpha}. We\nestimate the E(B-V) color excesses and the total Lyman continuum luminosities\nfor H II regions by combining the MIPAPS Pa{\\alpha} and IPHAS H{\\alpha} fluxes.\nThe E(B-V) values are found to be systematically lower than those estimated\nfrom point stars associated with H II regions. Utilizing the MIPAPS Pa{\\alpha}\nand IPHAS H{\\alpha} images, we obtain an E(B-V) map for the entire region of\nthe H II region Sh2-131 with an angular size of ~2.5{\\deg}. The E(B-V) map\nshows not only numerous high-extinction filamentary features but also negative\nE(B-V) regions, indicating H{\\alpha} excess. The H{\\alpha} excess and the\nsystematic underestimation of E(B-V) are attributed to light scattered by dust.", "cat": "astro-ph.GA", "authors": ["Il-Joong Kim", "Jeonghyun Pyo", "Woong-Seob Jeong", "Kwang-Il Seon", "Takao Nakagawa", "Min Gyu Kim", "Won-Kee Park", "Dae-Hee Lee", "Dukhang Lee", "Bongkon Moon", "Sung-Joon Park", "Youngsik Park", "Toshio Matsumoto", "Wonyong Han"]}, "839": {"id": "0904.4744v4", "title": "Duality, correspondences and the Lefschetz map in equivariant KK-theory: a survey", "url": "http://arxiv.org/pdf/0904.4744v4", "date": "2010-09-27 18:03:17", "abs": "We survey work by the author and Ralf Meyer on equivariant KK-theory. Duality\nplays a key role in our approach. We organize the survey around the objective\nof computing a certain homotopy-invariant of a space equipped with a proper\naction of a group or groupoid called the Lefschetz map. The Lefschetz map\nassociates an equivariant K-homology class to an equivariant Kasparov\nself-morphism of a space X admitting a dual. We want to describe it explicitly\nin the setting of bundles of smooth manifolds over the base space of a proper\ngroupoid, in which groupoid elements act by diffeomorphisms between fibres. To\nget the required description we describe a topological model of equivariant\nKK-theory by way of a theory of correspondences, building on ideas of Paul\nBaum, Alain Connes and Georges Skandalis that appeared in the 1980's. This\nmodel agrees with the analytic model for bundles of smooth manifolds under some\ntechnical conditions related to the existence of equivariant vector bundles.\nSubject to these conditions we obtain a computation of the Lefschetz map in\npurely topological terms.", "cat": "math.KT", "authors": ["Heath Emerson"]}, "840": {"id": "0810.3859v1", "title": "The UKIRT Infrared Deep Sky Survey and the search for the most distant quasars", "url": "http://arxiv.org/pdf/0810.3859v1", "date": "2008-10-21 15:27:10", "abs": "The UKIRT Infrared Deep Sky Survey (UKIDSS) Large Area Survey (LAS) has the\nnecessary combination of filters (Y, J, H and K), depth (Y <~ 20.2) and area\ncoverage (~4000 deg^2) to detect several redshift z >~ 6.4 quasars. The Third\nData Release (DR3) included ~1000 deg^2 of LAS observations which have so far\nyielded two previously known z ~= 6 quasars and two new discoveries: ULAS\nJ0203+0012, at z = 5.72; and ULAS J1319+0950, at z = 6.13.", "cat": "astro-ph", "authors": ["Daniel J. Mortlock", "Mitesh Patel", "Stephen J. Warren", "Bram P. Venemans", "Richard G. McMahon", "Paul Hewett", "Chris Simpson", "Rob G. Sharp"]}, "841": {"id": "2408.05275v3", "title": "Euclid preparation. The Cosmic Dawn Survey (DAWN) of the Euclid Deep and Auxiliary Fields", "url": "http://arxiv.org/pdf/2408.05275v3", "date": "2024-08-22 08:41:20", "abs": "Euclid will provide deep NIR imaging to $\\sim$26.5 AB magnitude over $\\sim$59\ndeg$^2$ in its deep and auxiliary fields. The Cosmic DAWN survey complements\nthe deep Euclid data with matched depth multiwavelength imaging and\nspectroscopy in the UV--IR to provide consistently processed Euclid selected\nphotometric catalogs, accurate photometric redshifts, and measurements of\ngalaxy properties to a redshift of $z\\sim 10$. In this paper, we present an\noverview of the survey, including the footprints of the survey fields, the\nexisting and planned observations, and the primary science goals for the\ncombined data set.", "cat": "astro-ph.GA", "authors": ["Euclid Collaboration", "C. J. R. McPartland", "L. Zalesky", "J. R. Weaver", "S. Toft", "D. B. Sanders", "B. Mobasher", "N. Suzuki", "I. Szapudi", "I. Valdes", "G. Murphree", "N. Chartab", "N. Allen", "S. Taamoli", "P. R. M. Eisenhardt", "S. Arnouts", "H. Atek", "J. Brinchmann", "M. Castellano", "R. Chary", "O. Ch\u00e1vez Ortiz", "J. -G. Cuby", "S. L. Finkelstein", "T. Goto", "S. Gwyn", "Y. Harikane", "A. K. Inoue", "H. J. McCracken", "J. J. Mohr", "P. A. Oesch", "M. Ouchi", "M. Oguri", "J. Rhodes", "H. J. A. Rottgering", "M. Sawicki", "R. Scaramella", "C. Scarlata", "J. D. Silverman", "D. Stern", "H. I. Teplitz", "M. Shuntov", "B. Altieri", "A. Amara", "S. Andreon", "N. Auricchio", "H. Aussel", "C. Baccigalupi", "M. Baldi", "S. Bardelli", "R. Bender", "D. Bonino", "E. Branchini", "M. Brescia", "S. Camera", "V. Capobianco", "C. Carbone", "J. Carretero", "S. Casas", "F. J. Castander", "G. Castignani", "S. Cavuoti", "A. Cimatti", "C. Colodro-Conde", "G. Congedo", "C. J. Conselice", "L. Conversi", "Y. Copin", "F. Courbin", "H. M. Courtois", "A. Da Silva", "H. Degaudenzi", "G. De Lucia", "A. M. Di Giorgio", "J. Dinis", "M. Douspis", "F. Dubath", "X. Dupac", "S. Dusini", "M. Fabricius", "M. Farina", "S. Farrens", "S. Ferriol", "S. Fotopoulou", "M. Frailis", "E. Franceschi", "M. Fumana", "S. Galeotta", "B. Garilli", "K. George", "B. Gillis", "C. Giocoli", "A. Grazian", "F. Grupp", "L. Guzzo", "H. Hoekstra", "W. Holmes", "I. Hook", "F. Hormuth", "A. Hornstrup", "P. Hudelot", "K. Jahnke", "E. Keih\u00e4nen", "S. Kermiche", "A. Kiessling", "M. Kilbinger", "T. Kitching", "B. Kubik", "M. Kunz", "H. Kurki-Suonio", "P. B. Lilje", "V. Lindholm", "I. Lloro", "G. Mainetti", "E. Maiorano", "O. Mansutti", "O. Marggraf", "K. Markovic", "M. Martinelli", "N. Martinet", "F. Marulli", "R. Massey", "S. Maurogordato", "E. Medinaceli", "S. Mei", "M. Melchior", "Y. Mellier", "M. Meneghetti", "E. Merlin", "G. Meylan", "M. Moresco", "L. Moscardini", "E. Munari", "R. Nakajima", "C. Neissner", "S. -M. Niemi", "J. W. Nightingale", "C. Padilla", "S. Paltani", "F. Pasian", "K. Pedersen", "W. J. Percival", "V. Pettorino", "G. Polenta", "M. Poncet", "L. A. Popa", "L. Pozzetti", "F. Raison", "R. Rebolo", "A. Renzi", "G. Riccio", "E. Romelli", "M. Roncarelli", "E. Rossetti", "R. Saglia", "Z. Sakr", "A. G. S\u00e1nchez", "D. Sapone", "B. Sartoris", "M. Schirmer", "P. Schneider", "T. Schrabback", "A. Secroun", "G. Seidel", "S. Serrano", "C. Sirignano", "G. Sirri", "L. Stanco", "J. Steinwagner", "C. Surace", "P. Tallada-Crespi", "D. Tavagnacco", "I. Tereno", "R. Toledo-Moreo", "F. Torradeflot", "I. Tutusaus", "E. A. Valentijn", "L. Valenziano", "T. Vassallo", "A. Veropalumbo", "Y. Wang", "J. Weller", "G. Zamorani", "J. Zoubian", "E. Zucca", "A. Biviano", "M. Bolzonella", "A. Boucaud", "E. Bozzo", "C. Burigana", "D. Di Ferdinando", "R. Farinelli", "J. Gracia-Carpio", "N. Mauri", "V. Scottez", "M. Tenti", "M. Viel", "M. Wiesmann", "Y. Akrami", "V. Allevato", "S. Anselmi", "M. Ballardini", "M. Bethermin", "S. Borgani", "A. S. Borlaff", "S. Bruton", "R. Cabanac", "A. Calabro", "G. Ca\u00f1as-Herrera", "A. Cappi", "C. S. Carvalho", "T. Castro", "K. C. Chambers", "S. Contarini", "A. R. Cooray", "J. Coupon", "S. Davini", "S. de la Torre", "G. Desprez", "A. D\u00edaz-S\u00e1nchez", "S. Di Domizio", "H. Dole", "J. A. Escartin Vigo", "S. Escoffier", "A. G. Ferrari", "P. G. Ferreira", "I. Ferrero", "F. Finelli", "F. Fornari", "L. Gabarra", "K. Ganga", "J. Garc\u00eda-Bellido", "V. Gautard", "E. Gaztanaga", "F. Giacomini", "G. Gozaliasl", "A. Gregorio", "A. Hall", "W. G. Hartley", "H. Hildebrandt", "J. Hjorth", "M. Huertas-Company", "O. Ilbert", "J. J. E. Kajava", "V. Kansal", "D. Karagiannis", "C. C. Kirkpatrick", "L. Legrand", "G. Libet", "A. Loureiro", "J. Macias-Perez", "G. Maggio", "M. Magliocchetti", "C. Mancini", "F. Mannucci", "R. Maoli", "C. J. A. P. Martins", "S. Matthew", "M. Maturi", "L. Maurin", "R. B. Metcalf", "P. Monaco", "C. Moretti", "G. Morgante", "P. Musi", "Nicholas A. Walton", "J. Odier", "L. Patrizii", "M. P\u00f6ntinen", "V. Popa", "C. Porciani", "D. Potter", "P. Reimberg", "I. Risso", "P. -F. Rocci", "M. Sahl\u00e9n", "A. Schneider", "M. Sereno", "P. Simon", "A. Spurio Mancini", "S. A. Stanford", "C. Tao", "G. Testera", "R. Teyssier", "S. Tosi", "A. Troja", "M. Tucci", "C. Valieri", "J. Valiviita", "D. Vergani", "G. Verza", "F. Shankar"]}, "842": {"id": "1707.09391v1", "title": "Interference Modeling in Cognitive Radio Networks: A Survey", "url": "http://arxiv.org/pdf/1707.09391v1", "date": "2017-07-28 19:42:39", "abs": "One of the fundamental elements impacting the performance of a wireless\nsystem is interference, which has been a long-term issue in wireless networks.\nIn the case of cognitive radio (CR) networks, the problem of interference is\ntremendously crucial. In other words, CR keeps the important promise of not\nproducing any harmful interference to the primary user (PU) system. Thus, it is\nessential to investigate the impact of interference caused to the PUs so that\nits detrimental effect on the performance of the PU system performance is\nreduced. Study of cognitive interference generally includes developing a model\nto statistically demonstrate the power of cognitive interference at the PUs,\nwhich then can be utilized to examine different performance measures. Having\ninspected the different models for channel interference present in the\nliterature, it can be obviously seen that interference models have been\ngradually evolved in terms of complication and sophistication. Although\nnumerous papers can be found in the literature that have investigated different\nmodels for interference, to the best of our knowledge, very few publications\nare available that provide a review of all models and their comparisons. This\npaper is a collection of state-of-the-art in interference modeling which\noverviews and compares different models in the literature to provide the\nvaluable insights for researchers when modeling the interference in a specific\nscenario.", "cat": "cs.NI", "authors": ["Mohsen Riahi Manesh", "Naima Kaabouch"]}, "843": {"id": "1007.4557v1", "title": "A submillimetre survey of the kinematics of the Perseus molecular cloud - III. Clump kinematics", "url": "http://arxiv.org/pdf/1007.4557v1", "date": "2010-07-26 20:07:37", "abs": "We explore the kinematics of continuum clumps in the Perseus molecular cloud,\nderived from C18O J=3-2 data. Two populations are examined, identified using\nthe automated algorithms CLFIND and GAUSSCLUMPS on existing SCUBA data. The\nclumps have supersonic linewidths with distributions which suggest the C18O\nline probes a lower-density 'envelope' rather than a dense inner core. Similar\nlinewidth distributions for protostellar and starless clumps implies protostars\ndo not have a significant impact on their immediate environment. The proximity\nto an active young stellar cluster seems to affect the linewidths: those in\nNGC1333 are greater than elsewhere. In IC348 the proximity to the old IR\ncluster has little influence, with the linewidths being the smallest of all. A\nvirial analysis suggests that the clumps are bound and close to equipartition.\nIn particular, the starless clumps occupy the same parameter space as the\nprotostars, suggesting they are true stellar precursors and will go on to form\nstars. We also search for ordered C18O velocity gradients across the face of\neach core, usually interpreted as rotation. We note a correlation between the\ndirections of the identified gradients and outflows across protostars,\nindicating we may not have a purely rotational signature. The fitted gradients\nare larger than found in previous work, probably as a result of the higher\nresolution of our data and/or outflow contamination. These gradients, if\ninterpreted solely in terms of rotation, suggest that rotation is not\ndynamically significant. Furthermore, derived specific angular momenta are\nsmaller than observed in previous studies, centred around j~0.001 km/s pc,\nwhich indicates we have identified lower levels of rotation, or that the C18O\nJ=3-2 line probes conditions significantly denser and/or colder than n~10^5 per\ncc and T~10 K.", "cat": "astro-ph.GA", "authors": ["Emily I. Curtis", "John S. Richer"]}, "844": {"id": "1206.7027v1", "title": "Gas emissions in Planck cold dust clumps---A Survey of the J=1-0 Transitions of $^{12}$CO, $^{13}$CO, and C$^{18}$O", "url": "http://arxiv.org/pdf/1206.7027v1", "date": "2012-06-29 13:44:07", "abs": "A survey toward 674 Planck cold clumps of the Early Cold Core Catalogue (ECC)\nin the J=1-0 transitions of $^{12}$CO, $^{13}$CO and C$^{18}$O has been carried\nout using the PMO 13.7 m telescope. 673 clumps were detected with the $^{12}$CO\nand $^{13}$CO, and 68% of the samples have C$^{18}$O emission. Additional\nvelocity components were also identified.A close consistency of the three line\npeak velocities was revealed for the first time. Kinematic distances are given\nout for all the velocity components and half of the clumps are located within\n0.5 and 1.5 kpc. Excitation temperatures range from 4 to 27 K, slightly larger\nthan those of $T_d$. Line width analysis shows that the majority of ECC clumps\nare low mass clumps. Column densities N$_{H_{2}}$ span from 10$^{20}$ to\n4.5$\\times10^{22}$ cm$^{-2}$ with an average value of\n(4.4$\\pm$3.6)$\\times10^{21}$ cm$^{-2}$. N$_{H_{2}}$ cumulative fraction\ndistribution deviates from the lognormal distribution, which is attributed to\noptical depth. The average abundance ratio of the $^{13}$CO to C$^{18}$O in\nthese clumps is 7.0$\\pm$3.8, higher than the terrestrial value. Dust and gas\nare well coupled in 95% of the clumps. Blue profile, red profile and line\nasymmetry in total was found in less than 10% of the clumps, generally\nindicating star formation is not developed yet. Ten clumps were mapped. Twelve\nvelocity components and 22 cores were obtained. Their morphologies include\nextended diffuse, dense isolated, cometary and filament, of which the last is\nthe majority. 20 cores are starless.Only 7 cores seem to be in gravitationally\nbound state. Planck cold clumps are the most quiescent among the samples of\nweak-red IRAS, infrared dark clouds, UC H{\\sc ii} region candidates, EGOs and\nmethanol maser sources, suggesting that Planck cold clumps have expanded the\nhorizon of cold Astronomy.", "cat": "astro-ph.SR", "authors": ["Yuefang Wu", "Tie Liu", "Fanyi Meng", "Di Li", "Sheng-Li Qin", "Bing-Gang Ju"]}, "845": {"id": "2303.16129v4", "title": "Unleashing the Power of Edge-Cloud Generative AI in Mobile Networks: A Survey of AIGC Services", "url": "http://arxiv.org/pdf/2303.16129v4", "date": "2023-10-31 13:37:40", "abs": "Artificial Intelligence-Generated Content (AIGC) is an automated method for\ngenerating, manipulating, and modifying valuable and diverse data using AI\nalgorithms creatively. This survey paper focuses on the deployment of AIGC\napplications, e.g., ChatGPT and Dall-E, at mobile edge networks, namely mobile\nAIGC networks, that provide personalized and customized AIGC services in real\ntime while maintaining user privacy. We begin by introducing the background and\nfundamentals of generative models and the lifecycle of AIGC services at mobile\nAIGC networks, which includes data collection, training, finetuning, inference,\nand product management. We then discuss the collaborative cloud-edge-mobile\ninfrastructure and technologies required to support AIGC services and enable\nusers to access AIGC at mobile edge networks. Furthermore, we explore\nAIGCdriven creative applications and use cases for mobile AIGC networks.\nAdditionally, we discuss the implementation, security, and privacy challenges\nof deploying mobile AIGC networks. Finally, we highlight some future research\ndirections and open issues for the full realization of mobile AIGC networks.", "cat": "cs.NI", "authors": ["Minrui Xu", "Hongyang Du", "Dusit Niyato", "Jiawen Kang", "Zehui Xiong", "Shiwen Mao", "Zhu Han", "Abbas Jamalipour", "Dong In Kim", "Xuemin Shen", "Victor C. M. Leung", "H. Vincent Poor"]}, "846": {"id": "1201.2954v1", "title": "The Galaxy Optical Luminosity Function from the AGN and Galaxy Evolution Survey (AGES)", "url": "http://arxiv.org/pdf/1201.2954v1", "date": "2012-01-12 19:26:10", "abs": "We present the galaxy optical luminosity function for the redshift range\n0.05-24$ mag are known to hold the key to the\ndetermination of the ultraviolet emissivity for the cosmic re-ionization. But\nonly a few have been identified so far because of the limitations on the survey\ndata. Here, we present the first results of the $z\\sim5$ faint quasar survey\nwith the Infrared Medium-deep Survey (IMS), which covers $\\sim100$ deg$^{2}$\nareas in $J$-band to the depths of $J_{\\rm AB}\\sim23$ mag. To improve selection\nmethods, the medium-band follow-up imaging has been carried out using the SED\ncamera for QUasars in Early uNiverse (SQUEAN) on the Otto Struve 2.1 m\nTelescope. The optical spectra of the candidates were obtained with 8-m class\ntelescopes. We newly discovered 10 quasars with $-25\n2\\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$) at 0.680.68, we find 5 OVI absorption systems along\nthe line of sight with identified galaxies lying at impact parameters of\n$b\\approx100-350$ kpc (proper), whilst we find a further 13 galaxies with no\nsignificant associated OVI absorption (i.e. $N({\\rm OVI})<10^{13.5-14}$\ncm$^{-2}$) in the same impact parameter and redshift range. We find a large\nscatter in the stellar mass and star-formation rates of the closest galaxies\nwith associated OVI. Whilst one of the OVI absorber systems is found to be\nassociated with a low mass galaxy group at $z\\approx1.08$, we infer that the\ndetected OVI absorbers typically lie in the proximity of dark matter halos of\nmasses $10^{11.5} {\\rm M_\\odot}\\lesssim M_{\\rm halo}\\lesssim10^{12} {\\rm\nM_\\odot}$.", "cat": "astro-ph.GA", "authors": ["R. M. Bielby", "J. P. Stott", "F. Cullen", "T. M. Tripp", "J. Burchett", "M. Fumagalli", "S. L. Morris", "N. Tejos", "R. A. Crain", "R. G. Bower", "J. X. Prochaska"]}, "889": {"id": "1201.1800v1", "title": "SHARDS: Survey for High-z Absorption Red & Dead Sources", "url": "http://arxiv.org/pdf/1201.1800v1", "date": "2012-01-09 15:28:50", "abs": "SHARDS, an ESO/GTC Large Program, is an ultra-deep (26.5 mag)\nspectro-photometric survey with GTC/OSIRIS designed to select and study massive\npassively evolving galaxies at z=1.0-2.3 in the GOODS-N field using a set of 24\nmedium-band filters (FWHM~17 nm) covering the 500-950 nm spectral range. Our\nobserving strategy has been planned to detect, for z>1 sources, the prominent\nMg absorption feature (at rest-frame ~280 nm), a distinctive, necessary, and\nsufficient feature of evolved stellar populations (older than 0.5 Gyr). These\nobservations are being used to: (1) derive for the first time an unbiased\nsample of high-z quiescent galaxies, which extends to fainter magnitudes the\nsamples selected with color techniques and spectroscopic surveys; (2) derive\naccurate ages and stellar masses based on robust measurements of spectral\nfeatures such as the Mg(UV) or D(4000) indices; (3) measure their redshift with\nan accuracy Delta(z)/(1+z)<0.02; and (4) study emission-line galaxies\n(starbursts and AGN) up to very high redshifts. The well-sampled optical SEDs\nprovided by SHARDS for all sources in the GOODS-N field are a valuable\ncomplement for current and future surveys carried out with other telescopes\n(e.g., Spitzer, HST, and Herschel).", "cat": "astro-ph.CO", "authors": ["Pablo G. P\u00e9rez-Gonz\u00e1lez", "Antonio Cava", "the SHARDS Team"]}, "890": {"id": "2204.02765v3", "title": "Code Search: A Survey of Techniques for Finding Code", "url": "http://arxiv.org/pdf/2204.02765v3", "date": "2022-10-05 13:17:29", "abs": "The immense amounts of source code provide ample challenges and opportunities\nduring software development. To handle the size of code bases, developers\ncommonly search for code, e.g., when trying to find where a particular feature\nis implemented or when looking for code examples to reuse. To support\ndevelopers in finding relevant code, various code search engines have been\nproposed. This article surveys 30 years of research on code search, giving a\ncomprehensive overview of challenges and techniques that address them. We\ndiscuss the kinds of queries that code search engines support, how to\npreprocess and expand queries, different techniques for indexing and retrieving\ncode, and ways to rank and prune search results. Moreover, we describe\nempirical studies of code search in practice. Based on the discussion of prior\nwork, we conclude the article with an outline of challenges and opportunities\nto be addressed in the future.", "cat": "cs.SE", "authors": ["Luca Di Grazia", "Michael Pradel"]}, "891": {"id": "0709.4219v1", "title": "Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys", "url": "http://arxiv.org/pdf/0709.4219v1", "date": "2007-09-26 17:31:53", "abs": "We have searched for in-falling stellar streams on to the local Milky Way\ndisc in the CORAVEL and RAVE surveys. The CORAVEL survey consists of local\ndwarf stars (Nordstrom et al. Geneva-Copenhagen survey) and local Famaey et al.\ngiant stars. We select RAVE stars with radial velocities that are sensitive to\nthe Galactic vertical space velocity (Galactic latitude b < -45 deg). Kuiper\nstatistics have been employed to test the symmetry of the Galactic vertical\nvelocity distribution functions in these samples for evidence of a net vertical\nflow that could be associated with a (tidal?) stream of stars with vertically\ncoherent kinematics. In contrast to the `Field of Streams' found in the outer\nhalo, we find that the local volumes of the solar neighbourhood sampled by the\nCORAVEL dwarfs (complete within ~3 x 10^-4 kpc^3), CORAVEL giants (complete\nwithin ~5 x 10^-2 kpc^3) and RAVE (5-15% complete within ~8 kpc^3) are devoid\nof any vertically coherent streams containing hundreds of stars. This is\nsufficiently sensitive to allow our RAVE sample to rule out the passing of the\ntidal stream of the disrupting Sagittarius (Sgr) dwarf galaxy through the solar\nneighbourhood. This agrees with the most recent determination of its orbit and\ndissociates it from the Helmi et al. halo stream. Our constraints on the\nabsence of the Sgr stream near the Sun could prove a useful tool for\ndiscriminating between Galactic potential models. The lack of a net vertical\nflow through the solar neighbourhood in the CORAVEL giants and RAVE samples\nargues against the Virgo overdensity crossing the disc near the Sun. There are\nno vertical streams in the CORAVEL giants and RAVE samples with stellar\ndensities >1.6 x 10^4 and 1.5 x 10^3 stars kpc^-3 respectively and therefore no\nevidence for locally enhanced dark matter.", "cat": "astro-ph", "authors": ["G. M. Seabroke", "G. Gilmore", "A. Siebert", "O. Bienayme", "J. Binney", "J. Bland-Hawthorn", "R. Campbell", "K. C. Freeman", "B. Gibson", "E. K. Grebel", "A. Helmi", "U. Munari", "J. F. Navarro", "Q. A. Parker", "A. Siviero", "M. Steinmetz", "F. G. Watson", "R. F. G. Wyse", "T. Zwitter", "J. Penarrubia", "M. C. Smith", "M. Williams"]}, "892": {"id": "2110.00111v1", "title": "Deep Learning-based Action Detection in Untrimmed Videos: A Survey", "url": "http://arxiv.org/pdf/2110.00111v1", "date": "2021-09-30 22:42:25", "abs": "Understanding human behavior and activity facilitates advancement of numerous\nreal-world applications, and is critical for video analysis. Despite the\nprogress of action recognition algorithms in trimmed videos, the majority of\nreal-world videos are lengthy and untrimmed with sparse segments of interest.\nThe task of temporal activity detection in untrimmed videos aims to localize\nthe temporal boundary of actions and classify the action categories. Temporal\nactivity detection task has been investigated in full and limited supervision\nsettings depending on the availability of action annotations. This paper\nprovides an extensive overview of deep learning-based algorithms to tackle\ntemporal action detection in untrimmed videos with different supervision levels\nincluding fully-supervised, weakly-supervised, unsupervised, self-supervised,\nand semi-supervised. In addition, this paper also reviews advances in\nspatio-temporal action detection where actions are localized in both temporal\nand spatial dimensions. Moreover, the commonly used action detection benchmark\ndatasets and evaluation metrics are described, and the performance of the\nstate-of-the-art methods are compared. Finally, real-world applications of\ntemporal action detection in untrimmed videos and a set of future directions\nare discussed.", "cat": "cs.CV", "authors": ["Elahe Vahdani", "Yingli Tian"]}, "893": {"id": "2304.06452v2", "title": "Origin of neutron capture elements with the Gaia-ESO survey: the evolution of s- and r-process elements across the Milky Way", "url": "http://arxiv.org/pdf/2304.06452v2", "date": "2023-08-28 09:39:22", "abs": "We study the abundance patterns and the radial gradients of s-process\nelements (Y, Zr, Ba, La and Ce), r-process elements (Eu) and mixed-process\nelements (Mo, Nd and Pr) in the Galactic thin disc by means of a detailed\ntwo-infall chemical evolution model for the Milky Way with state-of-the-art\nnucleosynthesis prescriptions. We consider r-process nucleosynthesis from\nmerging neutron stars (MNS), magneto-rotational supernovae (MR-SNe) and\ns-process synthesis from low- and intermediate- mass stars (LIMS) and rotating\nmassive stars. The predictions of our model are compared with data from the\nsixth data release of the Gaia-ESO survey, from which we consider 62 open\nclusters with age > 0.1 Gyr and 1300 Milky Way disc field stars. We conclude\nthat: i) the [Eu/Fe] vs. [Fe/H] is reproduced by both a prompt and a delayed\nsource, but the quick source completely dominates the Eu production; ii)\nrotation in massive stars contribute substantially to the s-process elements of\nthe first peak, but MNS and MR-SNe are necessary in order to reproduce the\nobservations; iii) due to the adopted yields, our model overpredicts Pr and\nunderpredicts Nd, while the [Mo/Fe] vs. [Fe/H] is nicely reproduced. For the\nradial gradients, we conclude that: i) our predicted slope of the [Fe/H]\ngradient is in agreement with the one observed in open clusters by Gaia-ESO and\nother high-resolution spectroscopic surveys. ii) The predicted slope of the\n[Eu/H] radial gradient is steeper than the observed one, independently on how\nquick the production of Eu is. We discuss the possible causes of this\ndiscrepancy in terms of both different Galaxy formation scenarios and stellar\nradial migration effects. iii) For all the elements belonging to the second\ns-process peak (Ba, La, Ce) as well as for Pr, we predict a plateau at low\nGalactocentric distances, which is probably due to the enhanced enrichment from\nLIMS in the inner regions.", "cat": "astro-ph.GA", "authors": ["Marta Molero", "Laura Magrini", "Francesca Matteucci", "Donatella Romano", "Marco Palla", "Gabriele Cescutti", "Carlos Viscasillas V\u00e1zquez", "Emanuele Spitoni"]}, "894": {"id": "1403.6593v1", "title": "A new distant Milky Way globular cluster in the Pan-STARRS1 3\u03c0 survey", "url": "http://arxiv.org/pdf/1403.6593v1", "date": "2014-03-26 09:04:30", "abs": "We present a new satellite in the outer halo of the Galaxy, the first Milky\nWay satellite found in the stacked photometric catalog of the Panoramic Survey\nTelescope and Rapid Response System 1 (Pan-STARRS1) Survey. From follow-up\nphotometry obtained with WFI on the MPG/ESO 2.2m telescope, we argue that the\nobject, located at a heliocentric distance of 145+/-17 kpc, is the most distant\nMilky Way globular cluster yet known. With a total magnitude of M_V=-4.3+/-0.2\nand a half-light radius of 20+/-2 pc, it shares the properties of extended\nglobular clusters found in the outer halo of our Galaxy and the Andromeda\ngalaxy. The discovery of this distant cluster shows that the full spatial\nextent of the Milky Way globular cluster system has not yet been fully\nexplored.", "cat": "astro-ph.GA", "authors": ["Benjamin P. M. Laevens", "Nicolas F. Martin", "Branimir Sesar", "Edouard J. Bernard", "Hans-Walter Rix", "Colin T. Slater", "Eric F. Bell", "Annette M. N. Ferguson", "Edward F. Schlafly", "William S. Burgett", "Kenneth C. Chambers", "Larry Denneau", "Peter W. Draper", "Nicholas Kaiser", "Rolf-Peter Kudritzki", "Eugene A. Magnier", "Nigel Metcalfe", "Jeffrey S. Morgan", "Paul A. Price", "William E. Sweeney", "John L. Tonry", "Richard J. Wainscoat", "Christopher Waters"]}, "895": {"id": "1110.4043v2", "title": "A survey of the parameter space of the compressible liquid drop model as applied to the neutron star inner crust", "url": "http://arxiv.org/pdf/1110.4043v2", "date": "2012-12-18 23:43:02", "abs": "We present a systematic survey the range of predictions of the neutron star\ninner crust composition, crust-core transition densities and pressures, and\ndensity range of the nuclear `pasta' phases at the bottom of the crust provided\nby the compressible liquid drop model in the light of current experimental and\ntheoretical constraints on model parameters. Using a Skyrme-like model for\nnuclear matter, we construct baseline sequences of crust models by consistently\nvarying the density dependence of the bulk symmetry energy at nuclear\nsaturation density, $L$, under two conditions: (i) that the magnitude of the\nsymmetry energy at saturation density $J$ is held constant, and (ii) $J$\ncorrelates with $L$ under the constraint that the pure neutron matter (PNM) EoS\nsatisfies the results of ab-initio calculations at low densities. Such baseline\ncrust models facilitate consistent exploration of the $L$ dependence of crustal\nproperties. The remaining surface energy and symmetric nuclear matter\nparameters are systematically varied around the baseline, and different\nfunctional forms of the PNM EoS at sub-saturation densities implemented, to\nestimate theoretical `error bars' for the baseline predictions. Inner crust\ncomposition and transition densities are shown to be most sensitive to the\nsurface energy at very low proton fractions and to the behavior of the\nsub-saturation PNM EoS. Recent calculations of the energies of neutron drops\nsuggest that the low-proton-fraction surface energy might be higher than\npredicted in Skyrme-like models, which our study suggests may result in a\ngreatly reduced volume of pasta in the crust than conventionally predicted.", "cat": "astro-ph.SR", "authors": ["W. G. Newton", "M. Gearheart", "Bao-An Li"]}, "896": {"id": "1701.04652v1", "title": "A Survey of XML Tree Patterns", "url": "http://arxiv.org/pdf/1701.04652v1", "date": "2017-01-17 12:50:56", "abs": "With XML becoming an ubiquitous language for data interoperability purposes\nin various domains, efficiently querying XML data is a critical issue. This has\nlead to the design of algebraic frameworks based on tree-shaped patterns akin\nto the tree-structured data model of XML. Tree patterns are graphic\nrepresentations of queries over data trees. They are actually matched against\nan input data tree to answer a query. Since the turn of the twenty-first\ncentury, an astounding research effort has been focusing on tree pattern models\nand matching optimization (a primordial issue). This paper is a comprehensive\nsurvey of these topics, in which we outline and compare the various features of\ntree patterns. We also review and discuss the two main families of approaches\nfor optimizing tree pattern matching, namely pattern tree minimization and\nholistic matching. We finally present actual tree pattern-based developments,\nto provide a global overview of this significant research topic.", "cat": "cs.DB", "authors": ["Marouane Hachicha", "J\u00e9r\u00f4me Darmont"]}, "897": {"id": "1807.08209v2", "title": "The HOSTS Survey for Exozodiacal Dust: Preliminary results and future prospects", "url": "http://arxiv.org/pdf/1807.08209v2", "date": "2018-08-19 19:48:50", "abs": "[abridged] The presence of large amounts of dust in the habitable zones of\nnearby stars is a significant obstacle for future exo-Earth imaging missions.\nWe executed an N band nulling interferometric survey to determine the typical\namount of such exozodiacal dust around a sample of nearby main sequence stars.\nThe majority of our data have been analyzed and we present here an update of\nour ongoing work. We find seven new N band excesses in addition to the high\nconfidence confirmation of three that were previously known. We find the first\ndetections around Sun-like stars and around stars without previously known\ncircumstellar dust. Our overall detection rate is 23%. The inferred occurrence\nrate is comparable for early type and Sun-like stars, but decreases from 71%\n[+11%/-20%] for stars with previously detected mid- to far-infrared excess to\n11% [+9%/-4%] for stars without such excess, confirming earlier results at high\nconfidence. For completed observations on individual stars, our sensitivity is\nfive to ten times better than previous results. Assuming a lognormal luminosity\nfunction of the dust, we find upper limits on the median dust level around all\nstars without previously known mid to far infrared excess of 11.5 zodis at 95%\nconfidence level. The corresponding upper limit for Sun-like stars is 16 zodis.\nAn LBTI vetted target list of Sun-like stars for exo-Earth imaging would have a\ncorresponding limit of 7.5 zodis. We provide important new insights into the\noccurrence rate and typical levels of habitable zone dust around main sequence\nstars. Exploiting the full range of capabilities of the LBTI provides a\ncritical opportunity for the detailed characterization of a sample of\nexozodiacal dust disks to understand the origin, distribution, and properties\nof the dust.", "cat": "astro-ph.EP", "authors": ["S. Ertel", "G. M. Kennedy", "D. Defr\u00e8re", "P. Hinz", "A. B. Shannon", "B. Mennesson", "W. C. Danchi", "C. Gelino", "J. M. Hill", "W. F. Hoffmann", "G. Rieke", "E. Spalding", "J. M. Stone", "A. Vaz", "A. J. Weinberger", "P. Willems", "O. Absil", "P. Arbo", "V. P. Bailey", "C. Beichman", "G. Bryden", "E. C. Downey", "O. Durney", "S. Esposito", "A. Gaspar", "P. Grenz", "C. A. Haniff", "J. M. Leisenring", "L. Marion", "T. J. McMahon", "R. Millan-Gabet", "M. Montoya", "K. M. Morzinski", "E. Pinna", "J. Power", "A. Puglisi", "A. Roberge", "E. Serabyn", "A. J. Skemer", "K. Stapelfeldt", "K. Y. L. Su", "V. Vaitheeswaran", "M. C. Wyatt"]}, "898": {"id": "2307.06643v2", "title": "Nowcasting Temporal Trends Using Indirect Surveys", "url": "http://arxiv.org/pdf/2307.06643v2", "date": "2023-12-14 08:45:27", "abs": "Indirect surveys, in which respondents provide information about other people\nthey know, have been proposed for estimating (nowcasting) the size of a\n\\emph{hidden population} where privacy is important or the hidden population is\nhard to reach. Examples include estimating casualties in an earthquake,\nconditions among female sex workers, and the prevalence of drug use and\ninfectious diseases. The Network Scale-up Method (NSUM) is the classical\napproach to developing estimates from indirect surveys, but it was designed for\none-shot surveys. Further, it requires certain assumptions and asking for or\nestimating the number of individuals in each respondent's network. In recent\nyears, surveys have been increasingly deployed online and can collect data\ncontinuously (e.g., COVID-19 surveys on Facebook during much of the pandemic).\nConventional NSUM can be applied to these scenarios by analyzing the data\nindependently at each point in time, but this misses the opportunity of\nleveraging the temporal dimension. We propose to use the responses from\nindirect surveys collected over time and develop analytical tools (i) to prove\nthat indirect surveys can provide better estimates for the trends of the hidden\npopulation over time, as compared to direct surveys and (ii) to identify\nappropriate temporal aggregations to improve the estimates. We demonstrate\nthrough extensive simulations that our approach outperforms traditional NSUM\nand direct surveying methods. We also empirically demonstrate the superiority\nof our approach on a real indirect survey dataset of COVID-19 cases.", "cat": "cs.SI", "authors": ["Ajitesh Srivastava", "Juan Marcos Ram\u00edrez", "Sergio D\u00edaz-Aranda", "Jose Aguilar", "Antonio Ortega", "Antonio Fern\u00e1ndez Anta", "Rosa Elvira Lillo"]}, "899": {"id": "1904.11726v3", "title": "Statistics of roughness for fluctuating interfaces: A survey of different scaling analyses", "url": "http://arxiv.org/pdf/1904.11726v3", "date": "2021-07-21 15:51:58", "abs": "Ferroic domain walls are known to display the characteristic scaling\nproperties of self-affine rough interfaces. Different methods have been used to\nextract roughness information in ferroelectric and ferromagnetic materials.\nHere, we review these different approaches, comparing roughness scaling\nanalysis based on displacement autocorrelation functions in real space, both\nlocally and globally, to reciprocal space methods. This allows us to address\nimportant practical issues such as the necessity of a sufficient statistical\naveraging. As an ideal, artifact-free reference case and particularly targeting\nfinite-size systems, we consider two cases of numerically simulated interfaces,\none in equilibrium with a disordered energy landscape and one corresponding to\nthe critical depinning state when the external applied driving force equals the\ndepinning force. We find that the use of the reciprocal space methods based on\nthe structure factor allows the most robust extraction of the roughness\nexponent when enough statistics is available, while real space analysis based\non the roughness function allows the most efficient exploitation of a dataset\ncontaining only a limited number of interfaces of variable length. This\ninformation is thus important for properly quantifying roughness exponents in\nferroic materials.", "cat": "cond-mat.dis-nn", "authors": ["J. Guyonnet", "E. Agoritsas", "P. Paruch", "S. Bustingorry"]}, "900": {"id": "1208.4740v1", "title": "The Brightest of Reionizing Galaxies (BoRG) survey", "url": "http://arxiv.org/pdf/1208.4740v1", "date": "2012-08-23 13:06:15", "abs": "Until now, investigating the early stages of galaxy formation has been\nprimarily the realm of theoretical modeling and computer simulations, which\nrequire many physical ingredients and are challenging to test observationally.\nHowever, the latest Hubble Space Telescope observations in the near infrared\nare shedding new light on the properties of galaxies within the first billion\nyears after the Big Bang, including our recent discovery of the most distant\nproto-cluster of galaxies at redshift z~8. Here, I compare predictions from\nmodels of primordial and metal-enriched star formation during the dark ages\nwith the latest Hubble observations of galaxies during the epoch of\nreionization. I focus in particular on the luminosity function and on galaxy\nclustering as measured from our Hubble Space Telescope Brightest of Reionizing\nGalaxies (BoRG) survey. BoRG has the largest area coverage to find luminous and\nrare z~8 sources that are among the first galaxies to have formed in the\nUniverse.", "cat": "astro-ph.CO", "authors": ["M. Trenti"]}, "901": {"id": "1804.06484v2", "title": "The APOGEE-2 Survey of the Orion Star Forming Complex: I. Target Selection and Validation with early observations", "url": "http://arxiv.org/pdf/1804.06484v2", "date": "2018-04-19 01:49:43", "abs": "The Orion Star Forming Complex (OSFC) is a central target for the APOGEE-2\nYoung Cluster Survey. Existing membership catalogs span limited portions of the\nOSFC, reflecting the difficulty of selecting targets homogeneously across this\nextended, highly structured region. We have used data from wide field\nphotometric surveys to produce a less biased parent sample of young stellar\nobjects (YSOs) with infrared (IR) excesses indicative of warm circumstellar\nmaterial or photometric variability at optical wavelengths across the full 420\nsquare degrees extent of the OSFC. When restricted to YSO candidates with H <\n12.4, to ensure S/N ~100 for a six visit source, this uniformly selected sample\nincludes 1307 IR excess sources selected using criteria vetted by Koenig &\nLiesawitz and 990 optical variables identified in the Pan-STARRS1 3$\\pi$\nsurvey: 319 sources exhibit both optical variability and evidence of\ncircumstellar disks through IR excess. Objects from this uniformly selected\nsample received the highest priority for targeting, but required fewer than\nhalf of the fibers on each APOGEE-2 plate. We fill the remaining fibers with\npreviously confirmed and new color-magnitude selected candidate OSFC members.\nRadial velocity measurements from APOGEE-1 and new APOGEE-2 observations taken\nin the survey's first year indicate that ~90% of the uniformly selected targets\nhave radial velocities consistent with Orion membership.The APOGEE-2 Orion\nsurvey will include >1100 bona fide YSOs whose uniform selection function will\nprovide a robust sample for comparative analyses of the stellar populations and\nproperties across all sub-regions of Orion.", "cat": "astro-ph.GA", "authors": ["J'Neil Cottle", "Kevin R. Covey", "Genaro Su\u00e1rez", "Carlos Rom\u00e1n-Z\u00fa\u00f1iga", "Edward Schlafly", "Juan Jose Downes", "Jason E. Ybarra", "Jesus Hernandez", "Keivan Stassun", "Guy S. Stringfellow", "Konstantin Getman", "Eric Feigelson", "Jura Borissova", "J. Serena Kim", "A. Roman-Lopes", "Nicola Da Rio", "Nathan De Lee", "Peter M. Frinchaboy", "Marina Kounkel", "Steven R. Majewski", "Ronald E. Mennickent", "David L. Nidever", "Christian Nitschelm", "Kaike Pan", "Matthew Shetrone", "Gail Zasowski", "Ken Chambers", "Eugene Magnier", "Jeff Valenti"]}, "902": {"id": "1407.1980v1", "title": "Automatic stellar spectral parameterization pipeline for LAMOST survey", "url": "http://arxiv.org/pdf/1407.1980v1", "date": "2014-07-08 07:43:04", "abs": "The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)\nproject performed its five year formal survey since Sep. 2012, already\nfulfilled the pilot survey and the 1st two years general survey with an output\n- spectroscopic data archive containing about 3.5 million observations. One of\nthe scientific objectives of the project is for better understanding the\nstructure and evolution of the Milky Way. Thus, credible derivation of the\nphysical properties of the stars plays a key role for the exploration. We\ndeveloped and implemented the LAMOST stellar parameter pipeline (LASP) which\ncan automatically determine the fundamental stellar atmospheric parameters\n(effective temperature Teff, surface gravity log g, metallicity [Fe/H], radial\nvelocity Vr) for late A, FGK type stars observed during the survey. An overview\nof the LASP, including the strategy, the algorithm and the process is presented\nin this work.", "cat": "astro-ph.IM", "authors": ["Yue Wu", "Ali Luo", "Bing Du", "Yongheng Zhao", "Hailong Yuan"]}, "903": {"id": "1601.01498v1", "title": "Security and Privacy of Sensitive Data in Cloud Computing: A Survey of Recent Developments", "url": "http://arxiv.org/pdf/1601.01498v1", "date": "2016-01-07 11:53:20", "abs": "Cloud computing is revolutionizing many ecosystems by providing organizations\nwith computing resources featuring easy deployment, connectivity,\nconfiguration, automation and scalability. This paradigm shift raises a broad\nrange of security and privacy issues that must be taken into consideration.\nMulti-tenancy, loss of control, and trust are key challenges in cloud computing\nenvironments. This paper reviews the existing technologies and a wide array of\nboth earlier and state-of-the-art projects on cloud security and privacy. We\ncategorize the existing research according to the cloud reference architecture\norchestration, resource control, physical resource, and cloud service\nmanagement layers, in addition to reviewing the existing developments in\nprivacy-preserving sensitive data approaches in cloud computing such as privacy\nthreat modeling and privacy enhancing protocols and solutions.", "cat": "cs.CR", "authors": ["Ali Gholami", "Erwin Laure"]}, "904": {"id": "2106.13591v1", "title": "The Problem of Distributed Consensus: A Survey", "url": "http://arxiv.org/pdf/2106.13591v1", "date": "2021-06-24 17:03:26", "abs": "A survey is given of approaches to the problem of distributed consensus,\nfocusing particularly on methods based on cellular automata and related\nsystems. A variety of new results are given, as well as a history of the field\nand an extensive bibliography. Distributed consensus is of current relevance in\na new generation of blockchain-related systems.", "cat": "cs.DC", "authors": ["Stephen Wolfram"]}, "905": {"id": "1312.5693v1", "title": "Pricing of vanilla and first generation exotic options in the local stochastic volatility framework: survey and new results", "url": "http://arxiv.org/pdf/1312.5693v1", "date": "2013-12-19 18:47:32", "abs": "Stochastic volatility (SV) and local stochastic volatility (LSV) processes\ncan be used to model the evolution of various financial variables such as FX\nrates, stock prices, and so on. Considerable efforts have been devoted to\npricing derivatives written on underliers governed by such processes. Many\nissues remain, though, including the efficacy of the standard alternating\ndirection implicit (ADI) numerical methods for solving SV and LSV pricing\nproblems. In general, the amount of required computations for these methods is\nvery substantial. In this paper we address some of these issues and propose a\nviable alternative to the standard ADI methods based on Galerkin-Ritz ideas. We\nalso discuss various approaches to solving the corresponding pricing problems\nin a semi-analytical fashion. We use the fact that in the zero correlation case\nsome of the pricing problems can be solved analytically, and develop a\nclosed-form series expansion in powers of correlation. We perform a thorough\nbenchmarking of various numerical solutions by using analytical and\nsemi-analytical solutions derived in the paper.", "cat": "q-fin.CP", "authors": ["Alexander Lipton", "Andrey Gal", "Andris Lasis"]}, "906": {"id": "1309.4774v2", "title": "The FMOS-COSMOS survey of star-forming galaxies at z ~ 1.6. I. H\u03b1 -based star formation rates and dust extinction", "url": "http://arxiv.org/pdf/1309.4774v2", "date": "2014-03-25 14:41:31", "abs": "We present the first results from a near-IR spectroscopic survey of the\nCOSMOS field, using the Fiber Multi-Object Spectrograph on the Subaru\ntelescope, designed to characterize the star-forming galaxy population at\n$1.43) SMGs. We derive a\nsimple redshift estimator for SMGs based on the 3.6 and 8um fluxes, which is\naccurate to Delta_z~0.4 for SMGs at z<4. A statistical analysis of sources\naround unidentified SMGs identifies a population of likely counterparts with a\nredshift distribution peaking at z=2.5\\pm0.3, which likely comprises ~60% of\nthe unidentified SMGs. This confirms that the bulk of the undetected SMGs are\ncoeval with those detected in the radio/mid-IR. We conclude that ~15% of all\nthe SMGs are below the flux limits of our survey and lie at z>3 and hence ~30%\nof all SMGs have z>3. We estimate that the full S_870um>4mJy SMG population has\na median redshift of 2.5\\pm0.6. In contrast to previous suggestions we find no\nsignificant correlation between S_870um and redshift. The median stellar mass\nof the SMGs derived from SED fitting is (9.2\\pm0.9)x10^10Msun and the\ninterquartile range is (4.7-14)x10^10Msun, although we caution that uncertainty\nin the star-formation histories results in a factor of ~5 uncertainty in these\nstellar masses. The median characteristic dust temperature of SMGs is\n35.9\\pm1.4K and the interquartile range is 28.5-43.3K. The infrared luminosity\nfunction shows that SMGs at z=2-3 typically have higher far-IR luminosities and\nluminosity density than those at z=1-2. This is mirrored in the evolution of\nthe star-formation rate density (SFRD) for SMGs which peaks at z~2. The maximum\ncontribution of bright SMGs to the global SFRD (~5% for SMGs with S_870um>4mJy;\n~50% for SMGs with S_870um>1mJy) also occurs at z~2.", "cat": "astro-ph.CO", "authors": ["J. L. Wardlow", "Ian Smail", "K. E. K. Coppin", "D. M. Alexander", "W. N. Brandt", "A. L. R. Danielson", "B. Luo", "A. M. Swinbank", "F. Walter", "A. Weiss", "Y. Q. Xue", "S. Zibetti", "F. Bertoldi", "A. D. Biggs", "S. C. Chapman", "H. Dannerbauer", "J. S. Dunlop", "E. Gawiser", "R. J. Ivison", "K. K. Knudsen", "A. Kovacs", "C. G. Lacey", "K. M. Menten", "N. Padilla", "H. -W. Rix", "P. P. van der Werf"]}, "912": {"id": "1408.5900v1", "title": "HST-COS Observations of AGN. II. Extended Survey of Ultraviolet Composite Spectra from 159 Active Galactic Nuclei", "url": "http://arxiv.org/pdf/1408.5900v1", "date": "2014-08-25 20:00:06", "abs": "The ionizing fluxes from quasars and other active galactic nuclei (AGN) are\ncritical for interpreting their emission-line spectra and for photoionizing and\nheating the intergalactic medium (IGM). Using far-ultraviolet spectra from the\nCosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST), we\ndirectly measure the rest-frame ionizing continua and emission lines for 159\nAGN at redshifts 0.001 < z_AGN < 1.476 and construct a composite spectrum from\n475-1875A. We identify the underlying AGN continuum and strong EUV emission\nlines from ions of oxygen, neon, and nitrogen after masking out absorption\nlines from the HI Lya forest, 7 Lyman-limit systems (N_HI > 10^17.2 cm^-2) and\n214 partial Lyman-limit systems (15.0 < log N_HI < 17.2). The 159 AGN exhibit a\nwide range of FUV/EUV spectral shapes, F_nu \\propto nu^(alpha_nu), typically\nwith -2 < alpha_nu < 0 and no discernible continuum edges at 912A (H I) or 504A\n(He I). The composite rest-frame continuum shows a gradual break at 1000 A,\nwith mean spectral index alpha_nu = -0.83 +/- 0.09 in the FUV (1200-2000A)\nsteepening to alpha_nu = -1.41 +/- 0.15 in the EUV (500-1000A). We discuss the\nimplications of the UV flux turnovers and lack of continuum edges for the\nstructure of accretion disks, AGN mass inflow rates, and luminosities relative\nto Eddington values.", "cat": "astro-ph.GA", "authors": ["Matthew L. Stevans", "J. Michael Shull", "Charles W. Danforth", "Evan M. Tilton"]}, "913": {"id": "1202.2801v2", "title": "Comparing HARPS and Kepler surveys: The alignment of multiple-planet systems", "url": "http://arxiv.org/pdf/1202.2801v2", "date": "2012-03-30 16:40:43", "abs": "Aims. We study a subset of the planetary population characterized both by\nHARPS and Kepler surveys. We compare the statistical properties of planets in\nsystems with m.sin i >5-10 M_Earth and R>2 R_Earth. If we assume that the\nunderlying population has the same characteristics, the different detection\nsensitivity to the orbital inclination relative to the line of sight allows us\nto probe the planets' mutual inclination.\n Methods. We considered the frequency of systems with one, two and three\nplanets as dictated by HARPS data. We used Kepler's planetary period and host\nmass and radii distributions (corrected from detection bias) to model planetary\nsystems in a simple yet physically plausible way. We then varied the mutual\ninclination between planets in a system according to different prescriptions\n(completely aligned, Rayleigh distributions and isotropic) and compared the\ntransit frequencies with one, two or three planets with those measured by\nKepler.\n Results. The results show that the two datasets are compatible, a remarkable\nresult especially because there are no tunable knobs other than the assumed\ninclination distribution. For m.sin i cutoffs of 7-10 M_Earth, which are those\nexpected to correspond to the radius cutoff of 2 R_Earth, we conclude that the\nresults are better described by a Rayleigh distribution with mode of 1 deg or\nsmaller. We show that the best-fit scenario only becomes a Rayleigh\ndistribution with mode of 5 deg if we assume a rather extreme mass-radius\nrelationship for the planetary population.\n Conclusions. These results have important consequences for our understanding\nof the role of several proposed formation and evolution mechanisms. They\nconfirm that planets are likely to have been formed in a disk and show that\nmost planetary systems evolve quietly without strong angular momentum exchanges\n(abridged).", "cat": "astro-ph.EP", "authors": ["P. Figueira", "M. Marmier", "G. Bou\u00e9", "C. Lovis", "N. C. Santos", "M. Montalto", "S. Udry", "F. Pepe", "M. Mayor"]}, "914": {"id": "2303.02063v2", "title": "Physics-Informed Deep Learning For Traffic State Estimation: A Survey and the Outlook", "url": "http://arxiv.org/pdf/2303.02063v2", "date": "2023-07-01 18:59:06", "abs": "For its robust predictive power (compared to pure physics-based models) and\nsample-efficient training (compared to pure deep learning models),\nphysics-informed deep learning (PIDL), a paradigm hybridizing physics-based\nmodels and deep neural networks (DNN), has been booming in science and\nengineering fields. One key challenge of applying PIDL to various domains and\nproblems lies in the design of a computational graph that integrates physics\nand DNNs. In other words, how physics are encoded into DNNs and how the physics\nand data components are represented. In this paper, we provide a variety of\narchitecture designs of PIDL computational graphs and how these structures are\ncustomized to traffic state estimation (TSE), a central problem in\ntransportation engineering. When observation data, problem type, and goal vary,\nwe demonstrate potential architectures of PIDL computational graphs and compare\nthese variants using the same real-world dataset.", "cat": "cs.LG", "authors": ["Xuan Di", "Rongye Shi", "Zhaobin Mo", "Yongjie Fu"]}, "915": {"id": "2401.09218v1", "title": "Complexity of some algorithmic problems in groups: a survey", "url": "http://arxiv.org/pdf/2401.09218v1", "date": "2024-01-17 13:58:22", "abs": "In this survey, we address the worst-case, average-case, and generic-case\ntime complexity of the word problem and some other algorithmic problems in\nseveral classes of groups and show that it is often the case that the\naverage-case complexity of the word problem is linear with respect to the\nlength of an input word, which is as good as it gets if one considers groups\ngiven by generators and defining relations. At the same time, there are other\nnatural algorithmic problems, for instance, the geodesic (decision) problem or\nWhitehead's automorphism problem, where the average-case time complexity can be\nsublinear, even constant.", "cat": "math.GR", "authors": ["Vladimir Shpilrain"]}, "916": {"id": "1705.03751v1", "title": "A Survey of Distant Supervision Methods using PGMs", "url": "http://arxiv.org/pdf/1705.03751v1", "date": "2017-05-10 13:19:38", "abs": "Relation Extraction refers to the task of populating a database with tuples\nof the form $r(e_1, e_2)$, where $r$ is a relation and $e_1$, $e_2$ are\nentities. Distant supervision is one such technique which tries to\nautomatically generate training examples based on an existing KB such as\nFreebase. This paper is a survey of some of the techniques in distant\nsupervision which primarily rely on Probabilistic Graphical Models (PGMs).", "cat": "cs.AI", "authors": ["Gagan Madan"]}, "917": {"id": "2408.14005v1", "title": "The Calibration of Polycyclic Aromatic Hydrocarbon Dust Emission as a Star Formation Rate Indicator in the AKARI NEP Survey", "url": "http://arxiv.org/pdf/2408.14005v1", "date": "2024-08-26 04:15:12", "abs": "Polycyclic aromatic hydrocarbon (PAH) dust emission has been proposed as an\neffective extinction-independent star formation rate (SFR) indicator in the\nmid-infrared (MIR), but this may depend on conditions in the interstellar\nmedium. The coverage of the AKARI/Infrared Camera (IRC) allows us to study the\neffects of metallicity, starburst intensity, and active galactic nuclei on PAH\nemission in galaxies with $f_{\\nu}(L18W)\\lesssim 19$ AB mag. Observations\ninclude follow-up, rest-frame optical spectra of 443 galaxies within the AKARI\nNorth Ecliptic Pole survey that have IRC detections from 7-24 $\\mu$m. We use\noptical emission line diagnostics to infer SFR based on H$\\alpha$ and [O\nII]$\\lambda\\lambda 3726,3729$ emission line luminosities. The PAH 6.2 $\\mu$m\nand PAH 7.7 $\\mu$m luminosities ($L(PAH\\ 6.2\\ \\mu m)$ and $L(PAH\\ 7.7\\ \\mu m)$,\nrespectively) derived using multi-wavelength model fits are consistent with\nthose derived from slitless spectroscopy within 0.2 dex. $L(PAH\\ 6.2\\ \\mu m)$\nand $L(PAH\\ 7.7\\ \\mu m)$ correlate linearly with the 24 $\\mu$m-dust corrected\nH$\\alpha$ luminosity only for normal, star-forming ``main-sequence\" galaxies.\nAssuming multi-linear correlations, we quantify the additional dependencies on\nmetallicity and starburst intensity, which we use to correct our PAH SFR\ncalibrations at $0 M_{AB}(B) > -18.8),\nextreme emission line galaxies (EELGs) at 0.2 < z < 0.9 identified by their\nunusually high rest-frame equivalent widths (100 < EW[OIII] < 1700 A) as part\nof the VIMOS Ultra Deep Survey (VUDS). VIMOS optical spectra of unprecedented\nsensitivity ($I_{AB}$ ~ 25 mag) along with multiwavelength photometry and HST\nimaging are used to investigate spectrophotometric properties of this unique\nsample and explore, for the first time, the very low stellar mass end (M* <\n10^8 M$_{\\odot}$) of the luminosity-metallicity (LZR) and mass-metallicity\n(MZR) relations at z < 1. Characterized by their extreme compactness (R50 < 1\nkpc), low stellar mass and enhanced specific star formation rates (SFR/M* ~\n10^{-9} - 10^{-7} yr^{-1}), the VUDS EELGs are blue dwarf galaxies likely\nexperiencing the first stages of a vigorous galaxy-wide starburst. Using\nT_e-sensitive direct and strong-line methods, we find that VUDS EELGs are\nlow-metallicity (7.5 < 12+log(O/H) < 8.3) galaxies with high ionization\nconditions, including at least three EELGs showing HeII 4686A emission and four\nEELGs of extremely metal-poor (<10% solar) galaxies. The LZR and MZR followed\nby EELGs show relatively large scatter, being broadly consistent with the\nextrapolation toward low luminosity and mass from previous studies at similar\nredshift. However, we find evidences that galaxies with younger and more\nvigorous star formation -- as characterized by their larger EWs, ionization and\nsSFR -- tend to be more metal-poor at a given stellar mass.", "cat": "astro-ph.GA", "authors": ["Ricardo Amor\u00edn", "V. Sommariva", "M. Castellano", "A. Grazian", "L. A. M. Tasca", "A. Fontana", "L. Pentericci", "P. Cassata", "B. Garilli", "V. Le Brun", "O. Le F\u00e8vre", "D. Maccagni", "R. Thomas", "E. Vanzella", "G. Zamorani", "E. Zucca", "S. Bardelli", "P. Capak", "L. Cassar\u00e1", "A. Cimatti", "J. G. Cuby", "O. Cucciati", "S. de la Torre", "A. Durkalec", "M. Giavalisco", "N. P. Hathi", "O. Ilbert", "B. C. Lemaux", "C. Moreau", "S. Paltani", "B. Ribeiro", "M. Salvato", "D. Schaerer", "M. Scodeggio", "M. Talia", "Y. Taniguchi", "L. Tresse", "D. Vergani", "P. W. Wang", "S. Charlot", "T. Contini", "S. Fotopoulou", "C. L\u00f3pez-Sanjuan", "Y. Mellier", "N. Scoville"]}, "919": {"id": "2008.00364v6", "title": "A Survey on Text Classification: From Shallow to Deep Learning", "url": "http://arxiv.org/pdf/2008.00364v6", "date": "2021-12-22 11:35:08", "abs": "Text classification is the most fundamental and essential task in natural\nlanguage processing. The last decade has seen a surge of research in this area\ndue to the unprecedented success of deep learning. Numerous methods, datasets,\nand evaluation metrics have been proposed in the literature, raising the need\nfor a comprehensive and updated survey. This paper fills the gap by reviewing\nthe state-of-the-art approaches from 1961 to 2021, focusing on models from\ntraditional models to deep learning. We create a taxonomy for text\nclassification according to the text involved and the models used for feature\nextraction and classification. We then discuss each of these categories in\ndetail, dealing with both the technical developments and benchmark datasets\nthat support tests of predictions. A comprehensive comparison between different\ntechniques, as well as identifying the pros and cons of various evaluation\nmetrics are also provided in this survey. Finally, we conclude by summarizing\nkey implications, future research directions, and the challenges facing the\nresearch area.", "cat": "cs.CL", "authors": ["Qian Li", "Hao Peng", "Jianxin Li", "Congying Xia", "Renyu Yang", "Lichao Sun", "Philip S. Yu", "Lifang He"]}, "920": {"id": "0906.1807v1", "title": "The zCOSMOS Survey. The dependence of clustering on luminosity and stellar mass at z=0.2-1", "url": "http://arxiv.org/pdf/0906.1807v1", "date": "2009-06-09 20:00:20", "abs": "We study the dependence of galaxy clustering on luminosity and stellar mass\nat redshifts z ~ [0.2-1] using the first zCOSMOS 10K sample.\n We measure the redshift-space correlation functions xi(rp,pi) and its\nprojection wp(rp) for sub-samples covering different luminosity, mass and\nredshift ranges. We quantify in detail the observational selection biases and\nwe check our covariance and error estimate techniques using ensembles of\nsemi-analytic mock catalogues. We finally compare our measurements to the\ncosmological model predictions from the mock surveys.\n At odds with other measurements, we find a weak dependence of galaxy\nclustering on luminosity in all redshift bins explored. A mild dependence on\nstellar mass is instead observed. At z~0.7, wp(rp) shows strong excess power on\nlarge scales. We interpret this as produced by large-scale structure dominating\nthe survey volume and extending preferentially in direction perpendicular to\nthe line-of-sight. We do not see any significant evolution with redshift of the\namplitude of clustering for bright and/or massive galaxies.\n The clustering measured in the zCOSMOS data at 0.5=10 is only marginally consistent with predictions from the mock\nsurveys. On scales larger than ~2 h^-1 Mpc, the observed clustering amplitude\nis compatible only with ~1% of the mocks. Thus, if the power spectrum of matter\nis LCDM with standard normalization and the bias has no unnatural\nscale-dependence, this result indicates that COSMOS has picked up a\nparticularly rare, ~2-3 sigma positive fluctuation in a volume of ~10^6 h^-1\nMpc^3. These findings underline the need for larger surveys of the z~1 Universe\nto appropriately characterize the level of structure at this epoch.", "cat": "astro-ph.CO", "authors": ["B. Meneux", "L. Guzzo", "S. de la Torre", "C. Porciani", "G. Zamorani", "U. Abbas", "M. Bolzonella", "B. Garilli", "A. Iovino", "L. Pozzetti", "E. Zucca", "S. Lilly", "O. Le Fevre", "J. -P. Kneib", "C. M. Carollo", "T. Contini", "V. Mainieri", "A. Renzini", "M. Scodeggio", "S. Bardelli", "A. Bongiorno", "K. Caputi", "G. Coppa", "O. Cucciati", "L. de Ravel", "P. Franzetti", "P. Kampczyk", "C. Knobel", "K. Kovac", "F. Lamareille", "J. -F. Le Borgne", "V. Le Brun", "C. Maier", "R. Pello", "Y. Peng", "E. Perez Montero", "E. Ricciardelli", "J. D. Silverman", "M. Tanaka", "L. Tasca", "L. Tresse", "D. Vergani", "D. Bottini", "A. Cappi", "A. Cimatti", "P. Cassata", "M. Fumana", "A. M. Koekemoer", "A. Leauthaud", "D. Maccagni", "C. Marinoni", "H. J. McCracken", "P. Memeo", "P. Oesch", "R. Scaramella"]}, "921": {"id": "0802.0497v1", "title": "The SCUBA HAlf Degree Extragalactic Survey (SHADES) - VII. Optical/IR photometry and stellar masses of sub-millimeter galaxies", "url": "http://arxiv.org/pdf/0802.0497v1", "date": "2008-02-04 21:27:42", "abs": "We present estimates of the photometric redshifts, stellar masses and star\nformation histories of sources in the SCUBA HAlf Degree Extragalactic Survey\n(SHADES). This paper describes the 60 SCUBA sources detected in the Lockman\nHole covering an area of ~320 square arcmin. Using photometry spanning the B\nband to 8um, we find that the average SCUBA source forms a significant fraction\nof its stars in an early period of star formation and that most of the\nremainder forms in a shorter more intense burst around the redshift it is\nobserved. This trend does not vary significantly with source redshift but the\nexact ratio of early to late mass is quite sensitive to the way extinction is\ntreated in the modelling. However, the sources show a clear increase in stellar\nmass with redshift, consistent with downsizing. In terms of SED types, only two\nout of the 51 sources we have obtained photometric redshifts for are best fit\nby a quasar-like spectral energy distribution, with approximately 80 per cent\nof the sources being best fit with late-type spectra (Sc, Im and starburst). By\nincluding photometry at 850um, we conclude that the average SCUBA source is\nforming stars at a rate somewhere between 6 and 30 times the rate implied from\nthe rest-frame optical in a dust obscured burst and that this burst creates\n15-65 per cent of the total stellar mass. Using a simplistic calculation, we\nestimate from the average star formation history that between one in five and\none in 15 bright (L_* +2 mag < L_optical < L_* -1 mag) galaxies in the field\nover the interval 0 < z < 3 will at some point in their lifetime experience a\nsimilar energetic dusty burst of star formation. Finally, we compute the\nevolution of the star formation rate density and find it peaks around z=2.", "cat": "astro-ph", "authors": ["Simon Dye", "S. A. Eales", "I. Aretxaga", "S. Serjeant", "J. S. Dunlop", "T. S. R. Babbedge", "S. C. Chapman", "M. Cirasuolo", "D. L. Clements", "K. E. K. Coppin", "L. Dunne", "E. Egami", "D. Farrah", "R. J. Ivison", "E. van Kampen", "A. Pope", "R. Priddey", "G. H. Rieke", "A. M. Schael", "D. Scott", "C. Simpson", "T. Takagi", "T. Takata", "M. Vaccari"]}, "922": {"id": "1802.02626v3", "title": "Interpolating Population Distributions using Public-use Data: An Application to Income Segregation using American Community Survey Data", "url": "http://arxiv.org/pdf/1802.02626v3", "date": "2021-11-23 16:25:29", "abs": "Income segregation measures the extent to which households choose to live\nnear other households with similar incomes. Sociologists theorize that income\nsegregation can exacerbate the impacts of income inequality, and have developed\nindices to measure it at the metro area level, including the information theory\nindex introduced in \\citet{reardon2011income}, and the divergence index\npresented in \\citet{roberto2015divergence}. To study their differences, we\nconstruct both indices using recent American Community Survey (ACS) estimates\nof features of the income distribution. Since the elimination of the decennial\ncensus long form, methods of computing these estimates must be updated to use\nACS estimates and account for survey error. We propose a model-based method to\ninterpolate estimates of features of the income distribution that accounts for\nthis error. This method improves on previous approaches by allowing for the use\nof more types of estimates, and by providing uncertainty quantification. We\napply this method to estimate U.S. census tract-level income distributions\nusing ACS tabulations, and in turn use these to construct both income\nsegregation indices. We find major differences between the two indices in the\nrelative ranking of metro areas, as well as differences in how both indices\ncorrelate with the Gini index.", "cat": "stat.ME", "authors": ["Matthew Simpson", "Scott H. Holan", "Christopher K. Wikle", "Jonathan R. Bradley"]}, "923": {"id": "0705.2773v1", "title": "A sharper view of the outer Galaxy at 1420 and 408 MHz from the Canadian Galactic Plane Survey - I. Revisiting the KR catalogue and new Gigahertz Peaked Spectrum Sources", "url": "http://arxiv.org/pdf/0705.2773v1", "date": "2007-05-18 20:07:26", "abs": "Arcminute-resolution radio continuum images at 408 and 1420 MHz from the\nCanadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources\nlisted in the Kallas and Reich (1980) catalogue. This catalogue is of\nparticular interest to Galactic studies as it lists both extended and compact\nradio sources found in the second Galactic quadrant. We have determined the\nnature (extended vs. compact, Galactic vs. extragalactic) of all of these\nbright radio sources. A number of large HII regions with no optical\ncounterparts are highlighted along with a sample of large radio galaxies. Many\nsources previously thought to be extended Galactic objects are shown to be\npoint sources. A sample of point sources with flat or rising spectra between\n408 and 1420 MHz has been compiled, and within this sample likely Gigahertz\nPeaked Spectrum sources have been identified.", "cat": "astro-ph", "authors": ["C. R. Kerton"]}, "924": {"id": "2004.13820v2", "title": "Evolution of Semantic Similarity -- A Survey", "url": "http://arxiv.org/pdf/2004.13820v2", "date": "2021-01-30 15:57:06", "abs": "Estimating the semantic similarity between text data is one of the\nchallenging and open research problems in the field of Natural Language\nProcessing (NLP). The versatility of natural language makes it difficult to\ndefine rule-based methods for determining semantic similarity measures. In\norder to address this issue, various semantic similarity methods have been\nproposed over the years. This survey article traces the evolution of such\nmethods, categorizing them based on their underlying principles as\nknowledge-based, corpus-based, deep neural network-based methods, and hybrid\nmethods. Discussing the strengths and weaknesses of each method, this survey\nprovides a comprehensive view of existing systems in place, for new researchers\nto experiment and develop innovative ideas to address the issue of semantic\nsimilarity.", "cat": "cs.CL", "authors": ["Dhivya Chandrasekaran", "Vijay Mago"]}, "925": {"id": "1408.1617v1", "title": "The First Source Counts at 18 microns from the AKARI NEP Survey", "url": "http://arxiv.org/pdf/1408.1617v1", "date": "2014-08-07 15:04:56", "abs": "We present the first galaxy counts at 18 microns using the Japanese AKARI\nsatellite's survey at the North Ecliptic Pole (NEP), produced from the images\nfrom the NEP-Deep and NEP-Wide surveys covering 0.6 and 5.8 square degrees\nrespectively. We describe a procedure using a point source filtering algorithm\nto remove background structure and a minimum variance method for our source\nextraction and photometry that delivers the optimum signal to noise for our\nextracted sources, confirming this by comparison with standard photometry\nmethods. The final source counts are complete and reliable over three orders of\nmagnitude in flux density, resulting in sensitivities (80 percent completeness)\nof 0.15mJy and 0.3mJy for the NEP-Deep and NEP-Wide surveys respectively, a\nfactor of 1.3 deeper than previous catalogues constructed from this field. The\ndifferential source counts exhibit a characteristic upturn from Euclidean\nexpectations at around a milliJansky and a corresponding evolutionary bump\nbetween 0.2-0.4 mJy consistent with previous mid-infrared surveys with ISO and\nSpitzer at 15 and 24 microns. We compare our results with galaxy evolution\nmodels confirming the striking divergence from the non-evolving scenario. The\nmodels and observations are in broad agreement implying that the source counts\nare consistent with a strongly evolving population of luminous infrared\ngalaxies at redshifts higher than unity. Integrating our source counts down to\nthe limit of the NEP survey at the 150 microJy level we calculate that AKARI\nhas resolved approximately 55 percent of the 18 micron cosmic infrared\nbackground relative to the predictions of contemporary source count models.", "cat": "astro-ph.GA", "authors": ["Chris Pearson", "S. Serjeant", "S. Oyabu", "H. Matsuhara", "T. Wada", "T. Goto", "T. Takagi", "H. M. Lee", "M. Im", "Y. Ohyama", "S. J. Kim", "K. Murata"]}, "926": {"id": "2310.14485v1", "title": "Intelligent Escape of Robotic Systems: A Survey of Methodologies, Applications, and Challenges", "url": "http://arxiv.org/pdf/2310.14485v1", "date": "2023-10-23 01:34:34", "abs": "Intelligent escape is an interdisciplinary field that employs artificial\nintelligence (AI) techniques to enable robots with the capacity to\nintelligently react to potential dangers in dynamic, intricate, and\nunpredictable scenarios. As the emphasis on safety becomes increasingly\nparamount and advancements in robotic technologies continue to advance, a wide\nrange of intelligent escape methodologies has been developed in recent years.\nThis paper presents a comprehensive survey of state-of-the-art research work on\nintelligent escape of robotic systems. Four main methods of intelligent escape\nare reviewed, including planning-based methodologies, partitioning-based\nmethodologies, learning-based methodologies, and bio-inspired methodologies.\nThe strengths and limitations of existing methods are summarized. In addition,\npotential applications of intelligent escape are discussed in various domains,\nsuch as search and rescue, evacuation, military security, and healthcare. In an\neffort to develop new approaches to intelligent escape, this survey identifies\ncurrent research challenges and provides insights into future research trends\nin intelligent escape.", "cat": "cs.RO", "authors": ["Junfei Li", "Simon X. Yang"]}, "927": {"id": "2210.14366v1", "title": "Joint Point and Variance Estimation under a Hierarchical Bayesian model for Survey Count Data", "url": "http://arxiv.org/pdf/2210.14366v1", "date": "2022-10-25 22:13:31", "abs": "We propose a novel Bayesian framework for the joint modeling of survey point\nand variance estimates for count data. The approach incorporates an induced\nprior distribution on the modeled true variance that sets it equal to the\ngenerating variance of the point estimate, a key property more readily achieved\nfor continuous data response type models. Our count data model formulation\nallows the input of domains at multiple resolutions (e.g., states, regions,\nnation) and simultaneously benchmarks modeled estimates at higher resolutions\n(e.g., states) to those at lower resolutions (e.g., regions) in a fashion that\nborrows more strength to sharpen our domain estimates at higher resolutions. We\nconduct a simulation study that generates a population of units within domains\nto produce ground truth statistics to compare to direct and modeled estimates\nperformed on samples taken from the population where we show improved\nreductions in error across domains. The model is applied to the job openings\nvariable and other data items published in the Job Openings and Labor Turnover\nSurvey administered by the U.S. Bureau of Labor Statistics.", "cat": "stat.ME", "authors": ["Terrance D. Savitsky", "Julie Gershunskaya", "Mark Crankshaw"]}, "928": {"id": "1409.0850v2", "title": "Galaxy Clusters Discovered via the Sunyaev-Zel'dovich Effect in the 2500-square-degree SPT-SZ survey", "url": "http://arxiv.org/pdf/1409.0850v2", "date": "2015-02-14 02:55:32", "abs": "We present a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich\n(SZ) effect signature from 2500 deg$^2$ of South Pole Telescope (SPT) data.\nThis work represents the complete sample of clusters detected at high\nsignificance in the 2500-square-degree SPT-SZ survey, which was completed in\n2011. A total of 677 (409) cluster candidates are identified above a\nsignal-to-noise threshold of $\\xi$ =4.5 (5.0). Ground- and space-based optical\nand near-infrared (NIR) imaging confirms overdensities of similarly colored\ngalaxies in the direction of 516 (or 76%) of the $\\xi$>4.5 candidates and 387\n(or 95%) of the $\\xi$>5 candidates; the measured purity is consistent with\nexpectations from simulations. Of these confirmed clusters, 415 were first\nidentified in SPT data, including 251 new discoveries reported in this work. We\nestimate photometric redshifts for all candidates with identified optical\nand/or NIR counterparts; we additionally report redshifts derived from\nspectroscopic observations for 141 of these systems. The mass threshold of the\ncatalog is roughly independent of redshift above $z$~0.25 leading to a sample\nof massive clusters that extends to high redshift. The median mass of the\nsample is $M_{\\scriptsize 500c}(\\rho_\\mathrm{crit})$ ~ 3.5 x 10$^{14} M_\\odot\nh^{-1}$, the median redshift is $z_{med}$ =0.55, and the highest-redshift\nsystems are at $z$>1.4. The combination of large redshift extent, clean\nselection, and high typical mass makes this cluster sample of particular\ninterest for cosmological analyses and studies of cluster formation and\nevolution.", "cat": "astro-ph.CO", "authors": ["L. E. Bleem", "B. Stalder", "T. de Haan", "K. A. Aird", "S. W. Allen", "D. E. Applegate", "M. L. N. Ashby", "M. Bautz", "M. Bayliss", "B. A. Benson", "S. Bocquet", "M. Brodwin", "J. E. Carlstrom", "C. L. Chang", "I. Chiu", "H. M. Cho", "A. Clocchiatti", "T. M. Crawford", "A. T. Crites", "S. Desai", "J. P. Dietrich", "M. A. Dobbs", "R. J. Foley", "W. R. Forman", "E. M. George", "M. D. Gladders", "A. H. Gonzalez", "N. W. Halverson", "C. Hennig", "H. Hoekstra", "G. P. Holder", "W. L. Holzapfel", "J. D. Hrubes", "C. Jones", "R. Keisler", "L. Knox", "A. T. Lee", "E. M. Leitch", "J. Liu", "M. Lueker", "D. Luong-Van", "A. Mantz", "D. P. Marrone", "M. McDonald", "J. J. McMahon", "S. S. Meyer", "L. Mocanu", "J. J. Mohr", "S. S. Murray", "S. Padin", "C. Pryke", "C. L. Reichardt", "A. Rest", "J. Ruel", "J. E. Ruhl", "B. R. Saliwanchik", "A. Saro", "J. T. Sayre", "K. K. Schaffer", "T. Schrabback", "E. Shirokoff", "J. Song", "H. G. Spieler", "S. A. Stanford", "Z. Staniszewski", "A. A. Stark", "K. T. Story", "C. W. Stubbs", "K. Vanderlinde", "J. D. Vieira", "A. Vikhlinin", "R. Williamson", "O. Zahn", "A. Zenteno"]}, "929": {"id": "1803.05900v1", "title": "Toolflows for Mapping Convolutional Neural Networks on FPGAs: A Survey and Future Directions", "url": "http://arxiv.org/pdf/1803.05900v1", "date": "2018-03-15 17:58:19", "abs": "In the past decade, Convolutional Neural Networks (CNNs) have demonstrated\nstate-of-the-art performance in various Artificial Intelligence tasks. To\naccelerate the experimentation and development of CNNs, several software\nframeworks have been released, primarily targeting power-hungry CPUs and GPUs.\nIn this context, reconfigurable hardware in the form of FPGAs constitutes a\npotential alternative platform that can be integrated in the existing deep\nlearning ecosystem to provide a tunable balance between performance, power\nconsumption and programmability. In this paper, a survey of the existing\nCNN-to-FPGA toolflows is presented, comprising a comparative study of their key\ncharacteristics which include the supported applications, architectural\nchoices, design space exploration methods and achieved performance. Moreover,\nmajor challenges and objectives introduced by the latest trends in CNN\nalgorithmic research are identified and presented. Finally, a uniform\nevaluation methodology is proposed, aiming at the comprehensive, complete and\nin-depth evaluation of CNN-to-FPGA toolflows.", "cat": "cs.CV", "authors": ["Stylianos I. Venieris", "Alexandros Kouris", "Christos-Savvas Bouganis"]}, "930": {"id": "2002.01290v4", "title": "Sparse Polynomial Chaos Expansions: Literature Survey and Benchmark", "url": "http://arxiv.org/pdf/2002.01290v4", "date": "2021-05-19 13:00:19", "abs": "Sparse polynomial chaos expansions (PCE) are a popular surrogate modelling\nmethod that takes advantage of the properties of PCE, the sparsity-of-effects\nprinciple, and powerful sparse regression solvers to approximate computer\nmodels with many input parameters, relying on only few model evaluations.\nWithin the last decade, a large number of algorithms for the computation of\nsparse PCE have been published in the applied math and engineering literature.\nWe present an extensive review of the existing methods and develop a framework\nfor classifying the algorithms. Furthermore, we conduct a unique benchmark on a\nselection of methods to identify which approaches work best in practical\napplications. Comparing their accuracy on several benchmark models of varying\ndimensionality and complexity, we find that the choice of sparse regression\nsolver and sampling scheme for the computation of a sparse PCE surrogate can\nmake a significant difference, of up to several orders of magnitude in the\nresulting mean-squared error. Different methods seem to be superior in\ndifferent regimes of model dimensionality and experimental design size.", "cat": "math.NA", "authors": ["Nora L\u00fcthen", "Stefano Marelli", "Bruno Sudret"]}, "931": {"id": "2408.14605v1", "title": "New supernova remnant candidates in the LOFAR Two Metre Sky Survey", "url": "http://arxiv.org/pdf/2408.14605v1", "date": "2024-08-26 19:55:06", "abs": "In spite of their key role in galaxy evolution and several decades of\nobservational efforts, the census of supernova remnants (SNRs) in our Galaxy\nremains incomplete. Theoretical predictions based on the local supernova rate\nestimate the expected number of SNRs in the Galaxy to be $\\gtrsim$ 1000. By\ncontrast, the number of detected SNRs amounts to about 300. High-resolution,\nwide-area radio surveys at low frequencies are ideal tools with which to find\nmissing SNRs, given the prominence of these sources at low radio frequencies.\nWe aim to find missing SNRs using proprietary data from the LOFAR Two-Metre Sky\nSurvey (LoTSS) at 144~MHz. We used LoTSS total intensity maps of two Galactic\nregions, one with $39^\\mathrm{o} < l < 66^\\mathrm{o}$ and $|b|<\n2.5^\\mathrm{o}$, and the other with $145^\\mathrm{o} < l < 150^\\mathrm{o}$ and\n$|b| < 3^\\mathrm{o}$, in addition to mid-infrared (MIR) data from the\nWide-field Infrared Survey Explorer (WISE) all-sky survey to search for SNR\ncandidates. We report the discovery of 14 new SNR candidates selected on the\nbasis of their morphology at 144 MHz and a lack of MIR emission. We also follow\nup on 24 previously reported SNR candidates, inferring their spectral index\nbetween the LoTSS frequency (144 MHz) and the frequency at which they were\nreported. The high resolution and sensitivity of LoTSS observations has\nresulted in the detection of 14 new SNR candidates. In order to unambiguously\nconfirm the SNR nature of these candidates, follow-up X-ray observations are\nrequired with facilities such as eROSITA.", "cat": "astro-ph.HE", "authors": ["K. Tsalapatas", "M. Arias", "T. Shimwell", "K. Rajwade", "M. J. Hardcastle", "A. Drabent"]}, "932": {"id": "2309.00154v1", "title": "Learning From Peers: A Survey of Perception and Utilization of Online Peer Support Among Informal Dementia Caregivers", "url": "http://arxiv.org/pdf/2309.00154v1", "date": "2023-08-31 22:03:32", "abs": "Informal dementia caregivers are those who care for a person living with\ndementia (PLWD) without receiving payment (e.g., family members, friends, or\nother unpaid caregivers). These informal caregivers are subject to substantial\nmental, physical, and financial burdens. Online communities enable these\ncaregivers to exchange caregiving strategies and communicate experiences with\nother caregivers whom they generally do not know in real life. Research has\ndemonstrated the benefits of peer support in online communities, but they are\nlimited in focusing merely on caregivers who are already online users. In this\npaper, we designed and administered a survey to investigate the perception and\nutilization of online peer support from 140 informal dementia caregivers (with\n100 online-community caregivers). Our findings show that the behavior to access\nany online community is only significantly associated with their belief in the\nvalue of online peer support (p = 0.006). Moreover, 33 (83%) of the 40\nnon-online-community caregivers had a belief score above 24, a score assigned\nwhen a neutral option is selected for each belief question. The reasons most\narticulated for not accessing any online community were no time to do so (14;\n10%), and insufficient online information searching skills (9; 6%). Our\nfindings suggest that online peer support is valuable, but practical strategies\nare needed to assist informal dementia caregivers who have limited time or\nsearching skills.", "cat": "cs.CY", "authors": ["Zhijun Yin", "Lauren Stratton", "Qingyuan Song", "Congning Ni", "Lijun Song", "Patricia A. Commiskey", "Qingxia Chen", "Monica Moreno", "Sam Fazio", "Bradley A. Malin"]}, "933": {"id": "2205.11734v1", "title": "Mass-Ratio Distribution of Binaries From the LAMOST-MRS Survey", "url": "http://arxiv.org/pdf/2205.11734v1", "date": "2022-05-24 03:00:47", "abs": "Binary evolution leads to the formation of important objects crucial to the\ndevelopment of astrophysics, but the statistical properties of binary\npopulations are still poorly understood. The LAMOST-MRS has provided a large\nsample of stars to study the properties of binary populations, especially for\nthe mass ratio distributions and the binary fractions. We have devised a Peak\nAmplitude Ratio (PAR) approach to derive the mass ratio of a binary system\nbased on results obtained from its spectrum. By computing a cross-correlation\nfunction (CCF), we established a relationship between the derived mass ratio\nand the PARs of the binary systems. By utilizing spectral observations obtained\nfrom LAMSOT DR6 & DR7, we applied the PAR approach to form distributions of the\nderived mass ratio of the binary systems to the spectral types. We selected the\nmass ratio within the range of $0.6-1.0$ for investigating the mass-ratio\ndistribution. Through a power-law fitting, we obtained the power index $\\gamma$\nvalues of $-0.42\\pm0.27$, $0.03\\pm0.12$, and $2.12\\pm0.19$ for A-, F-, and\nG-type stars identified in the sample, respectively. The derived\n$\\gamma$-values display an increasing trend toward lower primary star masses,\nand G-type binaries tend to be more in twins. The close binary fractions (for\n$P\\lesssim 150\\,{\\rm d}$ and $q\\gtrsim 0.6$) in our sample for A, F and G\nbinaries are $7.6\\pm 0.5 \\%$, $4.9\\pm 0.2 \\%$ and $3.7 \\pm 0.1 \\%$,\nrespectively. Note that the PAR approach can be applied to large spectroscopic\nsurveys of stars.", "cat": "astro-ph.SR", "authors": ["Jiangdan Li", "Jiao Li", "Chao Liu", "Chunqian Li", "Yanjun Guo", "Luqian Wang", "Xuefei Chen", "Lifeng Xing", "Yonghui Hou", "Zhanwen Han"]}, "934": {"id": "2405.04016v1", "title": "Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys", "url": "http://arxiv.org/pdf/2405.04016v1", "date": "2024-05-07 05:27:48", "abs": "In this study, we present the construction of a new proper motion catalog\nutilizing the photometric data from the Sloan Digital Sky Survey (SDSS) and\nDark Energy Spectroscopic Instrument (DESI) imaging surveys, with a median time\nbaseline of about 13 years. To mitigate systematic errors, the DESI galaxy\npositions are employed to establish a reference frame and to correct the\nposition-, magnitude-, and color-dependent discrepancies between SDSS and DESI\nimaging datasets. Spanning 12,589 square degrees, the catalog encompasses about\n206.6 million non-Gaia objects down to $m_r \\sim$ 23. Based on 734k quasars,\nthe assessment of the global systematic errors in DESI-SDSS proper motion\ncatalog yields values of 0.14 mas yr$^{-1}$ for $\\mu_{\\alpha *}$ and 0.11 mas\nyr$^{-1}$ for $\\mu_{\\delta}$. The catalog exhibits a precision surpassing 3.7\nmas yr$^{-1}$, albeit varying with position, color, and magnitude. An\nadditional evaluation employing approximately 5,300 distant star samples yields\nan overall precision of approximately 3.0 and 2.9 mas yr$^{-1}$ for\n$\\mu_{\\alpha *}$ and $\\mu_{\\delta}$, respectively. Further comparisons with\nproper motions from SDSS Stripe 82 reveal a strong consistency between the two\ndatasets. As a practical application, we utilize fainter non-Gaia objects in\nour catalog to update the proper motions of 17 star clusters. The resulting\nproper motions for these clusters exhibit excellent consistency with those\nderived from Gaia data. Our proper motion measurements, characterized by a\ndeeper limiting magnitude, stands as a valuable complement to the Gaia dataset.\nThe catalog is publicly available at \\url{https://www.scidb.cn/s/YzaIv2}.", "cat": "astro-ph.GA", "authors": ["Yun-Ao Xiao", "Hu Zou", "Xin Xu", "Lu Feng", "Wei-Jian Guo", "Wenxiong Li", "Zhixia Shen", "Gaurav Singh", "Jipeng Sui", "Jiali Wang", "Suijian Xue"]}, "935": {"id": "1603.00020v2", "title": "A Super-Jupiter Microlens Planet Characterized by High-Cadence KMTNet Microlensing Survey Observations of OGLE-2015-BLG-0954", "url": "http://arxiv.org/pdf/1603.00020v2", "date": "2016-06-23 12:37:27", "abs": "We report the characterization of a massive (m_p=3.9 +- 1.4 M_jup)\nmicrolensing planet (OGLE-2015-BLG-0954Lb) orbiting an M dwarf host (M=0.33 +-\n0.12 M_sun) at a distance toward the Galactic bulge of 0.6 (+0.4,-0.2) kpc,\nwhich is extremely nearby by microlensing standards. The planet-host projected\nseparation is a_perp ~ 1.2 AU. The characterization was made possible by the\nwide-field (4 sq. deg.) high cadence (Gamma = 6/hr) monitoring of the Korea\nMicrolensing Telescope Network (KMTNet), which had two of its three telescopes\nin commissioning operations at the time of the planetary anomaly. The source\ncrossing time t_* = 16 min is among the shortest ever published. The\nhigh-cadence, wide-field observations that are the hallmark of KMTNet are the\nonly way to routinely capture such short crossings. High-cadence resolution of\nshort caustic crossings will preferentially lead to mass and distance\nmeasurements for the lens. This is because the short crossing time typically\nimplies a nearby lens, which enables the measurement of additional effects\n(bright lens and/or microlens parallax). When combined with the measured\ncrossing time, these effects can yield planet/host masses and distance.", "cat": "astro-ph.EP", "authors": ["I. -G. Shin", "Y. -H. Ryu", "A. Udalski", "M. Albrow", "S. -M. Cha", "J. -Y. Choi", "S. -J. Chung", "C. Han", "K. -H. Hwang", "Y. K. Jung", "D. -J. Kim", "S. -L. Kim", "C. -U. Lee", "Y. Lee", "B. -G. Park", "H. Park", "R. W. Pogge", "J. C. Yee", "P. Pietrukowicz", "P. Mr\u00f3z", "S. Koz\u0142owski", "R. Poleski", "J. Skowron", "I. Soszy\u0144ski", "M. K. Szyma\u0144ski", "K. Ulaczyk", "\u0141. Wyrzykowski", "M. Pawlak", "A. Gould"]}, "936": {"id": "1605.05338v2", "title": "At the survey limits: discovery of the Aquarius 2 dwarf galaxy in the VST ATLAS and the SDSS data", "url": "http://arxiv.org/pdf/1605.05338v2", "date": "2016-08-15 14:00:33", "abs": "We announce the discovery of the Aquarius~2 dwarf galaxy, a new distant\nsatellite of the Milky Way, detected on the fringes of the VST ATLAS and the\nSDSS surveys. The object was originally identified as an overdensity of Red\nGiant Branch stars, but chosen for subsequent follow-up based on the presence\nof a strong Blue Horizontal Branch, which was also used to measure its distance\nof $\\sim 110$ kpc. Using deeper imaging from the IMACS camera on the 6.5m Baade\nand spectroscopy with DEIMOS on Keck, we measured the satellite's half-light\nradius $5.1\\pm 0.8$ arcmin, or $\\sim 160$ pc at this distance, and its stellar\nvelocity dispersion of $5.4^{+3.4}_{-0.9}$ km s$^{-1}$. With $\\mu=30.2$ mag\narcsec$^{-2}$ and $M_V=-4.36$, the new satellite lies close to two important\ndetection limits: one in surface brightness; and one in luminosity at a given\ndistance, thereby making Aquarius~2 one of the hardest dwarfs to find.", "cat": "astro-ph.GA", "authors": ["G. Torrealba", "S. E. Koposov", "V. Belokurov", "M. Irwin", "M. Collins", "M. Spencer", "R. Ibata", "M. Mateo", "A. Bonaca", "P. Jethwa"]}, "937": {"id": "2104.13667v2", "title": "A Survey on User-Centric Cell-Free Massive MIMO Systems", "url": "http://arxiv.org/pdf/2104.13667v2", "date": "2021-10-06 15:37:08", "abs": "The mobile data traffic has been exponentially growing during the last\ndecades, which has been enabled by the densification of the network\ninfrastructure in terms of increased cell density (i.e., ultra-dense network\n(UDN)) and/or increased number of active antennas per access point (AP) (i.e.,\nmassive multiple-input multiple-output (mMIMO)). However, neither UDN nor mMIMO\nwill meet the increasing data rate demands of the sixth generation (6G)\nwireless communications due to the inter-cell interference and large\nquality-of-service variations, respectively. Cell-free (CF) mMIMO, which\ncombines the best aspects of UDN and mMIMO, is viewed as a key solution to this\nissue. In such systems, each user equipment (UE) is served by a preferred set\nof surrounding APs cooperatively. In this paper, we provide a survey of the\nstate-of-the-art literature on CF mMIMO. As a starting point, the significance\nand the basic properties of CF mMIMO are highlighted. We then present the\ncanonical framework, where the essential details (i.e., transmission procedure\nand mathematical system model) are discussed. Next, we provide a deep look at\nthe resource allocation and signal processing problems related to CF mMIMO and\nsurvey the up-to-date schemes and algorithms. After that, we discuss the\npractical issues when implementing CF mMIMO. Potential future directions are\nthen pointed out. Finally, we conclude this paper with a summary of the key\nlessons learned in this field. This paper aims to provide a starting point for\nanyone who wants to conduct research on CF mMIMO for future wireless networks.", "cat": "cs.IT", "authors": ["Shuaifei Chen", "Jiayi Zhang", "Jing Zhang", "Emil Bj\u00f6rnson", "Bo Ai"]}, "938": {"id": "2403.00780v1", "title": "Empirical and Experimental Insights into Data Mining Techniques for Crime Prediction: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2403.00780v1", "date": "2024-02-17 15:00:45", "abs": "This survey paper presents a comprehensive analysis of crime prediction\nmethodologies, exploring the various techniques and technologies utilized in\nthis area. The paper covers the statistical methods, machine learning\nalgorithms, and deep learning techniques employed to analyze crime data, while\nalso examining their effectiveness and limitations. We propose a methodological\ntaxonomy that classifies crime prediction algorithms into specific techniques.\nThis taxonomy is structured into four tiers, including methodology category,\nmethodology sub-category, methodology techniques, and methodology\nsub-techniques. Empirical and experimental evaluations are provided to rank the\ndifferent techniques. The empirical evaluation assesses the crime prediction\ntechniques based on four criteria, while the experimental evaluation ranks the\nalgorithms that employ the same sub-technique, the different sub-techniques\nthat employ the same technique, the different techniques that employ the same\nmethodology sub-category, the different methodology sub-categories within the\nsame category, and the different methodology categories. The combination of\nmethodological taxonomy, empirical evaluations, and experimental comparisons\nallows for a nuanced and comprehensive understanding of crime prediction\nalgorithms, aiding researchers in making informed decisions. Finally, the paper\nprovides a glimpse into the future of crime prediction techniques, highlighting\npotential advancements and opportunities for further research in this field", "cat": "cs.LG", "authors": ["Kamal Taha"]}, "939": {"id": "1704.03766v1", "title": "PdBI U/LIRG Survey (PULS): Dense Molecular Gas in Arp 220 and NGC 6240", "url": "http://arxiv.org/pdf/1704.03766v1", "date": "2017-04-12 14:28:57", "abs": "Aims. We present new IRAM Plateau de Bure Interferometer observations of Arp\n220 in HCN, HCO$^{+}$, HN$^{13}$C J=1-0, C$_{2}$H N=1-0, SiO J = 2-1, HNCO\nJ$_{k,k'}$ = 5$_{0,4}$ - 4$_{0,4}$, CH$_{3}$CN(6-5), CS J=2-1 and 5-4 and\n$^{13}$CO J=1-0 and 2-1 and of NGC 6240 in HCN, HCO$^{+}$ J = 1-0 and C$_{2}$H\nN = 1-0. In addition, we present Atacama Large Millimeter/submillmeter Array\nscience verification observations of Arp 220 in CS J = 4-3 and\nCH$_{3}$CN(10-9). Various lines are used to analyse the physical conditions of\nthe molecular gas including the [$^{12}$CO]/[$^{13}$CO] and\n[$^{12}$CO]/[C$^{18}$O] abundance ratios. These observations will be made\navailable to the public. Methods. We create brightness temperature line ratio\nmaps to present the different physical conditions across Arp 220 and NGC 6240.\nIn addition, we use the radiative transfer code RADEX and a Monte Carlo Markov\nChain likelihood code to model the $^{12}$CO, $^{13}$CO and C$^{18}$O lines of\nArp 220 at ~2\" (~700 pc) scales, where the $^{12}$CO and C$^{18}$O measurements\nwere obtained from literature. Results. Line ratios of optically thick lines\nsuch as $^{12}$CO show smoothly varying ratios while the line ratios of\noptically thin lines such as $^{13}$CO show a east-west gradient across Arp\n220. The HCN/HCO$^{+}$ line ratio differs between Arp 220 and NGC 6240, where\nArp 220 has line ratios above 2 and NGC 6240 below 1. The radiative transfer\nanalysis solution is consistent with a warm (~40 K), moderately dense\n(~10$^{3.4}$ cm$^{-3}$) molecular gas component averaged over the two nuclei.\nWe find [$^{12}$CO]/[$^{13}$CO] and [$^{12}$CO]/[C$^{18}$O] abundance ratios of\n~90 for both. The abundance enhancement of C$^{18}$O can be explained by\nstellar nucleosynthesis enrichment of the interstellar medium.", "cat": "astro-ph.GA", "authors": ["Kazimierz Sliwa", "Dennis Downes"]}, "940": {"id": "2003.12948v3", "title": "When Autonomous Systems Meet Accuracy and Transferability through AI: A Survey", "url": "http://arxiv.org/pdf/2003.12948v3", "date": "2020-05-25 02:05:38", "abs": "With widespread applications of artificial intelligence (AI), the\ncapabilities of the perception, understanding, decision-making and control for\nautonomous systems have improved significantly in the past years. When\nautonomous systems consider the performance of accuracy and transferability,\nseveral AI methods, like adversarial learning, reinforcement learning (RL) and\nmeta-learning, show their powerful performance. Here, we review the\nlearning-based approaches in autonomous systems from the perspectives of\naccuracy and transferability. Accuracy means that a well-trained model shows\ngood results during the testing phase, in which the testing set shares a same\ntask or a data distribution with the training set. Transferability means that\nwhen a well-trained model is transferred to other testing domains, the accuracy\nis still good. Firstly, we introduce some basic concepts of transfer learning\nand then present some preliminaries of adversarial learning, RL and\nmeta-learning. Secondly, we focus on reviewing the accuracy or transferability\nor both of them to show the advantages of adversarial learning, like generative\nadversarial networks (GANs), in typical computer vision tasks in autonomous\nsystems, including image style transfer, image superresolution, image\ndeblurring/dehazing/rain removal, semantic segmentation, depth estimation,\npedestrian detection and person re-identification (re-ID). Then, we further\nreview the performance of RL and meta-learning from the aspects of accuracy or\ntransferability or both of them in autonomous systems, involving pedestrian\ntracking, robot navigation and robotic manipulation. Finally, we discuss\nseveral challenges and future topics for using adversarial learning, RL and\nmeta-learning in autonomous systems.", "cat": "cs.LG", "authors": ["Chongzhen Zhang", "Jianrui Wang", "Gary G. Yen", "Chaoqiang Zhao", "Qiyu Sun", "Yang Tang", "Feng Qian", "J\u00fcrgen Kurths"]}, "941": {"id": "2011.08211v1", "title": "The LOFAR Two Metre Sky Survey: Deep Fields. II. The ELAIS-N1 LOFAR deep field", "url": "http://arxiv.org/pdf/2011.08211v1", "date": "2020-11-16 19:00:36", "abs": "The LOFAR Two-metre Sky Survey (LoTSS) will cover the full northern sky and,\nadditionally, aims to observe the LoTSS deep fields to a noise level of ~10\nmicroJy/bm over several tens of square degrees in areas that have the most\nextensive ancillary data. This paper presents the ELAIS-N1 deep field, the\ndeepest of the LoTSS deep fields to date. With an effective observing time of\n163.7 hours, it reaches a root mean square (RMS) noise level below 20\nmicroJy/bm in the central region (and below 30 microJy/bm over 10 square\ndegrees). The resolution is 6 arcsecs and 84862 radio sources were detected in\nthe full area (68 sq. deg.) with 74127 sources in the highest quality area at\nless than 3 degrees from the pointing centre. The observation reaches a sky\ndensity of more than 5000 sources per sq. deg. in the central ~5 sq. deg.\nregion. We present the calibration procedure, which addresses the special\nconfiguration of some observations and the extended bandwidth covered (115 to\n177 MHz; central frequency 146.2 MHz) compared to standard LoTSS. We also\ndescribe the methods used to calibrate the flux density scale using\ncross-matching with sources detected by other radio surveys in the literature.\nWe find the flux density uncertainty related to the flux density scale to be\n~6.5%. By studying the variations of the flux density measurements between\ndifferent epochs, we show that relative flux density calibration is reliable\nout to about a 3 degree radius, but that additional flux density uncertainty is\npresent for all sources at about the 3 per cent level; this is likely to be\nassociated with residual calibration errors, and is shown to be more\nsignificant in datasets with poorer ionosphere conditions. We also provide\nintra-band spectral indices, which can be useful to detect sources with unusual\nspectral properties. The final uncertainty in the flux densities is estimated\nto be ~10% for ELAIS-N1.", "cat": "astro-ph.GA", "authors": ["J. Sabater", "P. N. Best", "C. Tasse", "M. J. Hardcastle", "T. W. Shimwell", "D. Nisbet", "V. Jelic", "J. R. Callingham", "H. J. A. Rottgering", "M. Bonato", "M. Bondi", "B. Ciardi", "R. K. Cochrane", "M. J. Jarvis", "R. Kondapally", "L. V. E. Koopmans", "S. P. O'Sullivan", "I. Prandoni", "D. J. Schwarz", "D. J. B. Smith", "L. Wang", "W. L. Williams", "S. Zaroubi"]}, "942": {"id": "1903.00846v2", "title": "A survey of security and privacy issues in the Internet of Things from the layered context", "url": "http://arxiv.org/pdf/1903.00846v2", "date": "2020-02-25 02:33:49", "abs": "Internet of Things (IoT) is a novel paradigm, which not only facilitates a\nlarge number of devices to be ubiquitously connected over the Internet but also\nprovides a mechanism to remotely control these devices. The IoT is pervasive\nand is almost an integral part of our daily life. As devices are becoming\nincreasingly connected, privacy and security issues become more and more\ncritical and these need to be addressed on an urgent basis. IoT implementations\nand devices are eminently prone to threats that could compromise the security\nand privacy of the consumers, which, in turn, could influence its practical\ndeployment. In recent past, some research has been carried out to secure IoT\ndevices with an intention to alleviate the security concerns of users. The\npurpose of this paper is to highlight the security and privacy issues in IoT\nsystems. To this effect, the paper examines the security issues at each layer\nin the IoT protocol stack, identifies the underlying challenges and key\nsecurity requirements and provides a brief overview of existing security\nsolutions to safeguard the IoT from the layered context.", "cat": "cs.NI", "authors": ["Samundra Deep", "Xi Zheng", "Alireza Jolfaei", "Dongjin Yu", "Pouya Ostovari", "Ali Kashif Bashir"]}, "943": {"id": "2402.08703v2", "title": "A Survey of Generative AI for de novo Drug Design: New Frontiers in Molecule and Protein Generation", "url": "http://arxiv.org/pdf/2402.08703v2", "date": "2024-06-26 11:03:21", "abs": "Artificial intelligence (AI)-driven methods can vastly improve the\nhistorically costly drug design process, with various generative models already\nin widespread use. Generative models for de novo drug design, in particular,\nfocus on the creation of novel biological compounds entirely from scratch,\nrepresenting a promising future direction. Rapid development in the field,\ncombined with the inherent complexity of the drug design process, creates a\ndifficult landscape for new researchers to enter. In this survey, we organize\nde novo drug design into two overarching themes: small molecule and protein\ngeneration. Within each theme, we identify a variety of subtasks and\napplications, highlighting important datasets, benchmarks, and model\narchitectures and comparing the performance of top models. We take a broad\napproach to AI-driven drug design, allowing for both micro-level comparisons of\nvarious methods within each subtask and macro-level observations across\ndifferent fields. We discuss parallel challenges and approaches between the two\napplications and highlight future directions for AI-driven de novo drug design\nas a whole. An organized repository of all covered sources is available at\nhttps://github.com/gersteinlab/GenAI4Drug.", "cat": "q-bio.BM", "authors": ["Xiangru Tang", "Howard Dai", "Elizabeth Knight", "Fang Wu", "Yunyang Li", "Tianxiao Li", "Mark Gerstein"]}, "944": {"id": "2309.03555v1", "title": "Compositional properties of planet-crossing asteroids from astronomical surveys", "url": "http://arxiv.org/pdf/2309.03555v1", "date": "2023-09-07 08:36:42", "abs": "Context. The study of planet-crossing asteroids is of both practical and\nfundamental importance. As they are closer than asteroids in the Main Belt, we\nhave access to a smaller size range, and this population frequently impacts\nplanetary surfaces and can pose a threat to life. Aims. We aim to characterize\nthe compositions of a large corpus of planet-crossing asteroids and to study\nhow these compositions are related to orbital and physical parameters. Methods.\nWe gathered publicly available visible colors of near-Earth objects (NEOs) from\nthe Sloan Digital Sky Survey (SDSS) and SkyMapper surveys. We also computed\nSDSS-compatible colors from reflectance spectra of the Gaia mission and a\ncompilation of ground-based observations. We determined the taxonomy of each\nNEO from its colors and studied the distribution of the taxonomic classes and\nspectral slope against the orbital parameters and diameter. Results. We provide\nupdated photometry for 470 NEOs from the SDSS, and taxonomic classification of\n7,401 NEOs. We classify 42 NEOs that are mission-accessible, including six of\nthe seven flyby candidates of the ESA Hera mission. We confirm the perihelion\ndependance of spectral slope among S-type NEOs, likely related to a\nrejuvenation mechanism linked with thermal fatigue. We also confirm the\nclustering of A-type NEOs around 1.5-2 AU, and predict the taxonomic\ndistribution of small asteroids in the NEO source regions in the Main Belt.", "cat": "astro-ph.EP", "authors": ["A. V. Sergeyev", "B. Carry", "M. Marsset", "P. Pravec", "D. Perna", "F. E. DeMeo", "V. Petropoulou", "M. Lazzarin", "F. La Forgia", "I. Di Petro", "the NEOROCKS team"]}, "945": {"id": "0710.2418v1", "title": "H.E.S.S. Galactic Plane Survey unveils a Milagro Hotspot", "url": "http://arxiv.org/pdf/0710.2418v1", "date": "2007-10-12 09:44:52", "abs": "We report here on a new VHE source, HESS J1908+063, disovered during the\nextended H.E.S.S. survey of the Galactic plane and which coincides with the\nrecently reported MILAGRO unidentied source MGRO J1908+06. The position,\nextension and spectrum measurements of the HESS source are presented and\ncompared to those of MGRO J1908+06. Possible counterparts at other wavelenghts\nare discussed. For the first time one of the low-lattitude MILAGRO sources is\nconfirmed.", "cat": "astro-ph", "authors": ["H. E. S. S. Collaboration", ":", "A. Djannati-Atai", "E. Ona-Wilhelmi", "M. Renaud", "S. Hoppe"]}, "946": {"id": "0712.2885v1", "title": "BAT X-ray Survey - I: Methodology and X-ray Identification", "url": "http://arxiv.org/pdf/0712.2885v1", "date": "2007-12-18 05:53:26", "abs": "We applied the Maximum Likelihood method, as an image reconstruction\nalgorithm, to the BAT X-ray Survey (BXS). This method was specifically designed\nto preserve the full statistical information in the data and to avoid\nmosaicking of many exposures with different pointing directions, thus reducing\nsystematic errors when co-adding images. We reconstructed, in the 14-170 keV\nenergy band, the image of a 90x90 deg$^2$ sky region, centered on\n(RA,DEC)=105$^{\\circ}$,-25$^{\\circ}$, which BAT surveyed with an exposure time\nof $\\sim1$ Ms (in Nov. 2005). The best sensitivity in our image is $\\sim0.85$\nmCrab or $2.0\\times 10^{-11}$ erg cm$^{-2}$. We detect 49 hard X-ray sources\nabove the 4.5 $\\sigma$ level; of these, only 12 were previously known as hard\nX-ray sources ($>$15 keV). Swift/XRT observations allowed us to firmly identify\nthe counterparts for 15 objects, while 2 objects have Einstein IPC counterparts\n\\citep{harris90}; in addition to those, we found a likely counterpart for 13\nobjects by correlating our sample with the ROSAT All-Sky Survey Bright Source\nCatalog \\citep{voges99}. 7 objects remain unidentified. Analysis of the noise\nproperties of our image shows that $\\sim75$% of the area is surveyed to a flux\nlimit of $\\sim$1 mCrab. This study shows that the coupling of the Maximum\nLikelihood method to the most sensitive, all-sky surveying, hard X-ray\ninstrument, BAT, is able to probe for the first time the hard X-ray sky to the\nmCrab flux level. The successful application of this method to BAT demonstrates\nthat it could also be applied with advantage to similar instruments like\nINTEGRAL-IBIS.", "cat": "astro-ph", "authors": ["M. Ajello", "J. Greiner", "G. Kanbach", "A. Rau", "A. W. Strong", "J. A. Kennea"]}, "947": {"id": "2405.13001v1", "title": "Large Language Models for Education: A Survey", "url": "http://arxiv.org/pdf/2405.13001v1", "date": "2024-05-12 01:50:01", "abs": "Artificial intelligence (AI) has a profound impact on traditional education.\nIn recent years, large language models (LLMs) have been increasingly used in\nvarious applications such as natural language processing, computer vision,\nspeech recognition, and autonomous driving. LLMs have also been applied in many\nfields, including recommendation, finance, government, education, legal\naffairs, and finance. As powerful auxiliary tools, LLMs incorporate various\ntechnologies such as deep learning, pre-training, fine-tuning, and\nreinforcement learning. The use of LLMs for smart education (LLMEdu) has been a\nsignificant strategic direction for countries worldwide. While LLMs have shown\ngreat promise in improving teaching quality, changing education models, and\nmodifying teacher roles, the technologies are still facing several challenges.\nIn this paper, we conduct a systematic review of LLMEdu, focusing on current\ntechnologies, challenges, and future developments. We first summarize the\ncurrent state of LLMEdu and then introduce the characteristics of LLMs and\neducation, as well as the benefits of integrating LLMs into education. We also\nreview the process of integrating LLMs into the education industry, as well as\nthe introduction of related technologies. Finally, we discuss the challenges\nand problems faced by LLMEdu, as well as prospects for future optimization of\nLLMEdu.", "cat": "cs.CL", "authors": ["Hanyi Xu", "Wensheng Gan", "Zhenlian Qi", "Jiayang Wu", "Philip S. Yu"]}, "948": {"id": "2204.04756v1", "title": "Towards Evaluation of Autonomously Generated Musical Compositions: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2204.04756v1", "date": "2022-04-10 19:42:52", "abs": "There are many applications that aim to create a complete model for an\nautonomously generated composition; systems are able to generate muzak songs,\nassist singers in transcribing songs or can imitate long-dead authors.\nSubjective understanding of creativity or aesthetics differs not only within\npreferences (popular authors or genres), but also differs on the basis of\nexperienced experience or socio-cultural environment. So, what do we want to\nachieve with such an adaptation? What is the benefit of the resulting work for\nthe author, who can no longer evaluate this composition? And in what ways\nshould we evaluate such a composition at all?", "cat": "cs.SD", "authors": ["Daniel Kvak"]}, "949": {"id": "1608.00700v2", "title": "A Survey of Visual Analysis of Human Motion and Its Applications", "url": "http://arxiv.org/pdf/1608.00700v2", "date": "2016-08-23 05:15:03", "abs": "This paper summarizes the recent progress in human motion analysis and its\napplications. In the beginning, we reviewed the motion capture systems and the\nrepresentation model of human's motion data. Next, we sketched the advanced\nhuman motion data processing technologies, including motion data filtering,\ntemporal alignment, and segmentation. The following parts overview the\nstate-of-the-art approaches of action recognition and dynamics measuring since\nthese two are the most active research areas in human motion analysis. The last\npart discusses some emerging applications of the human motion analysis in\nhealthcare, human robot interaction, security surveillance, virtual reality and\nanimation. The promising research topics of human motion analysis in the future\nis also summarized in the last part.", "cat": "cs.CV", "authors": ["Qifei Wang"]}, "950": {"id": "1202.3111v1", "title": "A BVRcIc Survey of W Ursae Majoris Binaries", "url": "http://arxiv.org/pdf/1202.3111v1", "date": "2012-02-14 18:25:54", "abs": "We report on a BVRcIc survey of field W Ursae Majoris binary stars and\npresent accurate colors for 606 systems that have been observed on at least\nthree photometric nights from a robotic observatory in southern Arizona.\nComparison with earlier photometry for a subset of the systems shows good\nagreement. We investigate two independent methods of determining the\ninterstellar reddening, although both have limitations that can render them\nless effective than desired. A subset of 101 systems shows good agreement\nbetween the two reddening methods.", "cat": "astro-ph.SR", "authors": ["Dirk Terrell", "John Gross", "Walter R. Cooney Jr"]}, "951": {"id": "1804.01972v1", "title": "A Survey of Miss-Ratio Curve Construction Techniques", "url": "http://arxiv.org/pdf/1804.01972v1", "date": "2018-04-05 17:48:29", "abs": "Miss-ratio curve (MRC), or equivalently hit-ratio curve (HRC), construction\ntechniques have recently gathered the attention of many researchers. Recent\nadvancements have allowed for approximating these curves in constant time,\nallowing for online working-set-size (WSS) measurement. Techniques span the\nalgorithmic design paradigm from classic dynamic programming to artificial\nintelligence inspired techniques. Our survey produces broad classification of\nthe current techniques primarily based on \\emph{what} locality metric is being\nrecorded and \\emph{how} that metric is stored for processing.\n Applications of theses curves span from dynamic cache partitioning in the\nprocessor, to improving block allocation at the operating system level. Our\nsurvey will give an overview of the historical, exact MRC construction methods,\nand compare them with the state-of-the-art methods present in today's\nliterature. In addition, we will show where there are still open areas of\nresearch and remain excited to see what this domain can produce with a strong\ntheoretical background.", "cat": "cs.PF", "authors": ["Daniel Byrne"]}, "952": {"id": "1811.07926v1", "title": "The LOFAR Two-metre Sky Survey - II. First data release", "url": "http://arxiv.org/pdf/1811.07926v1", "date": "2018-11-19 19:04:33", "abs": "The LOFAR Two-metre Sky Survey (LoTSS) is an ongoing sensitive,\nhigh-resolution 120-168MHz survey of the entire northern sky for which\nobservations are now 20% complete. We present our first full-quality public\ndata release. For this data release 424 square degrees, or 2% of the eventual\ncoverage, in the region of the HETDEX Spring Field (right ascension 10h45m00s\nto 15h30m00s and declination 45$^\\circ$00$'$00$''$ to 57$^\\circ$00$'$00$''$)\nwere mapped using a fully automated direction-dependent calibration and imaging\npipeline that we developed. A total of 325,694 sources are detected with a\nsignal of at least five times the noise, and the source density is a factor of\n$\\sim 10$ higher than the most sensitive existing very wide-area\nradio-continuum surveys. The median sensitivity is S$_{\\rm 144 MHz} =\n71\\,\\mu$Jy beam$^{-1}$ and the point-source completeness is 90% at an\nintegrated flux density of 0.45mJy. The resolution of the images is 6$''$ and\nthe positional accuracy is within 0.2$''$. This data release consists of a\ncatalogue containing location, flux, and shape estimates together with 58\nmosaic images that cover the catalogued area. In this paper we provide an\noverview of the data release with a focus on the processing of the LOFAR data\nand the characteristics of the resulting images. In two accompanying papers we\nprovide the radio source associations and deblending and, where possible, the\noptical identifications of the radio sources together with the photometric\nredshifts and properties of the host galaxies. These data release papers are\npublished together with a further $\\sim$20 articles that highlight the\nscientific potential of LoTSS.", "cat": "astro-ph.GA", "authors": ["T. W. Shimwell", "C. Tasse", "M. J. Hardcastle", "A. P. Mechev", "W. L. Williams", "P. N. Best", "H. J. A. R\u00f6ttgering", "J. R. Callingham", "T. J. Dijkema", "F. de Gasperin", "D. N. Hoang", "B. Hugo", "M. Mirmont", "J. B. R. Oonk", "I. Prandoni", "D. Rafferty", "J. Sabater", "O. Smirnov", "R. J. van Weeren", "G. J. White", "M. Atemkeng", "L. Bester", "E. Bonnassieux", "M. Br\u00fcggen", "G. Brunetti", "K. T. Chy\u017cy", "R. Cochrane", "J. E. Conway", "J. H. Croston", "A. Danezi", "K. Duncan", "M. Haverkorn", "G. H. Heald", "M. Iacobelli", "H. T. Intema", "N. Jackson", "M. Jamrozy", "M. J. Jarvis", "R. Lakhoo", "M. Mevius", "G. K. Miley", "L. Morabito", "R. Morganti", "D. Nisbet", "E. Orr\u00fa", "S. Perkins", "R. F. Pizzo", "C. Schrijvers", "D. J. B. Smith", "R. Vermeulen", "M. W. Wise", "L. Alegre", "D. J. Bacon", "I. M. van Bemmel", "R. J. Beswick", "A. Bonafede", "A. Botteon", "S. Bourke", "M. Brienza", "G. Calistro Rivera", "R. Cassano", "A. O. Clarke", "C. J. Conselice", "R. J. Dettmar", "A. Drabent", "C. Dumba", "K. L. Emig", "T. A. En\u00dflin", "C. Ferrari", "M. A. Garrett", "R. T. G\u00e9nova-Santos", "A. Goyal", "G. G\u00fcrkan", "C. Hale", "J. J. Harwood", "V. Heesen", "M. Hoeft", "C. Horellou", "C. Jackson", "G. Kokotanekov", "R. Kondapally", "M. Kunert-Bajraszewska", "V. Mahatma", "E. K. Mahony", "S. Mandal", "J. P. McKean", "A. Merloni", "B. Mingo", "A. Miskolczi", "S. Mooney", "B. Nikiel-Wroczy\u0144ski", "S. P. O'Sullivan", "J. Quinn", "W. Reich", "C. Roskowi\u0144ski", "A. Rowlinson", "F. Savini", "A. Saxena", "D. J. Schwarz", "A. Shulevski", "S. S. Sridhar", "H. R. Stacey", "S. Urquhart", "M. H. D. van der Wiel", "E. Varenius", "B. Webster", "A. Wilber"]}, "953": {"id": "2109.13543v1", "title": "The JCMT BISTRO Survey: An 850/450$\u03bc$m Polarization Study of NGC 2071IR in OrionB", "url": "http://arxiv.org/pdf/2109.13543v1", "date": "2021-09-28 07:50:29", "abs": "We present the results of simultaneous 450 $\\mu$m and 850 $\\mu$m polarization\nobservations toward the massive star forming region NGC 2071IR, a target of the\nBISTRO (B-fields in Star-Forming Region Observations) Survey, using the POL-2\npolarimeter and SCUBA-2 camera mounted on the James Clerk Maxwell Telescope. We\nfind a pinched magnetic field morphology in the central dense core region,\nwhich could be due to a rotating toroidal disk-like structure and a bipolar\noutflow originating from the central young stellar object, IRS 3. Using the\nmodified Davis-Chandrasekhar-Fermi method, we obtain a plane-of-sky magnetic\nfield strength of 563$\\pm$421 $\\mu$G in the central $\\sim$0.12 pc region from\n850 $\\mu$m polarization data. The corresponding magnetic energy density of\n2.04$\\times$10$^{-8}$ erg cm$^{-3}$ is comparable to the turbulent and\ngravitational energy densities in the region. We find that the magnetic field\ndirection is very well aligned with the whole of the IRS 3 bipolar outflow\nstructure. We find that the median value of polarization fractions, 3.0 \\%, at\n450 $\\mu$m in the central 3 arcminute region, which is larger than the median\nvalue of 1.2 \\% at 850 $\\mu$m. The trend could be due to the better alignment\nof warmer dust in the strong radiation environment. We also find that\npolarization fractions decrease with intensity at both wavelengths, with\nslopes, determined by fitting a Rician noise model, of $0.59 \\pm 0.03$ at 450\n$\\mu$m and $0.36 \\pm 0.04$ at 850 $\\mu$m, respectively. We think that the\nshallow slope at 850 $\\mu$m is due to grain alignment at the center being\nassisted by strong radiation from the central young stellar objects.", "cat": "astro-ph.GA", "authors": ["A-Ran Lyo", "Jongsoo Kim", "Sarah Sadavoy", "Doug Johnstone", "David Berry", "Kate Pattle", "Woojin Kwon", "Pierre Bastien", "Takashi Onaka", "James Di Francesco", "Ji-Hyun Kang", "Ray Furuya", "Charles L. H. Hull", "Motohide Tamura", "Patrick M. Koch", "Derek Ward-Thompson", "Tetsuo Hasegawa", "Thiem Hoang", "Doris Arzoumanian", "Chang Won Lee", "Chin-Fei Lee", "Do-Young Byun", "Florian Kirchschlager", "Yasuo Doi", "Kee-Tae Kim", "Jihye Hwang", "Pham Ngoc Diep", "Lapo Fanciullo", "Sang-Sung Lee", "Geumsook Park", "Hyunju Yoo", "Eun Jung Chung", "Anthony Whitworth", "Steve Mairs", "Archana Soam", "Tie Liu", "Xindi Tang", "Simon Coud\u00e9", "Philippe Andr\u00e9", "Tyler L. Bourke", "Huei-Ru Vivien Chen", "Zhiwei Chen", "Wen Ping Chen", "Mike Chen", "Tao-Chung Ching", "Jungyeon Cho", "Minho Choi", "Yunhee Choi", "Antonio Chrysostomou", "Sophia Dai", "C. Darren Dowell", "Hao-Yuan Duan", "Yan Duan", "David Eden", "Chakali Eswaraiah", "Stewart Eyres", "Jason Fiege", "Laura M. Fisse", "Erica Franzmann", "Per Friberg", "Rachel Friesen", "Gary Fuller", "Tim Gledhill", "Sarah Graves", "Jane Greaves", "Matt Griffin", "Qilao Gu", "Ilseung Han", "Jannifer Hatchell", "Saeko Hayashi", "Martin Houde", "Tsuyoshi Inoue", "Shu-ichiro Inutsuka", "Kazunari Iwasaki", "Il-Gyo Jeong", "Miju Kang", "Akimasa Kataoka", "Koji Kawabata", "Francisca Kemper", "Gwanjeong Kim", "Mi-Ryang Kim", "Shinyoung Kim", "Kyoung Hee Kim", "Jason Kirk", "Masato I. N. Kobayashi", "Vera K\u00f6nyves", "Takayoshi Kusune", "Jungmi Kwon", "Kevin Lacaille", "Shih-Ping Lai", "Chi-Yan Law", "Jeong-Eun Lee", "Yong-Hee Lee", "Hyeseung Lee", "Dalei Li", "Di Li", "Hua-Bai Li", "Hong-Li Liu", "Junhao Liu", "Sheng-Yuan Liu", "Xing Lu", "Masafumi Matsumura", "Brenda Matthews", "Gerald Moriarty-Schieven", "Tetsuya Nagata", "Fumitaka Nakamura", "Hiroyuki Nakanishi", "Nguyen Bich Ngoc", "Nagayoshi Ohashi", "Harriet Parsons", "Nicolas Peretto", "Felix Priestley", "Tae-soo Pyo", "Lei Qian", "Keping Qiu", "Ramprasad Rao", "Jonathan Rawlings", "Mark G. Rawlings", "Brendan Retter", "John Richer", "Andrew Rigby", "Hiro Saito", "Giorgio Savini", "Anna Scaife", "Masumichi Seta", "Yoshito Shimajiri", "Hiroko Shinnaga", "Mehrnoosh Tahani", "Ya-Wen Tang", "Kohji Tomisaka", "Le Ngoc Tram", "Yusuke Tsukamoto", "Serena Viti", "Jia-Wei Wang", "Hongchi Wang", "Jinjin Xie", "Hsi-Wei Yen", "Jinghua Yuan", "Hyeong-Sik Yun", "Tetsuya Zenko", "Guoyin Zhang", "Chuan-Peng Zhang", "Yapeng Zhang", "Jianjun Zhou", "Lei Zhu", "Ilse de Looze"]}, "954": {"id": "1703.05864v1", "title": "OH Survey along Sightlines of Galactic Observations of Terahertz C+", "url": "http://arxiv.org/pdf/1703.05864v1", "date": "2017-03-17 01:33:38", "abs": "We have obtained OH spectra of four transitions in the $^2\\Pi_{3/2}$ ground\nstate, at 1612, 1665, 1667, and 1720 MHz, toward 51 sightlines that were\nobserved in the Herschel project Galactic Observations of Terahertz C+. The\nobservations cover the longitude range of (32$^\\circ$, 64$^\\circ$) and\n(189$^\\circ$, 207$^\\circ$) in the northern Galactic plane. All of the diffuse\nOH emissions conform to the so-called 'Sum Rule' of the four brightness\ntemperatures, indicating optically thin emission condition for OH from diffuse\nclouds in the Galactic plane. The column densities of the HI `halos' N(HI)\nsurrounding molecular clouds increase monotonically with OH column density,\nN(OH), until saturating when N(HI)=1.0 x 10$^{21}$ cm$^{-2}$ and N (OH) $\\geq\n4.5\\times 10^{15}$ cm$^{-2}$, indicating the presence of molecular gas that\ncannot be traced by HI. Such a linear correlation, albeit weak, is suggestive\nof HI halos' contribution to the UV shielding required for molecular formation.\nAbout 18% of OH clouds have no associated CO emission (CO-dark) at a\nsensitivity of 0.07 K but are associated with C$^+$ emission. A weak\ncorrelation exists between C$^+$ intensity and OH column density for CO-dark\nmolecular clouds. These results imply that OH seems to be a better tracer of\nmolecular gas than CO in diffuse molecular regions.", "cat": "astro-ph.GA", "authors": ["Ningyu Tang", "Di Li", "Carl Heiles", "Nannan Yue", "J. R. Dawson", "Paul F. Goldsmith", "Marko Kr\u010do", "N. M. McClure-Griffiths", "Shen Wang", "Pei Zuo", "Jorge L. Pineda", "Jun-Jie Wang"]}, "955": {"id": "1807.04639v1", "title": "Moving Objects Analytics: Survey on Future Location & Trajectory Prediction Methods", "url": "http://arxiv.org/pdf/1807.04639v1", "date": "2018-07-11 08:01:38", "abs": "The tremendous growth of positioning technologies and GPS enabled devices has\nproduced huge volumes of tracking data during the recent years. This source of\ninformation constitutes a rich input for data analytics processes, either\noffline (e.g. cluster analysis, hot motion discovery) or online (e.g.\nshort-term forecasting of forthcoming positions). This paper focuses on\npredictive analytics for moving objects (could be pedestrians, cars, vessels,\nplanes, animals, etc.) and surveys the state-of-the-art in the context of\nfuture location and trajectory prediction. We provide an extensive review of\nover 50 works, also proposing a novel taxonomy of predictive algorithms over\nmoving objects. We also list the properties of several real datasets used in\nthe past for validation purposes of those works and, motivated by this, we\ndiscuss challenges that arise in the transition from conventional to Big Data\napplications.\n CCS Concepts: Information systems > Spatial-temporal systems; Information\nsystems > Data analytics; Information systems > Data mining; Computing\nmethodologies > Machine learning Additional Key Words and Phrases: mobility\ndata, moving object trajectories, trajectory prediction, future location\nprediction.", "cat": "cs.LG", "authors": ["Harris Georgiou", "Sophia Karagiorgou", "Yannis Kontoulis", "Nikos Pelekis", "Petros Petrou", "David Scarlatti", "Yannis Theodoridis"]}, "956": {"id": "1705.04517v1", "title": "Is there agreement on the prestige of scholarly book publishers in the Humanities? DELPHI over survey results", "url": "http://arxiv.org/pdf/1705.04517v1", "date": "2017-05-12 11:30:01", "abs": "Despite having an important role supporting assessment processes, criticism\ntowards evaluation systems and the categorizations used are frequent.\nConsidering the acceptance by the scientific community as an essential issue\nfor using rankings or categorizations in research evaluation, the aim of this\npaper is testing the results of rankings of scholarly book publishers'\nprestige, Scholarly Publishers Indicators (SPI hereafter). SPI is a public,\nsurvey-based ranking of scholarly publishers' prestige (among other\nindicators). The latest version of the ranking (2014) was based on an expert\nconsultation with a large number of respondents. In order to validate and\nrefine the results for Humanities' fields as proposed by the assessment\nagencies, a Delphi technique was applied with a panel of randomly selected\nexperts over the initial rankings. The results show an equalizing effect of the\ntechnique over the initial rankings as well as a high degree of concordance\nbetween its theoretical aim (consensus among experts) and its empirical results\n(summarized with Gini Index). The resulting categorization is understood as\nmore conclusive and susceptible of being accepted by those under evaluation.", "cat": "cs.DL", "authors": ["Elea Gim\u00e9nez-Toledo", "Jorge Ma\u00f1ana-Rodr\u00edguez"]}, "957": {"id": "2301.06263v1", "title": "Upcoming SKA precursor surveys and sensitivity to HI mass function", "url": "http://arxiv.org/pdf/2301.06263v1", "date": "2023-01-16 05:10:19", "abs": "We describe a simulation for the distribution of galaxies focusing on the\natomic Hydrogen content. We aim to make predictions for surveys of galaxies\nusing the redshifted 21 cm line emission. We take the expected distribution of\nHI masses, circular velocities, sizes of galaxies and orientations into account\nfor this simulation. We use the sensitivity of ASKAP and MeeKAT radio\ntelescopes to estimate the number of detections of HI galaxies in upcoming\nsurveys. We validate our simulation with earlier estimates carried out by using\nsome of these considerations. We show that unlike earlier simulations that take\nsome of the factors into account, the predicted number of galaxies and their\ndistribution across masses changes significantly when all of these are\naccounted for. We describe our predictions for the MIGHTEE-HI and WALLABY\nsurveys for blind detection of galaxies using the redshifted 21 cm radiation.\nWe study the dependence of the predicted number of detections on the HI mass\nfunction. We also describe our future plans for improving the simulation.", "cat": "astro-ph.CO", "authors": ["Sauraj Bharti", "J. S. Bagla"]}, "958": {"id": "2110.12394v1", "title": "Housing property rights and social integration of migrant population: based on the 2017 china migrants' dynamic survey", "url": "http://arxiv.org/pdf/2110.12394v1", "date": "2021-10-24 09:07:35", "abs": "Push-pull theory, one of the most important macro theories in demography,\nargues that population migration is driven by a combination of push (repulsive)\nforces at the place of emigration and pull (attractive) forces at the place of\nemigration. Based on the push-pull theory, this paper shows another practical\nperspective of the theory by measuring the reverse push and pull forces from\nthe perspective of housing property rights. We use OLS and sequential Probit\nmodels to analyze the impact of urban and rural property rights factors on the\nsocial integration of the migrant population-based, on \"China Migrants' Dynamic\nSurvey\". We found that after controlling for personal and urban\ncharacteristics, there is a significant negative effect of rural property\nrights (homestead) ownership of the mobile population on their socio-economic\nintegration, and cultural and psychological integration in the inflow area. The\neffect of urban house price on social integration of the migrant population is\nconsistent with the \"inverted U-shaped\" nonlinear assumption: when the house\nprice to income ratio of the migrant population in the inflow area increases\nbeyond the inflection point, its social integration level decreases. That is,\nthere is an inverse push force and pull force mechanism of housing property\nrights on population mobility.", "cat": "econ.GN", "authors": ["Jingwen Tan", "Shixi Kang"]}, "959": {"id": "2112.04669v2", "title": "A Survey on Parameterized Inapproximability: $k$-Clique, $k$-SetCover, and More", "url": "http://arxiv.org/pdf/2112.04669v2", "date": "2021-12-10 01:40:51", "abs": "In the past a few years, many interesting inapproximability results have been\nobtained from the parameterized perspective. This article surveys some of such\nresults, with a focus on $k$-Clique, $k$-SetCover, and other related problems.", "cat": "cs.CC", "authors": ["Xuandi Ren"]}, "960": {"id": "2108.09142v2", "title": "A multi-level model for estimating region-age-time-type specific male circumcision coverage from household survey and health system data in South Africa", "url": "http://arxiv.org/pdf/2108.09142v2", "date": "2021-09-30 10:07:56", "abs": "Voluntary medical male circumcision (VMMC) reduces the risk of male HIV\nacquisition by 60%. Programmes to provide male circumcision (MC) to prevent HIV\ninfection have been introduced in sub-Saharan African countries with high HIV\nburden. While large-scale provision of MMC is recent, traditional MC has long\nbeen conducted as part of male coming-of-age practices. How and at what age\ntraditional MC occurs varies by ethnic groups within countries. Accurate\nestimates of MC coverage by age and type of circumcision (traditional or\nmedical) over time at sub-national levels are essential for planning and\ndelivering VMMCs to meet targets and evaluating their impacts on HIV incidence.\nIn this paper, we developed a Bayesian competing risks time-to-event model to\nproduce region-age-time-type specific probabilities and coverage of MC with\nprobabilistic uncertainty. The model jointly synthesises data from household\nsurveys and health system data on the number of VMMCs conducted. We\ndemonstrated the model using data from five household surveys and VMMC\nprogramme data to produce estimates of MC coverage for 52 districts in South\nAfrica between 2008 and 2019. Nationally in 2008, 24.1% (CI: 23.4-24.8%) of men\naged 15-49 were traditionally circumcised and 19.4% (CI: 18.9-20.0%) were\nmedically circumcised. Between 2008 and 2019, five million VMMCs were\nconducted, and MC coverage among men aged 15-49 increased to 64.0% (CI:\n63.2-64.9%) and medical MC coverage to 42% (CI: 41.3-43.0%). MC coverage varied\nwidely across districts, ranging from 13.4-86.3%. The average age of\ntraditional MC ranged between 13 to 19 years, depending on local cultural\npractices.", "cat": "stat.AP", "authors": ["Matthew L. Thomas", "Khangelani Zuma", "Dayanund Loykissoonlal", "Bridget Dube", "Peter Vranken", "Sarah E. Porter", "Katharine Kripke", "Thapelo Seatlhodi", "Gesine Meyer-Rath", "Leigh F. Johnson", "Jeffrey W. Eaton"]}, "961": {"id": "1501.04088v1", "title": "Measuring baryon acoustic oscillations with future SKA surveys", "url": "http://arxiv.org/pdf/1501.04088v1", "date": "2015-01-16 20:02:31", "abs": "The imprint of baryon acoustic oscillations (BAO) in large-scale structure\ncan be used as a standard ruler for mapping out the cosmic expansion history,\nand hence for testing cosmological models. In this article we briefly describe\nthe scientific background to the BAO technique, and forecast the potential of\nthe Phase 1 and 2 SKA telescopes to perform BAO surveys using both galaxy\ncatalogues and intensity mapping, assessing their competitiveness with current\nand future optical galaxy surveys. We find that a 25,000 sq. deg. intensity\nmapping survey on a Phase 1 array will preferentially constrain the radial BAO,\nproviding a highly competitive 2% constraint on the expansion rate at z ~ 2. A\n30,000 sq. deg. galaxy redshift survey on SKA2 will outperform all other\nplanned experiments for z < 1.4.", "cat": "astro-ph.CO", "authors": ["Philip Bull", "Stefano Camera", "Alvise Raccanelli", "Chris Blake", "Pedro G. Ferreira", "Mario G. Santos", "Dominik J. Schwarz"]}, "962": {"id": "1404.7128v3", "title": "An ALMA survey of submillimetre galaxies in the Extended Chandra Deep Field South: radio properties and the far-infrared/radio correlation", "url": "http://arxiv.org/pdf/1404.7128v3", "date": "2014-05-21 15:02:48", "abs": "We present a study of the radio properties of 870$\\mu$m-selected\nsubmillimetre galaxies (SMGs), observed at high resolution with ALMA in the\nExtended Chandra Deep Field South. From our initial sample of 76 ALMA SMGs, we\ndetect 52 SMGs at $>3\\sigma$ significance in VLA 1400MHz imaging, of which 35\nare also detected at $>3\\sigma$ in new 610MHz GMRT imaging. Within this sample\nof radio-detected SMGs, we measure a median radio spectral index\n$\\alpha_{610}^{1400} = -0.79 \\pm 0.06$, (with inter-quartile range\n$\\alpha=[-1.16,-0.56]$) and investigate the far-infrared/radio correlation via\nthe parameter $q_{\\rm IR}$, the logarithmic ratio of the rest-frame\n8-1000$\\mu$m flux and monochromatic radio flux. Our median $q_{\\rm IR} = 2.56\n\\pm 0.05$ (inter-quartile range $q_{\\rm IR}=[2.42,2.78]$) is higher than that\ntypically seen in single-dish 870$\\mu$m-selected sources ($q_{\\rm IR} \\sim\n2.4$), which may reflect the fact that our ALMA-based study is not biased to\nradio-bright counterparts, as previous samples were. Finally, we search for\nevidence that $q_{\\rm IR}$ and $\\alpha$ evolve with age in a co-dependent\nmanner, as predicted by starburst models: the data populate the predicted\nregion of parameter space, with the stellar mass tending to increase along\ntracks of $q_{\\rm IR}$ versus $\\alpha$ in the direction expected, providing the\nfirst observational evidence in support of these models.", "cat": "astro-ph.GA", "authors": ["A. P. Thomson", "R. J. Ivison", "J. M. Simpson", "A. M. Swinbank", "Ian Smail", "V. Arumugam", "D. M. Alexander", "A. Beelen", "W. N. Brandt", "I. Chandra", "H. Dannerbauer", "T. R. Greve", "J. A. Hodge", "E. Ibar", "A. Karim", "E. J. Murphy", "E. Schinnerer", "S. Sirothia", "F. Walter", "J. L. Wardlow", "P. van der Werf"]}, "963": {"id": "1809.10738v1", "title": "BAO reconstruction: a swift numerical action method for massive spectroscopic surveys", "url": "http://arxiv.org/pdf/1809.10738v1", "date": "2018-09-27 19:37:25", "abs": "A new fully non-linear reconstruction algorithm for the accurate recovery of\nthe Baryonic Acoustic Oscillations (BAO) scale in two-point correlation\nfunctions is proposed, based on the least-action principle and extending the\nFast Action Minimisation method by Nusser & Branchini (2000). Especially\ndesigned for massive spectroscopic surveys, it is tested on dark-matter halo\ncatalogues extracted from the DEUS-FUR $\\Lambda$CDM simulation to trace the\ntrajectories of up to $\\sim207,000$ haloes backward-in-time, well beyond the\nfirst-order Lagrangian approximation. The new algorithm successfully recovers\nthe BAO feature in real and redshift-space in both the monopole and the\nanisotropic two-point correlation function, also for anomalous samples showing\nmisplaced or absent signature of BAO. In redshift-space the non-linear\ndisplacement parameter $\\Sigma_\\mathrm{NL}$ is reduced from\n$11.8\\pm0.3h^{-1}$Mpc at redshift $z=0$ (pre-reconstruction) to\n$4.0\\pm0.5h^{-1}$Mpc at $z\\simeq37$ after reconstruction. A comparison with the\nfirst-order Lagrangian reconstruction is presented, showing that this\ntechniques outperforms the linear approximation in recovering an unbiased\nmeasurement of the acoustic scale.", "cat": "astro-ph.CO", "authors": ["E. Sarpa", "C. Schimd", "E. Branchini", "S. Matarrese"]}, "964": {"id": "1012.4695v2", "title": "Blind surveys for radio pulsars and transients", "url": "http://arxiv.org/pdf/1012.4695v2", "date": "2010-12-22 18:36:26", "abs": "The main reasons for searching for pulsars are to: (i) get an accurate census\nof the neutron star population and its origin and evolution; (ii) connect\nneutron stars to other stellar populations in the Galaxy and globular clusters;\n(iii) study Galactic astronomy (the interstellar medium and magnetic field);\n(iv) find and study new interesting individual objects; (v) study pulsar\nphenomenology; (vi) find pulsars to add to the sensitivity of pulsar timing\narrays. This review focuses on blind (i.e. large area) searches for radio\npulsars. I'll summarize the methods we use, some of the challenges they\npresent, look at some of the recent and current efforts going on. I will also\nlook at outreach of this area to groups outside the traditional area of pulsar\nresearch, highlight the discoveries of radio transients and look ahead to the\nfuture. Pulsars found at other wavelengths will be reviewed elsewhere in this\nvolume.", "cat": "astro-ph.GA", "authors": ["D. R. Lorimer"]}, "965": {"id": "2108.10076v1", "title": "Development of A Fully Data-Driven Artificial Intelligence and Deep Learning for URLLC Application in 6G Wireless Systems: A Survey", "url": "http://arxiv.org/pdf/2108.10076v1", "date": "2021-08-04 03:05:18", "abs": "The full future of the sixth generation will develop a fully data-driven that\nprovide terabit rate per second, and adopt an average of 1000+ massive number\nof connections per person in 10 years 2030 virtually instantaneously.\nData-driven for ultra-reliable and low latency communication is a new service\nparadigm provided by a new application of future sixth-generation wireless\ncommunication and network architecture, involving 100+ Gbps data rates with one\nmillisecond latency. The key constraint is the amount of computing power\navailable to spread massive data and well-designed artificial neural networks.\nArtificial Intelligence provides a new technique to design wireless networks by\napply learning, predicting, and make decisions to manage the stream of big data\ntraining individuals, which provides more the capacity to transform that expert\nlearning to develop the performance of wireless networks. We study the\ndeveloping technologies that will be the driving force are artificial\nintelligence, communication systems to guarantee low latency. This paper aims\nto discuss the efficiency of the developing network and alleviate the great\nchallenge for application scenarios and study Holographic radio, enhanced\nwireless channel coding, enormous Internet of Things integration, and haptic\ncommunication for virtual and augmented reality provide new services on the 6G\nnetwork. Furthermore, improving a multi-level architecture for ultra-reliable\nand low latency in deep Learning allows for data-driven AI and 6G networks for\ndevice intelligence, as well as allowing innovations based on effective\nlearning capabilities. These difficulties must be solved in order to meet the\nneeds of future smart networks. Furthermore, this research categorizes various\nunexplored research gaps between machine learning and the sixth generation.", "cat": "eess.SP", "authors": ["Adeeb Salh", "Lukman Audah", "Qazwan Abdullah", "Abdullah Noorsaliza", "Nor Shahida Mohd Shah", "Jameel Mukred", "Shipun Hamzah"]}, "966": {"id": "1211.3977v1", "title": "New M, L, and T Dwarf Companions to Nearby Stars from the Wide-field Infrared Survey Explorer", "url": "http://arxiv.org/pdf/1211.3977v1", "date": "2012-11-16 18:16:44", "abs": "We present 11 candidate late-type companions to nearby stars identified with\ndata from the Wide-field Infrared Survey Explorer (WISE) and the Two Micron\nAll-Sky Survey (2MASS). Eight of the candidates are likely to be companions\nbased on their common proper motions with the primaries. The remaining three\nobjects are rejected as companions, one of which is a free-floating T7 dwarf.\nSpectral types are available for five of the companions, which consist of M2V,\nM8.5V, L5, T8, and T8. Based on their photometry, the unclassified companions\nare probably two mid-M dwarfs and one late-M/early-L dwarf. One of the T8\ncompanions, WISE J142320.84+011638.0, has already been reported by Pinfield and\ncoworkers. The other T8 companion, ULAS J095047.28+011734.3, was discovered by\nBurningham and coworkers through the United Kingdom Infrared Telescope Infrared\nDeep Sky Survey, but its companionship has not been previously recognized in\nthe literature. The L5 companion, 2MASS J17430860+8526594, is a new member of a\nclass of L dwarfs that exhibit unusually blue near-IR colors. Among the\npossible mechanisms that have been previously proposed for the peculiar colors\nof these L dwarfs, low metallicity does not appear to be a viable explanation\nfor 2MASS J17430860+8526594 since our spectrum of the primary suggests that its\nmetallicity is not significantly subsolar.", "cat": "astro-ph.GA", "authors": ["Kevin L. Luhman", "Nicholas P. Loutrel", "Nicholas S. McCurdy", "Gregory N. Mace", "Nicole D. Melso", "Kimberly M. Star", "Michael D. Young", "Ryan C. Terrien", "Ian S. McLean", "J. Davy Kirkpatrick", "Katherine L. Rhode"]}, "967": {"id": "1403.4865v1", "title": "The Gaia-ESO Survey: processing of the FLAMES-UVES spectra", "url": "http://arxiv.org/pdf/1403.4865v1", "date": "2014-03-19 16:04:14", "abs": "The Gaia-ESO Survey is a large public spectroscopic survey that aims to\nderive radial velocities and fundamental parameters of about 10^5 Milky Way\nstars in the field and in clusters. Observations are carried out with the\nmulti-object optical spectrograph FLAMES, using simultaneously the medium\nresolution (R~20,000) GIRAFFE spectrograph and the high resolution (R~47,000)\nUVES spectrograph. In this paper, we describe the methods and the software used\nfor the data reduction, the derivation of the radial velocities, and the\nquality control of the FLAMES-UVES spectra. Data reduction has been performed\nusing a workflow specifically developed for this project. This workflow runs\nthe ESO public pipeline optimizing the data reduction for the Gaia-ESO Survey,\nperforms automatically sky subtraction, barycentric correction and\nnormalisation, and calculates radial velocities and a first guess of the\nrotational velocities. The quality control is performed using the output\nparameters from the ESO pipeline, by a visual inspection of the spectra and by\nthe analysis of the signal-to-noise ratio of the spectra.\n Using the observations of the first 18 months, specifically targets observed\nmultiple times at different epochs, stars observed with both GIRAFFE and UVES,\nand observations of radial velocity standards, we estimated the precision and\nthe accuracy of the radial velocities. The statistical error on the radial\nvelocities is sigma~0.4 km s^-1 and is mainly due to uncertainties in the zero\npoint of the wavelength calibration. However, we found a systematic bias with\nrespect to the GIRAFFE spectra (~0.9 km s^-1) and to the radial velocities of\nthe standard stars (~0.5 kms^-1) retrieved from the literature. This bias will\nbe corrected in the future data releases, when a common zero point for all the\nsetups and instruments used for the survey will be established.", "cat": "astro-ph.IM", "authors": ["G. G. Sacco", "L. Morbidelli", "E. Franciosini", "E. Maiorca", "S. Randich", "A. Modigliani", "G. Gilmore", "M. Asplund", "J. Binney", "P. Bonifacio", "J. Drew", "S. Feltzing", "A. Ferguson", "R. Jeffries", "G. Micela", "I. Negueruela", "T. Prusti", "H. -W. Rix", "A. Vallenari", "E. Alfaro", "C. Allende Prieto", "C. Babusiaux", "T. Bensby", "R. Blomme", "A. Bragaglia", "E. Flaccomio", "P. Francois", "N. Hambly", "M. Irwin", "S. Koposov", "A. Korn", "A. Lanzafame", "E. Pancino", "A. Recio-Blanco", "R. Smiljanic", "S. Van Eck", "N. Walton", "M. Bergemann", "M. T. Costado", "P. de Laverny", "U. Heiter", "V. Hill", "A. Hourihane", "R. Jackson", "P. Jofre", "J. Lewis", "K. Lind", "C. Lardo", "L. Magrini", "T. Masseron", "L. Prisinzano", "C. Worley"]}, "968": {"id": "1812.05818v3", "title": "JCMT BISTRO survey: Magnetic Fields within the Hub-Filament Structure in IC 5146", "url": "http://arxiv.org/pdf/1812.05818v3", "date": "2019-03-28 02:10:04", "abs": "We present the 850 $\\mu$m polarization observations toward the IC5146\nfilamentary cloud taken using the Submillimetre Common-User Bolometer Array 2\n(SCUBA-2) and its associated polarimeter (POL-2), mounted on the James Clerk\nMaxwell Telescope (JCMT), as part of the B-fields In STar forming Regions\nObservations (BISTRO). This work is aimed at revealing the magnetic field\nmorphology within a core-scale ($\\lesssim 1.0$ pc) hub-filament structure (HFS)\nlocated at the end of a parsec-scale filament. To investigate whether or not\nthe observed polarization traces the magnetic field in the HFS, we analyze the\ndependence between the observed polarization fraction and total intensity using\na Bayesian approach with the polarization fraction described by the Rice\nlikelihood function, which can correctly describe the probability density\nfunction (PDF) of the observed polarization fraction for low signal-to-noise\nratio (SNR) data. We find a power-law dependence between the polarization\nfraction and total intensity with an index of 0.56 in $A_V\\sim$ 20--300 mag\nregions, suggesting that the dust grains in these dense regions can still be\naligned with magnetic fields in the IC5146 regions. Our polarization maps\nreveal a curved magnetic field, possibly dragged by the contraction along the\nparsec-scale filament. We further obtain a magnetic field strength of\n0.5$\\pm$0.2 mG toward the central hub using the Davis-Chandrasekhar-Fermi\nmethod, corresponding to a mass-to-flux criticality of $\\sim$ $1.3\\pm0.4$ and\nan Alfv\\'{e}nic Mach number of $<$0.6. These results suggest that gravity and\nmagnetic field is currently of comparable importance in the HFS, and turbulence\nis less important.", "cat": "astro-ph.GA", "authors": ["Jia-Wei Wang", "Shih-Ping Lai", "Chakali Eswaraiah", "Kate Pattle", "James Di Francesco", "Doug Johnstone", "Patrick M. Koch", "Tie Liu", "Motohide Tamura", "Ray S. Furuya", "Takashi Onaka", "Derek Ward-Thompson", "Archana Soam", "Kee-Tae Kim", "Chang Won Lee", "Chin-Fei Lee", "Steve Mairs", "Doris Arzoumanian", "Gwanjeong Kim", "Thiem Hoang", "Jihye Hwang", "Sheng-Yuan Liu", "David Berry", "Pierre Bastien", "Tetsuo Hasegawa", "Woojin Kwon", "Keping Qiu", "Philippe Andr\u00e9", "Yusuke Aso", "Do-Young Byun", "Huei-Ru Chen", "Michael C. Chen", "Wen Ping Chen", "Tao-Chung Ching", "Jungyeon Cho", "Minho Choi", "Antonio Chrysostomou", "Eun Jung Chung", "Simon Coud\u00e9", "Yasuo Doi", "C. Darren Dowell", "Emily Drabek-Maunder", "Hao-Yuan Duan", "Stewart P. S. Eyres", "Sam Falle", "Lapo Fanciullo", "Jason Fiege", "Erica Franzmann", "Per Friberg", "Rachel K. Friesen", "Gary Fuller", "Tim Gledhill", "Sarah F. Graves", "Jane S. Greaves", "Matt J. Griffin", "Qilao Gu", "Ilseung Han", "Jennifer Hatchell", "Saeko S. Hayashi", "Wayne Holland", "Martin Houde", "Tsuyoshi Inoue", "Shu-ichiro Inutsuka", "Kazunari Iwasaki", "Il-Gyo Jeong", "Yoshihiro Kanamori", "Ji-hyun Kang", "Miju Kang", "Sung-ju Kang", "Akimasa Kataoka", "Koji S. Kawabata", "Francisca Kemper", "Jongsoo Kim", "Kyoung Hee Kim", "Mi-Ryang Kim", "Shinyoung Kim", "Jason M. Kirk", "Masato I. N. Kobayashi", "Vera Konyves", "Jungmi Kwon", "Kevin M. Lacaille", "Hyeseung Lee", "Jeong-Eun Lee", "Sang-Sung Lee", "Yong-Hee Lee", "Dalei Li", "Di Li", "Hua-bai Li", "Hong-Li Liu", "Junhao Liu", "A-Ran Lyo", "Masafumi Matsumura", "Brenda C. Matthews", "Gerald H. Moriarty-Schieven", "Tetsuya Nagata", "Fumitaka Nakamura", "Hiroyuki Nakanishi", "Nagayoshi Ohashi", "Geumsook Park", "Harriet Parsons", "Enzo Pascale", "Nicolas Peretto", "Andy Pon", "Tae-Soo Pyo", "Lei Qian", "Ramprasad Rao", "Mark G. Rawlings", "Brendan Retter", "John Richer", "Andrew Rigby", "Jean-Fran\u00e7ois Robitaille", "Sarah Sadavoy", "Hiro Saito", "Giorgio Savini", "Anna M. M. Scaife", "Masumichi Seta", "Hiroko Shinnaga", "Ya-Wen Tang", "Kohji Tomisaka", "Yusuke Tsukamoto", "Sven van Loo", "Hongchi Wang", "Anthony P. Whitworth", "Hsi-Wei Yen", "Hyunju Yoo", "Jinghua Yuan", "Hyeong-Sik Yun", "Tetsuya Zenko", "Chuan-Peng Zhang", "Guoyin Zhang", "Ya-Peng Zhang", "Jianjun Zhou", "Zhu"]}, "969": {"id": "2008.06353v1", "title": "Survey of XAI in digital pathology", "url": "http://arxiv.org/pdf/2008.06353v1", "date": "2020-08-14 13:11:54", "abs": "Artificial intelligence (AI) has shown great promise for diagnostic imaging\nassessments. However, the application of AI to support medical diagnostics in\nclinical routine comes with many challenges. The algorithms should have high\nprediction accuracy but also be transparent, understandable and reliable. Thus,\nexplainable artificial intelligence (XAI) is highly relevant for this domain.\nWe present a survey on XAI within digital pathology, a medical imaging\nsub-discipline with particular characteristics and needs. The review includes\nseveral contributions. Firstly, we give a thorough overview of current XAI\ntechniques of potential relevance for deep learning methods in pathology\nimaging, and categorise them from three different aspects. In doing so, we\nincorporate uncertainty estimation methods as an integral part of the XAI\nlandscape. We also connect the technical methods to the specific prerequisites\nin digital pathology and present findings to guide future research efforts. The\nsurvey is intended for both technical researchers and medical professionals,\none of the objectives being to establish a common ground for cross-disciplinary\ndiscussions.", "cat": "cs.CV", "authors": ["Milda Pocevi\u010di\u016bt\u0117", "Gabriel Eilertsen", "Claes Lundstr\u00f6m"]}, "970": {"id": "1004.1638v2", "title": "The Field X-ray AGN Fraction to z=0.7 from the Chandra Multiwavelength Project and the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1004.1638v2", "date": "2010-09-10 18:55:05", "abs": "We employ the Chandra Multiwavelength Project (ChaMP) and the Sloan Digital\nSky Survey (SDSS) to study the fraction of X-ray-active galaxies in the field\nout to z = 0.7. We utilize spectroscopic redshifts from SDSS and ChaMP, as well\nas photometric redshifts from several SDSS catalogs, to compile a parent sample\nof more than 100,000 SDSS galaxies and nearly 1,600 Chandra X-ray detections.\nDetailed ChaMP volume completeness maps allow us to investigate the local\nfraction of active galactic nuclei (AGN), defined as those objects having\nbroad-band X-ray luminosities L_X (0.5-8 keV) > 10^42 erg s^-1, as a function\nof absolute optical magnitude, X-ray luminosity, redshift, mass, and host\ncolor/morphological type. In five independent samples complete in redshift and\ni-band absolute magnitude, we determine the field AGN fraction to be between\n0.16 +/- 0.06% (for z < 0.125 and -18 > M_i > -20) and 3.80 +/- 0.92% (for z <\n0.7 and M_i < -23). We find striking agreement between our ChaMP/SDSS field AGN\nfraction and the Chandra cluster AGN fraction, for samples restricted to\nsimilar redshift and absolute magnitude ranges: 1.19 +/- 0.11% of ChaMP/SDSS\nfield galaxies with 0.05 < z < 0.31 and absolute R-band magnitude more luminous\nthan M_R < -20 are AGN. Our results are also broadly consistent with measures\nof the field AGN fraction in narrow, deep fields, though differences in the\noptical selection criteria, redshift coverage, and possible cosmic variance\nbetween fields introduce larger uncertainties in these comparisons.", "cat": "astro-ph.HE", "authors": ["Daryl Haggard", "Paul J. Green", "Scott F. Anderson", "Anca Constantin", "Tom L. Aldcroft", "Dong-Woo Kim", "Wayne A. Barkhouse"]}, "971": {"id": "2307.15705v2", "title": "Integral Field Spectroscopy of 13 Tidal Disruption Event Hosts from the ZTF Survey", "url": "http://arxiv.org/pdf/2307.15705v2", "date": "2023-09-26 16:04:29", "abs": "The host galaxies of tidal disruption events (TDEs) have been shown to\npossess peculiar properties, including high central light concentrations,\nunusual star-formation histories, and ``green'' colors. The ubiquity of these\nlarge-scale galaxy characteristics among TDE host populations suggests they may\nserve to boost the TDE rate in such galaxies by influencing the nuclear stellar\ndynamics. We present the first population study of integral field spectroscopy\nfor thirteen TDE host galaxies across all spectral classes and X-ray\nbrightnesses with the purpose of investigating their large-scale properties. We\nderive the black hole masses via stellar kinematics (i.e., the $M-\\sigma$\nrelation) and find masses in the range $5.0 \\lesssim \\log(M_{\\rm BH}/M_\\odot)\n\\lesssim 8.0$, with a distribution dominated by black holes with $M_{\\rm BH}\n\\sim 10^6 M_\\odot$. We find one object with $M_{\\rm BH} \\gtrsim 10^8 M_\\odot$,\nabove the ``Hills mass'', which if the disrupted star was of solar type, allows\na lower limit of $a \\gtrsim 0.16$ to be placed on its spin, lending further\nsupport to the proposed connection between featureless TDEs and jetted TDEs. We\nalso explore the level of rotational support in the TDE hosts, quantified by\n$(V/\\sigma)_e$, a parameter which has been shown to correlate with stellar age\nand may explain the peculiar host galaxy preferences of TDEs. We find that the\nTDE hosts exhibit a broad range in $(V/\\sigma)_e$ following a similar\ndistribution as E+A galaxies, which have been shown to be overrepresented among\nTDE host populations.", "cat": "astro-ph.CO", "authors": ["Erica Hammerstein", "S. Bradley Cenko", "Suvi Gezari", "Sylvain Veilleux", "Brendan O'Connor", "Sjoert van Velzen", "Charlotte Ward", "Yuhan Yao", "Matthew Graham"]}, "972": {"id": "1911.00177v1", "title": "Discovery of s-process enhanced stars in the LAMOST survey", "url": "http://arxiv.org/pdf/1911.00177v1", "date": "2019-11-01 01:39:12", "abs": "Here we present the discovery of 895 s-process-rich candidates from 454,180\ngiant stars observed by the Large Sky Area Multi-Object Fibre Spectroscopic\nTelescope (LAMOST) using a data-driven approach. This sample constitutes the\nlargest number of s-process enhanced stars ever discovered. Our sample includes\n187 s-process-rich candidates that are enhanced in both barium and strontium,\n49 stars with significant barium enhancement only and 659 stars that show only\na strontium enhancement. Most of the stars in our sample are in the range of\neffective temperature and log g typical of red giant branch (RGB) populations,\nwhich is consistent with our observational selection bias towards finding RGB\nstars. We estimate that only a small fraction (0.5 per cent) of binary\nconfigurations are favourable for s-process enriched stars. The majority of our\ns-process-rich candidates (95 per cent) show strong carbon enhancements,\nwhereas only five candidates (less than 3 percent) show evidence of sodium\nenhancement. Our kinematic analysis reveals that 97 percent of our sample are\ndisc stars, with the other 3 percent showing velocities consistent with the\nGalactic halo. The scaleheight of the disc is estimated to be zh=0.634kpc,\ncomparable with values in the literature. A comparison with the yields from\nasymptotic giant branch (AGB) models suggests that the main neutron source\nresponsible for the Ba and Sr enhancements is the 13C(alpha,n)16O reaction. We\nconclude that the s-process-rich candidates may have received their\noverabundances via mass transfer from a previous ABG companion with an initial\nmass in the range 1-3Msun.", "cat": "astro-ph.SR", "authors": ["Brodie J Norfolk", "Andrew R Casey", "Amanda I Karakas", "Matthew T Miles", "Alex J Kemp", "Kevin C Schlaufman", "Melissa Ness", "Anna Y Q Ho", "John C Lattanzio", "Alexander P Ji"]}, "973": {"id": "2006.04627v3", "title": "A Survey on Split Manufacturing: Attacks, Defenses, and Challenges", "url": "http://arxiv.org/pdf/2006.04627v3", "date": "2020-10-12 11:06:44", "abs": "In today's integrated circuit (IC) ecosystem, owning a foundry is not\neconomically viable, and therefore most IC design houses are now working under\na fabless business model. In order to overcome security concerns associated\nwith the outsorcing of IC fabrication, the Split Manufacturing technique was\nproposed. In Split Manufacturing, the Front End of Line (FEOL) layers\n(transistors and lower metal layers) are fabricated at an untrusted high-end\nfoundry, while the Back End of Line (BEOL) layers (higher metal layers) are\nmanufactured at a trusted low-end foundry. This approach hides the BEOL\nconnections from the untrusted foundry, thus preventing overproduction and\npiracy threats. However, many works demonstrate that BEOL connections can be\nderived by exploiting layout characteristics that are introduced by heuristics\nemployed in typical floorplanning, placement, and routing algorithms. Since\nstraightforward Split Manufacturing may not afford a desirable security level,\nmany authors propose defense techniques to be used along with Split\nManufacturing. In our survey, we present a detailed overview of the technique,\nthe many types of attacks towards Split Manufacturing, as well as possible\ndefense techniques described in the literature. For the attacks, we present a\nconcise discussion on the different threat models and assumptions, while for\nthe defenses we classify the studies into three categories: proximity\nperturbation, wire lifting, and layout obfuscation. The main outcome of our\nsurvey is to highlight the discrepancy between many studies -- some claim\nnetlists can be reconstructed with near perfect precision, while others claim\nmarginal success in retrieving BEOL connections. Finally, we also discuss\nfuture trends and challenges inherent to Split Manufacturing, including the\nfundamental difficulty of evaluating the efficiency of the technique.", "cat": "cs.CR", "authors": ["Tiago D. Perez", "Samuel Pagliarini"]}, "974": {"id": "2309.05841v2", "title": "WALLABY Pilot Survey: the Potential Polar Ring Galaxies NGC~4632 and NGC~6156", "url": "http://arxiv.org/pdf/2309.05841v2", "date": "2023-09-14 14:26:55", "abs": "We report on the discovery of two potential polar ring galaxies (PRGs) in the\nWALLABY Pilot Data Release 1 (PDR1). These untargetted detections,\ncross-matched to NGC 4632 and NGC 6156, are some of the first galaxies where\nthe Hi observations show two distinct components. We used the iDaVIE virtual\nreality software to separate the anomalous gas from the galactic gas and find\nthat the anomalous gas comprises ~ 50% of the total H i content of both\nsystems. We have generated plausible 3D kinematic models for each galaxy\nassuming that the rings are circular and inclined at 90 degrees to the galaxy\nbodies. These models show that the data are consistent with PRGs, but do not\ndefinitively prove that the galaxies are PRGs. By projecting these models at\ndifferent combinations of main disk inclinations, ring orientations, and\nangular resolutions in mock datacubes, we have further investigated the\ndetectability of similar PRGs in WALLABY. Assuming that these galaxies are\nindeed PRGs, the detectability fraction, combined with the size distribution of\nWALLABY PDR1 galaxies, implies an incidence rate of ~ 1% - 3%. If this rate\nholds true, the WALLABY survey will detect hundreds of new polar ring galaxies.", "cat": "astro-ph.GA", "authors": ["N. Deg", "R. Palleske", "K. Spekkens", "J. Wang", "T. Jarrett", "J. English", "X. Lin", "J. Yeung", "J. R. Mould", "B. Catinella", "H. D\u00e9nes", "A. Elagali", "B. ~-Q. For", "P. Kamphuis", "B. S. Koribalski", "K. Lee-Waddell", "C. Murugeshan", "S. Oh", "J. Rhee", "P. Serra", "T. Westmeier", "O. I. Wong", "K. Bekki", "A. Bosma", "C. Carignan", "B. W. Holwerda", "N. Yu"]}, "975": {"id": "1505.00136v2", "title": "A survey on modeling of microgrids - from fundamental physics to phasors and voltage sources", "url": "http://arxiv.org/pdf/1505.00136v2", "date": "2016-05-17 16:19:42", "abs": "Microgrids have been identified as key components of modern electrical\nsystems to facilitate the integration of renewable distributed generation\nunits. Their analysis and controller design requires the development of\nadvanced (typically model-based) techniques naturally posing an interesting\nchallenge to the control community. Although there are widely accepted reduced\norder models to describe the dynamic behavior of microgrids, they are typically\npresented without details about the reduction procedure---hampering the\nunderstanding of the physical phenomena behind them. Preceded by an\nintroduction to basic notions and definitions in power systems, the present\nsurvey reviews key characteristics and main components of a microgrid. We\nintroduce the reader to the basic functionality of DC/AC inverters, as well as\nto standard operating modes and control schemes of inverter-interfaced power\nsources in microgrid applications. Based on this exposition and starting from\nfundamental physics, we present detailed dynamical models of the main microgrid\ncomponents. Furthermore, we clearly state the underlying assumptions which lead\nto the standard reduced model with inverters represented by controllable\nvoltage sources, as well as static network and load representations, hence,\nproviding a complete modular model derivation of a three-phase inverter-based\nmicrogrid.", "cat": "cs.SY", "authors": ["Johannes Schiffer", "Daniele Zonetti", "Romeo Ortega", "Aleksandar Stankovic", "Tevfik Sezi", "Joerg Raisch"]}, "976": {"id": "1910.05433v5", "title": "Orchestrating the Development Lifecycle of Machine Learning-Based IoT Applications: A Taxonomy and Survey", "url": "http://arxiv.org/pdf/1910.05433v5", "date": "2020-05-29 21:59:18", "abs": "Machine Learning (ML) and Internet of Things (IoT) are complementary\nadvances: ML techniques unlock complete potentials of IoT with intelligence,\nand IoT applications increasingly feed data collected by sensors into ML\nmodels, thereby employing results to improve their business processes and\nservices. Hence, orchestrating ML pipelines that encompasses model training and\nimplication involved in holistic development lifecycle of an IoT application\noften leads to complex system integration. This paper provides a comprehensive\nand systematic survey on the development lifecycle of ML-based IoT application.\nWe outline core roadmap and taxonomy, and subsequently assess and compare\nexisting standard techniques used in individual stage.", "cat": "cs.DC", "authors": ["Bin Qian", "Jie Su", "Zhenyu Wen", "Devki Nandan Jha", "Yinhao Li", "Yu Guan", "Deepak Puthal", "Philip James", "Renyu Yang", "Albert Y. Zomaya", "Omer Rana", "Lizhe Wang", "Maciej Koutny", "Rajiv Ranjan"]}, "977": {"id": "1812.07036v1", "title": "A Smart and Colorful Cadence for the LSST Wide Fast Deep Survey: Maximizing TDE Science", "url": "http://arxiv.org/pdf/1812.07036v1", "date": "2018-12-17 20:22:33", "abs": "Tidal disruption events (TDEs) are rare, 10^(-7)/yr/Mpc^3 (Hung et al. 2018),\nyet the large survey volume of LSST implies a very large detection rate of\n200/yr/(1000 deg^2) (van Velzen et al. 2011), a factor of 250 increase in the\ndetection capability of the current generation of optical synoptic surveys,\ne.g. ZTF, ASAS-SN, Pan-STARRS, and ATLAS. The goal of this LSST cadence white\npaper is to determine which survey strategy will ensure the efficient selection\nand characterization of TDEs in the LSST Wide-Fast-Deep Survey transient alert\nstream. We conclude that the baseline cadence design fails to 1) measure the\nu-r color and color evolution of transients, a critical parameter for\ndistinguishing TDEs from SNe, and to 2) catch the pre-peak light curves of\ntransients, an essential measurement for probing their rise times, which are in\nturn a probe of black hole mass in TDEs. If we do not harvest the fruits of the\nLSST transient alert stream with photometric classification and early\ndetections, both TDE and SN science will be greatly limited. Hence, we propose\nfor a \"smart\" and \"colorful\" rolling cadence in the Wide-Fast Deep (WFD)\nSurvey, that allows for efficient photometric transient classification from\nwell sampled multi-band light curves, with the 20,000 deg^2 survey divided into\neight 2500 deg^2 strips each observed for one year in Years 2-9, with the full\nWFD area observed in Years 1 & 10. This will yield a legacy sample of 200 TDEs\nper year with early detections in u, g, and r bands for efficient\nclassification and full light curve characterization.", "cat": "astro-ph.IM", "authors": ["Suvi Gezari", "Sjoert van Velzen", "Tiara Hung", "Brad Cenko", "Iair Arcavi"]}, "978": {"id": "2109.10138v1", "title": "Ionizing radiation from AGNs at z>3.3 with the Subaru Hyper Suprime-Cam Survey and the CFHT Large Area U-band Deep Survey (CLAUDS)", "url": "http://arxiv.org/pdf/2109.10138v1", "date": "2021-09-21 12:45:53", "abs": "We use deep and wide imaging data from the CFHT Large Area U-band Deep Survey\n(CLAUDS) and the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) to\nconstrain the ionizing radiation (Lyman Continuum; LyC) escape fraction from\nAGNs at $z \\sim 3 - 4$. For 94 AGNs with spectroscopic redshifts at $3.3 < z <\n4.0$, we use their U-band / i-band flux ratios to estimate LyC transmission of\nindividual AGNs. The distribution of their LyC transmission shows values lower\nthan the range of LyC transmission values for IGM of the same redshift range,\nwhich suggests that LyC escape fraction of AGNs at $z>3.3$ is considerably\nlower than unity in most cases. We do not find any trend in LyC transmission\nvalues depending on their UV luminosities. Based on the photometry of stacked\nimages we find the average flux ratio of LyC and non-ionizing UV photons\nescaping from the objects $(f_{LyC}/f_{UV})^{out} = 0.182 \\pm 0.043$ for AGNs\nat $3.32, and 4% have z>3, so this catalogue is\na huge resource for high redshift galaxies.\n A key parameter for understanding the evolutionary status of infrared\ngalaxies is L_{ir}/L_{opt}, which can be interpreted as the specific\nstar-formation rate for starbursts. For dust tori around Type 1 AGN,\nL_{tor}/L_{opt} is a measure of the torus covering factor and we deduce a mean\ncovering factor of 40%.", "cat": "astro-ph", "authors": ["Michael Rowan-Robinson", "Tom Babbedge", "Seb Oliver", "Markos Trichas", "Stefano Berta", "Carol Lonsdale", "Gene Smith", "David Shupe", "Jason Surace", "Stephane Arnouts", "Olivier LeFevre", "Alejandro Afonso-Luis", "Ismael Perez-Fournon", "Evanthia Hatziminaoglou", "Maria Polletta", "Duncan Farrah", "Mattia Vaccari"]}, "981": {"id": "1708.04649v1", "title": "Machine Learning for Survival Analysis: A Survey", "url": "http://arxiv.org/pdf/1708.04649v1", "date": "2017-08-15 19:03:36", "abs": "Accurately predicting the time of occurrence of an event of interest is a\ncritical problem in longitudinal data analysis. One of the main challenges in\nthis context is the presence of instances whose event outcomes become\nunobservable after a certain time point or when some instances do not\nexperience any event during the monitoring period. Such a phenomenon is called\ncensoring which can be effectively handled using survival analysis techniques.\nTraditionally, statistical approaches have been widely developed in the\nliterature to overcome this censoring issue. In addition, many machine learning\nalgorithms are adapted to effectively handle survival data and tackle other\nchallenging problems that arise in real-world data. In this survey, we provide\na comprehensive and structured review of the representative statistical methods\nalong with the machine learning techniques used in survival analysis and\nprovide a detailed taxonomy of the existing methods. We also discuss several\ntopics that are closely related to survival analysis and illustrate several\nsuccessful applications in various real-world application domains. We hope that\nthis paper will provide a more thorough understanding of the recent advances in\nsurvival analysis and offer some guidelines on applying these approaches to\nsolve new problems that arise in applications with censored data.", "cat": "cs.LG", "authors": ["Ping Wang", "Yan Li", "Chandan K. Reddy"]}, "982": {"id": "1506.03508v1", "title": "A historical survey of P-partitions", "url": "http://arxiv.org/pdf/1506.03508v1", "date": "2015-06-10 23:45:30", "abs": "We give a historical survey of the theory P-partitions, starting with\nMacMahon's work, describing Richard Stanley's contributions and his related\nwork, and continuing with more recent developments.", "cat": "math.CO", "authors": ["Ira M. Gessel"]}, "983": {"id": "2401.10864v1", "title": "The California-Kepler Survey. XI. A Survey of Chromospheric Activity Through the Lens of Precise Stellar Properties", "url": "http://arxiv.org/pdf/2401.10864v1", "date": "2024-01-19 18:06:40", "abs": "Surveys of exoplanet host stars are valuable tools for assessing population\nlevel trends in exoplanets, and their outputs can include stellar ages,\nactivity, and rotation periods. We extracted chromospheric activity\nmeasurements from the California-Kepler Survey (CKS) Gaia survey spectra in\norder to probe connections between stellar activity and fundamental stellar\nproperties. Building on the California Kepler Survey's legacy of 1189 planet\nhost star stellar properties including temperature, surface gravity metallicity\nand isochronal age, we add measurements of the Ca II H and K lines as a proxy\nfor chromospheric activity for 879 planet hosting stars. We used these\nchromospheric activity measurements to derive stellar rotation periods. We find\na discrepancy between photometrically derived and activity-derived rotation\nperiods for stars on the Rossby Ridge. These results support the theory of\nweakened magnetic braking. We find no evidence for metallicity-dependent\nactivity relations, within the metallicity range of -0.2 to +0.3 dex. With our\nsingle epoch spectra we identify stars that are potentially in Maunder Minimum\nlike state using a combination of log (R'HK) and position below the\nmain-sequence. We do not yet have the multi-year time series needed to verify\nstars in Maunder Minimum like states. These results can help inform future\ntheoretical studies that explore the relationship between stellar activity,\nstellar rotation, and magnetic dynamos.", "cat": "astro-ph.SR", "authors": ["Howard Isaacson", "Stephen R. Kane", "Brad Carter", "Andrew W. Howard", "Lauren Weiss", "Erik A. Petigura", "Benjamin Fulton"]}, "984": {"id": "1611.00036v2", "title": "The DESI Experiment Part I: Science,Targeting, and Survey Design", "url": "http://arxiv.org/pdf/1611.00036v2", "date": "2016-12-13 15:55:51", "abs": "DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark\nenergy experiment that will study baryon acoustic oscillations (BAO) and the\ngrowth of structure through redshift-space distortions with a wide-area galaxy\nand quasar redshift survey. To trace the underlying dark matter distribution,\nspectroscopic targets will be selected in four classes from imaging data. We\nwill measure luminous red galaxies up to $z=1.0$. To probe the Universe out to\neven higher redshift, DESI will target bright [O II] emission line galaxies up\nto $z=1.7$. Quasars will be targeted both as direct tracers of the underlying\ndark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the\nLy-$\\alpha$ forest absorption features in their spectra, which will be used to\ntrace the distribution of neutral hydrogen. When moonlight prevents efficient\nobservations of the faint targets of the baseline survey, DESI will conduct a\nmagnitude-limited Bright Galaxy Survey comprising approximately 10 million\ngalaxies with a median $z\\approx 0.2$. In total, more than 30 million galaxy\nand quasar redshifts will be obtained to measure the BAO feature and determine\nthe matter power spectrum, including redshift space distortions.", "cat": "astro-ph.IM", "authors": ["DESI Collaboration", "Amir Aghamousa", "Jessica Aguilar", "Steve Ahlen", "Shadab Alam", "Lori E. Allen", "Carlos Allende Prieto", "James Annis", "Stephen Bailey", "Christophe Balland", "Otger Ballester", "Charles Baltay", "Lucas Beaufore", "Chris Bebek", "Timothy C. Beers", "Eric F. Bell", "Jos\u00e9 Luis Bernal", "Robert Besuner", "Florian Beutler", "Chris Blake", "Hannes Bleuler", "Michael Blomqvist", "Robert Blum", "Adam S. Bolton", "Cesar Briceno", "David Brooks", "Joel R. Brownstein", "Elizabeth Buckley-Geer", "Angela Burden", "Etienne Burtin", "Nicolas G. Busca", "Robert N. Cahn", "Yan-Chuan Cai", "Laia Cardiel-Sas", "Raymond G. Carlberg", "Pierre-Henri Carton", "Ricard Casas", "Francisco J. Castander", "Jorge L. Cervantes-Cota", "Todd M. Claybaugh", "Madeline Close", "Carl T. Coker", "Shaun Cole", "Johan Comparat", "Andrew P. Cooper", "M. -C. Cousinou", "Martin Crocce", "Jean-Gabriel Cuby", "Daniel P. Cunningham", "Tamara M. Davis", "Kyle S. Dawson", "Axel de la Macorra", "Juan De Vicente", "Timoth\u00e9e Delubac", "Mark Derwent", "Arjun Dey", "Govinda Dhungana", "Zhejie Ding", "Peter Doel", "Yutong T. Duan", "Anne Ealet", "Jerry Edelstein", "Sarah Eftekharzadeh", "Daniel J. Eisenstein", "Ann Elliott", "St\u00e9phanie Escoffier", "Matthew Evatt", "Parker Fagrelius", "Xiaohui Fan", "Kevin Fanning", "Arya Farahi", "Jay Farihi", "Ginevra Favole", "Yu Feng", "Enrique Fernandez", "Joseph R. Findlay", "Douglas P. Finkbeiner", "Michael J. Fitzpatrick", "Brenna Flaugher", "Samuel Flender", "Andreu Font-Ribera", "Jaime E. Forero-Romero", "Pablo Fosalba", "Carlos S. Frenk", "Michele Fumagalli", "Boris T. Gaensicke", "Giuseppe Gallo", "Juan Garcia-Bellido", "Enrique Gaztanaga", "Nicola Pietro Gentile Fusillo", "Terry Gerard", "Irena Gershkovich", "Tommaso Giannantonio", "Denis Gillet", "Guillermo Gonzalez-de-Rivera", "Violeta Gonzalez-Perez", "Shelby Gott", "Or Graur", "Gaston Gutierrez", "Julien Guy", "Salman Habib", "Henry Heetderks", "Ian Heetderks", "Katrin Heitmann", "Wojciech A. Hellwing", "David A. Herrera", "Shirley Ho", "Stephen Holland", "Klaus Honscheid", "Eric Huff", "Timothy A. Hutchinson", "Dragan Huterer", "Ho Seong Hwang", "Joseph Maria Illa Laguna", "Yuzo Ishikawa", "Dianna Jacobs", "Niall Jeffrey", "Patrick Jelinsky", "Elise Jennings", "Linhua Jiang", "Jorge Jimenez", "Jennifer Johnson", "Richard Joyce", "Eric Jullo", "St\u00e9phanie Juneau", "Sami Kama", "Armin Karcher", "Sonia Karkar", "Robert Kehoe", "Noble Kennamer", "Stephen Kent", "Martin Kilbinger", "Alex G. Kim", "David Kirkby", "Theodore Kisner", "Ellie Kitanidis", "Jean-Paul Kneib", "Sergey Koposov", "Eve Kovacs", "Kazuya Koyama", "Anthony Kremin", "Richard Kron", "Luzius Kronig", "Andrea Kueter-Young", "Cedric G. Lacey", "Robin Lafever", "Ofer Lahav", "Andrew Lambert", "Michael Lampton", "Martin Landriau", "Dustin Lang", "Tod R. Lauer", "Jean-Marc Le Goff", "Laurent Le Guillou", "Auguste Le Van Suu", "Jae Hyeon Lee", "Su-Jeong Lee", "Daniela Leitner", "Michael Lesser", "Michael E. Levi", "Benjamin L'Huillier", "Baojiu Li", "Ming Liang", "Huan Lin", "Eric Linder", "Sarah R. Loebman", "Zarija Luki\u0107", "Jun Ma", "Niall MacCrann", "Christophe Magneville", "Laleh Makarem", "Marc Manera", "Christopher J. Manser", "Robert Marshall", "Paul Martini", "Richard Massey", "Thomas Matheson", "Jeremy McCauley", "Patrick McDonald", "Ian D. McGreer", "Aaron Meisner", "Nigel Metcalfe", "Timothy N. Miller", "Ramon Miquel", "John Moustakas", "Adam Myers", "Milind Naik", "Jeffrey A. Newman", "Robert C. Nichol", "Andrina Nicola", "Luiz Nicolati da Costa", "Jundan Nie", "Gustavo Niz", "Peder Norberg", "Brian Nord", "Dara Norman", "Peter Nugent", "Thomas O'Brien", "Minji Oh", "Knut A. G. Olsen", "Cristobal Padilla", "Hamsa Padmanabhan", "Nikhil Padmanabhan", "Nathalie Palanque-Delabrouille", "Antonella Palmese", "Daniel Pappalardo", "Isabelle P\u00e2ris", "Changbom Park", "Anna Patej", "John A. Peacock", "Hiranya V. Peiris", "Xiyan Peng", "Will J. Percival", "Sandrine Perruchot", "Matthew M. Pieri", "Richard Pogge", "Jennifer E. Pollack", "Claire Poppett", "Francisco Prada", "Abhishek Prakash", "Ronald G. Probst", "David Rabinowitz", "Anand Raichoor", "Chang Hee Ree", "Alexandre Refregier", "Xavier Regal", "Beth Reid", "Kevin Reil", "Mehdi Rezaie", "Constance M. Rockosi", "Natalie Roe", "Samuel Ronayette", "Aaron Roodman", "Ashley J. Ross", "Nicholas P. Ross", "Graziano Rossi", "Eduardo Rozo", "Vanina Ruhlmann-Kleider", "Eli S. Rykoff", "Cristiano Sabiu", "Lado Samushia", "Eusebio Sanchez", "Javier Sanchez", "David J. Schlegel", "Michael Schneider", "Michael Schubnell", "Aur\u00e9lia Secroun", "Uros Seljak", "Hee-Jong Seo", "Santiago Serrano", "Arman Shafieloo", "Huanyuan Shan", "Ray Sharples", "Michael J. Sholl", "William V. Shourt", "Joseph H. Silber", "David R. Silva", "Martin M. Sirk", "Anze Slosar", "Alex Smith", "George F. Smoot", "Debopam Som", "Yong-Seon Song", "David Sprayberry", "Ryan Staten", "Andy Stefanik", "Gregory Tarle", "Suk Sien Tie", "Jeremy L. Tinker", "Rita Tojeiro", "Francisco Valdes", "Octavio Valenzuela", "Monica Valluri", "Mariana Vargas-Magana", "Licia Verde", "Alistair R. Walker", "Jiali Wang", "Yuting Wang", "Benjamin A. Weaver", "Curtis Weaverdyck", "Risa H. Wechsler", "David H. Weinberg", "Martin White", "Qian Yang", "Christophe Yeche", "Tianmeng Zhang", "Gong-Bo Zhao", "Yi Zheng", "Xu Zhou", "Zhimin Zhou", "Yaling Zhu", "Hu Zou", "Ying Zu"]}, "985": {"id": "2207.14286v1", "title": "Density-clustering of continuous gravitational wave candidates from large surveys", "url": "http://arxiv.org/pdf/2207.14286v1", "date": "2022-07-28 17:59:30", "abs": "Searches for continuous gravitational waves target nearly monochromatic\ngravitational wave emission from e.g. non-axysmmetric fast-spinning neutron\nstars. Broad surveys often require to explicitly search for a very large number\nof different waveforms, easily exceeding $\\sim10^{17}$ templates. In such\ncases, for practical reasons, only the top, say $\\sim10^{10}$, results are\nsaved and followed-up through a hierarchy of stages. Most of these candidates\nare not completely independent of neighbouring ones, but arise due to some\ncommon cause: a fluctuation, a signal or a disturbance. By judiciously\nclustering together candidates stemming from the same root cause, the\nsubsequent follow-ups become more effective. A number of clustering algorithms\nhave been employed in past searches based on iteratively finding symmetric and\ncompact over-densities around candidates with high detection statistic values.\nThe new clustering method presented in this paper is a significant improvement\nover previous methods: it is agnostic about the shape of the over-densities, is\nvery efficient and it is effective: at a very high detection efficiency, it has\na noise rejection of $99.99\\%$ , is capable of clustering two orders of\nmagnitude more candidates than attainable before and, at fixed sensitivity it\nenables more than a factor of 30 faster follow-ups. We also demonstrate how to\noptimally choose the clustering parameters.", "cat": "gr-qc", "authors": ["Benjamin Steltner", "Thorben Menne", "Maria Alessandra Papa", "Heinz-Bernd Eggenstein"]}, "986": {"id": "1901.02401v1", "title": "The Buzzard Flock: Dark Energy Survey Synthetic Sky Catalogs", "url": "http://arxiv.org/pdf/1901.02401v1", "date": "2019-01-08 16:55:16", "abs": "We present a suite of 18 synthetic sky catalogs designed to support science\nanalysis of galaxies in the Dark Energy Survey Year 1 (DES Y1) data. For each\ncatalog, we use a computationally efficient empirical approach, ADDGALS, to\nembed galaxies within light-cone outputs of three dark matter simulations that\nresolve halos with masses above ~5x10^12 h^-1 m_sun at z <= 0.32 and 10^13 h^-1\nm_sun at z~2. The embedding method is tuned to match the observed evolution of\ngalaxy counts at different luminosities as well as the spatial clustering of\nthe galaxy population. Galaxies are lensed by matter along the line of sight\n--- including magnification, shear, and multiple images --- using CALCLENS, an\nalgorithm that calculates shear with 0.42 arcmin resolution at galaxy positions\nin the full catalog. The catalogs presented here, each with the same LCDM\ncosmology (denoted Buzzard), contain on average 820 million galaxies over an\narea of 1120 square degrees with positions, magnitudes, shapes, photometric\nerrors, and photometric redshift estimates. We show that the weak-lensing shear\ncatalog, redMaGiC galaxy catalogs and redMaPPer cluster catalogs provide\nplausible realizations of the same catalogs in the DES Y1 data by comparing\ntheir magnitude, color and redshift distributions, angular clustering, and\nmass-observable relations, making them useful for testing analyses that use\nthese samples. We make public the galaxy samples appropriate for the DES Y1\ndata, as well as the data vectors used for cosmology analyses on these\nsimulations.", "cat": "astro-ph.CO", "authors": ["Joseph DeRose", "Risa H. Wechsler", "Matthew R. Becker", "Michael T. Busha", "Eli S. Rykoff", "Niall MacCrann", "Brandon Erickson", "August E. Evrard", "Andrey Kravtsov", "Daniel Gruen", "Sahar Allam", "Santiago Avila", "Sarah Bridle", "David Brooks", "Elizabeth Buckley-Geer", "Aurelio Carnero Rosell", "Matias Carrasco Kind", "Jorge Carretero", "Francisco J. Castander", "Ross Cawthon", "Martin Crocce", "Luiz N. da Costa", "Christopher Davis", "Juan De Vicente", "J\u00f6rg P. Dietrich", "Peter Doel", "Alex Drlica-Wagner", "Pablo Fosalba", "Josh Frieman", "Juan Garcia-Bellido", "Gaston Gutierrez", "Will G. Hartley", "Devon L. Hollowood", "Ben Hoyle", "David J. James", "Elisabeth Krause", "Kyler Kuehn", "Nikolay Kuropatkin", "Marcos Lima", "Marcio A. G. Maia", "Felipe Menanteau", "Christopher J. Miller", "Ramon Miquel", "Ricardo L. C. Ogando", "Andr\u00e9s Plazas Malag\u00f3n", "A. Kathy Romer", "Eusebio Sanchez", "Rafe Schindler", "Santiago Serrano", "Ignacio Sevilla-Noarbe", "Mathew Smith", "Eric Suchyta", "Molly E. C. Swanson", "Gregory Tarle", "Vinu Vikram"]}, "987": {"id": "1405.2446v2", "title": "The Black Hole Mass - Galaxy Luminosity Relationship for Sloan Digital Sky Survey Quasars", "url": "http://arxiv.org/pdf/1405.2446v2", "date": "2015-02-05 20:17:11", "abs": "We investigate the relationship between the mass of the central supermassive\nblack hole, M_bh, and the host galaxy luminosity, L_gal, in a sample of quasars\nfrom the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7). We use composite\nquasar spectra binned by black hole mass and redshift to assess galaxy features\nthat would otherwise be overwhelmed by noise in individual spectra. The black\nhole mass is calculated using the photoionization method, and the host galaxy\nluminosity is inferred from the depth of the Ca II H + K features in the\ncomposite spectra. We evaluate the evolution in the M_bh - L_gal relationship\nby examining the redshift dependence of Delta log M_bh, the offset in black\nhole mass from the local black hole - bulge relationship. There is little\nsystematic trend in Delta log M_bh out to z = 0.8. Using the width of the [O\nIII] emission line as a proxy for the stellar velocity dispersion, sigma_*, we\nfind agreement of our derived host luminosities with the locally-observed\nFaber-Jackson relation. This supports the utility of the width of the [O III]\nline as a proxy for sigma_* in statistical studies.", "cat": "astro-ph.GA", "authors": ["S. Salviander", "G. A. Shields", "E. W. Bonning"]}, "988": {"id": "2304.06489v1", "title": "Domain Adaptation for Inertial Measurement Unit-based Human Activity Recognition: A Survey", "url": "http://arxiv.org/pdf/2304.06489v1", "date": "2023-04-07 01:33:42", "abs": "Machine learning-based wearable human activity recognition (WHAR) models\nenable the development of various smart and connected community applications\nsuch as sleep pattern monitoring, medication reminders, cognitive health\nassessment, sports analytics, etc. However, the widespread adoption of these\nWHAR models is impeded by their degraded performance in the presence of data\ndistribution heterogeneities caused by the sensor placement at different body\npositions, inherent biases and heterogeneities across devices, and personal and\nenvironmental diversities. Various traditional machine learning algorithms and\ntransfer learning techniques have been proposed in the literature to address\nthe underpinning challenges of handling such data heterogeneities. Domain\nadaptation is one such transfer learning techniques that has gained significant\npopularity in recent literature. In this paper, we survey the recent progress\nof domain adaptation techniques in the Inertial Measurement Unit (IMU)-based\nhuman activity recognition area, discuss potential future directions.", "cat": "eess.SP", "authors": ["Avijoy Chakma", "Abu Zaher Md Faridee", "Indrajeet Ghosh", "Nirmalya Roy"]}, "989": {"id": "2212.05778v1", "title": "Instrumental Variables in Causal Inference and Machine Learning: A Survey", "url": "http://arxiv.org/pdf/2212.05778v1", "date": "2022-12-12 08:59:04", "abs": "Causal inference is the process of using assumptions, study designs, and\nestimation strategies to draw conclusions about the causal relationships\nbetween variables based on data. This allows researchers to better understand\nthe underlying mechanisms at work in complex systems and make more informed\ndecisions. In many settings, we may not fully observe all the confounders that\naffect both the treatment and outcome variables, complicating the estimation of\ncausal effects. To address this problem, a growing literature in both causal\ninference and machine learning proposes to use Instrumental Variables (IV).\nThis paper serves as the first effort to systematically and comprehensively\nintroduce and discuss the IV methods and their applications in both causal\ninference and machine learning. First, we provide the formal definition of IVs\nand discuss the identification problem of IV regression methods under different\nassumptions. Second, we categorize the existing work on IV methods into three\nstreams according to the focus on the proposed methods, including two-stage\nleast squares with IVs, control function with IVs, and evaluation of IVs. For\neach stream, we present both the classical causal inference methods, and recent\ndevelopments in the machine learning literature. Then, we introduce a variety\nof applications of IV methods in real-world scenarios and provide a summary of\nthe available datasets and algorithms. Finally, we summarize the literature,\ndiscuss the open problems and suggest promising future research directions for\nIV methods and their applications. We also develop a toolkit of IVs methods\nreviewed in this survey at https://github.com/causal-machine-learning-lab/mliv.", "cat": "cs.LG", "authors": ["Anpeng Wu", "Kun Kuang", "Ruoxuan Xiong", "Fei Wu"]}, "990": {"id": "1301.5149v7", "title": "Perfect graphs: a survey", "url": "http://arxiv.org/pdf/1301.5149v7", "date": "2015-05-22 12:53:55", "abs": "Perfect graphs were defined by Claude Berge in the 1960s. They are important\nobjects for graph theory, linear programming and combinatorial optimization.\nClaude Berge made a conjecture about them, that was proved by Chudnovsky,\nRobertson, Seymour and Thomas in 2002, and is now called the strong perfect\ngraph theorem. This is a survey about perfect graphs, mostly focused on the\nstrong perfect graph theorem.", "cat": "math.CO", "authors": ["Nicolas Trotignon"]}, "991": {"id": "2009.03643v1", "title": "From Reflecting Brownian Motion to Reflected Stochastic Differential Equations: A Systematic Survey and Complementary Study", "url": "http://arxiv.org/pdf/2009.03643v1", "date": "2020-09-08 11:26:23", "abs": "This work contributes a systematic survey and complementary insights of\nreflecting Brownian motion and its properties. Extension of the Skorohod\nproblem's solution to more general cases is investigated, based on which a\ndiscussion is further conducted on the existence of solutions for a few\nparticular kinds of stochastic differential equations with a reflected\nboundary. It is proved that the multidimensional version of the Skorohod\nequation can be solved under the assumption of a convex domain (D).", "cat": "math.PR", "authors": ["Yunwen Wang", "Jinfeng Li"]}, "992": {"id": "1106.5026v1", "title": "Surveying the Agents of Galaxy Evolution in the Tidally-Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC) II. Cool Evolved Stars", "url": "http://arxiv.org/pdf/1106.5026v1", "date": "2011-06-24 17:42:33", "abs": "We investigate the infrared (IR) properties of cool, evolved stars in the\nSmall Magellanic Cloud (SMC), including the red giant branch (RGB) stars and\nthe dust-producing red supergiant (RSG) and asymptotic giant branch (AGB) stars\nusing observations from the Spitzer Space Telescope Legacy program entitled:\n\"Surveying the Agents of Galaxy Evolution in the Tidally-stripped, Low\nMetallicity SMC\", or SAGE-SMC. The survey includes, for the first time, full\nspatial coverage of the SMC bar, wing, and tail regions at infrared (IR)\nwavelengths (3.6 - 160 microns). We identify evolved stars using a combination\nof near-IR and mid-IR photometry and point out a new feature in the mid-IR\ncolor-magnitude diagram that may be due to particularly dusty O-rich AGB stars.\nWe find that the RSG and AGB stars each contribute ~20% of the global SMC flux\n(extended + point-source) at 3.6 microns, which emphasizes the importance of\nboth stellar types to the integrated flux of distant metal-poor galaxies. The\nequivalent SAGE survey of the higher-metallicity Large Magellanic Cloud\n(SAGE-LMC) allows us to explore the influence of metallicity on dust\nproduction. We find that the SMC RSG stars are less likely to produce a large\namount of dust (as indicated by the [3.6]-[8] color). There is a higher\nfraction of carbon-rich stars in the SMC, and these stars appear to able to\nreach colors as red as their LMC counterparts, indicating that C-rich dust\nforms efficiently in both galaxies. A preliminary estimate of the dust\nproduction in AGB and RSG stars reveals that the extreme C-rich AGB stars\ndominate the dust input in both galaxies, and that the O-rich stars may play a\nlarger role in the LMC than in the SMC.", "cat": "astro-ph.SR", "authors": ["Martha L. Boyer", "Sundar Srinivasan", "Jacco Th. van Loon", "Iain McDonald", "Margaret Meixner", "Dennis Zaritsky", "Karl D. Gordon", "F. Kemper", "Brian Babler", "Miwa Block", "Steve Bracker", "Charles W. Engelbracht", "Joe Hora", "Remy Indebetouw", "Marilyn Meade", "Karl Misselt", "Thomas Robitaille", "Marta Sewilo", "Bernie Shiao", "Barbara Whitney"]}, "993": {"id": "2408.16444v1", "title": "SurveySum: A Dataset for Summarizing Multiple Scientific Articles into a Survey Section", "url": "http://arxiv.org/pdf/2408.16444v1", "date": "2024-08-29 11:13:23", "abs": "Document summarization is a task to shorten texts into concise and\ninformative summaries. This paper introduces a novel dataset designed for\nsummarizing multiple scientific articles into a section of a survey. Our\ncontributions are: (1) SurveySum, a new dataset addressing the gap in\ndomain-specific summarization tools; (2) two specific pipelines to summarize\nscientific articles into a section of a survey; and (3) the evaluation of these\npipelines using multiple metrics to compare their performance. Our results\nhighlight the importance of high-quality retrieval stages and the impact of\ndifferent configurations on the quality of generated summaries.", "cat": "cs.CL", "authors": ["Leandro Car\u00edsio Fernandes", "Gustavo Bartz Guedes", "Thiago Soares Laitz", "Thales Sales Almeida", "Rodrigo Nogueira", "Roberto Lotufo", "Jayr Pereira"]}, "994": {"id": "1805.08247v1", "title": "The implementation of a Fast-Folding pipeline for long-period pulsar searching in the PALFA survey", "url": "http://arxiv.org/pdf/1805.08247v1", "date": "2018-05-21 18:28:40", "abs": "The Pulsar Arecibo L-Band Feed Array (PALFA) survey, the most sensitive blind\nsearch for radio pulsars yet conducted, is ongoing at the Arecibo Observatory\nin Puerto Rico. The vast majority of the 180 pulsars discovered by PALFA have\nspin periods shorter than 2 seconds. Pulsar surveys may miss long-period radio\npulsars due to the summing of a finite number of harmonic components in\nconventional Fourier analyses (typically $\\sim$16), or due to the strong effect\nof red noise at low modulation frequencies. We address this reduction in\nsensitivity by using a time-domain search technique: the Fast-Folding Algorithm\n(FFA). We designed a program that implements a FFA-based search in the PALFA\nprocessing pipeline, and tested the efficiency of the algorithm by performing\ntests under both ideal, white noise conditions, as well as with real PALFA\nobservational data. In the two scenarios, we show that the time-domain\nalgorithm has the ability to outperform the FFT-based periodicity search\nimplemented in the survey. We perform simulations to compare the previously\nreported PALFA sensitivity with that obtained using our new FFA implementation.\nThese simulations show that for a pulsar having a pulse duty cycle of roughly\n3%, the performance of our FFA pipeline exceeds that of our FFT pipeline for\npulses with DM $\\lesssim$ 40 pc cm$^{-3}$ and for periods as short as $\\sim$500\nms, and that the survey sensitivity is improved by at least a factor of two for\nperiods $\\gtrsim$ 6 sec. Discoveries from the implementation of the algorithm\nin PALFA are also presented in this paper.", "cat": "astro-ph.HE", "authors": ["E. Parent", "V. M. Kaspi", "S. M. Ransom", "M. Krasteva", "C. Patel", "P. Scholz", "A. Brazier", "M. A. McLaughlin", "M. Boyce", "W. W. Zhu", "Z. Pleunis", "B. Allen", "S. Bogdanov", "K. Caballero", "F. Camilo", "R. Camuccio", "S. Chatterjee", "J. M. Cordes", "F. Crawford", "J. S. Deneva", "R. Ferdman", "P. C. C. Freire", "J. W. T. Hessels", "F. A. Jenet", "B. Knispel", "P. Lazarus", "J. van Leeuwen", "A. G. Lyne", "R. Lynch", "A. Seymour", "X. Siemens", "I. H. Stairs", "K. Stovall", "J. Swiggum"]}, "995": {"id": "1202.3999v1", "title": "Ensemble Properties of Comets in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1202.3999v1", "date": "2012-02-17 20:00:08", "abs": "We present the ensemble properties of 31 comets (27 resolved and 4\nunresolved) observed by the Sloan Digital Sky Survey (SDSS). This sample of\ncomets represents about 1 comet per 10 million SDSS photometric objects.\nFive-band (u,g,r,i,z) photometry is used to determine the comets' colors,\nsizes, surface brightness profiles, and rates of dust production in terms of\nthe Af{\\rho} formalism. We find that the cumulative luminosity function for the\nJupiter Family Comets in our sample is well fit by a power law of the form N(<\nH) \\propto 10(0.49\\pm0.05)H for H < 18, with evidence of a much shallower fit\nN(< H) \\propto 10(0.19\\pm0.03)H for the faint (14.5 < H < 18) comets. The\nresolved comets show an extremely narrow distribution of colors (0.57 \\pm 0.05\nin g - r for example), which are statistically indistinguishable from that of\nthe Jupiter Trojans. Further, there is no evidence of correlation between color\nand physical, dynamical, or observational parameters for the observed comets.", "cat": "astro-ph.EP", "authors": ["Michael Solontoi", "Zeljko Ivezic", "Mario Juric", "Andrew C. Becker", "Lynne Jones", "Andrew A. West", "Steve Kent", "Robert H. Lupton", "Mark Claire", "Gillian R. Knapp", "Tom Quinn", "James E. Gunn", "Donald P. Schneider"]}, "996": {"id": "2208.06356v2", "title": "Finding Multiply-Lensed and Binary Quasars in the DESI Legacy Imaging Surveys", "url": "http://arxiv.org/pdf/2208.06356v2", "date": "2023-12-10 21:56:25", "abs": "The time delay between multiple images of strongly lensed quasars is a\npowerful tool for measuring the Hubble constant (H0). To achieve H0\nmeasurements with higher precision and accuracy using the time delay, it is\ncrucial to expand the sample of lensed quasars. We conduct a search for\nstrongly lensed quasars in the Dark Energy Spectroscopic Instrument (DESI)\nLegacy Imaging Surveys. The DESI Legacy Surveys comprise 19,000 deg2 of the\nextragalactic sky observed in three optical bands (g, r, and z), making it well\nsuited for the discovery of new strongly lensed quasars. We apply an\nautocorrelation algorithm to ~5 million objects classified as quasars in the\nDESI Quasar Sample. These systems are visually inspected and ranked. Here, we\npresent 436 new multiply lensed and binary quasar candidates, 65 of which have\nredshifts from Sloan Digital Sky Survey Data Release 16. We provide redshifts\nfor an additional 18 candidates from the SuperNova Integral Field Spectrograph.", "cat": "astro-ph.CO", "authors": ["C. Dawes", "C. Storfer", "X. Huang", "G. Aldering", "A. Cikota", "A. Dey", "D. J. Schlegel"]}, "997": {"id": "1911.02685v3", "title": "A Comprehensive Survey on Transfer Learning", "url": "http://arxiv.org/pdf/1911.02685v3", "date": "2020-06-23 15:52:46", "abs": "Transfer learning aims at improving the performance of target learners on\ntarget domains by transferring the knowledge contained in different but related\nsource domains. In this way, the dependence on a large number of target domain\ndata can be reduced for constructing target learners. Due to the wide\napplication prospects, transfer learning has become a popular and promising\narea in machine learning. Although there are already some valuable and\nimpressive surveys on transfer learning, these surveys introduce approaches in\na relatively isolated way and lack the recent advances in transfer learning.\nDue to the rapid expansion of the transfer learning area, it is both necessary\nand challenging to comprehensively review the relevant studies. This survey\nattempts to connect and systematize the existing transfer learning researches,\nas well as to summarize and interpret the mechanisms and the strategies of\ntransfer learning in a comprehensive way, which may help readers have a better\nunderstanding of the current research status and ideas. Unlike previous\nsurveys, this survey paper reviews more than forty representative transfer\nlearning approaches, especially homogeneous transfer learning approaches, from\nthe perspectives of data and model. The applications of transfer learning are\nalso briefly introduced. In order to show the performance of different transfer\nlearning models, over twenty representative transfer learning models are used\nfor experiments. The models are performed on three different datasets, i.e.,\nAmazon Reviews, Reuters-21578, and Office-31. And the experimental results\ndemonstrate the importance of selecting appropriate transfer learning models\nfor different applications in practice.", "cat": "cs.LG", "authors": ["Fuzhen Zhuang", "Zhiyuan Qi", "Keyu Duan", "Dongbo Xi", "Yongchun Zhu", "Hengshu Zhu", "Hui Xiong", "Qing He"]}, "998": {"id": "1502.03644v3", "title": "Random Sampling of Quantum States: A Survey of Methods", "url": "http://arxiv.org/pdf/1502.03644v3", "date": "2015-10-30 13:01:44", "abs": "The numerical generation of random quantum states (RQS) is an important\nprocedure for investigations in quantum information science. Here we review\nsome methods that may be used for performing that task. We start by presenting\na simple procedure for generating random state vectors, for which the main tool\nis the random sampling of unbiased discrete probability distributions (DPD).\nAfterwards the creation of random density matrices is addressed. In this\ncontext we first present the standard method, which consists in using the\nspectral decomposition of a quantum state for getting RQS from random DPDs and\nrandom unitary matrices. In the sequence the Bloch vector parametrization\nmethod is described. This approach, despite being useful in several instances,\nis not in general convenient for RQS generation. In the last part of the\narticle we regard the overparametrized method (OPM) and the related Ginibre and\nBures techniques. The OPM can be used to create random positive semidefinite\nmatrices with unit trace from randomly produced general complex matrices in a\nsimple way that is friendly for numerical implementations. We consider a\nphysically relevant issue related to the possible domains that may be used for\nthe real and imaginary parts of the elements of such general complex matrices.\nSubsequently a too fast concentration of measure in the quantum state space\nthat appears in this parametrization is noticed.", "cat": "quant-ph", "authors": ["Jonas Maziero"]}, "999": {"id": "1804.08245v1", "title": "Chemical survey toward young stellar objects in the Perseus molecular cloud complex", "url": "http://arxiv.org/pdf/1804.08245v1", "date": "2018-04-23 05:16:54", "abs": "Chemical diversity of the gas in low-mass protostellar cores is widely\nrecognized. In order to explore its origin, a survey of chemical composition\ntoward 36 Class 0/I protostars in the Perseus molecular cloud complex, which\nare selected in an unbiased way under certain physical conditions, has been\nconducted with IRAM 30 m and NRO 45 m telescope. Multiple lines of C2H, c-C3H2\nand CH3OH have been observed to characterize the chemical composition averaged\nover a 1000 au scale around the protostar. The derived beam-averaged column\ndensities show significant chemical diversity among the sources, where the\ncolumn density ratios of C2H/CH3OH are spread out by 2 orders of magnitude.\nFrom previous studies, the hot corino sources have abundant CH3OH but deficient\nC2H, their C2H/CH3OH column density ratios being relatively low. In contrast,\nthe warm-carbon-chain chemistry (WCCC) sources are found to reveal the high\nC2H/CH3OH column density ratios. We find that the majority of the sources have\nintermediate characters between these two distinct chemistry types. A possible\ntrend is seen between the C2H/CH3OH ratio and the distance of the source from\nthe edge of a molecular cloud. The sources located near cloud edges or in\nisolated clouds tend to have a high C2H/CH3OH ratio. On the other hand, the\nsources having a low C2H/CH3OH ratio tend to be located in inner regions of the\nmolecular cloud complex. This result gives an important clue to an\nunderstanding of the origin of the chemical diversity of protostellar cores in\nterms of environmental effects.", "cat": "astro-ph.GA", "authors": ["Aya E. Higuchi", "Nami Sakai", "Yoshimasa Watanabe", "Ana Lopez-Sepulcre", "Kento Yoshida", "Yoko Oya", "Muneaki Imai", "Yichen Zhang", "Cecilia Ceccarelli", "Bertrand Lefloch", "Claudio Codella", "Rafael Bachiller", "Tomoya Hirota", "Takeshi Sakai", "Satoshi Yamamoto"]}, "1000": {"id": "2009.14401v2", "title": "Using sex and gender in survey adjustment", "url": "http://arxiv.org/pdf/2009.14401v2", "date": "2022-03-24 03:11:21", "abs": "Accounting for sex and gender is a challenge in social science research.\nWhile other methodology papers consider issues surrounding appropriate\nmeasurement, we consider the problem of adjustment for survey nonresponse and\ngeneralization from samples to populations in the context of the recent push\ntoward measuring sex or gender as a non-binary construct. This is challenging\nnot only in that response categories differ between sex and gender measurement,\nbut also in that both these attributes are potentially multidimensional. We\nreflect on similarities to measuring race/ethnicity before considering the\nethical and statistical implications of the options available to us. We present\na simulation study to understand the statistical implications under a variety\nof scenarios, and demonstrate the application of the decision process with the\nNew York City Poverty Tracker. Overall, we conclude not with a single best\nrecommendation for all surveys but rather with an awareness of the complexity\nof the problem and the benefits and weaknesses of different approaches.", "cat": "stat.AP", "authors": ["Lauren Kennedy", "Katharine Khanna", "Daniel Simpson", "Andrew Gelman", "Yajun Jia", "Julien Teitler"]}, "1001": {"id": "1501.03452v2", "title": "Bright but slow - Type II supernovae from OGLE-IV - Implications for magnitude limited surveys", "url": "http://arxiv.org/pdf/1501.03452v2", "date": "2015-02-25 06:51:27", "abs": "We study a sample of 11 Type II supernovae (SNe) discovered by the OGLE-IV\nsurvey. All objects have well sampled I-band light curves, and at least one\nspectrum. We find that 2 or 3 of the 11 SNe have a declining light curve, and\nspectra consistent with other SNe II-L, while the rest have plateaus that can\nbe as short as 70d, unlike the 100d typically found in nearby galaxies. The\nOGLE SNe are also brighter, and show that magnitude limited surveys find SNe\nthat are different than usually found in nearby galaxies. We discuss this\nsample in the context of understanding Type II SNe as a class and their\nsuggested use as standard candles.", "cat": "astro-ph.HE", "authors": ["Dovi Poznanski", "Zuzanna Kostrzewa-Rutkowska", "Lukasz Wyrzykowski", "Nadejda Blagorodnova"]}, "1002": {"id": "2008.12372v1", "title": "Data-driven Computational Social Science: A Survey", "url": "http://arxiv.org/pdf/2008.12372v1", "date": "2020-08-10 09:28:36", "abs": "Social science concerns issues on individuals, relationships, and the whole\nsociety. The complexity of research topics in social science makes it the\namalgamation of multiple disciplines, such as economics, political science, and\nsociology, etc. For centuries, scientists have conducted many studies to\nunderstand the mechanisms of the society. However, due to the limitations of\ntraditional research methods, there exist many critical social issues to be\nexplored. To solve those issues, computational social science emerges due to\nthe rapid advancements of computation technologies and the profound studies on\nsocial science. With the aids of the advanced research techniques, various\nkinds of data from diverse areas can be acquired nowadays, and they can help us\nlook into social problems with a new eye. As a result, utilizing various data\nto reveal issues derived from computational social science area has attracted\nmore and more attentions. In this paper, to the best of our knowledge, we\npresent a survey on data-driven computational social science for the first time\nwhich primarily focuses on reviewing application domains involving human\ndynamics. The state-of-the-art research on human dynamics is reviewed from\nthree aspects: individuals, relationships, and collectives. Specifically, the\nresearch methodologies used to address research challenges in aforementioned\napplication domains are summarized. In addition, some important open challenges\nwith respect to both emerging research topics and research methods are\ndiscussed.", "cat": "cs.SI", "authors": ["Jun Zhang", "Wei Wang", "Feng Xia", "Yu-Ru Lin", "Hanghang Tong"]}, "1003": {"id": "2206.13309v2", "title": "A Survey of Family Unification Models with Bifundamental Matter", "url": "http://arxiv.org/pdf/2206.13309v2", "date": "2022-09-06 02:35:03", "abs": "Extensions of the Standard Model have been attempted from the bottom up and\nfrom the top down yet there remains a largely unexplored middle ground. In this\npaper, using the Mathematica package LieART, we exhaustively enumerate\nembeddings of the Standard Model within the class of theories with\nbifundamental fermions in product gauge group SU(a)XSU(b)XSU(c) with no more\ngenerators than E6, while achieving SM family unification rather than\nreplication. We incorporate simple phenomenological constrains and find 151\nunique models, including 9 that have only vector-like particle content\nbeyond-the-Standard Model (BSM) particles, which we conjecture belong to 5\ninfinite families of such models. We describe the potentially most viable\nmodels: namely, the 9 with strictly vector-like BSM content along with the 29\nmodels we found with no more than 30 additional BSM chiral particles. These\ninclude models with fractional electric charge color singlets, and hence\nmagnetic monopoles with multiple Dirac charge. This latter collection of models\npredicts chiral particles with masses near the electroweak scale accessible to\ncurrent and future collider experiments.", "cat": "hep-ph", "authors": ["Elijah Sheridan", "Thomas W. Kephart"]}, "1004": {"id": "2007.09013v2", "title": "The Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Growth rate of structure measurement from cosmic voids", "url": "http://arxiv.org/pdf/2007.09013v2", "date": "2022-05-27 11:35:22", "abs": "We present a void clustering analysis in configuration-space using the\ncompleted Sloan Digital Sky Survey IV (SDSS-IV) extended Baryon Oscillation\nSpectroscopic Survey (eBOSS) DR16 samples. These samples consist of Luminous\nRed Galaxies (LRG) combined with the high redshift tail of the SDSS-III Baryon\nOscillation Spectroscopic Survey (BOSS) DR12 CMASS galaxies (called as\nLRG+CMASS sample), Emission Line Galaxies (ELG) and quasars (QSO). We build\nvoid catalogues from the three eBOSS DR16 samples using a ZOBOV-based\nalgorithm, providing 2,814 voids, 1,801 voids and 4,347 voids in the LRG+CMASS,\nELG and QSO samples, respectively, spanning the redshift range $0.6 10 deg).\n In this paper we present the MGPS-2 compact source catalogue. The catalogue\nhas 48,850 sources above a limiting peak brightness of 10 mJy/beam. Positions\nin the catalogue are accurate to 1 arcsec - 2 arcsec. A full catalogue\nincluding extended sources is in preparation. We have carried out an analysis\nof the compact source density across the Galactic plane and find that the\nsource density is not statistically higher than the density expected from the\nextragalactic source density alone.\n We also present version 2.0 of the SUMSS image data and catalogue which are\nnow available online. The data consists of 629 4.3 deg x 4.3 deg mosaic images\ncovering the 8100 deg^2 of sky with dec <= -30 deg and |b| > 10 deg. The\ncatalogue contains 210,412 radio sources to a limiting peak brightness of 6\nmJy/beam at dec <= -50 deg and 10 mJy/beam at dec > -50 deg. We describe the\nupdates and improvements made to the SUMSS cataloguing process.", "cat": "astro-ph", "authors": ["T. Murphy", "T. Mauch", "A. Green", "R. W. Hunstead", "B. Piestrzynska", "A. P. Kels", "P. Sztajer"]}, "1007": {"id": "1104.3477v1", "title": "Deep wide-field near-infrared survey of the Carina Nebula", "url": "http://arxiv.org/pdf/1104.3477v1", "date": "2011-04-18 13:31:15", "abs": "(abbreviated) We used HAWK-I at the ESO VLT to produce a near-infrared survey\nof the Carina Nebula that is deep enough to detect the full low-mass stellar\npopulation. The results of a recent deep X-ray survey are used to distinguish\nbetween young stars in Carina and background contaminants. We find that the\nages of the low-mass stars (derived from color-magnitude diagrams of the\ninvidual cluster in the Carina Nebula) agree with previous age estimates for\nthe massive stars. About 3200 of the X-ray selected stars have masses >= 1\nMsun; this number is in good agreement with extrapolations of the field IMF\nbased on the number of high-mass stars and shows that there is no deficit of\nlow-mass stars. The near-infrared excess fractions for the stellar populations\nin Carina are lower than typical for other, less massive clusters of similar\nage, suggesting a faster timescale of circumstellar disk dispersal than in the\nmore quiescent regions, most likely due to the very high level of massive star\nfeedback. Narrow-band images reveal six molecular hydrogen jets. However, none\nof the optical HH objects shows molecular hydrogen emission, suggesting that\nthe jet-driving protostars are located very close to the edges of the globules\nin which they are embedded. This adds strong support to the scenario that their\nformation was triggered by the advancing ionization fronts.", "cat": "astro-ph.GA", "authors": ["Thomas Preibisch", "Thorsten Ratzka", "Benjamin Kuderna", "Henrike Ohlendorf", "Robert R. King", "Simon Hodgkin", "Mike Irwin", "James R. Lewis", "Mark J. McCaughrean", "Hans Zinnecker"]}, "1008": {"id": "1311.1698v1", "title": "A Survey on the State of the Practice in Distributed Software Development: Criteria for Task Allocation", "url": "http://arxiv.org/pdf/1311.1698v1", "date": "2013-11-05 13:24:14", "abs": "The allocation of tasks can be seen as a success-critical management activity\nin distributed development projects. However, such task allocation is still one\nof the major challenges in global software development due to an insufficient\nunderstanding of the criteria that influence task allocation decisions. This\narticle presents a qualitative study aimed at identifying and understanding\nsuch criteria that are used in practice. Based on interviews with managers from\nselected software development organizations, criteria currently applied in\nindustry are identified. One important result is, for instance, that the\nsourcing strategy and the type of software to be developed have a significant\neffect on the applied criteria. The article presents the goals, design, and\nresults of the study as well as an overview of related and future work.", "cat": "cs.SE", "authors": ["Ansgar Lamersdorf", "J\u00fcrgen M\u00fcnch", "Dieter Rombach"]}, "1009": {"id": "1705.01113v1", "title": "The Pristine survey I: Mining the Galaxy for the most metal-poor stars", "url": "http://arxiv.org/pdf/1705.01113v1", "date": "2017-05-02 18:02:34", "abs": "We present the Pristine survey, a new narrow-band photometric survey focused\non the metallicity-sensitive Ca H & K lines and conducted in the northern\nhemisphere with the wide-field imager MegaCam on the Canada-France-Hawaii\nTelescope (CFHT). This paper reviews our overall survey strategy and discusses\nthe data processing and metallicity calibration. Additionally we review the\napplication of these data to the main aims of the survey, which are to gather a\nlarge sample of the most metal-poor stars in the Galaxy, to further\ncharacterise the faintest Milky Way satellites, and to map the (metal-poor)\nsubstructure in the Galactic halo. The current Pristine footprint comprises\nover 1,000 deg2 in the Galactic halo ranging from b~30 to 78 and covers many\nknown stellar substructures. We demonstrate that, for SDSS stellar objects, we\ncan calibrate the photometry at the 0.02-magnitude level. The comparison with\nexisting spectroscopic metallicities from SDSS/SEGUE and LAMOST shows that,\nwhen combined with SDSS broad-band g and i photometry, we can use the CaHK\nphotometry to infer photometric metallicities with an accuracy of ~0.2 dex from\n[Fe/H]=-0.5 down to the extremely metal-poor regime ([Fe/H]<-3.0). After the\nremoval of various contaminants, we can efficiently select metal-poor stars and\nbuild a very complete sample with high purity. The success rate of uncovering\n[Fe/H]SEGUE<-3.0 stars among [Fe/H]Pristine<-3.0 selected stars is 24% and 85%\nof the remaining candidates are still very metal poor ([Fe/H]<-2.0). We further\ndemonstrate that Pristine is well suited to identify the very rare and pristine\nGalactic stars with [Fe/H]<-4.0, which can teach us valuable lessons about the\nearly Universe.", "cat": "astro-ph.GA", "authors": ["Else Starkenburg", "Nicolas Martin", "Kris Youakim", "David S. Aguado", "Carlos Allende Prieto", "Anke Arentsen", "Edouard J. Bernard", "Piercarlo Bonifacio", "Elisabetta Caffau", "Raymond G. Carlberg", "Patrick Cote", "Morgan Fouesneau", "Patrick Francois", "Oliver Franke", "Jonay I. Gonzalez Hernandez", "Stephen D. J. Gwyn", "Vanessa Hill", "Rodrigo A. Ibata", "Pascale Jablonka", "Nicolas Longeard", "Alan W. McConnachie", "Julio F. Navarro", "Ruben Sanchez-Janssen", "Eline Tolstoy", "Kim A. Venn"]}, "1010": {"id": "2006.06091v3", "title": "Autonomous Driving with Deep Learning: A Survey of State-of-Art Technologies", "url": "http://arxiv.org/pdf/2006.06091v3", "date": "2020-07-04 04:38:43", "abs": "Since DARPA Grand Challenges (rural) in 2004/05 and Urban Challenges in 2007,\nautonomous driving has been the most active field of AI applications. Almost at\nthe same time, deep learning has made breakthrough by several pioneers, three\nof them (also called fathers of deep learning), Hinton, Bengio and LeCun, won\nACM Turin Award in 2019. This is a survey of autonomous driving technologies\nwith deep learning methods. We investigate the major fields of self-driving\nsystems, such as perception, mapping and localization, prediction, planning and\ncontrol, simulation, V2X and safety etc. Due to the limited space, we focus the\nanalysis on several key areas, i.e. 2D and 3D object detection in perception,\ndepth estimation from cameras, multiple sensor fusion on the data, feature and\ntask level respectively, behavior modelling and prediction of vehicle driving\nand pedestrian trajectories.", "cat": "cs.CV", "authors": ["Yu Huang", "Yue Chen"]}, "1011": {"id": "1410.5427v2", "title": "Adding Context to JWST Surveys with Current and Future 21cm Radio Observations", "url": "http://arxiv.org/pdf/1410.5427v2", "date": "2014-12-27 21:08:02", "abs": "Infrared and radio observations of the Epoch of Reionization promise to\nrevolutionize our understanding of the cosmic dawn, and major efforts with the\nJWST, MWA and HERA are underway. While measurements of the ionizing sources\nwith infrared telescopes and the effect of these sources on the intergalactic\nmedium with radio telescopes \\emph{should} be complementary, to date the wildly\ndisparate angular resolutions and survey speeds have made connecting proposed\nobservations difficult. In this paper we develop a method to bridge the gap\nbetween radio and infrared studies. While the radio images may not have the\nsensitivity and resolution to identify individual bubbles with high fidelity,\nby leveraging knowledge of the measured power spectrum we are able to separate\nregions that are likely ionized from largely neutral, providing context for the\nJWST observations of galaxy counts and properties in each. By providing the\nionization context for infrared galaxy observations, this method can\nsignificantly enhance the science returns of JWST and other infrared\nobservations.", "cat": "astro-ph.CO", "authors": ["Adam P. Beardsley", "Miguel F. Morales", "Adam Lidz", "Matthew Malloy", "Paul M. Sutter"]}, "1012": {"id": "1810.10446v1", "title": "The Role of Data in Model Building and Prediction: A Survey Through Examples", "url": "http://arxiv.org/pdf/1810.10446v1", "date": "2018-10-24 15:20:51", "abs": "The goal of Science is to understand phenomena and systems in order to\npredict their development and gain control over them. In the scientific process\nof knowledge elaboration, a crucial role is played by models which, in the\nlanguage of quantitative sciences, mean abstract mathematical or algorithmical\nrepresentations. This short review discusses a few key examples from Physics,\ntaken from dynamical systems theory, biophysics, and statistical mechanics,\nrepresenting three paradigmatic procedures to build models and predictions from\navailable data. In the case of dynamical systems we show how predictions can be\nobtained in a virtually model-free framework using the methods of analogues,\nand we briefly discuss other approaches based on machine learning methods. In\ncases where the complexity of systems is challenging, like in biophysics, we\nstress the necessity to include part of the empirical knowledge in the models\nto gain the minimal amount of realism. Finally, we consider many body systems\nwhere many (temporal or spatial) scales are at play and show how to derive from\ndata a dimensional reduction in terms of a Langevin dynamics for their slow\ncomponents.", "cat": "cond-mat.stat-mech", "authors": ["Marco Baldovin", "Fabio Cecconi", "Massimo Cencini", "Andrea Puglisi", "Angelo Vulpiani"]}, "1013": {"id": "1810.04815v1", "title": "A Framework for Telescope Schedulers: With Applications to the Large Synoptic Survey Telescope", "url": "http://arxiv.org/pdf/1810.04815v1", "date": "2018-10-11 01:37:13", "abs": "How ground-based telescopes schedule their observations in response to\ncompeting science priorities and constraints, variations in the weather, and\nthe visibility of a particular part of the sky can significantly impact their\nefficiency. In this paper we introduce the Feature-Based telescope scheduler\nthat is an automated, proposal-free decision making algorithm that offers\n\\textit{controllability} of the behavior, \\textit{adjustability} of the\nmission, and quick \\textit{recoverability} from interruptions for large\nground-based telescopes. By framing this scheduler in the context of a coherent\nmathematical model the functionality and performance of the algorithm is simple\nto interpret and adapt to a broad range of astronomical applications. This\npaper presents a generic version of the Feature-Based scheduler, with minimal\nmanual tailoring, to demonstrate its potential and flexibility as a foundation\nfor large ground-based telescope schedulers which can later be adjusted for\nother instruments. In addition, a modified version of the Feature-Based\nscheduler for the Large Synoptic Survey Telescope (LSST) is introduced and\ncompared to previous LSST scheduler simulations.", "cat": "astro-ph.IM", "authors": ["Elahesadat Naghib", "Peter Yoachim", "Robert J. Vanderbei", "Andrew J. Connolly", "R. Lynne Jones"]}, "1014": {"id": "1301.5322v1", "title": "High-pressure, low-abundance water in bipolar outflows. Results from a Herschel-WISH survey", "url": "http://arxiv.org/pdf/1301.5322v1", "date": "2013-01-22 21:00:07", "abs": "(Abridged) We present a survey of the water emission in a sample of more than\n20 outflows from low mass young stellar objects with the goal of characterizing\nthe physical and chemical conditions of the emitting gas. We have used the HIFI\nand PACS instruments on board the Herschel Space Observatory to observe the two\nfundamental lines of ortho-water at 557 and 1670 GHz. These observations were\npart of the \"Water In Star-forming regions with Herschel\" (WISH) key program,\nand have been complemented with CO and H2 data. We find that the emission from\nwater has a different spatial and velocity distribution from that of the J=1-0\nand 2-1 transitions of CO, but it has a similar spatial distribution to H2, and\nits intensity follows the H2 intensity derived from IRAC images. This suggests\nthat water traces the outflow gas at hundreds of kelvins responsible for the H2\nemission, and not the component at tens of kelvins typical of low-J CO\nemission. A warm origin of the water emission is confirmed by a remarkable\ncorrelation between the intensities of the 557 and 1670 GHz lines, which also\nindicates the emitting gas has a narrow range of excitations. A non-LTE\nradiative transfer analysis shows that while there is some ambiguity on the\nexact combination of density and temperature values, the gas thermal pressure\nnT is constrained within less than a factor of 2. The typical nT over the\nsample is 4 10^{9} cm^{-3}K, which represents an increase of 10^4 with respect\nto the ambient value. The data also constrain within a factor of 2 the water\ncolumn density. When this quantity is combined with H2 column densities, the\ntypical water abundance is only 3 10^{-7}, with an uncertainty of a factor of\n3. Our data challenge current C-shock models of water production due to a\ncombination of wing-line profiles, high gas compressions, and low abundances.", "cat": "astro-ph.GA", "authors": ["M. Tafalla", "R. Liseau", "B. Nisini", "R. Bachiller", "J. Santiago-Garc\u00eda", "E. F. van Dishoeck", "L. E. Kristensen", "G. J. Herczeg", "U. A. Y\u0131ld\u0131z"]}, "1015": {"id": "1812.00978v3", "title": "A Survey on Semantic Parsing", "url": "http://arxiv.org/pdf/1812.00978v3", "date": "2019-05-29 18:08:07", "abs": "A significant amount of information in today's world is stored in structured\nand semi-structured knowledge bases. Efficient and simple methods to query them\nare essential and must not be restricted to only those who have expertise in\nformal query languages. The field of semantic parsing deals with converting\nnatural language utterances to logical forms that can be easily executed on a\nknowledge base. In this survey, we examine the various components of a semantic\nparsing system and discuss prominent work ranging from the initial rule based\nmethods to the current neural approaches to program synthesis. We also discuss\nmethods that operate using varying levels of supervision and highlight the key\nchallenges involved in the learning of such systems.", "cat": "cs.CL", "authors": ["Aishwarya Kamath", "Rajarshi Das"]}, "1016": {"id": "2007.04100v1", "title": "A Survey of Real-Time Social-Based Traffic Detection", "url": "http://arxiv.org/pdf/2007.04100v1", "date": "2020-07-07 17:51:50", "abs": "Online traffic news web sites do not always announce traffic events in areas\nin real-time. There is a capability to employ text mining and machine learning\ntechniques on the twitter stream to perform event detection, in order to\ndevelop a real-time traffic detection system. In this present survey paper, we\nwill deliberate the current state-of-art techniques in detecting traffic events\nin real-time focusing on five papers [1, 2, 3, 4, 5]. Lastly, applying text\nmining techniques and SVM classifiers in paper [2] gave the best results (i.e.\n95.75% accuracy and 95.8% F1-score).", "cat": "cs.SI", "authors": ["Hashim Abu-gellban"]}, "1017": {"id": "1511.01145v1", "title": "The VIMOS Public Extragalactic Redshift Survey (VIPERS). Environmental effects shaping the galaxy stellar mass function", "url": "http://arxiv.org/pdf/1511.01145v1", "date": "2015-11-03 22:29:03", "abs": "We exploit the first public data release of VIPERS to investigate\nenvironmental effects in galaxy evolution between $z\\sim0.5$ and $0.9$. The\nlarge number of spectroscopic redshifts over an area of about\n$10\\,\\mathrm{deg}^2$ provides a galaxy sample with high statistical power. The\naccurate redshift measurements, with $\\sigma_z = 0.00047(1+z_\\mathrm{spec})$,\nallow us to robustly isolate galaxies living in the lowest- and highest-density\nenvironments, as defined in terms of spatial 3D density contrast. We estimate\nthe stellar mass function (SMF) of galaxies residing in these two environments,\nand constrain its high-mass end with unprecedented precision. We find that the\ngalaxy SMF in the densest regions has a different shape than that measured at\nlow densities, with an enhancement of massive galaxies and a hint of a flatter\n(less negative) slope at $z<0.8$. We normalise each SMF to the comoving volume\noccupied by the corresponding environment, and relate estimates from different\nredshift bins. We observe an evolution of the SMF of VIPERS galaxies in high\ndensities, while the low-density one is nearly constant. We compare these\nresults to semi-analytical models and find consistent environmental signatures.\nWe discuss how the halo mass function and fraction of central/satellite\ngalaxies depend on the environments considered, making intrinsic and\nenvironmental properties of galaxies physically coupled, and therefore\ndifficult to disentangle. The evolution of our low-density regions is well\ndescribed by the formalism introduced by Peng et al.~(2010), and is consistent\nwith the idea that galaxies become progressively passive because of internal\nphysical processes. The same formalism could also describe the evolution of the\nSMF in the high density regions, but only if a significant contribution from\ndry mergers is considered. [Abridged]", "cat": "astro-ph.GA", "authors": ["I. Davidzon", "O. Cucciati", "M. Bolzonella", "G. De Lucia", "G. Zamorani", "S. Arnouts", "T. Moutard", "O. Ilbert", "B. Garilli", "M. Scodeggio", "L. Guzzo", "U. Abbas", "C. Adami", "J. Bel", "D. Bottini", "E. Branchini", "A. Cappi", "J. Coupon", "S. de la Torre", "C. Di Porto", "A. Fritz", "P. Franzetti", "M. Fumana", "B. R. Granett", "L. Guennou", "A. Iovino", "J. Krywult", "V. Le Brun", "O. Le Fevre", "D. Maccagni", "K. Ma\u0142ek", "F. Marulli", "H. J. McCracken", "Y. Mellier", "L. Moscardini", "M. Polletta", "A. Pollo", "L. A. M. Tasca", "R. Tojeiro", "D. Vergani", "A. Zanichelli"]}, "1018": {"id": "1506.05931v2", "title": "A blind HI Mass Function from the Arecibo Ultra-Deep Survey (AUDS)", "url": "http://arxiv.org/pdf/1506.05931v2", "date": "2015-08-05 14:52:51", "abs": "The Arecibo Ultra Deep Survey (AUDS) combines the unique sensitivity of the\ntelescope with the wide field of the Arecibo L-band Feed Array (ALFA) to\ndirectly detect 21cm HI emission from galaxies at distances beyond the local\nUniverse bounded by the lower frequency limit of ALFA (z=0.16). AUDS has\ncollected 700 hours of integration time in two fields with a combined area of\n1.35 square degrees. In this paper we present data from 60% of the total\nsurvey, corresponding to a sensitivity level of 80 micro-Jy. We discuss the\ndata reduction, the search for galaxies, parametrisation, optical\nidentification and completeness. We detect 102 galaxies in the mass range of\nlog M_HI/M_sun-2log h=5.6-10.3. We compute the HI mass function (HIMF) at the\nhighest redshifts so far measured. A fit of a Schechter function results in\nalpha=-1.37+-0.03, Phi=(7.72+-1.4)*10^3 h^3/Mpc^3 and log\nM_HI/M_sun=9.75+-0.041+2log h. Using the measured HIMF, we find a cosmic HI\ndensity of Omega_HI=(2.33+-0.07)*10^-4/h for the sample z=0.065. We discuss\nfurther uncertainties arising from cosmic variance. Because of its depth, AUDS\nis the first survey that can determine parameters for the HI mass function in\nindependent redshift bins from a single homogeneous data set. The results\nindicate little evolution of the co-moving mass function and Omega_HI within\nthis redshift range. We calculate a weighted average for Omega_HI in the range\n$0 11.73, in the local universe, z < 0.088. X-rays were\ndetected from 43 out of 44 objects, and their arcsec-resolution images,\nspectra, and radial brightness distributions are presented. With a selection by\nhard X-ray colour and the 6.4 keV iron line, AGN are found in 37% of the\nobjects, with higher luminosity sources more likely to contain an AGN. These\nAGN also tend to be found in late-stage mergers. The AGN fraction would\nincrease to 48% if objects with mid-IR [Ne V] detection are included. Double\nAGN are clearly detected only in NGC 6240 among 24 double/triple systems. Other\nAGN are found either in single nucleus objects or in one of the double nuclei\nat similar rates. Objects without conventional X-ray signatures of AGN appear\nto be hard X-ray quiet, relative to the X-ray to far-IR correlation for\nstarburst galaxies, as discussed elsewhere. Most objects also show extended\nsoft X-ray emission, which is likely related to an outflow from the nuclear\nregion, with a metal abundance pattern suggesting enrichment by core collapse\nsupernovae, as expected for a starburst.", "cat": "astro-ph.CO", "authors": ["K. Iwasawa", "D. B. Sanders", "Stacy H. Teng", "Vivian U", "L. Armus", "A. S. Evans", "J. H. Howell", "S. Komossa", "J. M. Mazzarella", "A. O. Petric", "J. A. Surace", "T. Vavilkin", "S. Veilleux", "N. Trentham"]}, "1021": {"id": "2303.04419v1", "title": "Probabilistic Descriptions of Fluid Flow: A Survey", "url": "http://arxiv.org/pdf/2303.04419v1", "date": "2023-03-08 07:45:08", "abs": "Fluids can behave in a highly irregular, turbulent way. It has long been\nrealised that, therefore, some weak notion of solution is required when\nstudying the fundamental partial differential equations of fluid dynamics, such\nas the compressible or incompressible Navier-Stokes or Euler equations. The\nstandard concept of weak solution (in the sense of distributions) is still a\ndeterministic one, as it gives exact values for the state variables (like\nvelocity or density) for almost every point in time and space. However,\nobservations and mathematical theory alike suggest that this deterministic\nviewpoint has certain limitations. Thus, there has been an increased recent\ninterest in the mathematical fluids community in probabilistic concepts of\nsolution. Due to the considerable number of such concepts, it has become\nchallenging to navigate the corresponding literature, both classical and\nrecent. We aim here to give a reasonably concise yet fairly detailed overview\nof probabilistic formulations of fluid equations, which can roughly be split\ninto measure-valued and statistical frameworks. We discuss both approaches and\ntheir relationship, as well as the interrelations between various statistical\nformulations, focusing on the compressible and incompressible Euler equations.", "cat": "math.AP", "authors": ["Dennis Gallenm\u00fcller", "Raphael Wagner", "Emil Wiedemann"]}, "1022": {"id": "1905.06056v1", "title": "Thermal properties of slowly rotating asteroids: Results from a targeted survey", "url": "http://arxiv.org/pdf/1905.06056v1", "date": "2019-05-15 09:49:48", "abs": "Context. Earlier work suggests that slowly rotating asteroids should have\nhigher thermal inertias than faster rotators because the heat wave penetrates\ndeeper into the sub-surface. However, thermal inertias have been determined\nmainly for fast rotators due to selection effects in the available photometry\nused to obtain shape models required for thermophysical modelling (TPM).\n Aims. Our aims are to mitigate these selection effects by producing shape\nmodels of slow rotators, to scale them and compute their thermal inertia with\nTPM, and to verify whether thermal inertia increases with the rotation period.\n Methods. To decrease the bias against slow rotators, we conducted a\nphotometric observing campaign of main-belt asteroids with periods longer than\n12 hours, from multiple stations worldwide, adding in some cases data from WISE\nand Kepler space telescopes. For spin and shape reconstruction we used the\nlightcurve inversion method, and to derive thermal inertias we applied a\nthermophysical model to fit available infrared data from IRAS, AKARI, and WISE.\n Results. We present new models of 11 slow rotators that provide a good fit to\nthe thermal data. In two cases, the TPM analysis showed a clear preference for\none of the two possible mirror solutions. We derived the diameters and albedos\nof our targets in addition to their thermal inertias, which ranged between\n3$^{+33}_{-3}$ and 45$^{+60}_{-30}$ Jm$^{-2}$s$^{-1/2}$K$^{-1}$.\n Conclusions. Together with our previous work, we have analysed 16 slow\nrotators from our dense survey with sizes between 30 and 150 km. The current\nsample thermal inertias vary widely, which does not confirm the earlier\nsuggestion that slower rotators have higher thermal inertias.", "cat": "astro-ph.EP", "authors": ["A. Marciniak", "V. Al\u00ed-Lagoa", "T. G. M\u00fcller", "R. Szak\u00e1ts", "L. Moln\u00e1r", "A. P\u00e1l", "E. Podlewska - Gaca", "N. Parley", "P. Antonini", "E. Barbotin", "R. Behrend", "L. Bernasconi", "M. Butkiewicz - B\u0105k", "R. Crippa", "R. Duffard", "R. Ditteon", "M. Feuerbach", "S. Fauvaud", "J. Garlitz", "S. Geier", "R. Goncalves", "J. Grice", "I. Grze\u015bkowiak", "R. Hirsch", "J. Horbowicz", "K. Kami\u0144ski", "M. K. Kami\u0144ska", "D. -H. Kim", "M. -J. Kim", "I. Konstanciak", "V. Kudak", "P. Kulczak", "J. L. Maestre", "F. Manzini", "S. Marks", "F. Monteiro", "W. Og\u0142oza", "D. Oszkiewicz", "F. Pilcher", "V. Perig", "T. Polakis", "M. Poli\u0144ska", "R. Roy", "J. J. Sanabria", "T. Santana-Ros", "B. Skiff", "J. Skrzypek", "K. Sobkowiak", "E. Sonbas", "O. Thizy", "P. Trela", "S. Urakawa", "M. \u017bejmo", "K. \u017bukowski"]}, "1023": {"id": "2104.12049v1", "title": "The MAVERIC Survey: Dynamical Origin of Radio Sources in Galactic Globular Clusters", "url": "http://arxiv.org/pdf/2104.12049v1", "date": "2021-04-25 02:19:26", "abs": "We investigate potential correlations between radio source counts (after\nbackground corrections) of 22 Galactic globular clusters (GCs) from the MAVERIC\nsurvey, and stellar encounter rates ($\\Gamma$) and masses ($M$) of the GCs.\nApplying a radio luminosity limit of $L_\\mathrm{lim}=5.0\\times\n10^{27}~\\mathrm{erg~s^{-1}}$, we take a census of radio sources in the core and\nthose within the half-light radius. By following a maximum likelihood method\nand adopting a simplified linear model, we find an unambiguous dependence of\ncore radio source counts on $\\Gamma$ and/or $M$ at 90% confidence, but no clear\ndependence of source counts within the half-light radius on either $\\Gamma$ or\n$M$. Five of the identified radio sources in cores above our adopted limit are\nmillisecond pulsars or neutron star X-ray binaries (XRBs), the dependence of\nwhich on $\\Gamma$ is well-known, but another is a published black hole (BH) XRB\ncandidate, and ten others are not identified. Accounting for the verified\ncluster members increases the significance of correlation with $M$ and/or\n$\\Gamma$ (to 99% confidence), for fits to core and half-light region source\ncounts, while excluding a dependence on $\\Gamma$ alone at 90% (core) and 68%\n(half-light) confidence. This is consistent with published dynamical\nsimulations of GC BH interactions that argue $\\Gamma$ will be a poor predictor\nof the distribution of accreting BHs in GCs. Future multiwavelength follow-up\nto verify cluster membership will enable stronger constraints on the dependence\nof radio source classes on cluster properties, promising a new view on the\ndynamics of BHs in GCs.", "cat": "astro-ph.HE", "authors": ["Yue Zhao", "Craig O. Heinke", "Laura Shishkovsky", "Jay Strader", "Laura Chomiuk", "Thomas J. Maccarone", "Arash Bahramian", "Gregory R. Sivakoff", "James C. A. Miller-Jones", "Evangelia Tremou"]}, "1024": {"id": "2101.01753v1", "title": "VLA Imaging of HI-bearing Ultra-Diffuse Galaxies from the ALFALFA Survey", "url": "http://arxiv.org/pdf/2101.01753v1", "date": "2021-01-05 19:37:22", "abs": "Ultra-diffuse galaxies have generated significant interest due to their large\noptical extents and low optical surface brightnesses, which challenge galaxy\nformation models. Here we present resolved synthesis observations of 12\nHI-bearing ultra-diffuse galaxies (HUDs) from the Karl G. Jansky Very Large\nArray (VLA), as well as deep optical imaging from the WIYN 3.5-meter telescope\nat Kitt Peak National Observatory. We present the data processing and images,\nincluding total intensity HI maps and HI velocity fields. The HUDs show ordered\ngas distributions and evidence of rotation, important prerequisites for the\ndetailed kinematic models in Mancera Pi\\~na et al. (2019b). We compare the HI\nand stellar alignment and extent, and find the HI extends beyond the already\nextended stellar component and that the HI disk is often misaligned with\nrespect to the stellar one, emphasizing the importance of caution when\napproaching inclination measurements for these extreme sources. We explore the\nHI mass-diameter scaling relation, and find that although the HUDs have diffuse\nstellar populations, they fall along the relation, with typical global HI\nsurface densities. This resolved sample forms an important basis for more\ndetailed study of the HI distribution in this extreme extragalactic population.", "cat": "astro-ph.GA", "authors": ["Lexi Gault", "Lukas Leisman", "Elizabeth A. K. Adams", "Pavel E. Mancera Pi\u00f1a", "Kameron Reiter", "Nicholas Smith", "Michael Battipaglia", "John M. Cannon", "Filippo Fraternali", "Martha P. Haynes", "Elizabeth McAllan", "Hannah J. Pagel", "Katherine L. Rhode", "John J. Salzer", "Quinton Singer"]}, "1025": {"id": "2403.04564v1", "title": "Estimating hidden population size from a single respondent-driven sampling survey", "url": "http://arxiv.org/pdf/2403.04564v1", "date": "2024-03-07 15:01:14", "abs": "This work is concerned with the estimation of hard-to-reach population sizes\nusing a single respondent-driven sampling (RDS) survey, a variant of\nchain-referral sampling that leverages social relationships to reach members of\na hidden population. The popularity of RDS as a standard approach for surveying\nhidden populations brings theoretical and methodological challenges regarding\nthe estimation of population sizes, mainly for public health purposes. This\npaper proposes a frequentist, model-based framework for estimating the size of\na hidden population using a network-based approach. An optimization algorithm\nis proposed for obtaining the identification region of the target parameter\nwhen model assumptions are violated. We characterize the asymptotic behavior of\nour proposed methodology and assess its finite sample performance under\ndepartures from model assumptions.", "cat": "stat.ME", "authors": ["Mamadou Yauck", "Erica EM Moodie", "Alain Fourmigue", "Milada Dvorakova", "Gilles Lambert", "Daniel Grace", "Joseph Cox"]}, "1026": {"id": "2403.13490v1", "title": "The ALPINE-ALMA [CII] Survey: Dust emission effective radius up to 3 kpc in the Early Universe", "url": "http://arxiv.org/pdf/2403.13490v1", "date": "2024-03-20 10:47:44", "abs": "Measurements of the size of dust continuum emission are an important tool for\nconstraining the spatial extent of star formation and hence the build-up of\nstellar mass. Compact dust emission has generally been observed at Cosmic Noon\n(z~2-3). However, at earlier epochs, toward the end of the Reionization\n(z~4-6), only the sizes of a handful of IR-bright galaxies have been measured.\nIn this work, we derive the dust emission sizes of main-sequence galaxies at\nz~5 from the ALPINE survey. We measure the dust effective radius r_e,FIR in the\nuv-plane in Band 7 of ALMA for seven ALPINE galaxies with resolved emission and\nwe compare it with rest-frame UV and [CII]158$\\mu$m measurements. We study the\nr_e,FIR-L_IR scaling relation by considering our dust size measurements and all\nthe data in literature at z~4-6. Finally, we compare our size measurements with\npredictions from simulations. The dust emission in the selected ALPINE galaxies\nis rather extended (r_e,FIR~1.5-3 kpc), similar to [CII]158 um but a factor of\n~2 larger than the rest-frame UV emission. Putting together all the\nmeasurements at z~5, spanning 2 decades in luminosity from L_IR ~ 10^11 L_sun\nto L_IR ~ 10^13 L_sun, the data highlight a steeply increasing trend of the\nr_e,FIR-L_IR relation at L_IR< 10^12 L_sun, followed by a downturn and a\ndecreasing trend at brighter luminosities. Finally, simulations that extend up\nto the stellar masses of the ALPINE galaxies considered in the present work\npredict a sub-set of galaxies (~25% at 10^10 M_sun < M_star < 10^11 M_sun) with\nsizes as large as those measured.", "cat": "astro-ph.GA", "authors": ["F. Pozzi", "F. Calura", "Q. D'Amato", "M. Gavarente", "M. Bethermin", "M. Boquien", "V. Casasola", "A. Cimatti", "R. Cochrane", "M. Dessauges-Zavadsky", "A. Enia", "F. Esposito", "A. L. Faisst", "R. Gilli", "M. Ginolfi", "R. Gobat", "C. Gruppioni", "C. C. Hayward", "E. Ibar", "A. M. Koekemoer", "B. C. Lemaux", "G. E. Magdis", "J. Molina", "M. Talia", "L. Vallini", "D. Vergani", "G. Zamorani"]}, "1027": {"id": "1905.06207v5", "title": "Asymptotics of correlations in the Ising model: a brief survey", "url": "http://arxiv.org/pdf/1905.06207v5", "date": "2023-12-20 18:34:55", "abs": "We present a brief survey of rigorous results on the asymptotic behavior of\ncorrelations between two local functions as the distance between their support\ndiverges, concentrating on the Ising model on $\\mathbb{Z}^d$ with finite-range\nferromagnetic interactions.", "cat": "math.PR", "authors": ["S\u00e9bastien Ott", "Yvan Velenik"]}, "1028": {"id": "2201.01794v2", "title": "The Perkins INfrared Exosatellite Survey (PINES) I. Survey Overview, Reduction Pipeline, and Early Results", "url": "http://arxiv.org/pdf/2201.01794v2", "date": "2022-04-21 07:13:05", "abs": "We describe the Perkins INfrared Exosatellite Survey (PINES), a near-infrared\nphotometric search for short-period transiting planets and moons around a\nsample of 393 spectroscopically confirmed L- and T-type dwarfs. PINES is\nperformed with Boston University's 1.8 m Perkins Telescope Observatory, located\non Anderson Mesa, Arizona. We discuss the observational strategy of the survey,\nwhich was designed to optimize the number of expected transit detections, and\ndescribe custom automated observing procedures for performing PINES\nobservations. We detail the steps of the $\\texttt{PINES Analysis Toolkit}$\n($\\texttt{PAT}$), software that is used to create light curves from PINES\nimages. We assess the impact of second-order extinction due to changing\nprecipitable water vapor on our observations and find that the magnitude of\nthis effect is minimized in Mauna Kea Observatories $\\textit{J}$-band. We\ndemonstrate the validity of $\\texttt{PAT}$ through the recovery of a transit of\nWASP-2 b and known variable brown dwarfs, and use it to identify a new variable\nL/T transition object: the T2 dwarf WISE J045746.08-020719.2. We report on the\nmeasured photometric precision of the survey and use it to estimate our transit\ndetection sensitivity. We find that for our median brightness targets, assuming\ncontributions from white noise only, we are sensitive to the detection of 2.5\n$R_\\oplus$ planets and larger. PINES will test whether the increase in\nsub-Neptune-sized planet occurrence with decreasing host mass continues into\nthe L and T dwarf regime.", "cat": "astro-ph.EP", "authors": ["Patrick Tamburo", "Philip S. Muirhead", "Allison M. McCarthy", "Murdock Hart", "David Gracia", "Johanna M. Vos", "Daniella C. Bardalez Gagliuffi", "Jacqueline Faherty", "Christopher Theissen", "Eric Agol", "Julie N. Skinner", "Sheila Sagear"]}, "1029": {"id": "1907.10128v1", "title": "Blind Deblurring using Deep Learning: A Survey", "url": "http://arxiv.org/pdf/1907.10128v1", "date": "2019-07-23 21:04:29", "abs": "We inspect all the deep learning based solutions and provide holistic\nunderstanding of various architectures that have evolved over the past few\nyears to solve blind deblurring. The introductory work used deep learning to\nestimate some features of the blur kernel and then moved onto predicting the\nblur kernel entirely, which converts the problem into non-blind deblurring. The\nrecent state of the art techniques are end to end, i.e., they don't estimate\nthe blur kernel rather try to estimate the latent sharp image directly from the\nblurred image. The benchmarking PSNR and SSIM values on standard datasets of\nGOPRO and Kohler using various architectures are also provided.", "cat": "eess.IV", "authors": ["Siddhant Sahu", "Manoj Kumar Lenka", "Pankaj Kumar Sa"]}, "1030": {"id": "1305.5254v1", "title": "The Stellar Mass Growth of Brightest Cluster Galaxies in the IRAC Shallow Cluster Survey", "url": "http://arxiv.org/pdf/1305.5254v1", "date": "2013-05-22 20:00:02", "abs": "The details of the stellar mass assembly of brightest cluster galaxies (BCGs)\nremain an unresolved problem in galaxy formation. We have developed a novel\napproach that allows us to construct a sample of clusters that form an\nevolutionary sequence, and have applied it to the Spitzer IRAC Shallow Cluster\nSurvey (ISCS) to examine the evolution of BCGs in progenitors of present-day\nclusters with mass of (2.5-4.5)x10^{14}Msun. We follow the cluster mass growth\nhistory extracted from a high resolution cosmological simulation, and then use\nan empirical method that infers the cluster mass based on the ranking of\ncluster luminosity to select high-z clusters of appropriate mass from ISCS to\nbe progenitors of the given set of z=0 clusters. We find that, between z=1.5\nand 0.5, the BCGs have grown in stellar mass by a factor of 2.3, which is\nwell-matched by the predictions from a state-of-the-art semi-analytic model.\nBelow z=0.5 we see hints of differences in behavior between the model and\nobservation.", "cat": "astro-ph.CO", "authors": ["Yen-Ting Lin", "Mark Brodwin", "Anthony H. Gonzalez", "Paul Bode", "Peter R. M. Eisenhardt", "S. A. Stanford", "Alexey Vikhlinin"]}, "1031": {"id": "1009.0715v1", "title": "Targeted deep surveys of high Galactic latitude HI with the GBT", "url": "http://arxiv.org/pdf/1009.0715v1", "date": "2010-09-03 16:24:09", "abs": "Over 800 sq. deg. of high Galactic latitude sky have been mapped at 21 cm\nwith the Robert C. Byrd Green Bank Telescope (GBT). An improved knowledge of\nthe telescope's beam characteristics has allowed us to reliably map not only\nregions of high column density, but also such regions as ELAIS N1, a targeted\nSpitzer field, which have very low HI column density. The additional fields we\nhave observed cover a cross-section of dynamically and chemically interesting\nregions as indicated by the presence of intermediate/high velocity gas and/or\nanomalous far-IR (dust) colour.", "cat": "astro-ph.GA", "authors": ["K. Blagrave", "F. J. Lockman", "P. G. Martin"]}, "1032": {"id": "1212.3613v1", "title": "Second data release of the Kepler-INT Survey", "url": "http://arxiv.org/pdf/1212.3613v1", "date": "2012-12-14 21:00:15", "abs": "This short document reports on the second data release of the Kepler-INT\nSurvey (KIS, Greiss et al. 2012). The Kepler field, a 116 sq.deg region of the\nCygnus and Lyra constellations, is the target of the most intensive search for\ntransiting planets to date. The Kepler mission provides superior time series\nphotometry, with an enormous impact on all areas of stellar variability. The\ninitial release catalogue (Greiss et al. 2012) concerned data taken between May\nand August 2011, using the Isaac Newton Telescope on the island of La Palma.\nFour broadband filters were used, U, g, r, i, as well as one narrowband one,\nH-alpha, reaching down to a limit of ~20th mag in the Vega system. Observations\ncovering ~50 sq.deg passed our quality control thresholds and constituted the\nfirst data release. Here we report on the second data release, covering an\nadditional ~63 sq.deg of the Kepler field. We apply the exact same quality\ncontrol criteria and photometric calibration as in the initial release\ncatalogue (see Greiss et al. (2012) for further details). The global\nphotometric calibration was derived by placing the KIS magnitudes as close as\npossible to the Kepler Input Catalog (KIC) ones. The second data release\ncatalogue containing ~14.5 million sources from all the good photometric KIS\nfields is available for download from the KIS webpage, as well as from the\nKepler Target Search page at MAST. It includes all the objects from the initial\ndata release catalogue and covers ~97% of the Kepler field. Therefore this\nrelease adds ~8.5 million sources to the initial data release catalogue, all\nobserved between May and August 2012. The remaining ~3% of the field will be\ncompleted once the Kepler field is visible in 2013.", "cat": "astro-ph.SR", "authors": ["S. Greiss", "D. T. H. Steeghs", "B. T. G\u00e4nsicke", "E. L. Mart\u00edn", "P. J. Groot", "M. J. Irwin", "E. Gonz\u00e1lez-Solares", "R. Greimel", "N. P. Gentile Fusillo", "M. Still", "the KIS collaboration"]}, "1033": {"id": "2203.12515v2", "title": "A Survey on Cross-Lingual Summarization", "url": "http://arxiv.org/pdf/2203.12515v2", "date": "2022-08-30 04:34:32", "abs": "Cross-lingual summarization is the task of generating a summary in one\nlanguage (e.g., English) for the given document(s) in a different language\n(e.g., Chinese). Under the globalization background, this task has attracted\nincreasing attention of the computational linguistics community. Nevertheless,\nthere still remains a lack of comprehensive review for this task. Therefore, we\npresent the first systematic critical review on the datasets, approaches, and\nchallenges in this field. Specifically, we carefully organize existing datasets\nand approaches according to different construction methods and solution\nparadigms, respectively. For each type of datasets or approaches, we thoroughly\nintroduce and summarize previous efforts and further compare them with each\nother to provide deeper analyses. In the end, we also discuss promising\ndirections and offer our thoughts to facilitate future research. This survey is\nfor both beginners and experts in cross-lingual summarization, and we hope it\nwill serve as a starting point as well as a source of new ideas for researchers\nand engineers interested in this area.", "cat": "cs.CL", "authors": ["Jiaan Wang", "Fandong Meng", "Duo Zheng", "Yunlong Liang", "Zhixu Li", "Jianfeng Qu", "Jie Zhou"]}, "1034": {"id": "1302.5444v2", "title": "Why multi-tracer surveys beat cosmic variance", "url": "http://arxiv.org/pdf/1302.5444v2", "date": "2013-02-28 09:02:13", "abs": "Galaxy surveys that map multiple species of tracers of large-scale structure\ncan improve the constraints on some cosmological parameters far beyond the\nlimits imposed by a simplistic interpretation of cosmic variance. This\nenhancement derives from comparing the relative clustering between different\ntracers of large-scale structure. We present a simple but fully generic\nexpression for the Fisher information matrix of surveys with any (discrete)\nnumber of tracers, and show that the enhancement of the constraints on\nbias-sensitive parameters are a straightforward consequence of this\nmulti-tracer Fisher matrix. In fact, the relative clustering amplitudes between\ntracers are eigenvectors of this multi-tracer Fisher matrix. The diagonalized\nmulti-tracer Fisher matrix clearly shows that while the effective volume is\nbounded by the physical volume of the survey, the relational information\nbetween species is unbounded. As an application, we study the expected\nenhancements in the constraints of realistic surveys that aim at mapping\nseveral different types of tracers of large-scale structure. The gain obtained\nby combining multiple tracers is highest at low redshifts, and in one\nparticular scenario we analyzed, the enhancement can be as large as a factor of\n~3 for the accuracy in the determination of the redshift distortion parameter,\nand a factor ~5 for the local non-Gaussianity parameter. Radial and angular\ndistance determinations from the baryonic features in the power spectrum may\nalso benefit from the multi-tracer approach.", "cat": "astro-ph.CO", "authors": ["L. Raul Abramo", "Katie E. Leonard"]}, "1035": {"id": "1812.10492v2", "title": "Serendipitous Discoveries of Kilonovae in the LSST Main Survey: Maximising Detections of Sub-Threshold Gravitational Wave Events", "url": "http://arxiv.org/pdf/1812.10492v2", "date": "2019-02-18 15:35:55", "abs": "We investigate the ability of the Large Synoptic Survey Telescope (LSST) to\ndiscover kilonovae (kNe) from binary neutron star (BNS) and neutron star-black\nhole (NSBH) mergers, focusing on serendipitous detections in the Wide-Fast-Deep\n(WFD) survey. We simulate observations of kNe with proposed LSST survey\nstrategies, paying particular attention to cadence choices that are compatible\nwith the broader LSST cosmology programme. We find that if all kNe are\nidentical to GW170817, the baseline survey strategy will yield 58 kNe over the\nsurvey lifetime. If we instead assume a representative population model of BNS\nkNe, we expect to detect only 27 kNe. However, we find the choice of survey\nstrategy significantly impacts these numbers and can increase them to 254 kNe\nand 82 kNe over the survey lifetime, respectively. This improvement arises from\nan increased cadence of observations between different filters with respect to\nthe baseline. We then consider the ability of the Advanced LIGO/Virgo (ALV)\ndetector network to detect these BNS mergers. If the optimal survey strategy is\nadopted, 202 of the GW170817-like kNe and 56 of the BNS population model kNe\nare detected with LSST but are below the threshold for detection by the ALV\nnetwork. This represents, for both models, an increase by a factor greater than\n4.5 in the number of detected sub-threshold events over the baseline survey\nstrategy. Such a population of sub-threshold events would provide an\nopportunity to conduct electromagnetic-triggered searches for signals in\ngravitational-wave detector data and assess selection effects in measurements\nof the Hubble constant from standard sirens, e.g., related to viewing angle\neffects.", "cat": "astro-ph.IM", "authors": ["Christian N. Setzer", "Rahul Biswas", "Hiranya V. Peiris", "Stephan Rosswog", "Oleg Korobkin", "Ryan T. Wollaeger"]}, "1036": {"id": "1911.08273v1", "title": "VLT/SINFONI study of black hole growth in high redshift radio-loud quasars from the CARLA survey", "url": "http://arxiv.org/pdf/1911.08273v1", "date": "2019-11-19 14:07:30", "abs": "We present VLT/SINFONI observations of 35 quasars at 2.1 < z < 3.2, the\nmajority of which were selected from the Clusters Around Radio-Loud AGN (CARLA)\nsurvey. CARLA quasars have large CIV-based black hole (BH) masses (M(BH) > 10^9\nMsun) and powerful radio emission (P(500MHz) > 27.5 W/Hz). We estimate Ha-based\nM(BH), finding a scatter of 0.35 dex compared to CIV. We evaluate several\nrecipes for correcting CIV-based masses, which reduce the scatter to 0.24 dex.\nThe radio power of the radio-loud quasars is at most weakly correlated with the\ninterconnected quantities Ha-width, L(5100A) and M(BH), suggesting that it is\ngoverned by different physical processes. However, we do find a strong inverse\ncorrelation between CIV blueshift and radio power linked to higher Eddington\nratios and L(5100A). Under standard assumptions, the BH growth time is longer\nthan the cosmic age for many CARLA quasars, suggesting that they must have\nexperienced more efficient growth in the past. If these BHs were growing from\nseeds since the epoch of reionization, it is possible that they grew at the\nEddington limit like the quasars at z ~ 6-7, and then continued to grow at the\nreduced rates observed until z ~ 2-3. Finally, we study the relation between\nM(BH) and environment, finding a weak positive correlation between M(BH) and\ngalaxy density measured by CARLA.", "cat": "astro-ph.GA", "authors": ["M. Marinello", "R. A. Overzier", "H. J. A. R\u00f6ttgering", "J. D. Kurk", "C. De Breuck", "J. Vernet", "D. Wylezalek", "D. Stern", "K. J. Duncan", "N. Hatch", "N. Kashikawa", "Y. -T. Lin", "R. S. Nemmen", "A. Saxena"]}, "1037": {"id": "0810.4180v4", "title": "Discovery of a redshift 6.13 quasar in the UKIRT Infrared Deep Sky Survey", "url": "http://arxiv.org/pdf/0810.4180v4", "date": "2009-09-17 12:21:43", "abs": "Optical and near-infrared (NIR) spectra are presented for ULAS\nJ131911.29+095951.4 (hereafter ULAS J1319+0950), a new redshift z = 6.127 +/-\n0.004 quasar discovered in the Third Data Release (DR3) of the UKIRT Infrared\nDeep Sky Survey (UKIDSS). The source has Y_Vega = 19.10 +/- 0.03, corresponding\nto M_1450,AB = -27.12, which is comparable to the absolute magnitudes of the z\n~= 6 quasars discovered in the SDSS. ULAS J1319+0950 was, in fact, registered\nby SDSS as a faint source with z_AB = 20.1 +/- 0.1, just below the\nsignal--to--noise ratio limit of the SDSS high-redshift quasar survey. The\nfaint z-band magnitude is a consequence of the weak Ly alpha/N V emission line,\nwhich has a rest-frame equivalent width of only ~20 A and provides only a small\nboost to the z-band flux. Nevertheless, there is no evidence from this\nUKIDSS-based search for a significant population of high-redshift quasars with\nweak emission lines. The Ly alpha optical depth to ULAS J1319+0950 is\nconsistent with that measured towards similarly distant SDSS quasars, implying\nthat results from optical- and NIR-selected quasars may be combined.\n Also presented is a new NIR-spectrum of the previously discovered UKIDSS\nquasar ULAS J020332.38+001229.2, which reveals the object to be a broad\nabsorption line quasar. The new spectrum shows that the emission line\npreviously identified as Ly alpha is actually N V, leading to a revised\nredshift of z = 5.72, rather than z = 5.86 as previously estimated.", "cat": "astro-ph", "authors": ["D. J. Mortlock", "M. Patel", "S. J. Warren", "B. P. Venemans", "R. G. McMahon", "P. C. Hewett", "C. Simpson", "R. G. Sharp", "B. Burningham", "S. Dye", "S. Ellis", "E. A. Gonzales-Solares", "N. Huelamo"]}, "1038": {"id": "2311.02297v3", "title": "Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys", "url": "http://arxiv.org/pdf/2311.02297v3", "date": "2024-06-19 15:15:47", "abs": "Photometric stellar surveys now cover a large fraction of the sky, probe to\nfainter magnitudes than large-scale spectroscopic surveys, and are relatively\nfree from the target-selection biases often associated with such studies.\nPhotometric-metallicity estimates that include narrow/medium-band filters can\nachieve comparable accuracy and precision to existing low-resolution\nspectroscopic surveys such as SDSS/SEGUE and LAMOST. Here we report on an\neffort to identify likely members of the Galactic disk system among the very\nmetal-poor (VMP; [Fe/H] $\\leq$ --2) and extremely metal-poor (EMP; [Fe/H]\n$\\leq$ --3) stars. Our analysis is based on an initial sample of $\\sim11.5$\nmillion stars with full space motions selected from the SkyMapper Southern\nSurvey (SMSS) and Stellar Abundance and Galactic Evolution Survey (SAGES).\nAfter applying a number of quality cuts to obtain the best available\nmetallicity and dynamical estimates, we analyze a total of $\\sim$5.86 million\nstars in the combined SMSS/SAGES sample. We employ two techniques that,\ndepending on the method, identify between 876 and 1,476 VMP stars (6.9%-11.7%\nof all VMP stars) and between 40 and 59 EMP stars (12.4%-18.3% of all EMP\nstars) that appear to be members of the Galactic disk system on highly prograde\norbits (v$_{\\phi} > 150$ km/s). The total number of candidate VMP/EMP disk-like\nstars is 1,496, the majority of which have low orbital eccentricities, ecc $\\le\n0.4$; many have ecc $\\le 0.2$. The large fractions of VMP/EMP stars associated\nwith the Milky Way disk system strongly suggest the presence of an early\nforming ``primordial\" disk.", "cat": "astro-ph.GA", "authors": ["Jihye Hong", "Timothy C. Beers", "Young Sun Lee", "Yang Huang", "Yutaka Hirai", "Jonathan Cabrera Garcia", "Derek Shank", "Shuai Xu", "Haibo Yuan", "Mohammad K. Mardini", "Thomas Catapano", "Gang Zhao", "Zhou Fan", "Jie Zheng", "Wei Wang", "Kefeng Tan", "Jingkun Zhao", "Chun Li"]}, "1039": {"id": "1406.4701v1", "title": "Comparative Study of MAC Layer Protocols in Wireless Sensor Networks: A Survey", "url": "http://arxiv.org/pdf/1406.4701v1", "date": "2014-06-18 12:55:40", "abs": "Wireless Sensor Networks (WSN) is the collection of many small size low cost,\nbattery operated sensor nodes distributed over the targeted region to collect\nthe information of interest. We can say these networks can be a fruitful\nsolution for many applications such as target tracking, intrusion detection\netc. Whenever we are talking about MAC layer protocols we need to give stress\non energy efficiency factor.", "cat": "cs.NI", "authors": ["Rahul R Lanjewar", "D S Adane"]}, "1040": {"id": "1805.00968v1", "title": "The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters - XV. The dynamical clock: reading cluster dynamical evolution from the segregation level of blue straggler stars", "url": "http://arxiv.org/pdf/1805.00968v1", "date": "2018-05-02 18:34:18", "abs": "The parameter A+, defined as the area enclosed between the cumulative radial\ndistribution of blue straggler stars (BSSs) and that of a reference population,\nis a powerful indicator of the level of BSS central segregation. As part of the\nHubble Space Telescope UV Legacy Survey of Galactic globular clusters (GCs),\nhere we present the BSS population and the determination of A+ in 27 GCs\nobserved out to about one half-mass radius. In combination with 21 additional\nclusters discussed in a previous paper this provides us with a global sample of\n48 systems (corresponding to \\sim 32\\% of the Milky Way GC population), for\nwhich we find a strong correlation between A+ and the ratio of cluster age to\nthe current central relaxation time. Tight relations have been found also with\nthe core radius and the central luminosity density, which are expected to\nchange with the long-term cluster dynamical evolution. An interesting relation\nis emerging between A+ and the ratio of the BSS velocity dispersion relative to\nthat of main sequence turn-off stars, which measures the degree of energy\nequipartition experienced by BSSs in the cluster. These results provide further\nconfirmation that BSSs are invaluable probes of GC internal dynamics and A+ is\na powerful dynamical clock.", "cat": "astro-ph.GA", "authors": ["F. R. Ferraro", "B. Lanzoni", "S. Raso", "D. Nardiello", "E. Dalessandro", "E. Vesperini", "G. Piotto", "C. Pallanca", "G. Beccari", "A. Bellini", "M. Libralato", "J. Anderson", "A. Aparicio", "L. R. Bedin", "S. Cassisi", "A. P. Milone", "S. Ortolani", "A. Renzini", "M. Salaris", "R. P. van der Marel"]}, "1041": {"id": "1410.4695v1", "title": "QoS Survey in IPv6 and Queuing Methods", "url": "http://arxiv.org/pdf/1410.4695v1", "date": "2014-10-17 11:47:48", "abs": "The routes in IP networks are determined by the IP destination address and\nthe routing tables in each router on the path to the destination. Hence all the\nIP packets follow the same route until the route is changes due to congestion,\nlink failure or topology updates. IPv4 tried using Type of Service (TOS) field\nin the IP header to classify traffic and that did not succeed as it was based\non fair self-classification of applications in comparison to the network\ntraffic of other applications. As multimedia applications were quite foreign at\nthe initial IPv4 stage, TOS field was not used uniformly. As there are\ndifferent existing Quality of Service (QoS) paradigms available, IPv6 QoS\napproach was designed to be more flexible. The IPv6 protocol thus has\nQoS-specific elements in Base header and Extension headers which can be used in\ndifferent ways to enhance multimedia application performance. In this paper, we\nplan to survey these options and other QoS architectures and discuss their\nstrengths and weaknesses. Some basic simulation for various queuing schemes is\npresented for comparison and a new queuing scheme prioritized WFQ with RR is\nproposed.", "cat": "cs.NI", "authors": ["B. Issac", "K. Hamid", "C. E. Tan"]}, "1042": {"id": "1903.11100v1", "title": "The Massive and Distant Clusters of WISE Survey VI: Stellar Mass Fractions of a Sample of High-Redshift Infrared-selected Clusters", "url": "http://arxiv.org/pdf/1903.11100v1", "date": "2019-03-26 18:12:26", "abs": "We present measurements of the stellar mass fractions ($f_\\star$) for a\nsample of high-redshift ($0.93 \\le z \\le 1.32$) infrared-selected galaxy\nclusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and\ncompare them to the stellar mass fractions of Sunyaev-Zel'dovich (SZ)\neffect-selected clusters in a similar mass and redshift range from the South\nPole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean\n$f_\\star$ between the two selection methods, though we do find an unexpectedly\nlarge range in $f_\\star$ for the SZ-selected clusters. In addition, we measure\nthe luminosity function of the MaDCoWS clusters and find $m^*= 19.41\\pm0.07$,\nsimilar to other studies of clusters at or near our redshift range. Finally, we\npresent SZ detections and masses for seven MaDCoWS clusters and new\nspectroscopic redshifts for five MaDCoWS clusters. One of these new clusters,\nMOO J1521+0452 at $z=1.31$, is the most distant MaDCoWS cluster confirmed to\ndate.", "cat": "astro-ph.GA", "authors": ["Bandon Decker", "Mark Brodwin", "Zubair Abdulla", "Anthony H. Gonzalez", "Daniel P. Marrone", "Christine O'Donnell", "S. A. Stanford", "Dominika Wylezalek", "John E. Carlstrom", "Peter R. M. Eisenhardt", "Adam Mantz", "Wenli Mo", "Emily Moravec", "Daniel Stern", "Greg Aldering", "Matthew L. N. Ashby", "Kyle Boone", "Brian Hayden", "Nikhel Gupta", "Michael A. McDonald"]}, "1043": {"id": "1704.02504v2", "title": "The EDGE-CALIFA Survey: Interferometric Observations of 126 Galaxies with CARMA", "url": "http://arxiv.org/pdf/1704.02504v2", "date": "2017-08-16 19:44:10", "abs": "We present interferometric CO observations made with the Combined Array for\nMillimeter-wave Astronomy (CARMA) of galaxies from the Extragalactic Database\nfor Galaxy Evolution survey (EDGE). These galaxies are selected from the Calar\nAlto Legacy Integral Field Area (CALIFA) sample, mapped with optical integral\nfield spectroscopy. EDGE provides good quality CO data (3$\\sigma$ sensitivity\n$\\Sigma_{\\rm mol}$ $\\sim$ 11 M$_\\odot$ pc$^{-2}$ before inclination correction,\nresolution $\\sim1.4$ kpc) for 126 galaxies, constituting the largest\ninterferometric CO survey of galaxies in the nearby universe. We describe the\nsurvey, the data characteristics, the data products, and present initial\nscience results. We find that the exponential scale-lengths of the molecular,\nstellar, and star-forming disks are approximately equal, and galaxies that are\nmore compact in molecular gas than in stars tend to show signs of interaction.\nWe characterize the molecular to stellar ratio as a function of Hubble type and\nstellar mass, present preliminary results on the resolved relations between the\nmolecular gas, stars, and star formation rate, and discuss the dependence of\nthe resolved molecular depletion time on stellar surface density, nebular\nextinction, and gas metallicity. EDGE provides a key dataset to address\noutstanding topics regarding gas and its role in star formation and galaxy\nevolution, which will be publicly available on completion of the quality\nassessment.", "cat": "astro-ph.GA", "authors": ["Alberto D. Bolatto", "Tony Wong", "Dyas Utomo", "Leo Blitz", "Stuart N. Vogel", "Sebasti\u00e1n F. S\u00e1nchez", "Jorge Barrera-Ballesteros", "Yixian Cao", "Dario Colombo", "Helmut Dannerbauer", "Rub\u00e9n Garc\u00eda-Benito", "Rodrigo Herrera-Camus", "Bernd Husemann", "Veselina Kalinova", "Adam K. Leroy", "Gigi Leung", "Rebecca C. Levy", "Dami\u00e1n Mast", "Eve Ostriker", "Erik Rosolowsky", "Karin M. Sandstrom", "Peter Teuben", "Glenn van de Ven", "Fabian Walter"]}, "1044": {"id": "0805.0537v1", "title": "A deep INTEGRAL hard X-ray survey of the 3C 273/Coma region", "url": "http://arxiv.org/pdf/0805.0537v1", "date": "2008-05-05 14:04:59", "abs": "(abridged) We present an analysis of the deepest hard X-ray survey to date of\nabout 2500 deg^2 performed by the IBIS instrument on board INTEGRAL in the\n20-60 keV band, with a total exposure time of 4 Ms. We find 34 candidate\nsources. The ratio of Seyfert 1 to Seyfert 2 is significantly more than the\nratio found in the optical, which may be evidence for a receding torus, but\ncould also be due to absorption columns > 10^{25} cm^{-2}. None of the\npredicted Compton-thick objects is detected unambiguously; when taking lower\nlimits on Nh into account, the fraction of these objects is found to be lower\nthan 24%. We do not see, but cannot exclude, a relationship between absorption\nand luminosity similar to what is seen in the 2-10 keV band. Our data suggests\nthe possibility of a lack of objects with 10^{21} < Nh < 10^{22} cm^{-2}, as\nexpected if absorption originates either in a torus-like structure or in the\nhost galaxy. We find that the Log N-Log S diagram of our sources is compatible\nwith those obtained in other surveys in hard X-rays. Compared to models of the\nAGN population selected in the 2-10 keV band, the Log N-Log S diagram is\ngenerally in good agreement, but the Nh distribution is significantly\ndifferent, with significantly less unabsorbed sources (Nh<10^{22} cm^{-2}) at a\ngiven flux limit compared to the models. We resolve here about 2.5% of the\ncosmic X-ray background. We also study the local hard X-ray luminosity\nfunction, which is compatible with what is found in other recent hard X-ray\nsurveys. The characteristic luminosity Log L*_{20-60 keV}=43.66 is found to be\na factor about 5 lower than the value observed in the 2-10 keV band. We find a\nspace density of 10^{-3} AGN with L>10^{41} per Mpc^3 and a corresponding\nluminosity density of 0.9 10^{39} erg s^{-1} Mpc^{-3}.", "cat": "astro-ph", "authors": ["S. Paltani", "R. Walter", "I. M. McHardy", "T. Dwelly", "C. Steiner", "T. J. -L. Courvoisier"]}, "1045": {"id": "2111.01788v2", "title": "Wide binaries from the H3 survey: the thick disk and halo have similar wide binary fractions", "url": "http://arxiv.org/pdf/2111.01788v2", "date": "2022-03-07 16:18:57", "abs": "Due to the different environments in the Milky Way's disk and halo, comparing\nwide binaries in the disk and halo is key to understanding wide binary\nformation and evolution. By using Gaia Early Data Release 3, we search for\nresolved wide binary companions in the H3 survey, a spectroscopic survey that\nhas compiled $\\sim$150,000 spectra for thick-disk and halo stars to date. We\nidentify 800 high-confidence (a contamination rate of 4%) wide binaries and two\nresolved triples, with binary separations mostly between $10^3$-$10^5$ AU and a\nlowest [Fe/H] of $-2.7$. Based on their Galactic kinematics, 33 of them are\nhalo wide binaries, and most of those are associated with the accreted\nGaia-Sausage-Enceladus galaxy. The wide binary fraction in the thick disk\ndecreases toward the low metallicity end, consistent with the previous findings\nfor the thin disk. Our key finding is that the halo wide binary fraction is\nconsistent with the thick-disk stars at a fixed [Fe/H]. There is no significant\ndependence of the wide binary fraction on the $\\alpha$-captured abundance.\nTherefore, the wide binary fraction is mainly determined by the iron abundance,\nnot their disk or halo origin nor the $\\alpha$-captured abundance. Our results\nsuggest that the formation environments play a major role for the wide binary\nfraction, instead of other processes like radial migration that only apply to\ndisk stars.", "cat": "astro-ph.GA", "authors": ["Hsiang-Chih Hwang", "Yuan-Sen Ting", "Charlie Conroy", "Nadia L. Zakamska", "Kareem El-Badry", "Phillip Cargile", "Dennis Zaritsky", "Vedant Chandra", "Jiwon Jesse Han", "Joshua S. Speagle", "Ana Bonaca"]}, "1046": {"id": "1903.04466v1", "title": "VEGAS: a VST Early-type GAlaxy Survey. IV. NGC 1533, IC 2038 and IC 2039: an interacting triplet in the Dorado group", "url": "http://arxiv.org/pdf/1903.04466v1", "date": "2019-03-11 17:42:31", "abs": "This paper focuses on NGC 1533 and the pair IC 2038 and IC 2039 in Dorado a\nnearby, clumpy, still un-virialized group. We obtained their surface photometry\nfrom deep OmegaCAM@ESO-VST images in g and r bands. For NGC 1533, we map the\nsurface brightness down to $\\mu_g \\simeq 30.11$ mag/arcsec$^{2}$ and $\\mu_r\n\\simeq 28.87$ mag/arcsec$^{2}$ and out to about $4R_e$. At such faint levels\nthe structure of NGC 1533 appear amazingly disturbed with clear structural\nasymmetry between inner and outer isophotes in the North-East direction. We\ndetect new spiral arm-like tails in the outskirts, which might likely be the\nsignature of a past interaction/merging event. Similarly, IC 2038 and IC 2039\nshow tails and distortions indicative of their ongoing interaction. Taking\nadvantages of deep images, we are able to detect the optical counterpart to the\nHI gas. The analysis of the new deep data suggests that NGC 1533 had a complex\nhistory made of several interactions with low-mass satellites that generated\nthe star-forming spiral-like structure in the inner regions and are shaping the\nstellar envelope. In addition, the VST observations show that also the two less\nluminous galaxies, IC 2038 and IC 2039, are probably interacting each-other\nand, in the past, IC 2038 could have also interacted with NGC 1533, which\nstripped away gas and stars from its outskirts. The new picture emerging from\nthis study is of an interacting triplet, where the brightest galaxy NGC 1533\nhas ongoing mass assembly in the outskirts.", "cat": "astro-ph.GA", "authors": ["A. Cattapan", "M. Spavone", "E. Iodice", "R. Rampazzo", "S. Ciroi", "E. Ryan-Weber", "P. Schipani", "M. Capaccioli", "A. Grado", "L. Limatola", "P. Mazzei", "E. V. Held", "A. Marino"]}, "1047": {"id": "2402.05849v2", "title": "ALMA Lensing Cluster Survey: Full SED Analysis of z~0.5-6 Lensed Galaxies Detected with Millimeter Observations", "url": "http://arxiv.org/pdf/2402.05849v2", "date": "2024-02-13 07:27:51", "abs": "Sub/millimeter galaxies are a key population for the study of galaxy\nevolution because the majority of star formation at high redshifts occurred in\ngalaxies deeply embedded in dust. To search for this population, we have\nperformed an extensive survey with ALMA, called the ALMA Lensing Cluster Survey\n(ALCS). This survey covers 133 arcmin^2 area and securely detects 180 sources\nat z~0.5-6 with a flux limit of ~0.2 mJy at 1.2 mm (Fujimoto et al. 2023). Here\nwe report the results of multi-wavelength spectral energy distribution (SED)\nanalysis of the whole ALCS sample, utilizing the observed-frame UV to\nmillimeter photometry. We find that the majority of the ALCS sources lie on the\nstar-forming main sequence, with a smaller fraction showing intense starburst\nactivities. The ALCS sample contains high infrared-excess sources\nIRX=log(Ldust/LUV)>1), including two extremely dust-obscured galaxies (IRX>5).\nWe also confirm that the ALCS sample probes a broader range in lower dust mass\nthan conventional SMG samples in the same redshift range. We identify six\nheavily obscured AGN candidates that are not detected in the archival Chandra\ndata in addition to the three X-ray AGNs reported by Uematsu et al. (2023). The\ninferred AGN luminosity density shows a possible excess at z=2-3 compared with\nthat determined from X-ray surveys below 10 keV.", "cat": "astro-ph.GA", "authors": ["Ryosuke Uematsu", "Yoshihiro Ueda", "Kotaro Kohno", "Yoshiki Toba", "Satoshi Yamada", "Ian Smail", "Hideki Umehata", "Seiji Fujimoto", "Bunyo Hatsukade", "Yiping Ao", "Franz Erik Bauer", "Gabriel Brammer", "Miroslava Dessauges-Zavadsky", "Daniel Espada", "Jean-Baptiste Jolly", "Anton M. Koekemoer", "Vasily Kokorev", "Georgios E. Magdis", "Masamune Oguri", "Fengwu Sun"]}, "1048": {"id": "0709.4211v1", "title": "Chandra ACIS Survey of M33 (ChASeM33): A First Look", "url": "http://arxiv.org/pdf/0709.4211v1", "date": "2007-09-26 16:02:28", "abs": "We present an overview of the Chandra ACIS Survey of M33 (ChASeM33): A Deep\nSurvey of the Nearest Face-on Spiral Galaxy. The 1.4 Ms survey covers the\ngalaxy out to $R \\approx 18\\arcmin (\\approx 4$ kpc). These data provide the\nmost intensive, high spatial resolution assessment of the X-ray source\npopulations available for the confused inner regions of M33. Mosaic images of\nthe ChASeM33 observations show several hundred individual X-ray sources as well\nas soft diffuse emission from the hot interstellar medium. Bright, extended\nemission surrounds the nucleus and is also seen from the giant \\hii regions NGC\n604 and IC 131. Fainter extended emission and numerous individual sources\nappear to trace the inner spiral structure. The initial source catalog, arising\nfrom $\\sim$~2/3 of the expected survey data, includes 394 sources significant\nat the $3\\sigma$ confidence level or greater, down to a limiting luminosity\n(absorbed) of $\\sim$1.6\\ergs{35} (0.35 -- 8.0 keV). The hardness ratios of the\nsources separate those with soft, thermal spectra such as supernova remnants\nfrom those with hard, non-thermal spectra such as X-ray binaries and background\nactive galactic nuclei. Emission extended beyond the Chandra point spread\nfunction is evident in 23 of the 394 sources. Cross-correlation of the ChASeM33\nsources against previous catalogs of X-ray sources in M33 results in matches\nfor the vast majority of the brighter sources and shows 28 ChASeM33 sources\nwithin 10\\arcsec of supernova remnants identified by prior optical and radio\nsearches. This brings the total number of such associations to 31 out of 100\nknown supernova remnants in M33.", "cat": "astro-ph", "authors": ["Paul P. Plucinsky", "Benjamin Williams", "Knox S. Long", "Terrance J. Gaetz", "Manami Sasaki", "Wolfgang Pietsch", "Ralph Tuellmann", "Randall K. Smith", "William P. Blair", "David Helfand", "John P. Hughes", "P. Frank Winkler", "Miguel de Avillez", "Luciana Bianchi", "Dieter Breitschwerdt", "Richard J. Edgar", "Parviz Ghavamian", "Jonathan Grindlay", "Frank Haberl", "Robert Kirshner", "Kip Kuntz", "Tsevi Mazeh", "Thomas G. Pannuti", "Avi Shporer", "David A. Thilker"]}, "1049": {"id": "2405.02485v1", "title": "A Survey of Few-Shot Learning for Biomedical Time Series", "url": "http://arxiv.org/pdf/2405.02485v1", "date": "2024-05-03 21:22:27", "abs": "Advancements in wearable sensor technologies and the digitization of medical\nrecords have contributed to the unprecedented ubiquity of biomedical time\nseries data. Data-driven models have tremendous potential to assist clinical\ndiagnosis and improve patient care by improving long-term monitoring\ncapabilities, facilitating early disease detection and intervention, as well as\npromoting personalized healthcare delivery. However, accessing extensively\nlabeled datasets to train data-hungry deep learning models encounters many\nbarriers, such as long-tail distribution of rare diseases, cost of annotation,\nprivacy and security concerns, data-sharing regulations, and ethical\nconsiderations. An emerging approach to overcome the scarcity of labeled data\nis to augment AI methods with human-like capabilities to leverage past\nexperiences to learn new tasks with limited examples, called few-shot learning.\nThis survey provides a comprehensive review and comparison of few-shot learning\nmethods for biomedical time series applications. The clinical benefits and\nlimitations of such methods are discussed in relation to traditional\ndata-driven approaches. This paper aims to provide insights into the current\nlandscape of few-shot learning for biomedical time series and its implications\nfor future research and applications.", "cat": "cs.LG", "authors": ["Chenqi Li", "Timothy Denison", "Tingting Zhu"]}, "1050": {"id": "2107.13586v1", "title": "Pre-train, Prompt, and Predict: A Systematic Survey of Prompting Methods in Natural Language Processing", "url": "http://arxiv.org/pdf/2107.13586v1", "date": "2021-07-28 18:09:46", "abs": "This paper surveys and organizes research works in a new paradigm in natural\nlanguage processing, which we dub \"prompt-based learning\". Unlike traditional\nsupervised learning, which trains a model to take in an input x and predict an\noutput y as P(y|x), prompt-based learning is based on language models that\nmodel the probability of text directly. To use these models to perform\nprediction tasks, the original input x is modified using a template into a\ntextual string prompt x' that has some unfilled slots, and then the language\nmodel is used to probabilistically fill the unfilled information to obtain a\nfinal string x, from which the final output y can be derived. This framework is\npowerful and attractive for a number of reasons: it allows the language model\nto be pre-trained on massive amounts of raw text, and by defining a new\nprompting function the model is able to perform few-shot or even zero-shot\nlearning, adapting to new scenarios with few or no labeled data. In this paper\nwe introduce the basics of this promising paradigm, describe a unified set of\nmathematical notations that can cover a wide variety of existing work, and\norganize existing work along several dimensions, e.g.the choice of pre-trained\nmodels, prompts, and tuning strategies. To make the field more accessible to\ninterested beginners, we not only make a systematic review of existing works\nand a highly structured typology of prompt-based concepts, but also release\nother resources, e.g., a website http://pretrain.nlpedia.ai/ including\nconstantly-updated survey, and paperlist.", "cat": "cs.CL", "authors": ["Pengfei Liu", "Weizhe Yuan", "Jinlan Fu", "Zhengbao Jiang", "Hiroaki Hayashi", "Graham Neubig"]}, "1051": {"id": "1207.4789v1", "title": "A Hubble Space Telescope Survey of H2 Emission in the Circumstellar Environments of Young Stars", "url": "http://arxiv.org/pdf/1207.4789v1", "date": "2012-07-19 20:00:01", "abs": "The formation timescale and final architecture of exoplanetary systems are\nclosely related to the properties of the molecular disks from which they form.\nObservations of the spatial distribution and lifetime of the molecular gas at\nplanet-forming radii (r < 10 AU) are important for understanding the formation\nand evolution of exoplanetary systems. Towards this end, we present the largest\nspectrally resolved survey of H2 emission around low-mass pre-main sequence\nstars compiled to date. We use a combination of new and archival\nfar-ultraviolet spectra from the COS and STIS instruments on the Hubble Space\nTelescope to sample 34 T Tauri stars (27 actively accreting CTTSs and 7\nnon-accreting WTTSs) with ages ranging from roughly 1-10 Myr. We observe\nfluorescent H2 emission, excited by LyA photons, in 100 of the accreting\nsources, including all of the transitional disks in our sample (CS Cha, DM Tau,\nGM Aur, UX Tau A, LkCa15, HD 135344B and TW Hya). The spatial distribution of\nthe emitting gas is inferred from spectrally resolved H2 line profiles. Some of\nthe emitting gas is produced in outflowing material, but the majority of H2\nemission appears to originate in a rotating disk. For the disk-dominated\ntargets, the H2 emission originates predominately at r < 3 AU. The emission\nline-widths and inner molecular radii are found to be roughly consistent with\nthose measured from mid-IR CO spectra.", "cat": "astro-ph.SR", "authors": ["Kevin France", "Rebecca Schindhelm", "Gregory J. Herczeg", "Alexander Brown", "Herve Abgrall", "Richard D. Alexander", "Edwin A. Bergin", "Joanna M. Brown", "Jeffrey L. Linsky", "Evelyne Roueff", "Hao Yang"]}, "1052": {"id": "1712.01205v1", "title": "The Extremely Luminous Quasar Survey (ELQS) in the SDSS footprint I.: Infrared Based Candidate Selection", "url": "http://arxiv.org/pdf/1712.01205v1", "date": "2017-12-04 17:13:09", "abs": "Studies of the most luminous quasars at high redshift directly probe the\nevolution of the most massive black holes in the early Universe and their\nconnection to massive galaxy formation. However, extremely luminous quasars at\nhigh redshift are very rare objects. Only wide area surveys have a chance to\nconstrain their population. The Sloan Digital Sky Survey (SDSS) has so far\nprovided the most widely adopted measurements of the quasar luminosity function\n(QLF) at $z>3$. However, a careful re-examination of the SDSS quasar sample\nrevealed that the SDSS quasar selection is in fact missing a significant\nfraction of $z\\gtrsim3$ quasars at the brightest end. We have identified the\npurely optical color selection of SDSS, where quasars at these redshifts are\nstrongly contaminated by late-type dwarfs, and the spectroscopic incompleteness\nof the SDSS footprint as the main reasons. Therefore we have designed the\nExtremely Luminous Quasar Survey (ELQS), based on a novel near-infrared JKW2\ncolor cut using WISE AllWISE and 2MASS all-sky photometry, to yield high\ncompleteness for very bright ($m_{\\rm{i}} < 18.0$) quasars in the redshift\nrange of $3.0\\leq z\\leq5.0$. It effectively uses random forest machine-learning\nalgorithms on SDSS and WISE photometry for quasar-star classification and\nphotometric redshift estimation. The ELQS will spectroscopically follow-up\n$\\sim 230$ new quasar candidates in an area of $\\sim12000\\,\\rm{deg}^2$ in the\nSDSS footprint, to obtain a well-defined and complete quasars sample for an\naccurate measurement of the bright-end quasar luminosity function at $3.0\\leq\nz\\leq5.0$. In this paper we present the quasar selection algorithm and the\nquasar candidate catalog.", "cat": "astro-ph.GA", "authors": ["Jan-Torge Schindler", "Xiaohui Fan", "Ian. D. McGreer", "Qian Yang", "Jin Wu", "Linhua Jiang", "Richard Green"]}, "1053": {"id": "1908.04310v2", "title": "Euclid preparation: V. Predicted yield of redshift 78$ may be selected from Euclid $OYJH$ photometry\nalone, but selection over the redshift interval $77.5$ should be\nfound in the DR1 data release, expected in 2024. It will be possible to\ndetermine the bright-end slope of the QLF, $7 4 \\times 10^{11} M_\\odot$, within 108 Mpc. Our wide-field\n107\" $\\times$ 107\" IFS data cover radii as large as 40 kpc, for which we\nquantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes\n$\\gamma_{\\rm inner}$ and $\\gamma_{\\rm outer}$ of $\\sigma(R)$. While\n$\\gamma_{\\rm inner}$ is mostly negative, of the 56 galaxies with sufficient\nradial coverage to determine $\\gamma_{\\rm outer}$ we find 36% to have rising\nouter dispersion profiles, 30% to be flat within the uncertainties, and 34% to\nbe falling. The fraction of galaxies with rising outer profiles increases with\n$M_*$ and in denser galaxy environment, with 10 of the 11 most massive galaxies\nin our sample having flat or rising dispersion profiles. The strongest\nenvironmental correlations are with local density and halo mass, but a weaker\ncorrelation with large-scale density also exists. The average $\\gamma_{\\rm\nouter}$ is similar for brightest group galaxies, satellites, and isolated\ngalaxies in our sample. We find a clear positive correlation between the\ngradients of the outer dispersion profile and the gradients of the velocity\nkurtosis $h_4$. Altogether, our kinematic results suggest that the increasing\nfraction of rising dispersion profiles in the most massive ETGs are caused (at\nleast in part) by variations in the total mass profiles rather than in the\nvelocity anisotropy alone.", "cat": "astro-ph.GA", "authors": ["Melanie Veale", "Chung-Pei Ma", "Jenny E. Greene", "Jens Thomas", "John P. Blakeslee", "Jonelle L. Walsh", "Jennifer Ito"]}, "1058": {"id": "1709.01452v1", "title": "A millisecond pulsar discovery in a survey of unidentified Fermi $\u03b3$-ray sources with LOFAR", "url": "http://arxiv.org/pdf/1709.01452v1", "date": "2017-09-05 15:28:40", "abs": "Using LOFAR, we have performed a very-low-frequency (115-155 MHz) radio\nsurvey for millisecond pulsars (MSPs). The survey targeted 52 unidentified\nFermi $\\gamma$-ray sources. Employing a combination of coherent and incoherent\ndedispersion, we have mitigated the dispersive effects of the interstellar\nmedium while maintaining sensitivity to fast-spinning pulsars. Toward 3FGL\nJ1553.1+5437 we have found PSR J1552+5437, the first MSP to be discovered\n(through its pulsations) at a radio frequency $<$ 200 MHz. PSR J1552+5437 is an\nisolated MSP with a 2.43 ms spin period and a dispersion measure of 22.9 pc\ncm$^{-3}$. The pulsar has a very steep radio spectral index ($\\alpha < -$2.8\n$\\pm$ 0.4). We obtain a phase-connected timing solution combining the 0.74\nyears of radio observations with $\\gamma$-ray photon arrival times covering 7.5\nyears of Fermi observations. We find that the radio and $\\gamma$-ray pulse\nprofiles of PSR J1552+5437 appear to be nearly aligned. The very steep spectrum\nof PSR J1552+5437, along with other recent discoveries, hints at a population\nof radio MSPs that have been missed in surveys using higher observing\nfrequencies. Detecting such steep spectrum sources is important for mapping the\npopulation of MSPs down to the shortest spin periods, understanding their\nemission in comparison to slow pulsars, and quantifying the prospects for\nfuture surveys with low-frequency radio telescopes like SKA-Low and its\nprecursors.", "cat": "astro-ph.HE", "authors": ["Z. Pleunis", "C. G. Bassa", "J. W. T. Hessels", "V. I. Kondratiev", "F. Camilo", "I. Cognard", "J. -M. Griessmeier", "B. W. Stappers", "A. S. van Amesfoort", "S. Sanidas"]}, "1059": {"id": "2201.11459v1", "title": "Alleviating the Transit Timing Variations bias in transit surveys. II. RIVERS: Twin resonant Earth-sized planets around Kepler-1972 recovered from Kepler's false positive", "url": "http://arxiv.org/pdf/2201.11459v1", "date": "2022-01-27 11:53:13", "abs": "Transit Timing Variations (TTVs) can provide useful information for systems\nobserved by transit, by putting constraints on the masses and eccentricities of\nthe observed planets, or even constrain the existence of non-transiting\ncompanions. However, TTVs can also prevent the detection of small planets in\ntransit surveys, or bias the recovered planetary and transit parameters. Here\nwe show that Kepler-1972 c, initially the \"not transit-like\" false positive\nKOI-3184.02, is an Earth-sized planet whose orbit is perturbed by Kepler-1972 b\n(initially KOI-3184.01). The pair is locked in a 3:2 Mean-motion resonance,\neach planet displaying TTVs of more than 6h hours of amplitude over the\nduration of the Kepler mission. The two planets have similar masses $m_b/m_c\n=0.956_{-0.051}^{+0.056}$ and radii $R_b=0.802_{-0.041}^{+0.042}R_{Earth}$,\n$R_c=0.868_{-0.050}^{+0.051}R_{Earth}$, and the whole system, including the\ninner candidate KOI-3184.03, appear to be coplanar. Despite the faintness of\nthe signals (SNR of 1.35 for each transit of Kepler-1972 b and 1.10 for\nKepler-1972 c), we recovered the transits of the planets using the RIVERS\nmethod, based on the recognition of the tracks of planets in river diagrams\nusing machine learning, and a photo-dynamic fit of the lightcurve. Recovering\nthe correct ephemerides of the planets is essential to have a complete picture\nof the observed planetary systems. In particular, we show that in Kepler-1972,\nnot taking into account planet-planet interactions yields an error of $\\sim\n30\\%$ on the radii of planets b and c, in addition to generating in-transit\nscatter, which leads to mistake KOI3184.02 for a false positive. Alleviating\nthis bias is essential for an unbiased view of Kepler systems, some of the TESS\nstars, and the upcoming PLATO mission.", "cat": "astro-ph.EP", "authors": ["A. Leleu", "J. -B. Delisle", "R. Mardling", "S. Udry", "G. Chatel", "Y. Alibert", "P. Eggenberger"]}, "1060": {"id": "1409.0447v2", "title": "The FMOS-COSMOS survey of star-forming galaxies at z~1.6 III. Survey design, performance, and sample characteristics", "url": "http://arxiv.org/pdf/1409.0447v2", "date": "2015-07-24 05:47:44", "abs": "We present a spectroscopic survey of galaxies in the COSMOS field using the\nFiber Multi-Object Spectrograph (FMOS), a near-infrared instrument on the\nSubaru Telescope. Our survey is specifically designed to detect the Halpha\nemission line that falls within the H-band (1.6-1.8 um) spectroscopic window\nfrom star-forming galaxies with 1.4 < z < 1.7 and M_stellar>~10^10 Msolar. With\nthe high multiplex capability of FMOS, it is now feasible to construct samples\nof over one thousand galaxies having spectroscopic redshifts at epochs that\nwere previously challenging. The high-resolution mode (R~2600) effectively\nseparates Halpha and [NII]6585 thus enabling studies of the gas-phase\nmetallicity and photoionization state of the interstellar medium. The primary\naim of our program is to establish how star formation depends on stellar mass\nand environment, both recognized as drivers of galaxy evolution at lower\nredshifts. In addition to the main galaxy sample, our target selection places\npriority on those detected in the far-infrared by Herschel/PACS to assess the\nlevel of obscured star formation and investigate, in detail, outliers from the\nstar formation rate - stellar mass relation. Galaxies with Halpha detections\nare followed up with FMOS observations at shorter wavelengths using the J-long\n(1.11-1.35 um) grating to detect Hbeta and [OIII]5008 that provides an\nassessment of extinction required to measure star formation rates not hampered\nby dust, and an indication of embedded Active Galactic Nuclei. With 460\nredshifts measured from 1153 spectra, we assess the performance of the\ninstrument with respect to achieving our goals, discuss inherent biases in the\nsample, and detail the emission-line properties. Our higher-level data\nproducts, including catalogs and spectra, are available to the community.", "cat": "astro-ph.GA", "authors": ["J. D. Silverman", "D. Kashino", "D. Sanders", "J. Kartaltepe", "N. Arimoto", "A. Renzini", "G. Rodighiero", "E. Daddi", "J. Zahid", "T. Nagao", "L. J. Kewley", "S. J. Lilly", "N. Sugiyama", "I. Baronchelli", "P. Capak", "C. M. Carollo", "J. Chu", "G. Hasinger", "O. Ilbert", "S. Juneau", "M. Kajisawa", "A. M. Koekemoer", "K. Kovac", "O. Le Fevre", "D. Masters", "H. J. McCracken", "M. Onodera", "N. Scoville", "V. Strazzullo", "Y. Taniguchi"]}, "1061": {"id": "1804.01652v1", "title": "The VMC Survey. XXIX. Turbulence-Controlled Hierarchical Star Formation in the Small Magellanic Cloud", "url": "http://arxiv.org/pdf/1804.01652v1", "date": "2018-04-05 02:12:07", "abs": "In this paper we report a clustering analysis of upper main-sequence stars in\nthe Small Magellanic Cloud, using data from the VMC survey (the VISTA\nnear-infrared YJKs survey of the Magellanic system). Young stellar structures\nare identified as surface overdensities on a range of significance levels. They\nare found to be organized in a hierarchical pattern, such that larger\nstructures at lower significance levels contain smaller ones at higher\nsignificance levels. They have very irregular morphologies, with a\nperimeter-area dimension of 1.44 +/- 0.02 for their projected boundaries. They\nhave a power-law mass-size relation, power-law size/mass distributions, and a\nlognormal surface density distribution. We derive a projected fractal dimension\nof 1.48 +/- 0.03 from the mass-size relation, or of 1.4 +/- 0.1 from the size\ndistribution, reflecting significant lumpiness of the young stellar structures.\nThese properties are remarkably similar to those of a turbulent interstellar\nmedium (ISM), supporting a scenario of hierarchical star formation regulated by\nsupersonic turbulence.", "cat": "astro-ph.GA", "authors": ["Ning-Chen Sun", "Richard de Grijs", "Maria-Rosa L. Cioni", "Stefano Rubele", "Smitha Subramanian", "Jacco Th. van Loon", "Kenji Bekki", "Cameron P. M. Bell", "Valentin D. Ivanov", "Marcella Marconi", "Tatiana Muraveva", "Joana M. Oliveira", "Vincenzo Ripepi"]}, "1062": {"id": "1901.00549v2", "title": "Rubio de Francia extrapolation theorem and related topics in the theory of elliptic and parabolic equations. A survey", "url": "http://arxiv.org/pdf/1901.00549v2", "date": "2020-04-05 21:59:57", "abs": "We give a brief overview of the history of the Sobolev mixed norm theory of\nlinear elliptic and parabolic equations and the recent development in this\ntheory based on the Rubio de Francia extrapolation theorem. A self contained\nproof of this theorem along with other relevant tools of Real Analysis are also\npresented as well as an application to mixed norm estimates for fully nonlinear\nequations.", "cat": "math.AP", "authors": ["N. V. Krylov"]}, "1063": {"id": "1904.08312v2", "title": "Mean value properties of harmonic functions and related topics (a survey)", "url": "http://arxiv.org/pdf/1904.08312v2", "date": "2019-05-22 16:08:12", "abs": "Results involving various mean value properties are reviewed for harmonic,\nbiharmonic and metaharmonic functions. It is also considered how the standard\nmean value property can be weakened to imply harmonicity and belonging to other\nclasses of functions.", "cat": "math.AP", "authors": ["Nikolay Kuznetsov"]}, "1064": {"id": "1201.5955v2", "title": "Constraining inflation with future galaxy redshift surveys", "url": "http://arxiv.org/pdf/1201.5955v2", "date": "2012-04-05 11:28:58", "abs": "With future galaxy surveys, a huge number of Fourier modes of the\ndistribution of the large scale structures in the Universe will become\navailable. These modes are complementary to those of the CMB and can be used to\nset constraints on models of the early universe, such as inflation. Using a\nMCMC analysis, we compare the power of the CMB with that of the combination of\nCMB and galaxy survey data, to constrain the power spectrum of primordial\nfluctuations generated during inflation. We base our analysis on the Planck\nsatellite and a spectroscopic redshift survey with configuration parameters\nclose to those of the Euclid mission as examples. We first consider models of\nslow-roll inflation, and show that the inclusion of large scale structure data\nimproves the constraints by nearly halving the error bars on the scalar\nspectral index and its running. If we attempt to reconstruct the inflationary\nsingle-field potential, a similar conclusion can be reached on the parameters\ncharacterizing the potential. We then study models with features in the power\nspectrum. In particular, we consider ringing features produced by a break in\nthe potential and oscillations such as in axion monodromy. Adding large scale\nstructures improves the constraints on features by more than a factor of two.\nIn axion monodromy we show that there are oscillations with small amplitude and\nfrequency in momentum space that are undetected by CMB alone but can be\nmeasured by including galaxy surveys in the analysis.", "cat": "astro-ph.CO", "authors": ["Zhiqi Huang", "Licia Verde", "Filippo Vernizzi"]}, "1065": {"id": "2008.05972v1", "title": "A Survey on Knowledge integration techniques with Artificial Neural Networks for seq-2-seq/time series models", "url": "http://arxiv.org/pdf/2008.05972v1", "date": "2020-08-13 15:40:38", "abs": "In recent years, with the advent of massive computational power and the\navailability of huge amounts of data, Deep neural networks have enabled the\nexploration of uncharted areas in several domains. But at times, they\nunder-perform due to insufficient data, poor data quality, data that might not\nbe covering the domain broadly, etc. Knowledge-based systems leverage expert\nknowledge for making decisions and suitably take actions. Such systems retain\ninterpretability in the decision-making process. This paper focuses on\nexploring techniques to integrate expert knowledge to the Deep Neural Networks\nfor sequence-to-sequence and time series models to improve their performance\nand interpretability.", "cat": "cs.LG", "authors": ["Pramod Vadiraja", "Muhammad Ali Chattha"]}, "1066": {"id": "1504.01876v1", "title": "Halpha Imaging of the Herschel Reference Survey. The star formation properties of a volume-limited, K-band-selected sample of nearby late-type galaxies", "url": "http://arxiv.org/pdf/1504.01876v1", "date": "2015-04-08 09:26:18", "abs": "We present new Halpha+[NII] imaging data of late-type galaxies in the\nHerschel Reference Survey aimed at studying the star formation properties of a\nK-band-selected, volume-limited sample of nearby galaxies. The Halpha+[NII]\ndata are corrected for [NII] contamination and dust attenuation using different\nrecipes based on the Balmer decrement and the 24mic luminosities. We show that\nthe L(Halpha) derived with different corrections give consistent results only\nwhenever the uncertainty on the estimate of the Balmer decrement is <=0.1. We\nuse these data to derive the SFR of the late-type galaxies of the sample, and\ncompare these estimates to those determined using independent monochromatic\ntracers (FUV, radio) or the output of SED fitting codes. This comparison\nsuggests that the 24mic based dust extinction correction for Halpha might be\nnon universal, and that it should be used with caution in all objects with a\nSFA, where dust heating can be dominated by the old stellar population.\nFurthermore, because of the sudden truncation of the SFA of cluster galaxies\noccurring after their interaction with the surrounding environment, the\nstationarity conditions required to transform monochromatic fluxes into SFR\nmight not always be satisfied in tracers other than L(Halpha). In a similar\nway, the parametrisation of the SFH generally used in SED fitting codes might\nnot be adequate for these recently interacting systems. We then study the SFR\nluminosity distribution and the typical scaling relations of late-type\ngalaxies. We observe a systematic decrease of the SSFR with increasing stellar\nmass, stellar mass surface density, and metallicity. We also observe an\nincrease of the asymmetry and smoothness parameters measured in the Halpha-band\nwith increasing SSFR, probably induced by an increase of the contribution of\ngiant HII regions to the Halpha luminosity function in SF low-luminosity\ngalaxies.", "cat": "astro-ph.GA", "authors": ["A. Boselli", "M. Fossati", "G. Gavazzi", "L. Ciesla", "V. Buat", "S. Boissier", "T. Hughes"]}, "1067": {"id": "2208.13912v1", "title": "Li distribution, kinematics and detailed abundance analysis among very metal-poor stars in the Galactic halo from the HESP-GOMPA survey", "url": "http://arxiv.org/pdf/2208.13912v1", "date": "2022-08-29 22:18:39", "abs": "We present a study on the detailed elemental abundances of newly identified\nbright very metal-poor stars with the detection of lithium, initially observed\nas part of the SDSS/MARVELS pre-survey. These stars were selected for\nhigh-resolution spectroscopic follow-up as part of the HESP-GOMPA survey. In\nthis work, we discuss the Li abundances detected for several stars in the\nsurvey, which include main-sequence stars, subgiants, and red giants. Different\nclasses of stars are found to exhibit very similar distributions of Li, which\npoint towards a common origin. We derive a scaling relation for the depletion\nof Li as a function of temperature for giants and main-sequence stars; the\nmajority of the samples from the literature were found to fall within 1sigma\n(0.19 and 0.12 dex/K for giants and dwarfs respectively) of this relationship.\nWe also report the existence of a slope of the Li abundances as a function of\ndistances from the Galactic plane, indicating mixed stellar populations. Most\nLi-rich stars are found to be in or close to the galactic plane. Along with Li,\nwe have derived detailed abundances for C, odd-Z, alpha-, Fe-peak, and\nneutron-capture elements for each star. We have also used astrometric\nparameters from Gaia-EDR3 to complement our study, and derived kinematics to\ndifferentiate between the motions of the stars; those formed in situ and\naccreted. The stellar population of the Spite plateau, including additional\nstars from the literature, is found to have significant contributions from\nstars formed in situ and through accretion. The orbits for the program stars\nhave also been derived and studied for a period of 5 Gyr backward in time.", "cat": "astro-ph.SR", "authors": ["Avrajit Bandyopadhyay", "Thirupathi Sivarani", "Timothy C. Beers", "A. Susmitha", "Prasanta K Nayak", "Jeewan C Pandey"]}, "1068": {"id": "1905.08505v1", "title": "Verification Artifacts in Cooperative Verification: Survey and Unifying Component Framework", "url": "http://arxiv.org/pdf/1905.08505v1", "date": "2019-05-21 08:57:10", "abs": "The goal of cooperative verification is to combine verification approaches in\nsuch a way that they work together to verify a system model. In particular,\ncooperative verifiers provide exchangeable information (verification artifacts)\nto other verifiers or consume such information from other verifiers with the\ngoal of increasing the overall effectiveness and efficiency of the verification\nprocess. This paper first gives an overview over approaches for leveraging\nstrengths of different techniques, algorithms, and tools in order to increase\nthe power and abilities of the state of the art in software verification.\nSecond, we specifically outline cooperative verification approaches and discuss\ntheir employed verification artifacts. We formalize all artifacts in a uniform\nway, thereby fixing their semantics and providing verifiers with a precise\nmeaning of the exchanged information.", "cat": "cs.SE", "authors": ["Dirk Beyer", "Heike Wehrheim"]}, "1069": {"id": "2405.20385v1", "title": "The PAU Survey: galaxy stellar population properties estimate with narrow-band data", "url": "http://arxiv.org/pdf/2405.20385v1", "date": "2024-05-30 18:00:06", "abs": "Narrowband galaxy surveys have recently gained interest as a promising method\nto achieve the necessary accuracy on the photometric redshift estimate of\nindividual galaxies for stage-IV cosmological surveys. One key advantage is the\nability to provide higher spectral resolution information about galaxies that\nshould allow a more accurate and precise estimation of galaxy stellar\npopulation properties. However, the impact of adding narrow-band photometry on\nthe stellar population properties estimate is largely unexplored. The scope of\nthis work is two-fold: on one side, leveraging the predictive power of\nbroad-band and narrow-band data to infer galaxy physical properties such as\nstellar masses, ages, star formation rates and metallicities. On the other\nhand, evaluating the improvement of performance in estimating galaxy properties\nwhen we use narrow-band data instead of broad-band. In this work we measure the\nstellar population properties of a sample of galaxies in the COSMOS field for\nwhich both narrowband and broadband data are available. In particular, we\nemploy narrowband data from PAUS and broad-band data from CFHTLS. We use two\ndifferent spectral energy distribution fitting codes to measure galaxy\nproperties, namely CIGALE and Prospector. We find that the increased spectral\nresolution of narrow-band photometry does not yield a substantial improvement\non constraining galaxy properties using spectral energy distribution fitting.\nStill we find that we obtain a more diverse distribution of metallicities and\ndust optical depths with cigale when employing the narrowband data. The effect\nis not as prominent as expected, which we relate this to the low narrowband SNR\nof a majority of the galaxies, the respective drawbacks of both codes as well\nas the coverage only in the optical regime. The measured properties are\nafterwards compared to the COSMOS2020 catalogue, showing good agreement.", "cat": "astro-ph.GA", "authors": ["Benjamin Csizi", "Luca Tortorelli", "Ma\u0142gorzata Siudek", "Daniel Gruen", "Pablo Renard", "Pau Tallada-Cresp\u00ed", "Eusebio Sanchez", "Ramon Miquel", "Cristobal Padilla", "Juan Garc\u00eda-Bellido", "Enrique Gazta\u00f1aga", "Ricard Casas", "Santiago Serrano", "Juan De Vicente", "Enrique Fernandez", "Martin Eriksen", "Giorgio Manzoni", "Carlton M. Baugh", "Jorge Carretero", "Francisco J. Castander"]}, "1070": {"id": "2208.09199v1", "title": "Searching for nascent planetary nebulae: OHPNe candidates in the SPLASH survey", "url": "http://arxiv.org/pdf/2208.09199v1", "date": "2022-08-19 07:55:30", "abs": "The evolution of asymptotic giant branch stars from the spherical symmetry\ninto the diverse shapes of planetary nebulae (PNe) is a topic of intensive\nresearch. Young PNe provide a unique opportunity to characterize the onset of\nthis transitional phase. In particular, OH maser-emitting PNe (OHPNe) are\nconsidered nascent PNe. In fact, only 6 OHPNe have been confirmed to date. In\norder to identify and characterize more OHPNe, we processed the unpublished\ncontinuum data of the interferometric follow-up of the Southern Parkes\nLarge-Area Survey in Hydroxyl (SPLASH). We then matched the interferometric\npositions of OH maser and radio continuum emission, considering the latter as a\npossible tracer of free-free emission from photoionized gas, characteristic of\nPNe. We report 8 objects with a positive coincidence, 4 of which are classified\nas candidate OHPNe here for the first time (IRAS 16372-4808, IRAS 17494-2645,\nIRAS 18019-2216 and OH 341.6811+00.2634). Available evidence strongly indicates\nthat they are evolved stars, while the comparison with confirmed OHPNe\nindicates that they are likely to be PNe. Their final confirmation as bona fide\nPNe, however, requires optical/infrared spectroscopy. The obtained spectral\nindices of the radio continuum emission (between $\\simeq$ 0.4 - 1.3) are\nconsistent with partially optically thick free-free emission from photoionized\ngas. Also, they cluster in the same region of a WISE colour-colour diagram as\nthat of the confirmed OHPNe ($9.5 \\lesssim [3.4]-[22] \\lesssim 13.5$, and $4.0\n\\lesssim [4.6]-[12] \\lesssim 7.0$), thus this diagram could help to identify\nmore OHPNe candidates in the future.", "cat": "astro-ph.SR", "authors": ["Rold\u00e1n A. Cala", "Jos\u00e9 F. G\u00f3mez", "Luis F. Miranda", "Lucero Uscanga", "Shari L. Breen", "Joanne R. Dawson", "Itziar de Gregorio-Monsalvo", "Hiroshi Imai", "Hai-Hua Qiao", "Olga Su\u00e1rez"]}, "1071": {"id": "2205.08072v1", "title": "A Survey on Machine Learning for Geo-Distributed Cloud Data Center Management", "url": "http://arxiv.org/pdf/2205.08072v1", "date": "2022-05-17 03:14:54", "abs": "Cloud workloads today are typically managed in a distributed environment and\nprocessed across geographically distributed data centers. Cloud service\nproviders have been distributing data centers globally to reduce operating\ncosts while also improving quality of service by using intelligent workload and\nresource management strategies. Such large scale and complex orchestration of\nsoftware workload and hardware resources remains a difficult problem to solve\nefficiently. Researchers and practitioners have been trying to address this\nproblem by proposing a variety of cloud management techniques. Mathematical\noptimization techniques have historically been used to address cloud management\nissues. But these techniques are difficult to scale to geo-distributed problem\nsizes and have limited applicability in dynamic heterogeneous system\nenvironments, forcing cloud service providers to explore intelligent\ndata-driven and Machine Learning (ML) based alternatives. The characterization,\nprediction, control, and optimization of complex, heterogeneous, and\never-changing distributed cloud resources and workloads employing ML\nmethodologies have received much attention in recent years. In this article, we\nreview the state-of-the-art ML techniques for the cloud data center management\nproblem. We examine the challenges and the issues in current research focused\non ML for cloud management and explore strategies for addressing these issues.\nWe also discuss advantages and disadvantages of ML techniques presented in the\nrecent literature and make recommendations for future research directions.", "cat": "cs.DC", "authors": ["Ninad Hogade", "Sudeep Pasricha"]}, "1072": {"id": "0901.4592v1", "title": "High Frequency GPS sources in the AT20G Survey", "url": "http://arxiv.org/pdf/0901.4592v1", "date": "2009-01-29 02:08:55", "abs": "The Australia Telescope 20GHz (AT20G) survey was used to select a complete\nsample of 656 Gigahertz Peaked Spectrum (GPS) sources with spectral turnovers\nabove 5GHz. The AT20G has near simultaneous observations at 4.8, 8.6 and 20GHz,\nwhich makes it possible to exclude flat spectrum variability as a cause of a\nsource's peaked spectrum. Optical identification of the sample results in 361\nQSOs and 104 galaxies and 191 blank fields. Redshifts are known for 104 of the\nGPS sources. The GPS sources from the AT20G are discussed and compared to\npreviously known samples. The new sample of high frequency peaking GPS sources\nis found at a lower redshift than previous samples and to also have a lower\n5GHz radio power. Evidence is found to support the idea that the origin of the\nGPS spectral shape are intrinsically different for galaxies and QSOs. This\npaper is an elaboration and extension of the talk given at the $4^{th}$ CSS/GPS\nconference in Riccione in May 2008.", "cat": "astro-ph.GA", "authors": ["P. J. Hancock"]}, "1073": {"id": "2308.03441v1", "title": "The elemental abundances of quiescent galaxies in the LEGA-C survey: the (non-)evolution of [\u03b1/Fe] from z = 0.75 to z = 0", "url": "http://arxiv.org/pdf/2308.03441v1", "date": "2023-08-07 09:48:51", "abs": "We measure the [${\\alpha}$/Fe] abundances for 183 quiescent galaxies at z =\n0.60 - 0.75 with stellar masses ranging 10.4 \\leq log10 10.4 $\\leq$ log10\n(M$_*$ /M$_\\odot$) $\\leq$ 11.6 selected from the LEGA-C survey. We estimate\n[${\\alpha}$/Fe] from the ratio of the spectral indices Mgb (${\\lambda} \\sim\n5177$ {\\AA}) and Fe4383, compared to predictions of simple stellar population\nmodels. We find that 91% of quiescents in our sample have supersolar\n[${\\alpha}$/Fe], with an average value of [${\\alpha}$/Fe] = +0.24 $\\pm$ 0.01.\nWe find no significant correlation between [${\\alpha}$/Fe] and stellar\nmetallicity, mass, velocity dispersion, and average formation time. Galaxies\nthat formed the bulk of their stellar mass on time scales shorter than 1 Gyr\nfollow the same [${\\alpha}$/Fe] distribution as those which formed on longer\ntime scales. In comparison to local early-type galaxies and to stacked spectra\nof quiescent galaxies at z = 0.38 and z = 0.07, we find that the average\n[${\\alpha}$/Fe] has not changed between z = 0.75 and the present time. Our work\nshows that the vast majority of massive quiescent galaxies at z $\\sim$ 0.7 are\n${\\alpha}$-enhanced, and that no detectable evolution of the average\n[${\\alpha}$/Fe] has taken place over the last $\\sim$ 6.5 Gyr.", "cat": "astro-ph.GA", "authors": ["Davide Bevacqua", "Paolo Saracco", "Francesco La Barbera", "Giuseppe D'Ago", "Roberto de Propris", "Ignacio Ferreras", "Anna Gallazzi", "Anna Pasquali", "Chiara Spiniello"]}, "1074": {"id": "1702.01636v2", "title": "Slice-to-volume medical image registration: a survey", "url": "http://arxiv.org/pdf/1702.01636v2", "date": "2017-04-27 14:49:15", "abs": "During the last decades, the research community of medical imaging has\nwitnessed continuous advances in image registration methods, which pushed the\nlimits of the state-of-the-art and enabled the development of novel medical\nprocedures. A particular type of image registration problem, known as\nslice-to-volume registration, played a fundamental role in areas like image\nguided surgeries and volumetric image reconstruction. However, to date, and\ndespite the extensive literature available on this topic, no survey has been\nwritten to discuss this challenging problem. This paper introduces the first\ncomprehensive survey of the literature about slice-to-volume registration,\npresenting a categorical study of the algorithms according to an ad-hoc\ntaxonomy and analyzing advantages and disadvantages of every category. We draw\nsome general conclusions from this analysis and present our perspectives on the\nfuture of the field.", "cat": "cs.CV", "authors": ["Enzo Ferrante", "Nikos Paragios"]}, "1075": {"id": "1811.11767v1", "title": "The MOSDEF Survey: Significant Evolution in the Rest-Frame Optical Emission Line Equivalent Widths of Star-Forming Galaxies at z=1.4-3.8", "url": "http://arxiv.org/pdf/1811.11767v1", "date": "2018-11-28 19:00:04", "abs": "We use extensive spectroscopy from the MOSFIRE Deep Evolution Field (MOSDEF)\nsurvey to investigate the relationships between rest-frame optical emission\nline equivalent widths ($W$) and a number of galaxy and ISM characteristics for\na sample of $1134$ star-forming galaxies at redshifts $1.4\\lesssim z\\lesssim\n3.8$. We examine how the equivalent widths of [OII]$\\lambda\\lambda 3727, 3730$,\nH$\\beta$, [OIII]$\\lambda\\lambda 4960, 5008$, [OIII]$+$H$\\beta$, H$\\alpha$, and\nH$\\alpha$+[NII]$\\lambda\\lambda 6550, 6585$, depend on stellar mass, UV slope,\nage, star-formation rate (SFR) and specific SFR (sSFR), ionization parameter\nand excitation conditions (O32 and [OIII]/H$\\beta$), gas-phase metallicity, and\nionizing photon production efficiency ($\\xi_{\\rm ion}$). The trend of\nincreasing $W$ with decreasing stellar mass is strongest for [OIII] (and\n[OIII]+H$\\beta$). More generally, the equivalent widths of all the lines\nincrease with redshift at a fixed stellar mass or fixed gas-phase metallicity,\nsuggesting that high equivalent width galaxies are common at high redshift.\nThis redshift evolution in equivalent widths can be explained by the increase\nin SFR and decrease in metallicity with redshift at a fixed stellar mass.\nConsequently, the dependence of $W$ on sSFR is largely invariant with redshift,\nparticularly when examined for galaxies of a given metallicity. Our results\nshow that high equivalent width galaxies, specifically those with high $W({\\rm\n[OIII]})$, have low stellar masses, blue UV slopes, young ages, high sSFRs, ISM\nline ratios indicative of high ionization parameters, high $\\xi_{\\rm ion}$, and\nlow metallicities. As these characteristics are often attributed to galaxies\nwith high ionizing escape fractions, galaxies with high $W$ are likely\ncandidates for the population that dominates cosmic reionization.", "cat": "astro-ph.GA", "authors": ["Naveen A. Reddy", "Alice E. Shapley", "Ryan L. Sanders", "Mariska Kriek", "Alison L. Coil", "Irene Shivaei", "William R. Freeman", "Bahram Mobasher", "Brian Siana", "Mojegan Azadi", "Tara Fetherolf", "Francesca M. Fornasini", "Gene Leung", "Sedona H. Price", "Tom Zick", "Guillermo Barro"]}, "1076": {"id": "1708.01534v1", "title": "Dark Energy Survey Year 1 Results: The Impact of Galaxy Neighbours on Weak Lensing Cosmology with im3shape", "url": "http://arxiv.org/pdf/1708.01534v1", "date": "2017-08-04 14:52:31", "abs": "We use a suite of simulated images based on Year 1 of the Dark Energy Survey\nto explore the impact of galaxy neighbours on shape measurement and shear\ncosmology. The hoopoe image simulations include realistic blending, galaxy\npositions, and spatial variations in depth and PSF properties. Using the\nim3shape maximum-likelihood shape measurement code, we identify four mechanisms\nby which neighbours can have a non-negligible influence on shear estimation.\nThese effects, if ignored, would contribute a net multiplicative bias of $m\n\\sim 0.03 - 0.09$ in the DES Y1 im3shape catalogue, though the precise impact\nwill be dependent on both the measurement code and the selection cuts applied.\nThis can be reduced to percentage level or less by removing objects with close\nneighbours, at a cost to the effective number density of galaxies\n$n_\\mathrm{eff}$ of 30%. We use the cosmological inference pipeline of DES Y1\nto explore the cosmological implications of neighbour bias and show that\nomitting blending from the calibration simulation for DES Y1 would bias the\ninferred clustering amplitude $S_8\\equiv \\sigma_8 (\\Omega _\\mathrm{m}\n/0.3)^{0.5}$ by $2 \\sigma$ towards low values. Finally, we use the hoopoe\nsimulations to test the effect of neighbour-induced spatial correlations in the\nmultiplicative bias. We find the impact on the recovered $S_8$ of ignoring such\ncorrelations to be subdominant to statistical error at the current level of\nprecision.", "cat": "astro-ph.CO", "authors": ["S. Samuroff", "S. L. Bridle", "J. Zuntz", "M. A. Troxel", "D. Gruen", "R. P. Rollins", "G. M. Bernstein", "T. F. Eifler", "E. M. Huff", "T. Kacprzak", "E. Krause", "N. MacCrann", "F. B. Abdalla", "S. Allam", "J. Annis", "K. Bechtol", "A. Benoit-Levy", "E. Bertin", "D. Brooks", "E. Buckley-Geer", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "M. Crocce", "C. B. D'Andrea", "L. N. da Costa", "C. Davis", "S. Desai", "P. Doel", "A. Fausti Neto", "B. Flaugher", "P. Fosalba", "J. Frieman", "J. Garcia-Bellido", "D. W. Gerdes", "R. A. Gruendl", "J. Gschwend", "G. Gutierrez", "K. Honscheid", "D. J. James", "M. Jarvis", "T. Jeltema", "D. Kirk", "K. Kuehn", "S. Kuhlmann", "T. S. Li", "M. Lima", "M. A. G. Maia", "M. March", "J. L. Marshall", "P. Martini", "P. Melchior", "F. Menanteau", "R. Miquel", "B. Nord", "R. L. C. Ogando", "A. A. Plazas", "A. Roodman", "E. Sanchez", "V. Scarpine", "R. Schindler", "M. Schubnell", "I. Sevilla-Noarbe", "E. Sheldon", "M. Smith", "M. Soares-Santos", "F. Sobreira", "E. Suchyta", "G. Tarle", "D. Thomas", "D. L. Tucker"]}, "1077": {"id": "2103.01656v1", "title": "A survey of IRAS young stellar object candidates. Searching for large-scale Herbig-Haro objects", "url": "http://arxiv.org/pdf/2103.01656v1", "date": "2021-03-02 11:35:36", "abs": "Jets and outflows are associated with young stellar objects across the\nstellar mass spectrum, from brown dwarf protostars to massive, Ae/Be stars.\nFrequently, the jet morphology is spatially discontinuous because of the\ntemporal variability of the ejection from the driving source. Images covering a\nwide field of view around the jet driving-source are useful to map the\nlarge-scale jet emission and to explore the mass ejection history. The aim of\nthis work was to search for large-scale optical Herbig-Haro (HH) objects lying\nin a wide field around a sample of IRAS sources, candidates to trace young\nstellar objects. Deep, narrow-band images through the H$\\alpha$ and [SII]\nemission lines, and through an off-line continuum filter, covering a wide\n($\\sim15'$) field around the IRAS targets were acquired. The images in the\nthree filters were analyzed to identify shock-excited line emission (i.e., HH)\nin contrast to scattered line emission. New images of a sample of fifteen IRAS\nsources, obtained in an homogeneous way are presented. HH emission was detected\nin six fields, and the astrometry of the knot features is given. The nature of\nthe extended emission as scattered emission around nine of the IRAS targets is\nconfirmed. For seven IRAS sources, with unclear optical counterpart, a more\nplausible counterpart is proposed. A refined value of the source distance is\nreported for seven targets. An update of the main data available for each of\nthe sampled fields, including images from public data archives, is also\npresented.", "cat": "astro-ph.SR", "authors": ["Rosario L\u00f3pez", "Angels Riera", "Robert Estalella", "Gabriel G\u00f3mez"]}, "1078": {"id": "2304.05811v1", "title": "A Survey on Distributed Evolutionary Computation", "url": "http://arxiv.org/pdf/2304.05811v1", "date": "2023-04-12 12:39:24", "abs": "The rapid development of parallel and distributed computing paradigms has\nbrought about great revolution in computing. Thanks to the intrinsic\nparallelism of evolutionary computation (EC), it is natural to implement EC on\nparallel and distributed computing systems. On the one hand, the computing\npower provided by parallel computing systems can significantly improve the\nefficiency and scalability of EC. On the other hand, data are collected and\nprocessed in a distributed manner, which brings a novel development direction\nand new challenges to EC. In this paper, we intend to give a systematic review\non distributed EC (DEC). First, a new taxonomy for DEC is proposed from top\ndesign mechanism to bottom implementation mechanism. Based on this taxonomy,\nexisting studies on DEC are reviewed in terms of purpose, parallel structure of\nthe algorithm, parallel model for implementation, and the implementation\nenvironment. Second, we clarify two major purposes of DEC, i.e., improving\nefficiency through parallel processing for centralized optimization and\ncooperating distributed individuals/sub-populations with partial information to\nperform distributed optimization. Third, noting that the latter purpose of DEC\nis an emerging and attractive trend for EC with the booming of spatially\ndistributed paradigms, this paper gives a systematic definition of the\ndistributed optimization and classifies it into dimension distributed-, data\ndistributed-, and objective distributed-optimization problems. Formal\nformulations for these problems are provided and various DEC studies on these\nproblems are reviewed. We also discuss challenges and potential research\ndirections, aiming to enlighten the design of DEC and pave the way for future\ndevelopments.", "cat": "cs.NE", "authors": ["Wei-Neng Chen", "Feng-Feng Wei", "Tian-Fang Zhao", "Kay Chen Tan", "Jun Zhang"]}, "1079": {"id": "1507.08289v1", "title": "HeCS-SZ: The Hectospec Survey of Sunyaev-Zeldovich Selected Clusters", "url": "http://arxiv.org/pdf/1507.08289v1", "date": "2015-07-29 20:12:37", "abs": "We estimate cluster masses and velocity dispersions for 123 clusters from\noptical spectroscopy to compare the Sunyaev-Zeldovich (SZ) mass proxy and\ndynamical masses. Our new survey, HeCS-SZ (Hectospec Cluster Survey of\nSZ-selected clusters), includes 7,721 new or remeasured redshifts from\nMMT/Hectospec observations of 24 SZ-selected clusters at redshifts\n$z$=0.05-0.20 and not in previous surveys. We supplement the Hectospec data\nwith spectra from the Sloan Digital Sky Survey (SDSS) and cluster data from the\nCluster Infall Regions in SDSS (CIRS) project and the Hectospec Cluster Survey\n(HeCS), our Hectospec survey of clusters selected by X-ray flux. We measure the\nscaling relation between velocity dispersion and SZ mass estimates from the\nintegrated Compton parameter for an SZ complete sample of 83 clusters. The\nobserved relation agrees very well with a simple virial scaling from mass\n(based on SZ) to velocity dispersion. The SZ mass estimates (calibrated with\nhydrostatic X-ray mass estimates) are not significantly biased. Further, the\nvelocity dispersion of cluster galaxies is consistent with the expected\nvelocity dispersion of dark matter particles, indicating that galaxies are good\ndynamical tracers (i.e., velocity bias is small). Significant mass bias in SZ\nmass estimates could relieve tension between cosmological results from Planck\nSZ cluster counts and Planck CMB data. However, the excellent agreement between\nour measured velocity dispersions and those predicted from a virial scaling\nrelation suggests that any SZ mass bias is too small to reconcile SZ and CMB\nresults. In principle, SZ mass bias and velocity bias of galaxies could\nconspire to yield good agreement, but the required velocity bias is\n$\\sigma_{galaxy}\\approx 0.77\\sigma_{DM}$, outside the range of plausible models\nof velocity bias in the literature.", "cat": "astro-ph.CO", "authors": ["Kenneth J. Rines", "Margaret J. Geller", "Antonaldo Diaferio", "Ho Seong Hwang"]}, "1080": {"id": "2207.09255v1", "title": "First results of a magnetic survey of classical Cepheids", "url": "http://arxiv.org/pdf/2207.09255v1", "date": "2022-07-19 13:12:08", "abs": "We report recent ESPaDOnS and HARPSpol spectropolarimetric observations from\nour ongoing magnetic survey of the brightest twenty-five classical Cepheids.\nStokes $V$ magnetic signatures are detected in eight of fifteen targets\nobserved to date. The Stokes $V$ profiles show a diversity of morphologies with\nweak associated longitudinal field measurements of order 1 G. Many of the\nStokes $V$ profiles are difficult to interpret in the context of the normal\nZeeman effect. They consist of approximately unipolar single or double lobe(s)\nof positive or negative circular polarization. We hypothesize that these\nunusual signatures are due to the Zeeman effect modified by atmospheric\nvelocity or magnetic field gradients. In contrast, the Stokes $V$ profiles of\nPolaris and MY Pup appear qualitatively similar to the complex magnetic\nsignatures of non-pulsating cool supergiants, possibly due to the low pulsation\namplitudes of these two stars.", "cat": "astro-ph.SR", "authors": ["James A. Barron", "Gregg A. Wade", "Colin P. Folsom", "Oleg Kochukhov"]}, "1081": {"id": "2209.01610v3", "title": "Generalization in Neural Networks: A Broad Survey", "url": "http://arxiv.org/pdf/2209.01610v3", "date": "2024-07-31 21:06:23", "abs": "This paper reviews concepts, modeling approaches, and recent findings along a\nspectrum of different levels of abstraction of neural network models including\ngeneralization across (1) Samples, (2) Distributions, (3) Domains, (4) Tasks,\n(5) Modalities, and (6) Scopes. Strategies for (1) sample generalization from\ntraining to test data are discussed, with suggestive evidence presented that,\nat least for the ImageNet dataset, popular classification models show\nsubstantial overfitting. An empirical example and perspectives from statistics\nhighlight how models' (2) distribution generalization can benefit from\nconsideration of causal relationships and counterfactual scenarios. Transfer\nlearning approaches and results for (3) domain generalization are summarized,\nas is the wealth of domain generalization benchmark datasets available. Recent\nbreakthroughs surveyed in (4) task generalization include few-shot\nmeta-learning approaches and the emergence of transformer-based foundation\nmodels such as those used for language processing. Studies performing (5)\nmodality generalization are reviewed, including those that integrate image and\ntext data and that apply a biologically-inspired network across olfactory,\nvisual, and auditory modalities. Higher-level (6) scope generalization results\nare surveyed, including graph-based approaches to represent symbolic knowledge\nin networks and attribution strategies for improving networks' explainability.\nAdditionally, concepts from neuroscience are discussed on the modular\narchitecture of brains and the steps by which dopamine-driven conditioning\nleads to abstract thinking.", "cat": "cs.LG", "authors": ["Chris Rohlfs"]}, "1082": {"id": "2011.01314v1", "title": "Automatic Detection of Machine Generated Text: A Critical Survey", "url": "http://arxiv.org/pdf/2011.01314v1", "date": "2020-11-02 20:59:26", "abs": "Text generative models (TGMs) excel in producing text that matches the style\nof human language reasonably well. Such TGMs can be misused by adversaries,\ne.g., by automatically generating fake news and fake product reviews that can\nlook authentic and fool humans. Detectors that can distinguish text generated\nby TGM from human written text play a vital role in mitigating such misuse of\nTGMs. Recently, there has been a flurry of works from both natural language\nprocessing (NLP) and machine learning (ML) communities to build accurate\ndetectors for English. Despite the importance of this problem, there is\ncurrently no work that surveys this fast-growing literature and introduces\nnewcomers to important research challenges. In this work, we fill this void by\nproviding a critical survey and review of this literature to facilitate a\ncomprehensive understanding of this problem. We conduct an in-depth error\nanalysis of the state-of-the-art detector and discuss research directions to\nguide future work in this exciting area.", "cat": "cs.CL", "authors": ["Ganesh Jawahar", "Muhammad Abdul-Mageed", "Laks V. S. Lakshmanan"]}, "1083": {"id": "1011.4156v1", "title": "Exoplanet-atmospheres at high spectral resolution: A CRIRES survey of hot-Jupiters", "url": "http://arxiv.org/pdf/1011.4156v1", "date": "2010-11-18 09:05:18", "abs": "Recently, we presented the detection of carbon monoxide in the transmission\nspectrum of extrasolar planet HD209458b, using CRIRES, the Cryogenic\nhigh-resolution Infrared Echelle Spectrograph at ESO's Very Large Telescope\n(VLT). The high spectral resolution observations (R=100,000) provide a wealth\nof information on the planet's orbit, mass, composition, and even on its\natmospheric dynamics. The new observational strategy and data analysis\ntechniques open up a whole world of opportunities. We therefore started an ESO\nlarge program using CRIRES to explore these, targeting both transiting and\nnon-transiting planets in carbon monoxide, water vapour, and methane.\nObservations of the latter molecule will also serve as a test-bed for METIS,\nthe proposed mid-infrared imager and spectrograph for the European Extremely\nLarge Telescope.", "cat": "astro-ph.EP", "authors": ["Ignas Snellen", "Remco de Kok", "Ernst de Mooij", "Matteo Brogi", "Bas Nefs", "Simon Albrecht"]}, "1084": {"id": "2211.07886v1", "title": "A Survey for Efficient Open Domain Question Answering", "url": "http://arxiv.org/pdf/2211.07886v1", "date": "2022-11-15 04:18:53", "abs": "Open domain question answering (ODQA) is a longstanding task aimed at\nanswering factual questions from a large knowledge corpus without any explicit\nevidence in natural language processing (NLP). Recent works have predominantly\nfocused on improving the answering accuracy and achieved promising progress.\nHowever, higher accuracy often comes with more memory consumption and inference\nlatency, which might not necessarily be efficient enough for direct deployment\nin the real world. Thus, a trade-off between accuracy, memory consumption and\nprocessing speed is pursued. In this paper, we provide a survey of recent\nadvances in the efficiency of ODQA models. We walk through the ODQA models and\nconclude the core techniques on efficiency. Quantitative analysis on memory\ncost, processing speed, accuracy and overall comparison are given. We hope that\nthis work would keep interested scholars informed of the advances and open\nchallenges in ODQA efficiency research, and thus contribute to the further\ndevelopment of ODQA efficiency.", "cat": "cs.CL", "authors": ["Qin Zhang", "Shangsi Chen", "Dongkuan Xu", "Qingqing Cao", "Xiaojun Chen", "Trevor Cohn", "Meng Fang"]}, "1085": {"id": "1512.03833v1", "title": "The XXL Survey III. Luminosity-temperature relation of the Bright Cluster Sample", "url": "http://arxiv.org/pdf/1512.03833v1", "date": "2015-12-11 21:31:51", "abs": "The XXL Survey is the largest homogeneous survey carried out with XMM-Newton.\nCovering an area of 50 deg$^{2}$, the survey contains several hundred galaxy\nclusters out to a redshift of $\\approx$2 above an X-ray flux limit of\n$\\sim$5$\\times10^{-15}$ erg cm$^{-2}$ s$^{-1}$. This paper belongs to the first\nseries of XXL papers focusing on the bright cluster sample. We investigate the\nluminosity-temperature (LT) relation for the brightest clusters detected in the\nXXL Survey, taking fully into account the selection biases. We investigate the\nform of the LT relation, placing constraints on its evolution. We have\nclassified the 100 brightest clusters in the XXL Survey based on their measured\nX-ray flux. These 100 clusters have been analysed to determine their luminosity\nand temperature to evaluate the LT relation. We used three methods to fit the\nLT relation, with two of these methods providing a prescription to fully take\ninto account the selection effects of the survey. We measure the evolution of\nthe LT relation internally using the broad redshift range of the sample. Taking\ninto account selection effects, we find a slope of the bolometric LT relation\nof B$_{\\rm LT}=3.08\\pm$0.15, steeper than the self-similar expectation (B$_{\\rm\nLT}$=2). Our best-fit result for the evolution factor is $E(z)^{1.64\\pm0.77}$,\nconsistent with \"strong self-similar\" evolution where clusters scale\nself-similarly with both mass and redshift. However, this result is marginally\nstronger than \"weak self-similar\" evolution, where clusters scale with redshift\nalone. We investigate the sensitivity of our results to the assumptions made in\nour model, finding that using an external LT relation as a low-z baseline can\nhave a profound effect on the measured evolution. However, more clusters are\nneeded to break the degeneracy between the choice of likelihood model and\nmass-temperature relation on the derived evolution.", "cat": "astro-ph.CO", "authors": ["P. A. Giles", "B. J. Maughan", "F. Pacaud", "M. Lieu", "N. Clerc", "M. Pierre", "C. Adami", "L. Chiappetti", "J. D\u00e9mocl\u00e9s", "S. Ettori", "J. P. Le F\u00e9vre", "T. Ponman", "T. Sadibekova", "G. P. Smith", "J. P. Willis", "F. Ziparo"]}, "1086": {"id": "0806.4019v1", "title": "Probing the Large-Scale Structure Around the Most Distant Galaxy Clusters from the Massive Cluster Survey", "url": "http://arxiv.org/pdf/0806.4019v1", "date": "2008-06-25 03:35:05", "abs": "We present maps of the cosmic large-scale structure around the twelve most\ndistant galaxy clusters from the Massive Cluster Survey (MACS) as traced by the\nprojected surface density of galaxies on the cluster red sequence. Taken with\nthe Suprime-Cam wide-field camera on the Subaru telescope, the images used in\nthis study cover a 27x27 arcmin^2 area around each cluster, corresponding to 10\nx 10 Mpc^2 at the median redshift of z = 0.55 of our sample. We directly detect\nsatellite clusters and filaments extending over the full size of our imaging\ndata in the majority of the clusters studied, supporting the picture of mass\naccretion via infall along filaments suggested by numerical simulations of the\ngrowth of clusters and the evolution of large-scale structure. A comparison of\nthe galaxy distribution near the cluster cores with the X-ray surface\nbrightness as observed with Chandra reveals, in several cases, significant\noffsets between the gas and galaxy distribution, indicative of ongoing merger\nevents. The respective systems are ideally suited for studies of the dynamical\nproperties of gas, galaxies, and dark matter. In addition, the large-scale\nfilaments viewed at high contrast in these MACS clusters are prime targets for\nthe direct detection and study of the warm-hot intergalactic medium (WHIM).", "cat": "astro-ph", "authors": ["Jeyhan S. Kartaltepe", "Harald Ebeling", "C. J. Ma", "David Donovan"]}, "1087": {"id": "1207.0972v1", "title": "The slowly evolving role of environment in a spectroscopic survey of star formation in Mstar > 5E8 Msun galaxies since z=1", "url": "http://arxiv.org/pdf/1207.0972v1", "date": "2012-07-04 13:25:31", "abs": "We present a deep [OII] emission line survey of faint galaxies (22.5 +0.1 dex) in the sample, and in particular in the\nSolar neighbourhood. We find that RAVE is rich in super-solar metallicity\nstars, and that the local metallicity distribution function declines remarkably\nslowly up to +0.4 dex. Our results show that the kinematics and height\ndistributions of the super-solar metallicity stars are identical to those of\nthe [M/H] < 0 thin-disc giants that we presume were locally manufactured. The\neccentricities of the super-solar metallicity stars indicate that half of them\nare on a roughly circular orbit (e < 0.15), so under the assumption that the\nmetallicity of the interstellar medium at a given radius never decreases with\ntime, they must have increased their angular momenta by scattering at\ncorotation resonances of spiral arms from regions far inside the Solar annulus.\nThe likelihood that a star will migrate radially does not seem to decrease\nsignificantly with increasing amplitude of vertical oscillations within range\nof oscillation amplitudes encountered in the disc.", "cat": "astro-ph.GA", "authors": ["G. Kordopatis", "J. Binney", "G. Gilmore", "R. F. G. Wyse", "V. Belokurov", "P. J. McMillan", "P. Hatfield", "E. K. Grebel", "M. Steinmetz", "J. F. Navarro", "G. Seabroke", "I. Minchev", "C. Chiappini", "O. Bienayme", "J. Bland-Hawthorn", "K. C. Freeman", "B. K. Gibson", "A. Helmi", "U. Munari", "Q. Parker", "W. A. Reid", "A. Siebert", "A. Siviero", "T. Zwitter"]}, "1094": {"id": "2305.07153v1", "title": "Towards best practices in AGI safety and governance: A survey of expert opinion", "url": "http://arxiv.org/pdf/2305.07153v1", "date": "2023-05-11 21:54:30", "abs": "A number of leading AI companies, including OpenAI, Google DeepMind, and\nAnthropic, have the stated goal of building artificial general intelligence\n(AGI) - AI systems that achieve or exceed human performance across a wide range\nof cognitive tasks. In pursuing this goal, they may develop and deploy AI\nsystems that pose particularly significant risks. While they have already taken\nsome measures to mitigate these risks, best practices have not yet emerged. To\nsupport the identification of best practices, we sent a survey to 92 leading\nexperts from AGI labs, academia, and civil society and received 51 responses.\nParticipants were asked how much they agreed with 50 statements about what AGI\nlabs should do. Our main finding is that participants, on average, agreed with\nall of them. Many statements received extremely high levels of agreement. For\nexample, 98% of respondents somewhat or strongly agreed that AGI labs should\nconduct pre-deployment risk assessments, dangerous capabilities evaluations,\nthird-party model audits, safety restrictions on model usage, and red teaming.\nUltimately, our list of statements may serve as a helpful foundation for\nefforts to develop best practices, standards, and regulations for AGI labs.", "cat": "cs.CY", "authors": ["Jonas Schuett", "Noemi Dreksler", "Markus Anderljung", "David McCaffary", "Lennart Heim", "Emma Bluemke", "Ben Garfinkel"]}, "1095": {"id": "2203.14727v1", "title": "Deep ASKAP EMU Survey of the GAMA23 field: Properties of radio sources", "url": "http://arxiv.org/pdf/2203.14727v1", "date": "2022-03-28 13:18:24", "abs": "We present the Australian Square Kilometre Array Pathfinder (ASKAP)\nobservations of the Galaxy and Mass Assembly (GAMA)-23h field. The survey was\ncarried out at 887.5 MHz and covers a 83 square degree field. We imaged the\ncalibrated visibility data, taken as part of the Evolutionary Mapping of\nUniverse (EMU) Early Science Programme, using the latest version of the\nASKAPSoft pipeline. The final mosaic has an angular resolution of 10 arcsec and\na central rms noise of around 38 $\\mu$Jy beam$^{-1}$. The derived radio source\ncatalogue has 39812 entries above a peak flux density threshold of 5$\\sigma$.\nWe searched for the radio source host galaxy counterparts using the GAMA\nspectroscopic (with an i-band magnitude limit of 19.2 mag) and multi-wavelength\ncatalogues that are available as part of the collaboration. We identified hosts\nwith GAMA spectroscopic redshifts for 5934 radio sources. We describe the data\nreduction, imaging, and source identification process, and present the source\ncounts. Thanks to the wide area covered by our survey, we obtain very robust\ncounts down to 0.2 mJy. ASKAP's exceptional survey speed, providing efficient,\nsensitive and high resolution mapping of large regions of the sky in\nconjunction with the multi-wavelength data available for the GAMA23 field,\nallowed us to discover 63 giant radio galaxies. The data presented here\ndemonstrate the excellent capabilities of ASKAP in the pre-SKA era.", "cat": "astro-ph.GA", "authors": ["G\u00fclay G\u00fcrkan", "I. Prandoni", "A. O'Brien", "W. Raja", "L. Marchetti", "M. Vaccari", "S. Driver", "E. Taylor", "T. Franzen", "M. J. I. Brown", "S. Shabala", "H. Andernach", "A. M. Hopkins", "R. P. Norris", "D. Leahy", "M. Bilicki", "H. Farajollahi", "T. Galvin", "G. Heald", "B. S. Koribalski", "T. An", "K. Warhurst"]}, "1096": {"id": "0907.4046v2", "title": "Motives: an introductory survey for physicists", "url": "http://arxiv.org/pdf/0907.4046v2", "date": "2009-10-01 08:35:41", "abs": "We survey certain accessible aspects of Grothendieck's theory of motives in\narithmetic algebraic geometry for mathematical physicists, focussing on areas\nthat have recently found applications in quantum field theory. An appendix (by\nMatilde Marcolli) sketches further connections between motivic theory and\ntheoretical physics.", "cat": "hep-th", "authors": ["Abhijnan Rej", "Matilde Marcolli"]}, "1097": {"id": "1509.06376v2", "title": "Detecting Effects of Filaments on Galaxy Properties in the Sloan Digital Sky Survey III", "url": "http://arxiv.org/pdf/1509.06376v2", "date": "2017-01-12 23:04:11", "abs": "We study the effects of filaments on galaxy properties in the Sloan Digital\nSky Survey (SDSS) Data Release 12 using filaments from the `Cosmic Web\nReconstruction' catalogue (Chen et al. 2016), a publicly available filament\ncatalogue for SDSS. Since filaments are tracers of medium-to-high density\nregions, we expect that galaxy properties associated with the environment are\ndependent on the distance to the nearest filament. Our analysis demonstrates\nthat a red galaxy or a high-mass galaxy tend to reside closer to filaments than\na blue or low-mass galaxy. After adjusting the effect from stellar mass, on\naverage, early-forming galaxies or large galaxies have a shorter distance to\nfilaments than late-forming galaxies or small galaxies. For the Main galaxy\nsample (MGS), all signals are very significant ($>6\\sigma$). For the LOWZ and\nCMASS sample, the stellar mass and size are significant ($>2 \\sigma$). The\nfilament effects we observe persist until $z = 0.7$ (the edge of the CMASS\nsample). Comparing our results to those using the galaxy distances from\nredMaPPer galaxy clusters as a reference, we find a similar result between\nfilaments and clusters. Moreover, we find that the effect of clusters on the\nstellar mass of nearby galaxies depends on the galaxy's filamentary\nenvironment. Our findings illustrate the strong correlation of galaxy\nproperties with proximity to density ridges, strongly supporting the claim that\ndensity ridges are good tracers of filaments.", "cat": "astro-ph.GA", "authors": ["Yen-Chi Chen", "Shirley Ho", "Rachel Mandelbaum", "Neta A. Bahcall", "Joel R. Brownstein", "Peter E. Freeman", "Christopher R. Genovese", "Donald P. Schneider", "Larry Wasserman"]}, "1098": {"id": "2303.06143v2", "title": "Cosmological measurements from void-galaxy and galaxy-galaxy clustering in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/2303.06143v2", "date": "2023-07-29 15:59:43", "abs": "We present the cosmological implications of measurements of void-galaxy and\ngalaxy-galaxy clustering from the Sloan Digital Sky Survey (SDSS) Main Galaxy\nSample (MGS), Baryon Oscillation Spectroscopic Survey (BOSS), and extended BOSS\n(eBOSS) luminous red galaxy catalogues from SDSS Data Release 7, 12, and 16,\ncovering the redshift range $0.07 < z < 1.0$. We fit a standard $\\Lambda$CDM\ncosmological model as well as various extensions including a constant dark\nenergy equation of state not equal to $-1$, a time-varying dark energy equation\nof state, and these same models allowing for spatial curvature. Results on key\nparameters of these models are reported for void-galaxy and galaxy-galaxy\nclustering alone, both of these combined, and all these combined with\nmeasurements from the cosmic microwave background (CMB) and supernovae (SN).\nFor the combination of void-galaxy and galaxy-galaxy clustering, we find tight\nconstraints of $\\Omega_\\mathrm{m} = 0.356\\pm 0.024$ for a base $\\Lambda$CDM\ncosmology, $\\Omega_\\mathrm{m} = 0.391^{+0.028}_{-0.021}, w =\n-1.50^{+0.43}_{-0.28}$ additionally allowing the dark energy equation of state\n$w$ to vary, and $\\Omega_\\mathrm{m} = 0.331^{+0.067}_{-0.094},\nw=-1.41^{+0.70}_{-0.31},\\ \\mathrm{and}\\ \\Omega_\\mathrm{k} =\n0.06^{+0.18}_{-0.13}$ further extending to non-flat models. The combined SDSS\nresults from void-galaxy and galaxy-galaxy clustering in combination with\nCMB+SN provide a 30% improvement in parameter $\\Omega_\\mathrm{m}$ over CMB+SN\nfor $\\Lambda$CDM, a 5% improvement in parameter $\\Omega_\\mathrm{m}$ when $w$ is\nallowed to vary, and a 32% and 68% improvement in parameters\n$\\Omega_\\mathrm{m}$ and $\\Omega_\\mathrm{k}$ when allowing for spatial\ncurvature.", "cat": "astro-ph.CO", "authors": ["Alex Woodfinden", "Will J. Percival", "Seshadri Nadathur", "Hans A. Winther", "T. S. Fraser", "Elena Massara", "Enrique Paillas", "Sla\u0111ana Radinovi\u0107"]}, "1099": {"id": "1812.00022v1", "title": "Sub-national levels and trends in contraceptive prevalence, unmet need, and demand for family planning in Nigeria with survey uncertainty", "url": "http://arxiv.org/pdf/1812.00022v1", "date": "2018-11-30 19:06:42", "abs": "Ambitious global goals have been established to provide universal access to\naffordable modern contraceptive methods. The UN's sustainable development goal\n3.7.1 proposes satisfying the demand for family planning (FP) services by\nincreasing the proportion of women of reproductive age using modern methods. To\nmeasure progress toward such goals in populous countries like Nigeria, it's\nessential to characterize the current levels and trends of FP indicators such\nas unmet need and modern contraceptive prevalence rates (mCPR). Moreover, the\nsubstantial heterogeneity across Nigeria and scale of programmatic\nimplementation requires a sub-national resolution of these FP indicators.\nHowever, significant challenges face estimating FP indicators sub-nationally in\nNigeria. In this article, we develop a robust, data-driven model to utilize all\navailable surveys to estimate the levels and trends of FP indicators in\nNigerian states for all women and by age-parity demographic subgroups. We\nestimate that overall rates and trends of mCPR and unmet need have remained low\nin Nigeria: the average annual rate of change for mCPR by state is 0.5%\n(0.4%,0.6%) from 2012-2017. Unmet need by age-parity demographic groups varied\nsignificantly across Nigeria; parous women express much higher rates of unmet\nneed than nulliparous women. Our hierarchical Bayesian model incorporates data\nfrom a diverse set of survey instruments, accounts for survey uncertainty,\nleverages spatio-temporal smoothing, and produces probabilistic estimates with\nuncertainty intervals. Our flexible modeling framework directly informs\nprogrammatic decision-making by identifying age-parity-state subgroups with\nlarge rates of unmet need, highlights conflicting trends across survey\ninstruments, and holistically interprets direct survey estimates.", "cat": "stat.AP", "authors": ["Laina D. Mercer", "Fred Lu", "Joshua L. Proctor"]}, "1100": {"id": "1508.04199v1", "title": "The Optical Luminosity Function of Void Galaxies in the SDSS and ALFALFA Surveys", "url": "http://arxiv.org/pdf/1508.04199v1", "date": "2015-08-18 02:34:05", "abs": "We measure the r-band galaxy luminosity function (LF) across environments\nover the redshift range 0<$z$<0.107 using the SDSS. We divide our sample into\ngalaxies residing in large scale voids (void galaxies) and those residing in\ndenser regions (wall galaxies). The best fitting Schechter parameters for void\ngalaxies are: log$\\Phi^*$= -3.40$\\pm$0.03 log(Mpc$^{-3}$), $M^*$=\n-19.88$\\pm$0.05, and $\\alpha$=-1.20$\\pm$0.02. For wall galaxies, the best\nfitting parameters are: log$\\Phi^*$=-2.86$\\pm$0.02 log(Mpc$^{-3}$),\n$M^*$=-20.80$\\pm$0.03, and $\\alpha$=-1.16$\\pm$0.01. We find a shift in the\ncharacteristic magnitude, $M^*$, towards fainter magnitudes for void galaxies\nand find no significant difference between the faint-end slopes of the void and\nwall galaxy LFs. We investigate how low surface brightness selections effects\ncan affect the galaxy LF. To attempt to examine a sample of galaxies that is\nrelatively free of surface brightness selection effects, we compute the optical\ngalaxy LF of galaxies detected by the blind HI survey, ALFALFA. We find that\nthe global LF of the ALFALFA sample is not well fit by a Schechter function,\nbecause of the presence of a wide dip in the LF around $M_r$=-18 and an upturn\nat fainter magnitudes ($\\alpha$~-1.47). We compare the HI selected r-band LF to\nvarious LFs of optically selected populations to determine where the HI\nselected optical LF obtains its shape. We find that sample selection plays a\nlarge role in determining the shape of the LF.", "cat": "astro-ph.GA", "authors": ["Crystal M. Moorman", "Michael S. Vogeley", "Fiona Hoyle", "Danny C. Pan", "Martha P. Haynes", "Riccardo Giovanelli"]}, "1101": {"id": "1512.05784v1", "title": "A SCUBA-2 survey of FeLoBAL QSOs: Are FeLoBALs in a `transition phase' between ULIRGs and QSOs?", "url": "http://arxiv.org/pdf/1512.05784v1", "date": "2015-12-17 21:00:08", "abs": "It is thought that a class of broad absorption line (BAL) QSOs, characterised\nby Fe absorption features in their UV spectra (called `FeLoBALs'), could mark a\ntransition stage between the end of an obscured starburst event and a youthful\nQSO beginning to shed its dust cocoon, where Fe has been injected into the\ninterstellar medium by the starburst. To test this hypothesis we have\nundertaken deep SCUBA-2 850 $\\mu$m observations of a sample of 17 FeLoBAL QSOs\nwith 0.89 $\\leq$ z $\\leq$ 2.78 and -23.31 $\\leq$ M$_{B}$ $\\leq$-28.50 to\ndirectly detect an excess in the thermal emission of the dust which would probe\nenhanced star-formation activity. We find that FeLoBALs are not luminous\nsources in the submillimetre, none of them are individually detected at 850\n$\\mu$m, nor as a population through stacking ($F_{s}=1.14\\pm0.58$ mJy).\nStatistical and survival analyses reveal that FeLoBALs have sub-mm properties\nconsistent with BAL and non-BAL QSOs with matched redshifts and magnitudes. An\nSED fitting analysis shows that the FIR emission is dominated by AGN activity,\nand a starburst component is required only in 6/17 sources of our sample;\nmoreover the integrated total luminosity of 16/17 sources is\nL$\\geq$10$^{12}$L$_{\\odot}$, high enough to classify FeLoBALs as infrared\nluminous. In conclusion, we do not find any evidence in support of FeLoBAL QSOs\nbeing a transition population between a ULIRG and an unobscured QSO; in\nparticular, FeLoBALs are not characterized by a cold starburst which would\nsupport this hypothesis.", "cat": "astro-ph.GA", "authors": ["Giulio Violino", "Kristen E. K. Coppin", "Jason A. Stevens", "Duncan Farrah", "James E. Geach", "Dave M. Alexander", "Ryan Hickox", "Daniel J. B. Smith", "Julie L. Wardlow"]}, "1102": {"id": "2209.09088v2", "title": "The shape of dark matter haloes: results from weak lensing in the Ultraviolet Near-Infrared Optical Northern Survey (UNIONS)", "url": "http://arxiv.org/pdf/2209.09088v2", "date": "2023-05-19 20:53:30", "abs": "Cold dark matter haloes are expected to be triaxial, and so appear elliptical\nin projection. We use weak gravitational lensing from the Canada-France Imaging\nSurvey (CFIS) component of the Ultraviolet-Near Infrared Optical Northern\nSurvey (UNIONS) to measure the ellipticity of the dark matter haloes around\nLuminous Red Galaxies (LRGs) from the Sloan Digital Sky Survey Data Release 7\n(DR7) and from the CMASS and LOWZ samples of the Baryon Oscillation\nSpectroscopic Survey (BOSS), assuming their major axes are aligned with the\nstellar light. We find that DR7 LRGs with masses $M \\sim 2.7\\times10^{13}\n\\mathrm{M}_{\\odot}/h$ have halo ellipticities $e=0.46\\pm0.10$. Expressed as a\nfraction of the galaxy ellipticity, we find $f_h = 2.2\\pm0.6$. For BOSS LRGs,\nthe detection is of marginal significance: $e = 0.20\\pm0.10$ and\n$f_h=0.7\\pm0.7$. These results are in agreement with other measurements of halo\nellipticity from weak lensing and, taken together with previous results,\nsuggest an increase of halo ellipticity of $0.10\\pm0.06$ per decade in halo\nmass. This trend agrees with the predictions from hydrodynamical simulations,\nwhich find that at higher halo masses, not only do dark matter haloes become\nmore elliptical, but that the misalignment between major axis of the stellar\nlight in the central galaxy and that of the dark matter decreases.", "cat": "astro-ph.GA", "authors": ["Bailey Robison", "Michael J. Hudson", "Jean-Charles Cuillandre", "Thomas Erben", "S\u00e9bastien Fabbro", "Rapha\u00ebl Gavazzi", "Axel Guinot", "Stephen Gwyn", "Hendrik Hildebrandt", "Martin Kilbinger", "Alan McConnachie", "Lance Miller", "Isaac Spitzer", "Ludovic van Waerbeke"]}, "1103": {"id": "2006.13191v1", "title": "FUGIN hot core survey. I. Survey method and initial results for $l = 10^\\circ-20^\\circ$", "url": "http://arxiv.org/pdf/2006.13191v1", "date": "2020-06-23 17:45:07", "abs": "We have developed a method to make a spectral-line-based survey of hot cores,\nwhich represent an important stage of high-mass star formation, and applied the\nmethod to the data of the FUGIN (FOREST Unbiased Galactic plane Imaging survey\nwith the Nobeyama 45-m telescope) survey. First, we select hot core candidates\nby searching the FUGIN data for the weak hot core tracer lines (HNCO and\nCH$_3$CN) by stacking, and then we conduct follow-up pointed observations on\nthese candidates in C$^{34}$S, SO, OCS, HC$_3$N, HNCO, CH$_3$CN, and CH$_3$OH\n$J=2-1$ and $J=8-7$ lines to confirm and characterize them. We applied this\nmethod to the $l = 10^\\circ-20^\\circ$ portion of the FUGIN data and identified\n22 \"Hot Cores\" (compact sources with more than two significant detection of the\nhot core tracer lines, i.e., SO, OCS, HC$_3$N, HNCO, CH$_3$CN, or CH$_3$OH\n$J=8-7$ lines) and 14 \"Dense Clumps\" (sources with more than two significant\ndetection of C$^{34}$S, CH$_3$OH $J=2-1$, or the hot core tracer lines). The\nidentified Hot Cores are found associated with signposts of high-mass star\nformation such as ATLASGAL clumps, WISE HII regions, and Class II methanol\nmasers. For those associated with ATLASGAL clumps, their bolometric luminosity\nto clump mass ratios are consistent with the star formation stages centered at\nthe hot core phase. The catalog of FUGIN Hot Cores provides a useful starting\npoint for further statistical studies and detailed observations of high-mass\nstar forming regions.", "cat": "astro-ph.GA", "authors": ["Kazuki Sato", "Tetsuo Hasegawa", "Tomofumi Umemoto", "Hiro Saito", "Nario Kuno", "Masumichi Seta", "Seiichi Sakamoto"]}, "1104": {"id": "1006.0095v1", "title": "\"TNOs are cool\": A survey of the trans-neptunian region. II. The thermal lightcurve of (136108) Haumea", "url": "http://arxiv.org/pdf/1006.0095v1", "date": "2010-06-01 09:39:42", "abs": "Thermal emission from Kuiper Belt object (136108) Haumea was measured with\nHerschel-PACS at 100 and 160 micrometers for almost a full rotation period.\nObservations clearly indicate a 100-micrometer thermal lightcurve with an\namplitude of a factor of ~ 2, which is positively correlated with the optical\nlightcurve. This confirms that both are primarily due to shape effects. A\n160-micrometer lightcurve is marginally detected. Radiometric fits of the mean\nHerschel- and Spitzer- fluxes indicate an equivalent diameter D ~ 1300 km and a\ngeometric albedo p_v ~ 0.70-0.75. These values agree with inferences from the\noptical lightcurve, supporting the hydrostatic equilibrium hypothesis. The\nlarge amplitude of the 100-micrometer lightcurve suggests that the object has a\nhigh projected a/b axis ratio (~ 1.3) and a low thermal inertia as well as\npossible variable infrared beaming. This may point to fine regolith on the\nsurface, with a lunar-type photometric behavior. The quality of the thermal\ndata is not sufficient to clearly detect the effects of a surface dark spot.", "cat": "astro-ph.EP", "authors": ["E. Lellouch", "C. Kiss", "P. Santos-Sanz", "T. G. M\u00fcller", "S. Fornasier", "O. Groussin", "P. Lacerda", "J. L. Ortiz", "A. Thirouin", "A. Delsanti", "R. Duffard", "A. W. Harris", "F. Henry", "T. Lim", "R. Moreno", "M. Mommert", "M. Mueller", "S. Protopapa", "J. Stansberry", "D. Trilling", "E. Vilenius", "A. Barucci", "J. Crovisier", "A. Doressoundiram", "E. Dotto", "P. J. Guti\u00e9rrez", "O. Hainaut", "P. Hartogh", "D. Hestroffer", "J. Horner", "L. Jorda", "M. Kidger", "L. Lara", "M. Rengel", "B. Swinyard", "N. Thomas"]}, "1105": {"id": "2101.00443v1", "title": "Semantics for Robotic Mapping, Perception and Interaction: A Survey", "url": "http://arxiv.org/pdf/2101.00443v1", "date": "2021-01-02 12:34:39", "abs": "For robots to navigate and interact more richly with the world around them,\nthey will likely require a deeper understanding of the world in which they\noperate. In robotics and related research fields, the study of understanding is\noften referred to as semantics, which dictates what does the world \"mean\" to a\nrobot, and is strongly tied to the question of how to represent that meaning.\nWith humans and robots increasingly operating in the same world, the prospects\nof human-robot interaction also bring semantics and ontology of natural\nlanguage into the picture. Driven by need, as well as by enablers like\nincreasing availability of training data and computational resources, semantics\nis a rapidly growing research area in robotics. The field has received\nsignificant attention in the research literature to date, but most reviews and\nsurveys have focused on particular aspects of the topic: the technical research\nissues regarding its use in specific robotic topics like mapping or\nsegmentation, or its relevance to one particular application domain like\nautonomous driving. A new treatment is therefore required, and is also timely\nbecause so much relevant research has occurred since many of the key surveys\nwere published. This survey therefore provides an overarching snapshot of where\nsemantics in robotics stands today. We establish a taxonomy for semantics\nresearch in or relevant to robotics, split into four broad categories of\nactivity, in which semantics are extracted, used, or both. Within these broad\ncategories we survey dozens of major topics including fundamentals from the\ncomputer vision field and key robotics research areas utilizing semantics,\nincluding mapping, navigation and interaction with the world. The survey also\ncovers key practical considerations, including enablers like increased data\navailability and improved computational hardware, and major application areas\nwhere...", "cat": "cs.RO", "authors": ["Sourav Garg", "Niko S\u00fcnderhauf", "Feras Dayoub", "Douglas Morrison", "Akansel Cosgun", "Gustavo Carneiro", "Qi Wu", "Tat-Jun Chin", "Ian Reid", "Stephen Gould", "Peter Corke", "Michael Milford"]}, "1106": {"id": "1604.05321v2", "title": "Effect of observational holes in fractal analysis of galaxy survey masks", "url": "http://arxiv.org/pdf/1604.05321v2", "date": "2018-04-21 19:16:05", "abs": "Observations reveal that the Universe has a hierarchy of galaxy clustering\nwith transition to homogeneity on large scales according to the $\\Lambda$CDM\nmodel. On the other hand some observational estimates suggest a multifractal\nbehavior where galactic clustering is based on generalization of the\ncorrelation dimension. We study the influence of veto areas on fractal\nmeasurements in masks of galaxy surveys. We investigate if these holes can\nproduce fractal behaviors or modify the scale of cosmic homogeneity. From the\nfootprint of BOSS-DR12, we build a homogeneous sample following the radial\nselection function for 73,412 points limited to the redshift range\n$0.002 1.5$\\,{\\it dex}. A large number of works\ndedicated to search for and investigate this minority of the giant family, and\nthe amount of Li-rich giants has been largely expanded, especially in the era\nof big data. In this paper, we present a catalog of Li-rich giants found from\nthe Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) survey\nwith Li abundances derived from a template matching method developed for LAMOST\nlow-resolution spectra. The catalog contains $10,535$ Li-rich giants with Li\nabundances from $\\sim 1.5$\\,{\\it dex} to $\\sim 4.9$\\,{\\it dex}. We also confirm\nthat the ratio of Li-rich phenomenon among giant stars is about one percent, or\nfor a more expression, $1.29\\%$ from our statistically important sample. This\nis the largest Li-rich giant sample ever reported to date, which significantly\nexceeds amount of all the reported Li-rich giants combined. The catalog will\nhelp the community to better understand the Li-rich phenomenon in giant stars.", "cat": "astro-ph.SR", "authors": ["Qi Gao", "Jian-Rong Shi", "Hong-Liang Yan", "Chun-Qian Li", "Tian-Yi Chen", "Jing- Hua Zhang", "Shuai Liu", "Tai-Sheng Yan", "Xiao-Jin Xie", "Ming-Yi Ding", "Yong Zhang", "Yong-Hui Hou"]}, "1113": {"id": "2311.10469v2", "title": "The PAU Survey: a new constraint on galaxy formation models using the observed colour redshift relation", "url": "http://arxiv.org/pdf/2311.10469v2", "date": "2024-03-04 07:56:06", "abs": "We use the GALFORM semi-analytical galaxy formation model implemented in the\nPlanck Millennium N-body simulation to build a mock galaxy catalogue on an\nobserver's past lightcone. The mass resolution of this N-body simulation is\nalmost an order of magnitude better than in previous simulations used for this\npurpose, allowing us to probe fainter galaxies and hence build a more complete\nmock catalogue at low redshifts. The high time cadence of the simulation\noutputs allows us to make improved calculations of galaxy properties and\npositions in the mock. We test the predictions of the mock against the Physics\nof the Accelerating Universe Survey, a narrow band imaging survey with highly\naccurate and precise photometric redshifts, which probes the galaxy population\nover a lookback time of 8 billion years. We compare the model against the\nobserved number counts, redshift distribution and evolution of the observed\ncolours and find good agreement; these statistics avoid the need for\nmodel-dependent processing of the observations. The model produces red and blue\npopulations that have similar median colours to the observations. However, the\nbimodality of galaxy colours in the model is stronger than in the observations.\nThis bimodality is reduced on including a simple model for errors in the\nGALFORM photometry. We examine how the model predictions for the observed\ngalaxy colours change when perturbing key model parameters. This exercise shows\nthat the median colours and relative abundance of red and blue galaxies provide\nconstraints on the strength of the feedback driven by supernovae used in the\nmodel.", "cat": "astro-ph.GA", "authors": ["G. Manzoni", "C. M. Baugh", "P. Norberg", "L. Cabayol", "J. L. van den Busch", "A. Wittje", "D. Navarro-Girones", "M. Eriksen", "P. Fosalba", "J. Carretero", "F. J. Castander", "R. Casas", "J. De Vicente", "E. Fernandez", "J. Garcia-Bellido", "E. Gaztanaga", "J. C. Helly", "H. Hoekstra", "H. Hildebrandt", "E. J. Gonzalez", "S. Koonkor", "R. Miquel", "C. Padilla", "P. Renard", "E. Sanchez", "I. Sevilla-Noarbe", "M. Siudek", "J. Y. H. Soo", "P. Tallada-Crespi", "L. Tortorelli"]}, "1114": {"id": "2301.12778v3", "title": "Investigating Feature and Model Importance in Android Malware Detection: An Implemented Survey and Experimental Comparison of ML-Based Methods", "url": "http://arxiv.org/pdf/2301.12778v3", "date": "2024-08-26 07:19:33", "abs": "The popularity of Android means it is a common target for malware. Over the\nyears, various studies have found that machine learning models can effectively\ndiscriminate malware from benign applications. However, as the operating system\nevolves, so does malware, bringing into question the findings of these previous\nstudies, many of which report very high accuracies using small, outdated, and\noften imbalanced datasets. In this paper, we reimplement 18 representative past\nworks and reevaluate them using a balanced, relevant, and up-to-date dataset\ncomprising 124,000 applications. We also carry out new experiments designed to\nfill holes in existing knowledge, and use our findings to identify the most\neffective features and models to use for Android malware detection within a\ncontemporary environment. We show that high detection accuracies (up to 96.8%)\ncan be achieved using features extracted through static analysis alone,\nyielding a modest benefit (1%) from using far more expensive dynamic analysis.\nAPI calls and opcodes are the most productive static and TCP network traffic\nprovide the most predictive dynamic features. Random forests are generally the\nmost effective model, outperforming more complex deep learning approaches.\nWhilst directly combining static and dynamic features is generally ineffective,\nensembling models separately leads to performances comparable to the best\nmodels but using less brittle features.", "cat": "cs.LG", "authors": ["Ali Muzaffar", "Hani Ragab Hassen", "Hind Zantout", "Michael A Lones"]}, "1115": {"id": "2303.06255v2", "title": "BatAnalysis -- A Comprehensive Python Pipeline for Swift BAT Survey Analysis", "url": "http://arxiv.org/pdf/2303.06255v2", "date": "2023-06-28 13:23:48", "abs": "The Swift Burst Alert Telescope (BAT) is a coded aperture gamma-ray\ninstrument with a large field of view that primarily operates in survey mode\nwhen it is not triggering on transient events. The survey data consists of\neighty-channel detector plane histograms that accumulate photon counts over\ntime periods of at least 5 minutes. These histograms are processed on the\nground and are used to produce the survey dataset between $14$ and $195$ keV.\nSurvey data comprises $> 90\\%$ of all BAT data by volume and allows for the\ntracking of long term light curves and spectral properties of cataloged and\nuncataloged hard X-ray sources. Until now, the survey dataset has not been used\nto its full potential due to the complexity associated with its analysis and\nthe lack of easily usable pipelines. Here, we introduce the BatAnalysis python\npackage , a wrapper for HEASoftpy, which provides a modern, open-source\npipeline to process and analyze BAT survey data. BatAnalysis allows members of\nthe community to use BAT survey data in more advanced analyses of astrophysical\nsources including pulsars, pulsar wind nebula, active galactic nuclei, and\nother known/unknown transient events that may be detected in the hard X-ray\nband. We outline the steps taken by the python code and exemplify its\nusefulness and accuracy by analyzing survey data from the Crab Pulsar, NGC\n2992, and a previously uncataloged MAXI Transient. The BatAnalysis package\nallows for $\\sim$ 18 years of BAT survey to be used in a systematic way to\nstudy a large variety of astrophysical sources.", "cat": "astro-ph.HE", "authors": ["Tyler Parsotan", "Sibasish Laha", "David M. Palmer", "Amy Lien", "S. Bradley Cenko", "Hans Krimm", "Craig Markwardt"]}, "1116": {"id": "0906.2178v1", "title": "The Arecibo Legacy Fast ALFA Survey: IX. The Leo Region HI Catalog, Group Membership and the HI Mass Function for the Leo I Group", "url": "http://arxiv.org/pdf/0906.2178v1", "date": "2009-06-11 18:47:13", "abs": "We present the catalog of HI sources extracted from the ongoing Arecibo\nLegacy Fast ALFA (ALFALFA) extragalactic HI line survey, found within the sky\nregion bounded by 9h36m < RA < 11h36m and +08deg < DEC < +12deg. The HI catalog\npresented here for this 118-deg^2 region is combined with ones derived from\nsurrounding regions also covered by the ALFALFA survey to examine the large\nscale structure in the complex Leo region. Because of the combination of wide\nsky coverage and superior sensitivity, spatial and spectral resolution, the\nALFALFA HI catalog of the Leo region improves significantly on the numbers of\nlow HI mass sources as compared with those found in previous HI surveys. The HI\nmass function of the Leo I group presented here is dominated by low-mass\nobjects: 45 of the 65 Leo I members have M_HI < 10^8 Msun, yielding tight\nconstraints on the low-mass slope of the Leo I HI mass function. The best-fit\nslope is alpha < -1.41 + 0.2 - 0.1. A direct comparison between the ALFALFA HI\nline detections and an optical search of the Leo I region proves the advantage\nof the ALFALFA strategy in finding low mass, gas-rich dwarfs. These results\nsuggest the existence of a significant population of low surface brightness,\ngas-rich, yet still very low HI mass galaxies, and may reflect the same type of\nmorphological segregation as is seen in the Local Group. While the low mass end\nslope of the Leo I HI mass function is steeper than that determined for\nluminosity functions of the group, the slope still falls short of the values\npredicted by simulations of structure formation in the LCDM paradigm.", "cat": "astro-ph.CO", "authors": ["S. Stierwalt", "M. P. Haynes", "R. Giovanelli", "B. R. Kent", "A. M. Martin", "A. Saintonge", "I. D. Karachentsev", "V. E. Karachentseva"]}, "1117": {"id": "0704.1267v1", "title": "Text Line Segmentation of Historical Documents: a Survey", "url": "http://arxiv.org/pdf/0704.1267v1", "date": "2007-04-10 16:26:42", "abs": "There is a huge amount of historical documents in libraries and in various\nNational Archives that have not been exploited electronically. Although\nautomatic reading of complete pages remains, in most cases, a long-term\nobjective, tasks such as word spotting, text/image alignment, authentication\nand extraction of specific fields are in use today. For all these tasks, a\nmajor step is document segmentation into text lines. Because of the low quality\nand the complexity of these documents (background noise, artifacts due to\naging, interfering lines),automatic text line segmentation remains an open\nresearch field. The objective of this paper is to present a survey of existing\nmethods, developed during the last decade, and dedicated to documents of\nhistorical interest.", "cat": "cs.CV", "authors": ["Laurence Likforman-Sulem", "Abderrazak Zahour", "Bruno Taconet"]}, "1118": {"id": "2403.15291v1", "title": "Wastewater-based Epidemiology for COVID-19 Surveillance: A Survey", "url": "http://arxiv.org/pdf/2403.15291v1", "date": "2024-03-22 15:40:05", "abs": "The pandemic of COVID-19 has imposed tremendous pressure on public health\nsystems and social economic ecosystems over the past years. To alleviate its\nsocial impact, it is important to proactively track the prevalence of COVID-19\nwithin communities. The traditional way to estimate the disease prevalence is\nto estimate from reported clinical test data or surveys. However, the coverage\nof clinical tests is often limited and the tests can be labor-intensive,\nrequires reliable and timely results, and consistent diagnostic and reporting\ncriteria. Recent studies revealed that patients who are diagnosed with COVID-19\noften undergo fecal shedding of SARS-CoV-2 virus into wastewater, which makes\nwastewater-based epidemiology (WBE) for COVID-19 surveillance a promising\napproach to complement traditional clinical testing. In this paper, we survey\nthe existing literature regarding WBE for COVID-19 surveillance and summarize\nthe current advances in the area. Specifically, we have covered the key aspects\nof wastewater sampling, sample testing, and presented a comprehensive and\norganized summary of wastewater data analytical methods. Finally, we provide\nthe open challenges on current wastewater-based COVID-19 surveillance studies,\naiming to encourage new ideas to advance the development of effective\nwastewater-based surveillance systems for general infectious diseases.", "cat": "stat.AP", "authors": ["Chen Chen", "Gursharn Kaur", "Aniruddha Adiga", "Baltazar Espinoza", "Srinivasan Venkatramanan", "Andrew Warren", "Bryan Lewis", "Justin Crow", "Rekha Singh", "Alexandra Lorentz", "Denise Toney", "Madhav Marathe"]}, "1119": {"id": "1802.04043v2", "title": "The HIX galaxy survey II: HI kinematics of HI eXtreme galaxies", "url": "http://arxiv.org/pdf/1802.04043v2", "date": "2018-12-17 13:17:26", "abs": "By analysing a sample of galaxies selected from the HI Parkes All Sky Survey\n(HIPASS) to contain more than 2.5 times their expected HI content based on\ntheir optical properties, we investigate what drives these HI eXtreme (HIX)\ngalaxies to be so HI-rich. We model the HI kinematics with the Tilted Ring\nFitting Code TiRiFiC and compare the observed HIX galaxies to a control sample\nof galaxies from HIPASS as well as simulated galaxies built with the\nsemi-analytic model Dark Sage. We find that (1) HI discs in HIX galaxies are\nmore likely to be warped and more likely to host HI arms and tails than in the\ncontrol galaxies, (2) the average HI and average stellar column density of HIX\ngalaxies is comparable to the control sample, (3) HIX galaxies have higher HI\nand baryonic specific angular momenta than control galaxies, (4) most HIX\ngalaxies live in higher-spin haloes than most control galaxies. These results\nsuggest that HIX galaxies are HI-rich because they can support more HI against\ngravitational instability due to their high specific angular momentum. The\nmajority of the HIX galaxies inherits their high specific angular momentum from\ntheir halo. The HI content of HIX galaxies might be further increased by\ngas-rich minor mergers. This paper is based on data obtained with the Australia\nTelescope Compact Array (ATCA) through the large program C 2705.", "cat": "astro-ph.GA", "authors": ["K. A. Lutz", "V. A. Kilborn", "B. S. Koribalski", "B. Catinella", "G. I. G. J\u00f3zsa", "O. I. Wong", "A. R. H. Stevens", "D. Obreschkow", "H. D\u00e9nes"]}, "1120": {"id": "2107.02391v1", "title": "The GRAVITY Young Stellar Object Survey. VI. Mapping the variable inner disk of HD 163296 at sub-au scales", "url": "http://arxiv.org/pdf/2107.02391v1", "date": "2021-07-06 05:11:45", "abs": "Protoplanetary disks drive some of the formation process (e.g., accretion,\ngas dissipation, formation of structures, etc.) of stars and planets.\nUnderstanding such physical processes is one of the main astrophysical\nquestions. HD 163296 is an interesting young stellar object for which infrared\nand sub-millimeter observations have shown a prominent circumstellar disk with\ngaps plausibly created by forming planets. This study aims at characterizing\nthe morphology of the inner disk in HD 163296 with multi-epoch near-infrared\ninterferometric observations performed with GRAVITY at the Very Large Telescope\nInterferometer (VLTI). Our goal is to depict the K-band (lambda_0 ~ 2.2 um)\nstructure of the inner rim with milliarcsecond (sub-au) angular resolution. Our\ndata is complemented with archival PIONIER (H-band; lambda_0 ~ 1.65 um) data of\nthe source. We performed a Gradient Descent parametric model fitting to recover\nthe sub-au morphology of our source. Our analysis shows the existence of an\nasymmetry in the disk surrounding the central star of HD 163296. We confirm\nvariability of the disk structure in the inner ~2 mas (0.2 au). While\nvariability of the inner disk structure in this source has been suggested by\nprevious interferometric studies, this is the first time that it is confirmed\nin the H- and K-bands by using a complete analysis of the closure phases and\nsquared visibilities over several epochs. Because of the separation from the\nstar, position changes, and persistence of this asymmetric structure on\ntimescales of several years, we argue that it is a dusty feature (e.g., a\nvortex or dust clouds), probably, made by a mixing of sillicate and carbon dust\nand/or refractory grains, inhomogeneously distributed above the mid-plane of\nthe disk.", "cat": "astro-ph.SR", "authors": ["J. Sanchez-Bermudez", "A. Caratti o Garatti", "R. Garcia Lopez", "K. Perraut", "L. Labadie", "M. Benisty", "W. Brandner", "C. Dougados", "P. J. V. Garcia", "Th. Henning", "L. Klarmann", "A. Amorim", "M. Baub\u00f6ck", "J. P. Berger", "J. B. Le Bouquin", "P. Caselli", "Y. Cl\u00e9net", "V. Coud\u00e9 du Foresto", "P. T. de Zeeuw", "A. Drescher", "G. Duvert", "A. Eckart", "F. Eisenhauer", "M. Filho", "F. Gao", "E. Gendron", "R. Genzel", "S. Gillessen", "R. Grellmann", "G. Heissel", "M. Horrobin", "Z. Hubert", "A. Jim\u00e9nez-Rosales", "L. Jocou", "P. Kervella", "S. Lacour", "V. Lapeyr\u00e8re", "P. L\u00e9na", "T. Ott", "T. Paumard", "G. Perrin", "J. E. Pineda", "G. Rodr\u00edguez-Coira", "G. Rousset", "D. M. Segura-Cox", "J. Shangguan", "T. Shimizu", "J. Stadler", "O. Straub", "C. Straubmeier", "E. Sturm", "E. van Dishoeck", "F. Vincent", "S. D. von Fellenberg", "F. Widmann", "J. Woillez"]}, "1121": {"id": "1811.02111v2", "title": "UNIT project: Universe $N$-body simulations for the Investigation of Theoretical models from galaxy surveys", "url": "http://arxiv.org/pdf/1811.02111v2", "date": "2019-05-08 22:06:42", "abs": "We present the UNIT $N$-body cosmological simulations project, designed to\nprovide precise predictions for nonlinear statistics of the galaxy\ndistribution. We focus on characterizing statistics relevant to emission line\nand luminous red galaxies in the current and upcoming generation of galaxy\nsurveys. We use a suite of precise particle mesh simulations (FastPM) as well\nas with full $N$-body calculations with a mass resolution of $\\sim\n1.2\\times10^9\\,h^{-1}$M$_{\\odot}$ to investigate the recently suggested\ntechnique of Angulo & Pontzen 2016 to suppress the variance of cosmological\nsimulations We study redshift space distortions, cosmic voids, higher order\nstatistics from $z=2$ down to $z=0$. We find that both two- and three-point\nstatistics are unbiased. Over the scales of interest for baryon acoustic\noscillations and redshift-space distortions, we find that the variance is\ngreatly reduced in the two-point statistics and in the cross correlation\nbetween halos and cosmic voids, but is not reduced significantly for the\nthree-point statistics. We demonstrate that the accuracy of the two-point\ncorrelation function for a galaxy survey with effective volume of 20\n($h^{-1}$Gpc)$^3$ is improved by about a factor of 40, indicating that two\npairs of simulations with a volume of 1 ($h^{-1}$Gpc)$^3$ lead to the\nequivalent variance of $\\sim$150 such simulations. The $N$-body simulations\npresented here thus provide an effective survey volume of about seven times the\neffective survey volume of DESI or Euclid. The data from this project,\nincluding dark matter fields, halo catalogues, and their clustering statistics,\nare publicly available at http://www.unitsims.org.", "cat": "astro-ph.CO", "authors": ["Chia-Hsun Chuang", "Gustavo Yepes", "Francisco-Shu Kitaura", "Marcos Pellejero-Ibanez", "Sergio Rodriguez-Torres", "Yu Feng", "R. Benton Metcalf", "Risa H. Wechsler", "Cheng Zhao", "Chun-Hao To", "Shadab Alam", "Arka Banerjee", "Joseph DeRose", "Carlo Giocoli", "Alexander Knebe", "Guillermo Reyes"]}, "1122": {"id": "1503.04272v1", "title": "Surveys, Astrometric Follow-up & Population Statistics", "url": "http://arxiv.org/pdf/1503.04272v1", "date": "2015-03-14 05:24:10", "abs": "Asteroid surveys are the backbone of asteroid science, and with this in mind\nwe begin with a broad review of the impact of asteroid surveys on our field. We\nthen provide a brief history of asteroid discoveries so as to place\ncontemporary and future surveys in perspective. Surveys in the United States\nhave discovered the vast majority of the asteroids and this dominance has been\nconsolidated since the publication of Asteroids III. Our descriptions of the\nasteroid surveys that have been operational since that time are focussed upon\nthose that have contributed the vast majority of asteroid observations and\ndiscoveries. We also provide some insight into upcoming next-generation surveys\nthat are sure to alter our understanding of the small bodies in the inner solar\nsystem and provide evidence to untangle their complicated dynamical and\nphysical histories. The Minor Planet Center, the nerve center of the asteroid\ndiscovery effort, has improved its operations significantly in the past decade\nso that it can manage the increasing discovery rate, and ensure that it is\nwell-placed to handle the data rates expected in the next decade. We also\nconsider the difficulties associated with astrometric follow-up of newly\nidentified objects. It seems clear that both of these efforts must operate in\nnew modes in order to keep pace with expected discovery rates of\nnext-generation ground- and space-based surveys.", "cat": "astro-ph.EP", "authors": ["Robert Jedicke", "Mikael Granvik", "Marco Micheli", "Eileen Ryan", "Timothy Spahr", "Donald K. Yeomans"]}, "1123": {"id": "1602.01336v2", "title": "The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 additional O-type systems", "url": "http://arxiv.org/pdf/1602.01336v2", "date": "2016-02-08 16:50:09", "abs": "This is the third installment of GOSSS, a massive spectroscopic survey of\nGalactic O stars, based on new homogeneous, high signal-to-noise ratio, R~2500\ndigital observations selected from the Galactic O-Star Catalog (GOSC). In this\npaper we present 142 additional stellar systems with O stars from both\nhemispheres, bringing the total of O-type systems published within the project\nto 590. Among the new objects there are 20 new O stars. We also identify 11 new\ndouble-lined spectroscopic binaries (SB2s), of which 6 are of O+O type and 5 of\nO+B type, and an additional new tripled-lined spectroscopic binary (SB3) of\nO+O+B type. We also revise some of the previous GOSSS classifications, present\nsome egregious examples of stars erroneously classified as O-type in the past,\nintroduce the use of luminosity class IV at spectral types O4-O5.5, and adapt\nthe classification scheme to the work of Arias et al. (2016).", "cat": "astro-ph.SR", "authors": ["J. Ma\u00edz Apell\u00e1niz", "A. Sota", "J. I. Arias", "R. H. Barb\u00e1", "N. R. Walborn", "S. Sim\u00f3n-D\u00edaz", "I. Negueruela", "A. Marco", "J. R. S. Le\u00e3o", "A. Herrero", "R. C. Gamen", "E. J. Alfaro"]}, "1124": {"id": "2002.04377v2", "title": "The Sixth Data Release of the Radial Velocity Experiment (RAVE) -- I: Survey Description, Spectra and Radial Velocities", "url": "http://arxiv.org/pdf/2002.04377v2", "date": "2020-06-09 11:37:54", "abs": "The Radial Velocity Experiment (RAVE) is a magnitude-limited (9= 3.5. Counterpart identification using radio and near/mid-infrared data was\nperformed and one or more counterpart candidates were found for 59 SMGs.\nPhotometric redshifts based on optical to near-infrared images were evaluated\nfor 45 SMGs of these SMGs with Spitzer/IRAC data, and the median value is found\nto be z=2.4. By combining these estimation with estimates from the literature\nwe determined that 10 SMGs might lie within the large-scale structure at z=3.1.\nThe two-point angular cross-correlation function between LAEs and SMGs\nindicates that the positions of the SMGs are correlated with the z=3.1\nprotocluster. These results suggest that the SMGs were formed and evolved\nselectively in the high dense environment of the high redshift universe. This\npicture is consistent with the predictions of the standard model of\nhierarchical structure formation.", "cat": "astro-ph.CO", "authors": ["H. Umehata", "Y. Tamura", "K. Kohno", "B. Hatsukade", "K. S. Scott", "M. Kubo", "T. Yamada", "R. J. Ivison", "R. Cybulski", "I. Aretxaga", "J. Austermann", "D. H. Hughes", "H. Ezawa", "T. Hayashino", "S. Ikarashi", "D. Iono", "R. Kawabe", "Y. Matsuda", "H. Matsuo", "K. Nakanishi", "T. Oshima", "T. Perera", "T. Takata", "G. W. Wilson", "M. S. Yun"]}, "1130": {"id": "2306.05126v1", "title": "Mapping Brains with Language Models: A Survey", "url": "http://arxiv.org/pdf/2306.05126v1", "date": "2023-06-08 11:50:58", "abs": "Over the years, many researchers have seemingly made the same observation:\nBrain and language model activations exhibit some structural similarities,\nenabling linear partial mappings between features extracted from neural\nrecordings and computational language models. In an attempt to evaluate how\nmuch evidence has been accumulated for this observation, we survey over 30\nstudies spanning 10 datasets and 8 metrics. How much evidence has been\naccumulated, and what, if anything, is missing before we can draw conclusions?\nOur analysis of the evaluation methods used in the literature reveals that some\nof the metrics are less conservative. We also find that the accumulated\nevidence, for now, remains ambiguous, but correlations with model size and\nquality provide grounds for cautious optimism.", "cat": "cs.CL", "authors": ["Antonia Karamolegkou", "Mostafa Abdou", "Anders S\u00f8gaard"]}, "1131": {"id": "2306.15880v4", "title": "Towards Open Vocabulary Learning: A Survey", "url": "http://arxiv.org/pdf/2306.15880v4", "date": "2024-02-01 08:31:59", "abs": "In the field of visual scene understanding, deep neural networks have made\nimpressive advancements in various core tasks like segmentation, tracking, and\ndetection. However, most approaches operate on the close-set assumption,\nmeaning that the model can only identify pre-defined categories that are\npresent in the training set. Recently, open vocabulary settings were proposed\ndue to the rapid progress of vision language pre-training. These new approaches\nseek to locate and recognize categories beyond the annotated label space. The\nopen vocabulary approach is more general, practical, and effective compared to\nweakly supervised and zero-shot settings. This paper provides a thorough review\nof open vocabulary learning, summarizing and analyzing recent developments in\nthe field. In particular, we begin by comparing it to related concepts such as\nzero-shot learning, open-set recognition, and out-of-distribution detection.\nThen, we review several closely related tasks in the case of segmentation and\ndetection, including long-tail problems, few-shot, and zero-shot settings. For\nthe method survey, we first present the basic knowledge of detection and\nsegmentation in close-set as the preliminary knowledge. Next, we examine\nvarious scenarios in which open vocabulary learning is used, identifying common\ndesign elements and core ideas. Then, we compare the recent detection and\nsegmentation approaches in commonly used datasets and benchmarks. Finally, we\nconclude with insights, issues, and discussions regarding future research\ndirections. To our knowledge, this is the first comprehensive literature review\nof open vocabulary learning. We keep tracing related works at\nhttps://github.com/jianzongwu/Awesome-Open-Vocabulary.", "cat": "cs.CV", "authors": ["Jianzong Wu", "Xiangtai Li", "Shilin Xu", "Haobo Yuan", "Henghui Ding", "Yibo Yang", "Xia Li", "Jiangning Zhang", "Yunhai Tong", "Xudong Jiang", "Bernard Ghanem", "Dacheng Tao"]}, "1132": {"id": "1104.3554v2", "title": "Thermal Expansion in 3d-Metal Prussian Blue Analogs - A Survey Study", "url": "http://arxiv.org/pdf/1104.3554v2", "date": "2011-08-15 23:09:18", "abs": "We present a comprehensive study of the structural properties and the thermal\nexpansion behavior of 17 different Prussian Blue Analogs (PBAs) with\ncompositions MII3[(M')III(CN)6]2.nH2O and MII2[FeII(CN)6].nH2O, where MII = Mn,\nFe, Co, Ni, Cu and Zn, (M')III = Co, Fe and n is the number of water molecules,\nwhich range from 5 to 18 for these compounds. The PBAs were synthesized via\nstandard chemical precipitation methods, and temperature-dependent X-ray\ndiffraction studies were performed in the temperature range between -150oC (123\nK) and room-temperature. The vast majority of the studied PBAs were found to\ncrystallize in cubic structures of space groups, and . The temperature\ndependence of the lattice parameters was taken to compute an average\ncoefficient of linear thermal expansion in the studied temperature range. Of\nthe 17 compounds, 9 display negative values for the average coefficient of\nlinear thermal expansion, which can be as large as 39.7 x 10-6 K-1 for\nCo3[Co(CN)6]2.12H2O. All of the MII3[CoIII(CN)6]2.nH2O compounds show negative\nthermal expansion behavior, which correlates with the Irving-Williams series\nfor metal complex stability. The thermal expansion behavior for the PBAs of the\nMII3[FeIII(CN)6]2.nH2O family are found to switch between positive (for M = Mn,\nCo, Ni) and negative (M = Cu, Zn) behavior, depending on the choice of the\nmetal cation (M). On the other hand, all of the MII2[FeII(CN)6].nH2O compounds\nshow positive thermal expansion behavior.", "cat": "cond-mat.mtrl-sci", "authors": ["Sourav Adak", "Luke L. Daemen", "Monika Hartl", "Darrick Williams", "Jennifer Summerhill", "Heinz Nakotte"]}, "1133": {"id": "1202.6005v1", "title": "The Clustering Characteristics of HI-Selected Galaxies from the 40% ALFALFA Survey", "url": "http://arxiv.org/pdf/1202.6005v1", "date": "2012-02-27 17:29:04", "abs": "The 40% Arecibo Legacy Fast ALFA (ALFALFA) survey catalog (\\alpha.40) of\napproximately 10,150 HI-selected galaxies is used to analyze the clustering\nproperties of gas-rich galaxies. By employing the Landy-Szalay estimator and a\nfull covariance analysis for the two-point galaxy-galaxy correlation function,\nwe obtain the real-space correlation function and model it as a power law,\n\\xi(r) = (r/r_0)^(-\\gamma), on scales less than 10 h^{-1} Mpc. As the largest\nsample of blindly HI-selected galaxies to date, \\alpha.40 provides detailed\nunderstanding of the clustering of this population. We find \\gamma = 1.51 +/-\n0.09 and r_0 = 3.3 +0.3, -0.2 h^{-1} Mpc, reinforcing the understanding that\ngas-rich galaxies represent the most weakly clustered galaxy population known;\nwe also observe a departure from a pure power law shape at intermediate scales,\nas predicted in \\Lambda CDM halo occupation distribution models. Furthermore,\nwe measure the bias parameter for the \\alpha.40 galaxy sample and find that HI\ngalaxies are severely antibiased on small scales, but only weakly antibiased on\nlarge scales. The robust measurement of the correlation function for gas-rich\ngalaxies obtained via the \\alpha.40 sample constrains models of the\ndistribution of HI in simulated galaxies, and will be employed to better\nunderstand the role of gas in environmentally-dependent galaxy evolution.", "cat": "astro-ph.CO", "authors": ["Ann M. Martin", "Riccardo Giovanelli", "Martha P. Haynes", "Luigi Guzzo"]}, "1134": {"id": "0706.0914v2", "title": "Four quasars above redshift 6 discovered by the Canada-France High-z Quasar Survey", "url": "http://arxiv.org/pdf/0706.0914v2", "date": "2007-08-30 15:41:28", "abs": "The Canada-France High-z Quasar Survey (CFHQS) is an optical survey designed\nto locate quasars during the epoch of reionization. In this paper we present\nthe discovery of the first four CFHQS quasars at redshift greater than 6,\nincluding the most distant known quasar, CFHQS J2329-0301 at z=6.43. We\ndescribe the observational method used to identify the quasars and present\noptical, infrared, and millimeter photometry and optical and near-infrared\nspectroscopy. We investigate the dust properties of these quasars finding an\nunusual dust extinction curve for one quasar and a high far-infrared luminosity\ndue to dust emission for another. The mean millimeter continuum flux for CFHQS\nquasars is substantially lower than that for SDSS quasars at the same redshift,\nlikely due to a correlation with quasar UV luminosity. For two quasars with\nsufficiently high signal-to-noise optical spectra, we use the spectra to\ninvestigate the ionization state of hydrogen at z>5. For CFHQS J1509-1749 at\nz=6.12, we find significant evolution (beyond a simple extrapolation of lower\nredshift data) in the Gunn-Peterson optical depth at z>5.4. The line-of-sight\nto this quasar has one of the highest known optical depths at z~5.8. An\nanalysis of the sizes of the highly-ionized near-zones in the spectra of two\nquasars at z=6.12 and z=6.43 suggest the IGM surrounding these quasars was\nsubstantially ionized before these quasars turned on. Together, these\nobservations point towards an extended reionization process, but we caution\nthat cosmic variance is still a major limitation in z>6 quasar observations.", "cat": "astro-ph", "authors": ["Chris J. Willott", "Philippe Delorme", "Alain Omont", "Jacqueline Bergeron", "Xavier Delfosse", "Thierry Forveille", "Loic Albert", "Celine Reyle", "Gary J. Hill", "Michael Gully-Santiago", "Phillip Vinten", "David Crampton", "John B. Hutchings", "David Schade", "Luc Simard", "Marcin Sawicki", "Alexandre Beelen", "Pierre Cox"]}, "1135": {"id": "2201.09811v1", "title": "Imputing Missing Values in the Occupational Requirements Survey", "url": "http://arxiv.org/pdf/2201.09811v1", "date": "2022-01-24 17:21:45", "abs": "The U.S. Bureau of Labor Statistics allows public access to much of the data\nacquired through its Occupational Requirements Survey (ORS). This data can be\nused to draw inferences about the requirements of various jobs and job classes\nwithin the United States workforce. However, the dataset contains a multitude\nof missing observations and estimates, which somewhat limits its utility. Here,\nwe propose a method by which to impute these missing values that leverages many\nof the inherent features present in the survey data, such as known population\nlimit and correlations between occupations and tasks. An iterative regression\nfit, implemented with a recent version of XGBoost and executed across a set of\nsimulated values drawn from the distribution described by the known values and\ntheir standard deviations reported in the survey, is the approach used to\narrive at a distribution of predicted values for each missing estimate. This\nallows us to calculate a mean prediction and bound said estimate with a 95%\nconfidence interval. We discuss the use of our method and how the resulting\nimputations can be utilized to inform and pursue future areas of study stemming\nfrom the data collected in the ORS. Finally, we conclude with an outline of\nWIGEM, a generalized version of our weighted, iterative imputation algorithm\nthat could be applied to other contexts.", "cat": "stat.ME", "authors": ["Terry Leitch", "Debjani Saha"]}, "1136": {"id": "1203.6068v2", "title": "The High Time Resolution Universe Survey - V: Single-pulse energetics and modulation properties of 315 pulsars", "url": "http://arxiv.org/pdf/1203.6068v2", "date": "2012-04-04 15:58:13", "abs": "We report on the pulse-to-pulse energy distributions and phase-resolved\nmodulation properties for catalogued pulsars in the southern High Time\nResolution Universe intermediate-latitude survey. We selected the 315 pulsars\ndetected in a single-pulse search of this survey, allowing a large sample\nunbiased regarding any rotational parameters of neutron stars. We found that\nthe energy distribution of many pulsars is well-described by a log-normal\ndistribution, with few deviating from a small range in log-normal scale and\nlocation parameters. Some pulsars exhibited multiple energy states\ncorresponding to mode changes, and implying that some observed \"nulling\" may\nactually be a mode-change effect. PSRJ1900-2600 was found to emit weakly in its\npreviously-identified \"null\" state. We found evidence for another state-change\neffect in two pulsars, which show bimodality in their nulling time scales; that\nis, they switch between a continuous-emission state and a single-pulse-emitting\nstate. Large modulation occurs in many pulsars across the full integrated\nprofile, with increased sporadic bursts at leading and trailing sub-beam edges.\nSome of these high-energy outbursts may indicate the presence of \"giant pulse\"\nphenomena. We found no correlation with modulation and pulsar period, age, or\nother parameters. Finally, the deviation of integrated pulse energy from its\naverage value was generally quite small, despite the significant phase-resolved\nmodulation in some pulsars; we interpret this as tenuous evidence of energy\nregulation between distinct pulsar sub-beams.", "cat": "astro-ph.SR", "authors": ["S. Burke-Spolaor", "S. Johnston", "M. Bailes", "S. D. Bates", "N. D. R. Bhat", "M. Burgay", "D. J. Champion", "N. D'Amico", "M. J. Keith", "M. Kramer", "L. Levin", "S. Milia A. Possenti", "B. Stappers", "W. van Straten"]}, "1137": {"id": "2404.04657v2", "title": "Main-belt and Trojan Asteroid Phase Curves from the ATLAS Survey", "url": "http://arxiv.org/pdf/2404.04657v2", "date": "2024-07-10 14:03:44", "abs": "Sparse and serendipitous asteroid photometry obtained by wide field surveys\nsuch as the Asteroid Terrestrial-impact Last Alert System (\\ATLAS) is a\nvaluable resource for studying the properties of large numbers of small Solar\nSystem bodies. We have gathered a large database of \\ATLAS photometry in\nwideband optical cyan and orange filters, consisting of 9.6\\e{7} observations\nof 4.5\\e{5} main belt asteroids and Jupiter Trojans. We conduct a phase curve\nanalysis of these asteroids considering each apparition separately, allowing us\nto accurately reject outlying observations and to remove apparitions and\nasteroids not suitable for phase curve determination. We obtain a dataset of\nabsolute magnitudes and phase parameters for over 100,000 selected asteroids\nobserved by \\ATLAS, $\\sim66,000$ of which had sufficient measurements to derive\ncolours in the \\ATLAS filters. To demonstrate the power of our dataset we\nconsider the properties of the Nysa-Polana complex, for which the \\ATLAS\ncolours and phase parameters trace the S-like and C-like compositions amongst\nfamily members. We also compare the properties of the leading and trailing\ngroups of Jupiter Trojans, finding no significant differences in their phase\nparameters or colours as measured by \\ATLAS, supporting the consensus that\nthese groups were captured from a common source population during planetary\nmigration. Furthermore, we identify $\\sim9000$ asteroids that exhibit large\nshifts in derived absolute magnitude between apparitions, indicating that these\nobjects have both elongated shapes and spin axes with obliquity $\\sim 90$\ndegrees.", "cat": "astro-ph.EP", "authors": ["James E. Robinson", "Alan Fitzsimmons", "David R. Young", "Michele Bannister", "Larry Denneau", "Nicolas Erasmus", "Amanda Lawrence", "Robert J. Siverd", "John Tonry"]}, "1138": {"id": "1211.0323v1", "title": "A selection of hot subluminous stars in the GALEX survey II. Subdwarf atmospheric parameters", "url": "http://arxiv.org/pdf/1211.0323v1", "date": "2012-11-01 22:38:20", "abs": "We present an update of our low-resolution spectroscopic follow-up and model\natmosphere analysis of hot subdwarf stars from the Galaxy Evolution Explorer\n(GALEX) survey. Targets were selected on the basis of colour indices calculated\nfrom the GALEX GR6 N_UV, Guide Star Catalogue (GSC2.3.2) V and the Two Micron\nAll Sky Survey (2MASS) J and H photometry. High signal-to-noise ratio spectra\nwere obtained at the European Southern Observatory (ESO) and the Kitt Peak\nNational Observatory (KPNO) over the course of three years. Detailed H, He and\nCNO abundance analysis helped us improve our T_eff, log g and He abundance\ndetermination and to constrain CNO abundances. We processed 191 observations of\n180 targets and found 124 sdB and 42 sdO stars in this sample while some blue\nhorizontal branch stars were also found in this programme. With quantitative\nbinary decomposition of 29 composite spectra we investigated the incidence of\nA, F and G type companions. The incidence of late G and K type companions and\ntheir effects on subdwarf atmospheric parameters were also examined.", "cat": "astro-ph.SR", "authors": ["P\u00e9ter N\u00e9meth", "Ad\u00e9la Kawka", "St\u00e9phane Vennes"]}, "1139": {"id": "2312.09972v4", "title": "The Next Generation Deep Extragalactic Exploratory Public Near-Infrared Slitless Survey Epoch 1 (NGDEEP-NISS1): Extra-Galactic Star-formation and Active Galactic Nuclei at 0.5 < z < 3.6", "url": "http://arxiv.org/pdf/2312.09972v4", "date": "2024-04-20 12:42:07", "abs": "The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) survey\nprogram was designed specifically to include Near Infrared Slitless\nSpectroscopic observations (NGDEEP-NISS) to detect multiple emission lines in\nas many galaxies as possible and across a wide redshift range using the Near\nInfrared Imager and Slitless Spectrograph (NIRISS). We present early results\nobtained from the the first set of observations (Epoch 1, 50$\\%$ of the\nallocated orbits) of this program (NGDEEP-NISS1). Using a set of independently\ndeveloped calibration files designed to deal with a complex combination of\noverlapping spectra, multiple position angles, and multiple cross filters and\ngrisms, in conjunction with a robust and proven algorithm for quantifying\ncontamination from overlapping dispersed spectra, NGDEEP-NISS1 has achieved a\n3$\\sigma$ sensitivity limit of 2 $\\times$ 10$^{-18}$ erg/s/cm$^2$. We\ndemonstrate the power of deep wide field slitless spectroscopy (WFSS) to\ncharacterize the star-formation rates, and metallicity ([OIII]/H$\\beta$), and\ndust content, of galaxies at $1 2 Msun/yr was found by our\nphotometric search in 4.03 x 10^5 Mpc^3 in the SDF. This result disfavors low\nfeedback models for PopIII star clusters, and implies an upper-limit of the\nPopIII SFR density of SFRD_PopIII < 5 x 10^-6 Msun/yr/Mpc^3. This new selection\nmethod to search for PopIII-hosting galaxies should be useful in future\nnarrow-band surveys to achieve the first observational detection of\nPopIII-hosting galaxies at high redshifts.", "cat": "astro-ph", "authors": ["Tohru Nagao", "Shunji Sasaki", "Roberto Maiolino", "Celestine Grady", "Nobunari Kashikawa", "Chun Ly", "Matthew Malkan", "Kentaro Motohara", "Takashi Murayama", "Daniel Schaerer", "Yasuhiro Shioya", "Yoshiaki Taniguchi"]}, "1146": {"id": "1411.1288v1", "title": "The High Time Resolution Universe Survey - XI. Discovery of five recycled pulsars and the optical detectability of survey white dwarf companions", "url": "http://arxiv.org/pdf/1411.1288v1", "date": "2014-11-05 15:00:46", "abs": "We present the discovery of a further five recycled pulsar systems in the\nmid-Galactic latitude portion of the High Time Resolution Universe (HTRU)\nSurvey. The pulsars have rotational periods ranging from 2 ms to 66 ms, and\nfour are in binary systems with orbital periods between 10.8 hours and 9.0\ndays. Three of these binary systems are particularly interesting; PSR\nJ1227-6208 has a pulse period of 34.5 ms and the highest mass function of all\npulsars with near-circular orbits. The circular orbit suggests that the\ncompanion is not another neutron star, so future timing experiments may reveal\none of the heaviest white dwarfs ever found ($>$ 1.3 M$_\\odot$). Timing\nobservations of PSR J1431$-$4715 indicate that it is eclipsed by its companion\nwhich has a mass indicating it belongs to the redback class of eclipsing\nmillisecond pulsars. PSR J1653-2054 has a companion with a minimum mass of only\n$0.08$ M$_\\odot$, placing it among the class of pulsars with low-mass\ncompanions. Unlike the majority of such systems, however, no evidence of\neclipses is seen at 1.4 GHz.", "cat": "astro-ph.SR", "authors": ["S. D. Bates", "D. Thornton", "M. Bailes", "E. Barr", "C. G. Bassa", "N. D. R. Bhat", "M. Burgay", "S. Burke-Spolaor", "D. J. Champion", "C. M. L. Flynn", "A. Jameson", "S. Johnston", "M. J. Keith", "M. Kramer", "L. Levin", "A. Lyne", "S. Milia", "C. Ng", "E. Petroff", "A. Possenti", "B. W. Stappers", "W. van Straten", "C. Tiburzi"]}, "1147": {"id": "1903.08413v1", "title": "Simulation of Sky Surveys with the Flyeye Telescope", "url": "http://arxiv.org/pdf/1903.08413v1", "date": "2019-03-20 09:57:23", "abs": "ESA's Flyeye telescope is designed with a very large field of view (FoV) in\norder to scan the sky for unknown near-Earth Objects (NEOs). For typical\nexposure times of 40 s, the telescope is able to detect objects with a limiting\nmagnitude up to 21.5. The aim is to observe those NEOs that are going to hit\nthe Earth within a few weeks or days, in advance of impact. In order to\nestimate the detection rate of NEOs with the Flyeye telescope, a synthetic\npopulation of Earth threatening asteroids is created by means of the software\nNEOPOP. Then, the true anomalies and longitudes of the ascending node of these\nobjects are modified in order to generate about 2500 impactors. In the\nsimulations almost three impacts can be detected per year from NEOs down to 1 m\nusing only one Flyeye telescope. When operating two telescopes simultaneously,\none at Monte Mufara and one at La Silla, four detected impacts per year are\nexpected. Nonetheless, it is estimated that about 15.6% of the Earth impactors\nwill be very difficult to be detected using ground-based telescopes due to the\nfact that they are approaching us from the Sun.", "cat": "astro-ph.EP", "authors": ["Olga Ramirez Torralba", "R\u00fcdiger Jehn", "Detlef Koschny", "Michael Fr\u00fchauf", "Laura S. Jehn", "Alexander Praus"]}, "1148": {"id": "0909.2853v3", "title": "Evidence for a fast evolution of the UV luminosity function beyond redshift 6 from a deep HAWK-I survey of the GOODS-S field", "url": "http://arxiv.org/pdf/0909.2853v3", "date": "2009-11-16 10:06:25", "abs": "We perform a deep search for galaxies in the redshift range 6.51, Y-J<1.5 and Y-K<2. The other public data in the UBVRIJHK bands are used\nto reject possible low redshift interlopers. The output has been compared with\nextensive Monte Carlo simulations to quantify the observational effects of our\nselection criteria as well as the effects of photometric errors. We detect 7\nhigh quality candidates in the magnitude range Y=25.5-26.7. This interval\nsamples the critical range for M* at z>6 (M_1500 ~- 19.5 to -21.5). After\naccounting for the expected incompleteness, we rule out at a 99% confidence\nlevel a Luminosity Function constant from z=6 to z=7, even including the\neffects of cosmic variance. For galaxies brighter than M_1500=-19.0 we derive a\nluminosity density rho_UV=1.5^{+2.0}_{-0.9} 10^25 erg/s/Hz/Mpc3, implying a\ndecrease by a factor 3.5 from z=6 to z~6.8. On the basis of our findings, we\nmake predictions for the surface densities expected in future surveys surveys,\nbased on ULTRA-VISTA, HST-WFC3 or JWST-NIRCam, evaluating the best\nobservational strategy to maximise their impact.", "cat": "astro-ph.CO", "authors": ["M. Castellano", "A. Fontana", "K. Boutsia", "A. Grazian", "L. Pentericci", "R. Bouwens", "M. Dickinson", "M. Giavalisco", "P. Santini", "S. Cristiani", "F. Fiore", "S. Gallozzi", "E. Giallongo", "R. Maiolino", "F. Mannucci", "N. Menci", "A. Moorwood", "M. Nonino", "D. Paris", "A. Renzini", "P. Rosati", "S. Salimbeni", "V. Testa", "E. Vanzella"]}, "1149": {"id": "1803.08504v1", "title": "AGN mass estimates in large spectroscopic surveys: the effect of host galaxy light", "url": "http://arxiv.org/pdf/1803.08504v1", "date": "2018-03-22 18:00:00", "abs": "Virial-based methods for estimating active supermassive black hole masses are\nnow commonly used on extremely large spectroscopic quasar catalogues. Most\nspectral analyses, though, do not pay enough attention to a detailed continuum\ndecomposition. To understand how this affects virial mass estimate results, we\ntest the influence of host galaxy light on them, along with Balmer continuum\ncomponent. A detailed fit with the new spectroscopic analysis software QSFit\ndemonstrated that the presence or absence of continuum components do not affect\nsignificantly the virial-based results for our sample. Taking or not in\nconsideration a host galaxy component, instead, affects the emission line\nfitting in a more pronounced way at lower redshifts, where in fact we observe\ndimmer quasars and more visible host galaxies.", "cat": "astro-ph.GA", "authors": ["Ludovica Varisco", "Tullia Sbarrato", "Giorgio Calderone", "Massimo Dotti"]}, "1150": {"id": "2212.09334v1", "title": "HyGAL: Characterizing the Galactic ISM with observations of hydrides and other small molecules II. The absorption line survey with the IRAM 30 m telescope", "url": "http://arxiv.org/pdf/2212.09334v1", "date": "2022-12-19 10:00:54", "abs": "As a complement to the HyGAL Stratospheric Observatory for Infrared Astronomy\nLegacy Program, we report the results of a ground-based absorption line survey\nof simple molecules in diffuse and translucent Galactic clouds. Using the\nInstitut de Radioastronomie Millim\\'etrique (IRAM) 30 m telescope, we surveyed\nmolecular lines in the 2 mm and 3 mm wavelength ranges toward 15 millimeter\ncontinuum sources. These sources, which are all massive star-forming regions\nlocated mainly in the first and second quadrants of the Milky Way, form the\nsubset of the HyGAL sample that can be observed by the IRAM 30 m telescope. We\ndetected HCO$^+$ absorption lines toward 14 sightlines, toward which we\nidentified 78 foreground cloud components, as well as lines from HCN, HNC,\nC$_2$H, and c-C$_3$H$_2$ toward most sightlines. In addition, CS and H$_2$S\nabsorption lines are found toward at least half of the continuum sources.\nStatic Meudon photodissociation region (PDR) isobaric models that consider\nultraviolet-dominated chemistry were unable to reproduce the column densities\nof all seven molecular species by just a factor of a few, except for H$_2$S.\nThe inclusion of other formation routes driven by turbulent dissipation could\npossibly explain the observed high column densities of these species in diffuse\nclouds. There is a tentative trend for H$_2$S and CS abundances relative to\nH$_2$ to be larger in diffuse clouds ($X$(H$_2$S) and $X$(CS) $\\sim 10^{-8} -\n10^{-7}$) than in translucent clouds ($X$(H$_2$S) and $X$(CS) $\\sim 10^{-9} -\n10^{-8}$) toward a small sample; however, a larger sample is required in order\nto confirm this trend. The derived H$_2$S column densities are higher than the\nvalues predicted from the isobaric PDR models, suggesting that chemical\ndesorption of H$_2$S from sulfur-containing ice mantles may play a role in\nincreasing the H$_2$S abundance.", "cat": "astro-ph.GA", "authors": ["W. -J. Kim", "P. Schilke", "D. A. Neufeld", "A. M. Jacob", "\u00c1. S\u00e1nchez-Monge", "D. Seifried", "B. Godard", "K. M. Menten", "S. Walch", "E. Falgarone", "V. S. Veena", "S. Bialy", "T. M\u00f6ller", "F. Wyrowski"]}, "1151": {"id": "1312.6565v1", "title": "Mobile Multimedia Recommendation in Smart Communities: A Survey", "url": "http://arxiv.org/pdf/1312.6565v1", "date": "2013-12-23 15:01:35", "abs": "Due to the rapid growth of internet broadband access and proliferation of\nmodern mobile devices, various types of multimedia (e.g. text, images, audios\nand videos) have become ubiquitously available anytime. Mobile device users\nusually store and use multimedia contents based on their personal interests and\npreferences. Mobile device challenges such as storage limitation have however\nintroduced the problem of mobile multimedia overload to users. In order to\ntackle this problem, researchers have developed various techniques that\nrecommend multimedia for mobile users. In this survey paper, we examine the\nimportance of mobile multimedia recommendation systems from the perspective of\nthree smart communities, namely, mobile social learning, mobile event guide and\ncontext-aware services. A cautious analysis of existing research reveals that\nthe implementation of proactive, sensor-based and hybrid recommender systems\ncan improve mobile multimedia recommendations. Nevertheless, there are still\nchallenges and open issues such as the incorporation of context and social\nproperties, which need to be tackled in order to generate accurate and\ntrustworthy mobile multimedia recommendations.", "cat": "cs.IR", "authors": ["Feng Xia", "Nana Yaw Asabere", "Ahmedin Mohammed Ahmed", "Jing Li", "Xiangjie Kong"]}, "1152": {"id": "2204.04859v1", "title": "A Survey on Legal Judgment Prediction: Datasets, Metrics, Models and Challenges", "url": "http://arxiv.org/pdf/2204.04859v1", "date": "2022-04-11 04:06:28", "abs": "Legal judgment prediction (LJP) applies Natural Language Processing (NLP)\ntechniques to predict judgment results based on fact descriptions\nautomatically. Recently, large-scale public datasets and advances in NLP\nresearch have led to increasing interest in LJP. Despite a clear gap between\nmachine and human performance, impressive results have been achieved in various\nbenchmark datasets. In this paper, to address the current lack of comprehensive\nsurvey of existing LJP tasks, datasets, models and evaluations, (1) we analyze\n31 LJP datasets in 6 languages, present their construction process and define a\nclassification method of LJP with 3 different attributes; (2) we summarize 14\nevaluation metrics under four categories for different outputs of LJP tasks;\n(3) we review 12 legal-domain pretrained models in 3 languages and highlight 3\nmajor research directions for LJP; (4) we show the state-of-art results for 8\nrepresentative datasets from different court cases and discuss the open\nchallenges. This paper can provide up-to-date and comprehensive reviews to help\nreaders understand the status of LJP. We hope to facilitate both NLP\nresearchers and legal professionals for further joint efforts in this problem.", "cat": "cs.CL", "authors": ["Junyun Cui", "Xiaoyu Shen", "Feiping Nie", "Zheng Wang", "Jinglong Wang", "Yulong Chen"]}, "1153": {"id": "0801.1156v1", "title": "The dark matter environment of the Abell 901/902 supercluster: a weak lensing analysis of the HST STAGES survey", "url": "http://arxiv.org/pdf/0801.1156v1", "date": "2008-01-08 04:46:28", "abs": "We present a high resolution dark matter reconstruction of the z=0.165 Abell\n901/902 supercluster from a weak lensing analysis of the HST STAGES survey. We\ndetect the four main structures of the supercluster at high significance,\nresolving substructure within and between the clusters. We find that the\ndistribution of dark matter is well traced by the cluster galaxies, with the\nbrightest cluster galaxies marking out the strongest peaks in the dark matter\ndistribution. We also find a significant extension of the dark matter\ndistribution of Abell 901a in the direction of an infalling X-ray group Abell\n901alpha. We present mass, mass-to-light and mass-to-stellar mass ratio\nmeasurements of the structures and substructures that we detect. We find no\nevidence for variation of the mass-to-light and mass-to-stellar mass ratio\nbetween the different clusters. We compare our space-based lensing analysis\nwith an earlier ground-based lensing analysis of the supercluster to\ndemonstrate the importance of space-based imaging for future weak lensing dark\nmatter 'observations'.", "cat": "astro-ph", "authors": ["Catherine Heymans", "Meghan E. Gray", "Chien Y. Peng", "Ludovic Van Waerbeke", "Eric F. Bell", "Christian Wolf", "David Bacon", "Michael Balogh", "Fabio D. Barazza", "Marco Barden", "Asmus Boehm", "John A. R. Caldwell", "Boris Haeussler", "Knud Jahnke", "Shardha Jogee", "Eelco van Kampen", "Kyle Lane", "Daniel H. McIntosh", "Klaus Meisenheimer", "Yannick Mellier", "Sebastian F. Sanchez", "Andy N. Taylor", "Lutz Wisotzki", "Xianzhong Zheng"]}, "1154": {"id": "1506.00055v3", "title": "The Application of Autocorrelation SETI Search Techniques in an ATA Survey", "url": "http://arxiv.org/pdf/1506.00055v3", "date": "2018-09-14 01:17:45", "abs": "We report a novel radio autocorrelation (AC) search for extraterrestrial\nintelligence (SETI). For selected frequencies across the terrestrial microwave\nwindow (1-10 GHz) observations were conducted at the Allen Telescope Array to\nidentify artificial non-sinusoidal periodic signals with radio bandwidths\ngreater than 4 Hz, which are capable of carrying substantial messages with\nsymbol-rates from 4-1000000 Hz. Out of 243 observations, about half (101) were\ndirected toward sources with known continuum flux > ~1 Jy over the sampled\nbandwidth (quasars, pulsars, supernova remnants, and masers), based on the\nhypothesis that they might harbor heretofore undiscovered natural or\nartificial, repetitive, phase or frequency modulation. The rest of the targets\nwere mostly toward exoplanet stars with no previously discovered continuum\nflux. No signals attributable to extraterrestrial technology were found in this\nstudy. We conclude that the maximum probability that future observations like\nthe ones described here will reveal repetitively modulated emissions is less\nthan 1% for continuum sources and exoplanets, alike. The paper concludes by\ndescribing a new approach to expanding this survey to many more targets and\nmuch greater sensitivity using archived data from interferometers all over the\nworld.", "cat": "astro-ph.IM", "authors": ["G. R. Harp", "R. F. Ackermann", "Alfredo Astorga", "Jack Arbunich", "Kristin Hightower", "Seth Meitzner", "W. C. Barott", "Michael C. Nolan", "D. G. Messerschmitt", "Douglas A. Vakoch", "Seth Shostak", "J. C. Tarter"]}, "1155": {"id": "0811.3596v2", "title": "Physical Properties of Four SZE-Selected Galaxy Clusters in the Southern Cosmology Survey", "url": "http://arxiv.org/pdf/0811.3596v2", "date": "2009-02-06 05:51:22", "abs": "We present the optical and X-ray properties of four clusters recently\ndiscovered by the South Pole Telescope (SPT) using the Sunyaev-Zel'dovich\neffect (SZE). The four clusters are located in one of the common survey areas\nof the southern sky that is also being targeted by the Atacama Cosmology\nTelescope (ACT) and imaged by the CTIO Blanco 4-m telescope. Based on publicly\navailable griz optical images and XMM-Newton and ROSAT X-ray observations we\nanalyse the physical properties of these clusters and obtain photometric\nredshifts, luminosities, richness and mass estimates. Each cluster contains a\ncentral elliptical whose luminosity is consistent with SDSS cluster studies.\nOur mass estimates are well above the nominal detection limit of SPT and ACT;\nthe new SZE clusters are very likely massive systems with M>~5x10^14 M_sun.", "cat": "astro-ph", "authors": ["Felipe Menanteau", "John P. Hughes"]}, "1156": {"id": "2405.05562v2", "title": "Review-based Recommender Systems: A Survey of Approaches, Challenges and Future Perspectives", "url": "http://arxiv.org/pdf/2405.05562v2", "date": "2024-05-11 18:25:29", "abs": "Recommender systems play a pivotal role in helping users navigate an\noverwhelming selection of products and services. On online platforms, users\nhave the opportunity to share feedback in various modes, including numerical\nratings, textual reviews, and likes/dislikes. Traditional recommendation\nsystems rely on users explicit ratings or implicit interactions (e.g. likes,\nclicks, shares, saves) to learn user preferences and item characteristics.\nBeyond these numerical ratings, textual reviews provide insights into users\nfine-grained preferences and item features. Analyzing these reviews is crucial\nfor enhancing the performance and interpretability of personalized\nrecommendation results. In recent years, review-based recommender systems have\nemerged as a significant sub-field in this domain. In this paper, we provide a\ncomprehensive overview of the developments in review-based recommender systems\nover recent years, highlighting the importance of reviews in recommender\nsystems, as well as the challenges associated with extracting features from\nreviews and integrating them into ratings. Specifically, we present a\ncategorization of these systems and summarize the state-of-the-art methods,\nanalyzing their unique features, effectiveness, and limitations. Finally, we\npropose potential directions for future research, including the integration of\nmultimodal data, multi-criteria rating information, and ethical considerations.", "cat": "cs.IR", "authors": ["Emrul Hasan", "Mizanur Rahman", "Chen Ding", "Jimmy Xiangji Huang", "Shaina Raza"]}, "1157": {"id": "2107.02126v6", "title": "A Survey on Deep Learning Event Extraction: Approaches and Applications", "url": "http://arxiv.org/pdf/2107.02126v6", "date": "2022-11-15 14:45:20", "abs": "Event extraction (EE) is a crucial research task for promptly apprehending\nevent information from massive textual data. With the rapid development of deep\nlearning, EE based on deep learning technology has become a research hotspot.\nNumerous methods, datasets, and evaluation metrics have been proposed in the\nliterature, raising the need for a comprehensive and updated survey. This\narticle fills the research gap by reviewing the state-of-the-art approaches,\nespecially focusing on the general domain EE based on deep learning models. We\nintroduce a new literature classification of current general domain EE research\naccording to the task definition. Afterward, we summarize the paradigm and\nmodels of EE approaches, and then discuss each of them in detail. As an\nimportant aspect, we summarize the benchmarks that support tests of predictions\nand evaluation metrics. A comprehensive comparison among different approaches\nis also provided in this survey. Finally, we conclude by summarizing future\nresearch directions facing the research area.", "cat": "cs.CL", "authors": ["Qian Li", "Jianxin Li", "Jiawei Sheng", "Shiyao Cui", "Jia Wu", "Yiming Hei", "Hao Peng", "Shu Guo", "Lihong Wang", "Amin Beheshti", "Philip S. Yu"]}, "1158": {"id": "1903.08813v2", "title": "Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters", "url": "http://arxiv.org/pdf/1903.08813v2", "date": "2019-11-18 22:36:26", "abs": "We introduce a galaxy cluster mass observable, $\\mu_\\star$, based on the\nstellar masses of cluster members, and we present results for the Dark Energy\nSurvey (DES) Year 1 observations. Stellar masses are computed using a Bayesian\nModel Averaging method, and are validated for DES data using simulations and\nCOSMOS data. We show that $\\mu_\\star$ works as a promising mass proxy by\ncomparing our predictions to X-ray measurements. We measure the X-ray\ntemperature-$\\mu_\\star$ relation for a total of 150 clusters matched between\nthe wide-field DES Year 1 redMaPPer catalogue, and Chandra and XMM archival\nobservations, spanning the redshift range $0.1=3, over\n0.6 square degrees of the UKIRT Infrared Deep Survey (UKIDSS) Ultra Deep Survey\n(UDS). Using photometry from the U band through 4.5 microns, we have obtained\nphotometric redshifts and derived stellar masses for our sources. Only two of\nour galaxies potentially lie at z>5. We have studied the galaxy stellar mass\nfunction at 3<=z<5, based on the 1213 galaxies in our catalogue with [4.5]<=\n24.0. We find that: i) the number density of M > 10^11 Msun galaxies increased\nby a factor > 10 between z=5 and 3, indicating that the assembly rate of these\ngalaxies proceeded > 20 times faster at these redshifts than at 0 10^11 Msun galaxies would be missed by optical\nsurveys with R<27 or z<26. Thus, our study demonstrates the importance of deep\nmid-IR surveys over large areas to perform a complete census of massive\ngalaxies at high z and trace the early stages of massive galaxy assembly.", "cat": "astro-ph.CO", "authors": ["K. I. Caputi", "M. Cirasuolo", "J. S. Dunlop", "R. J. McLure", "D. Farrah", "O. Almaini"]}, "1167": {"id": "1907.07684v1", "title": "Mapping the Stellar Halo with the H3 Spectroscopic Survey", "url": "http://arxiv.org/pdf/1907.07684v1", "date": "2019-07-17 18:00:00", "abs": "Modern theories of galaxy formation predict that the Galactic stellar halo\nwas hierarchically assembled from the accretion and disruption of smaller\nsystems. This hierarchical assembly is expected to produce a high degree of\nstructure in the combined phase and chemistry space; this structure should\nprovide a relatively direct probe of the accretion history of our Galaxy.\nRevealing this structure requires precise 3D positions (including distances),\n3D velocities, and chemistry for large samples of stars. The Gaia satellite is\ndelivering proper motions and parallaxes for >1 billion stars to G~20. However,\nradial velocities and metallicities will only be available to G~15, which is\ninsufficient to probe the outer stellar halo (>10 kpc). Moreover, parallaxes\nwill not be precise enough to deliver high-quality distances for stars beyond\n~10 kpc. Identifying accreted systems throughout the stellar halo therefore\nrequires a large ground-based spectroscopic survey to complement Gaia. Here we\nprovide an overview of the H3 Stellar Spectroscopic Survey, which will deliver\nprecise stellar parameters and spectrophotometric distances for 200,000 stars\nto r=18. Spectra are obtained with the Hectochelle instrument at the MMT, which\nis configured for the H3 Survey to deliver resolution R~23,000 spectra covering\nthe wavelength range 5150A-5300A. The survey is optimized for stellar halo\nscience and therefore focuses on high Galactic latitude fields (|b|>30 deg.),\nsparsely sampling 15,000 sq. degrees. Targets are selected on the basis of Gaia\nparallaxes, enabling very efficient selection of bone fide halo stars. The\nsurvey began in the Fall of 2017 and has collected 88,000 spectra to-date. All\nof the data, including the derived stellar parameters, will eventually be made\npublicly available via the survey website: h3survey.rc.fas.harvard.edu.", "cat": "astro-ph.GA", "authors": ["Charlie Conroy", "Ana Bonaca", "Phillip Cargile", "Benjamin D. Johnson", "Nelson Caldwell", "Rohan P. Naidu", "Dennis Zaritsky", "Daniel Fabricant", "Sean Moran", "Jaehyon Rhee", "Andrew Szentgyorgyi"]}, "1168": {"id": "2306.16021v3", "title": "Structure in Deep Reinforcement Learning: A Survey and Open Problems", "url": "http://arxiv.org/pdf/2306.16021v3", "date": "2024-04-25 14:40:51", "abs": "Reinforcement Learning (RL), bolstered by the expressive capabilities of Deep\nNeural Networks (DNNs) for function approximation, has demonstrated\nconsiderable success in numerous applications. However, its practicality in\naddressing various real-world scenarios, characterized by diverse and\nunpredictable dynamics, noisy signals, and large state and action spaces,\nremains limited. This limitation stems from poor data efficiency, limited\ngeneralization capabilities, a lack of safety guarantees, and the absence of\ninterpretability, among other factors. To overcome these challenges and improve\nperformance across these crucial metrics, one promising avenue is to\nincorporate additional structural information about the problem into the RL\nlearning process. Various sub-fields of RL have proposed methods for\nincorporating such inductive biases. We amalgamate these diverse methodologies\nunder a unified framework, shedding light on the role of structure in the\nlearning problem, and classify these methods into distinct patterns of\nincorporating structure. By leveraging this comprehensive framework, we provide\nvaluable insights into the challenges of structured RL and lay the groundwork\nfor a design pattern perspective on RL research. This novel perspective paves\nthe way for future advancements and aids in developing more effective and\nefficient RL algorithms that can potentially handle real-world scenarios\nbetter.", "cat": "cs.LG", "authors": ["Aditya Mohan", "Amy Zhang", "Marius Lindauer"]}, "1169": {"id": "1507.01952v1", "title": "The WiFeS S7 AGN survey: Current status and recent results on NGC 6300", "url": "http://arxiv.org/pdf/1507.01952v1", "date": "2015-07-07 20:01:42", "abs": "The Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) is a\ntargeted survey probing the narrow-line regions (NLRs) of a representative\nsample of ~140 nearby (z<0.02) Seyfert galaxies by means of optical integral\nfield spectroscopy. The survey is based on a homogeneous data set observed\nusing the Wide Field Spectrograph WiFeS. The data provide a 25x38 arcsec$^2$\nfield-of-view around the galaxy centre at typically ~1.5 arcsec spatial\nresolution and cover a wavelength range between ~3400 - 7100 $\\AA$ at spectral\nresolutions of ~100 km s$^{-1}$ and ~50 km s$^{-1}$ in the blue and red parts,\nrespectively. The survey is primarily designed to study gas excitation and star\nformation around AGN, with a special focus on the shape of the AGN ionising\ncontinuum, the interaction between radio jets and the NLR gas, and the nature\nof nuclear LINER emission. We provide an overview of the current status of\nS7-based results and present new results for NGC 6300.", "cat": "astro-ph.GA", "authors": ["J. Scharw\u00e4chter", "M. A. Dopita", "P. Shastri", "R. Davies", "L. Kewley", "E. Hampton", "R. Sutherland", "P. Kharb", "J. Jose", "H. Bhatt", "S. Ramya", "C. Jin", "J. Banfield", "I. Zaw", "S. Juneau", "B. James", "S. Srivastava"]}, "1170": {"id": "2309.16757v2", "title": "A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at $z\\sim5.5$", "url": "http://arxiv.org/pdf/2309.16757v2", "date": "2023-11-08 12:07:18", "abs": "The launch of ${\\it JWST}$ opens a new window for studying the connection\nbetween metal-line absorbers and galaxies at the end of the Epoch of\nReionization (EoR). Previous studies have detected absorber-galaxy pairs in\nlimited quantities through ground-based observations. To enhance our\nunderstanding of the relationship between absorbers and their host galaxies at\n$z>5$, we utilized the NIRCam Wide Field Slitless Spectroscopy (WFSS) to search\nfor absorber-associated galaxies by detecting their rest-frame optical emission\nlines (e.g., [OIII] + H$\\beta$). We report the discovery of a MgII-associated\ngalaxy at $z=5.428$ using data from the ${\\it JWST}$ ASPIRE program. The MgII\nabsorber is detected on the spectrum of quasar J0305--3150 with a rest-frame\nequivalent width of 0.74$\\mathring{A}$. The associated galaxy has an [OIII]\nluminosity of $10^{42.5}\\ {\\rm erg\\ s^{-1}}$ with an impact parameter of 24.9\nproper kiloparsecs (pkpc). The joint ${\\it HST}$-${\\it JWST}$ spectral energy\ndistribution (SED) implies a stellar mass and star-formation rate of ${\\rm M_*\n\\approx 10^{8.8}}$ ${\\rm M_{\\odot}}$, ${\\rm SFR}\\approx 10\\ {\\rm M_{\\odot}\\\nyr^{-1}}$. Its [OIII] equivalent width and stellar mass are typical of [OIII]\nemitters at this redshift. Furthermore, connecting the outflow starting time to\nthe SED-derived stellar age, the outflow velocity of this galaxy is $\\sim300\\\n{\\rm km\\ s^{-1}}$, consistent with theoretical expectations. We identified six\nadditional [OIII] emitters with impact parameters of up to $\\sim300$ pkpc at\nsimilar redshifts ($|dv|<1000\\ {\\rm km\\ s^{-1}}$). The observed number is\nconsistent with that in cosmological simulations. This pilot study suggests\nthat systematically investigating the absorber-galaxy connection within the\nASPIRE program will provide insights into the metal-enrichment history in the\nearly universe.", "cat": "astro-ph.GA", "authors": ["Yunjing Wu", "Feige Wang", "Zheng Cai", "Xiaohui Fan", "Kristian Finlator", "Jinyi Yang", "Joseph F. Hennawi", "Fengwu Sun", "Jaclyn B. Champagne", "Xiaojing Lin", "Zihao Li", "Zuyi Chen", "Eduardo Ba\u00f1ados", "George D. Becker", "Sarah E. I. Bosman", "Gstavo Bruzual", "Stephane Charlot", "Hsiao-Wen Chen", "Jacopo Chevallard", "Anna-Christina Eilers", "Emanuele Paolo Farina", "Xiangyu Jin", "Hyunsung D. Jun", "Koki Kakiichi", "Mingyu Li", "Weizhe Liu", "Maria A. Pudoka", "Wei Leong Tee", "Zhang-Liang Xie", "Siwei Zou"]}, "1171": {"id": "2407.03166v2", "title": "Neutral Atomic Hydrogen Surveys: past, present and future", "url": "http://arxiv.org/pdf/2407.03166v2", "date": "2024-08-15 13:05:38", "abs": "Neutral atomic hydrogen (HI) observations are fundamental to understand the\ndynamics of galaxies, their assembly, the fuelling of their star formation and\nenvironmental interactions. HI studies have so far been limited by the\ncapabilities of single-dish radio telescopes or synthesis arrays to either\nsmall samples or low resolution and sensitivities. Now, the Square Kilometer\nArray precursors and pathfinders are providing a novel view of the HI in and\naround galaxies allowing wide-field high resolution deep surveys in nearby\ngalaxies. We give an overview of past, current and future HI surveys\nconsistently comparing their HI column density and spatial resolutions\nhighlighting their main scientific key goals and results.", "cat": "astro-ph.GA", "authors": ["F. M. Maccagni", "W. J. G. de Blok"]}, "1172": {"id": "1811.11597v1", "title": "Automated Algorithm Selection: Survey and Perspectives", "url": "http://arxiv.org/pdf/1811.11597v1", "date": "2018-11-28 14:43:49", "abs": "It has long been observed that for practically any computational problem that\nhas been intensely studied, different instances are best solved using different\nalgorithms. This is particularly pronounced for computationally hard problems,\nwhere in most cases, no single algorithm defines the state of the art; instead,\nthere is a set of algorithms with complementary strengths. This performance\ncomplementarity can be exploited in various ways, one of which is based on the\nidea of selecting, from a set of given algorithms, for each problem instance to\nbe solved the one expected to perform best. The task of automatically selecting\nan algorithm from a given set is known as the per-instance algorithm selection\nproblem and has been intensely studied over the past 15 years, leading to major\nimprovements in the state of the art in solving a growing number of discrete\ncombinatorial problems, including propositional satisfiability and AI planning.\nPer-instance algorithm selection also shows much promise for boosting\nperformance in solving continuous and mixed discrete/continuous optimisation\nproblems.\n This survey provides an overview of research in automated algorithm\nselection, ranging from early and seminal works to recent and promising\napplication areas. Different from earlier work, it covers applications to\ndiscrete and continuous problems, and discusses algorithm selection in context\nwith conceptually related approaches, such as algorithm configuration,\nscheduling or portfolio selection. Since informative and cheaply computable\nproblem instance features provide the basis for effective per-instance\nalgorithm selection systems, we also provide an overview of such features for\ndiscrete and continuous problems. Finally, we provide perspectives on future\nwork in the area and discuss a number of open research challenges.", "cat": "cs.LG", "authors": ["Pascal Kerschke", "Holger H. Hoos", "Frank Neumann", "Heike Trautmann"]}, "1173": {"id": "1712.03350v1", "title": "ALMA Twenty-six arcmin$^2$ Survey of GOODS-S at One-millimeter (ASAGAO): X-ray AGN Properties of Millimeter-Selected Galaxies", "url": "http://arxiv.org/pdf/1712.03350v1", "date": "2017-12-09 07:36:08", "abs": "We investigate the X-ray active galactic nucleus (AGN) properties of\nmillimeter galaxies in the Great Observatories Origins Deep Survey South\n(GOODS-S) field detected with the Atacama Large Millimeter/submillimeter Array\n(ALMA), by utilizing the Chandra 7-Ms data, the deepest X-ray survey to date.\nOur millimeter galaxy sample comes from the ASAGAO survey covering 26\narcmin$^2$ (12 sources at a 1.2-mm flux-density limit of $\\approx$0.6 mJy),\nsupplemented by the deeper but narrower 1.3-mm survey of a part of the ASAGAO\nfield by Dunlop et al.\\ (2017). Fourteen out of the total 25 millimeter\ngalaxies have Chandra counterparts. The observed AGN fractions at $z=1.5-3$ is\nfound to be 90$^{+8}_{-19}$\\% and $57^{+23}_{-25}$\\% for the ultra/luminous\ninfrared galaxies with $\\log L_{\\rm IR}/L_{\\odot} = 12-12.8$ and $\\log L_{\\rm\nIR}/L_{\\odot} = 11.5-12$, respectively. The majority ($\\sim$2/3) of the ALMA\nand/or Herschel detected X-ray AGNs at $z=1.5-3$ appear to be star-formation\ndominant populations, having $L_{\\rm X}$/ $L_{\\rm IR}$ ratios smaller than the\n\"simultaneous evolution\" value expected from the local black-hole mass to\nstellar mass ($M_{\\rm BH}$-$M_*$) relation. On the basis of the $L_{\\rm X}$ and\nstellar mass relation, we infer that a large fraction of star-forming galaxies\nat $z=1.5-3$ have black hole masses smaller than those expected from the local\n$M_{\\rm BH}$-$M_*$ relation. This is opposite to previous reports on luminous\nAGN at same redshifts detected in wider and shallower surveys, which are\nsubject to selection biases against lower luminosity AGN. Our results are\nconsistent with an evolutionary scenario that star formation occurs first, and\nan AGN-dominant phase follows later, in objects finally evolving into galaxies\nwith classical bulges.", "cat": "astro-ph.HE", "authors": ["Y. Ueda", "B. Hatsukade", "K. Kohno", "Y. Yamaguchi", "Y. Tamura", "H. Umehata", "M. Akiyama", "Y. Ao", "I. Aretxaga", "K. Caputi", "J. S. Dunlop", "D. Espada", "S. Fujimoto", "N. H. Hayatsu", "M. Imanishi", "A. K. Inoue", "R. J. Ivison", "T. Kodama", "M. M. Lee", "K. Matsuoka", "T. Miyaji", "K. Morokuma-Matsui", "T. Nagao", "K. Nakanishi", "K. Nyland", "K. Ohta", "M. Ouchi", "W. Rujopakarn", "T. Saito", "K. Tadaki", "I. Tanaka", "Y. Taniguchi", "T. Wang", "W. -H. Wang", "Y. Yoshimura", "M. S. Yun"]}, "1174": {"id": "1807.05390v2", "title": "A survey on zeros of random holomorphic sections", "url": "http://arxiv.org/pdf/1807.05390v2", "date": "2020-11-06 08:56:43", "abs": "We survey results on the distribution of zeros of random polynomials and of\nrandom holomorphic sections of line bundles, especially for large classes of\nprobability measures on the spaces of holomorphic sections. We provide\nfurthermore some new examples of measures supported in totally real subsets of\nthe complex probability space.", "cat": "math.CV", "authors": ["Turgay Bayraktar", "Dan Coman", "Hendrik Herrmann", "George Marinescu"]}, "1175": {"id": "0704.2949v3", "title": "Optimizing future imaging survey of galaxies to confront dark energy and modified gravity models", "url": "http://arxiv.org/pdf/0704.2949v3", "date": "2007-07-22 08:01:09", "abs": "We consider the extent to which future imaging surveys of galaxies can\ndistinguish between dark energy and modified gravity models for the origin of\nthe cosmic acceleration. Dynamical dark energy models may have similar\nexpansion rates as models of modified gravity, yet predict different growth of\nstructure histories. We parameterize the cosmic expansion by the two\nparameters, $w_0$ and $w_a$, and the linear growth rate of density fluctuations\nby Linder's $\\gamma$, independently. Dark energy models generically predict\n$\\gamma \\approx 0.55$, while the DGP model $\\gamma \\approx 0.68$. To determine\nif future imaging surveys can constrain $\\gamma$ within 20 percent (or\n$\\Delta\\gamma<0.1$), we perform the Fisher matrix analysis for a weak lensing\nsurvey such as the on-going Hyper Suprime-Cam (HSC) project. Under the\ncondition that the total observation time is fixed, we compute the Figure of\nMerit (FoM) as a function of the exposure time $\\texp$. We find that the\ntomography technique effectively improves the FoM, which has a broad peak\naround $\\texp\\simeq {\\rm several}\\sim 10$ minutes; a shallow and wide survey is\npreferred to constrain the $\\gamma$ parameter. While $\\Delta\\gamma < 0.1$\ncannot be achieved by the HSC weak-lensing survey alone, one can improve the\nconstraints by combining with a follow-up spectroscopic survey like WFMOS\nand/or future CMB observations.", "cat": "astro-ph", "authors": ["Kazuhiro Yamamoto", "David Parkinson", "Takashi Hamana", "Robert C. Nichol", "Yasushi Suto"]}, "1176": {"id": "2402.17250v1", "title": "A chemodynamical analysis of bright metal-poor stars from the HESP-GOMPA survey -- Indications of a non-prevailing site for light r-process elements", "url": "http://arxiv.org/pdf/2402.17250v1", "date": "2024-02-27 06:48:29", "abs": "We present a comprehensive analysis of the detailed chemical abundances for a\nsample of 11 metal-poor, very metal-poor and extremely metal-poor stars ([Fe/H]\n= -1.65 to [Fe/H] = -3.0) as part of the HESP-GOMPA (Galactic survey Of Metal\nPoor stArs) survey. The abundance determinations encompass a range of elements,\nincluding C, Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, and\nBa, with a subset of the brighter objects allowing for the measurement of\nadditional key elements. Notably, the abundance analysis of a relatively bright\nhighly r-process-enhanced (r-II) star (SDSS J0019+3141) exhibits a\npredominantly main r-process signature and variations in the lighter r-process\nelements. Moreover, successful measurements of thorium in this star facilitate\nstellar age determinations. We find a consistent odd-even nucleosynthesis\npattern in these stars, aligning with expectations for their respective\nmetallicity levels, thus implicating Type II supernovae as potential\nprogenitors. From the interplay between the light and heavy r-process elements,\nwe infer a diminishing relative production of light r-process elements with\nincreasing Type II supernova contributions, challenging the notion that Type II\nsupernovae are the primary source of these light r-process elements in the\nearly Milky Way. A chemodynamical analysis based on Gaia astrometric data and\nour derived abundances indicates that all but one of our program stars are\nlikely to be of accreted origin. Additionally, our examination of alpha-poor\nstars underscores the occurrence of an early accretion event from a satellite\non a prograde orbit, similar to that of the Galactic disc.", "cat": "astro-ph.SR", "authors": ["Avrajit Bandyopadhyay", "Timothy C Beers", "Rana Ezzeddine", "Thirupathi Sivarani", "Prasanta K Nayak", "Jeewan C Pandey", "Pallavi Saraf", "Antony Susmitha"]}, "1177": {"id": "2310.09455v1", "title": "A survey on classifying hyperbolic actions of groups", "url": "http://arxiv.org/pdf/2310.09455v1", "date": "2023-10-14 00:24:18", "abs": "This paper is a survey of results proved in recent years that pertain to\nclassifying cobounded hyperbolic actions of any group $G$. In other words, we\ndiscuss results that allow us to describe the partially ordered set\n$\\mathcal{H}(G)$, first introduced in by Abbott-Balasubramanya-Osin. In certain\ncases, a complete classification of the poset is possible. In cases where this\nseems out of reach, we provide descriptions of large subsets of the poset. This\ncovers a wide range of groups, including acylindrically hyperbolic groups,\nnilpotent groups, many solvable groups and ``Thompson-like\" groups. We also\ncover the range of strategies utilized to obtain these classification results.\nAs a result, we produce some new examples of groups with interesting\n$\\mathcal{H}(G)$ structure.", "cat": "math.GR", "authors": ["Sahana H. Balasubramanya"]}, "1178": {"id": "1807.00807v3", "title": "Transfer learning for galaxy morphology from one survey to another", "url": "http://arxiv.org/pdf/1807.00807v3", "date": "2019-01-16 20:21:02", "abs": "Deep Learning (DL) algorithms for morphological classification of galaxies\nhave proven very successful, mimicking (or even improving) visual\nclassifications. However, these algorithms rely on large training samples of\nlabelled galaxies (typically thousands of them). A key question for using DL\nclassifications in future Big Data surveys is how much of the knowledge\nacquired from an existing survey can be exported to a new dataset, i.e. if the\nfeatures learned by the machines are meaningful for different data. We test the\nperformance of DL models, trained with Sloan Digital Sky Survey (SDSS) data, on\nDark Energy survey (DES) using images for a sample of $\\sim$5000 galaxies with\na similar redshift distribution to SDSS. Applying the models directly to DES\ndata provides a reasonable global accuracy ($\\sim$ 90%), but small completeness\nand purity values. A fast domain adaptation step, consisting in a further\ntraining with a small DES sample of galaxies ($\\sim$500-300), is enough for\nobtaining an accuracy > 95% and a significant improvement in the completeness\nand purity values. This demonstrates that, once trained with a particular\ndataset, machines can quickly adapt to new instrument characteristics (e.g.,\nPSF, seeing, depth), reducing by almost one order of magnitude the necessary\ntraining sample for morphological classification. Redshift evolution effects or\nsignificant depth differences are not taken into account in this study.", "cat": "astro-ph.GA", "authors": ["H. Dom\u00ednguez S\u00e1nchez", "M. Huertas-Company", "M. Bernardi", "S. Kaviraj", "J. L. Fischer", "T. M. C. Abbott", "F. B. Abdalla", "J. Annis", "S. Avila", "D. Brooks", "E. Buckley-Geer", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "C. E. Cunha", "C. B. D'Andrea", "L. N. da Costa", "C. Davis", "J. De Vicente", "P. Doel", "A. E. Evrard", "P. Fosalba", "J. Frieman", "J. Garc\u00eda-Bellido", "E. Gaztanaga", "D. W. Gerdes", "D. Gruen", "R. A. Gruendl", "J. Gschwend", "G. Gutierrez", "W. G. Hartley", "D. L. Hollowood", "K. Honscheid", "B. Hoyle", "D. J. James", "K. Kuehn", "N. Kuropatkin", "O. Lahav", "M. A. G. Maia", "M. March", "P. Melchior", "F. Menanteau", "R. Miquel", "B. Nord", "A. A. Plazas", "E. Sanchez", "V. Scarpine", "R. Schindler", "M. Schubnell", "M. Smith", "R. C. Smith", "M. Soares-Santos", "F. Sobreira", "E. Suchyta", "M. E. C. Swanson", "G. Tarle", "D. Thomas", "A. R. Walker", "J. Zuntz"]}, "1179": {"id": "2106.12714v2", "title": "Circuit Masking: From Theory to Standardization, A Comprehensive Survey for Hardware Security Researchers and Practitioners", "url": "http://arxiv.org/pdf/2106.12714v2", "date": "2021-06-30 01:29:25", "abs": "Side-channel attacks extracting sensitive data from implementations have been\nconsidered a major threat to the security of cryptographic schemes. This has\nelevated the need for improved designs by embodying countermeasures, with\nmasking being the most prominent example. To formally verify the security of a\nmasking scheme, numerous attack models have been developed to capture the\nphysical properties of the information leakage as well as the capabilities of\nthe adversary. With regard to these models, extensive research has been\nperformed to realize masking schemes. These research efforts have led to\nsignificant progress in the development of security assessment methodologies\nand further initiated standardization activities. However, since the majority\nof this work is theoretical, it is challenging for the more practice-oriented\nhardware security community to fully grasp and contribute to. To bridge the\ngap, these advancements are reviewed and discussed in this survey, mainly from\nthe perspective of hardware security. In doing so, a clear taxonomy is provided\nthat is helpful for a systematic treatment of the masking-related topics. By\ngiving an extensive overview of the existing methods, this survey (1) provides\na research landscape of circuit masking for newcomers to the field, (2) offers\nguidelines on which attack model and verification tool to choose when designing\nmasking schemes, and (3) identifies interesting new research directions where\nmasking models and assessment tools can be applied. Thus, this survey serves as\nan essential reference for hardware security practitioners interested in the\ntheory behind masking techniques, the tools useful to verify the security of\nmasked circuits, and their potential applications.", "cat": "cs.CR", "authors": ["Ana Covic", "Fatemeh Ganji", "Domenic Forte"]}, "1180": {"id": "2406.20026v1", "title": "FAST survey of H I and OH absorption towards extragalactic radio sources", "url": "http://arxiv.org/pdf/2406.20026v1", "date": "2024-06-28 16:14:49", "abs": "Neutral atomic hydrogen and molecular gas in the host galaxies of radio\nactive galactic nuclei (AGN) can be traced using H I 21-cm and OH-1667 MHz\nabsorption lines to understand the fueling and feedback processes. We present\nthe results of an H I and OH absorption survey with the Five-hundred-meter\nAperture Spherical radio Telescope (FAST) towards 40 radio sources of\nlow-intermediate radio luminosity ($\\sim$10$^{23}$-10$^{26}$ W Hz$^{-1}$ at 1.4\nGHz), red mid-infrared color (W2[4.6 $\\mu$m]$-$W3[12 $\\mu$m] $>$ 2.5 mag) and\nredshift up to 0.35. From 13 sources with good data at H I observing\nfrequencies, we report the detection of H I absorption towards 8 sources, 5 of\nwhich are new detections including 4 in the redshift range 0.25 to 0.35. Our\ndetection rates are consistent with our previous results with dependence on the\nstar-formation history of the host galaxy reflected in the mid-infrared\n\\textit{WISE} W2$-$W3 colors and the compactness of the radio source. We find\nno significant dependence of detection rates on radio luminosity or redshift.\nWe also find that H I column densities are anti-correlated with the\nlow-frequency spectral indices ($\\alpha_{\\rm 150 MHz}^{\\rm 1.4 GHz}$,\n$S_{\\nu}\\propto \\nu^{-\\alpha}$). We do not have any detection from 23 sources\nwith good data at OH observing frequencies. However, by stacking the spectra we\nestimate the 3$\\sigma$ upper limit of OH column density to be\n2.27$\\times$10$^{14}$$T_{\\rm ex}$/10 K $\\times$1/$f_{\\rm c}$ cm$^{-2}$. By\nstacking the OH spectra for 7 associated H I absorbers, we get a 3$\\sigma$\nupper limit of 3.47$\\times$10$^{14}$ $T_{\\rm ex}$/10 K $\\times$1/$f_{\\rm c}$\ncm$^{-2}$ on OH column density and 1.78$\\times$10$^{-7}$ on [OH]/[H I] ratio.", "cat": "astro-ph.GA", "authors": ["Yogesh Chandola", "D. J. Saikia", "Yin-Zhe Ma", "Zheng Zheng", "Chao-Wei Tsai", "Di Li", "Denis Tramonte", "Hengxing Pan"]}, "1181": {"id": "1908.00473v1", "title": "A Survey on Deep Learning of Small Sample in Biomedical Image Analysis", "url": "http://arxiv.org/pdf/1908.00473v1", "date": "2019-08-01 16:01:31", "abs": "The success of deep learning has been witnessed as a promising technique for\ncomputer-aided biomedical image analysis, due to end-to-end learning framework\nand availability of large-scale labelled samples. However, in many cases of\nbiomedical image analysis, deep learning techniques suffer from the small\nsample learning (SSL) dilemma caused mainly by lack of annotations. To be more\npractical for biomedical image analysis, in this paper we survey the key SSL\ntechniques that help relieve the suffering of deep learning by combining with\nthe development of related techniques in computer vision applications. In order\nto accelerate the clinical usage of biomedical image analysis based on deep\nlearning techniques, we intentionally expand this survey to include the\nexplanation methods for deep models that are important to clinical decision\nmaking. We survey the key SSL techniques by dividing them into five categories:\n(1) explanation techniques, (2) weakly supervised learning techniques, (3)\ntransfer learning techniques, (4) active learning techniques, and (5)\nmiscellaneous techniques involving data augmentation, domain knowledge,\ntraditional shallow methods and attention mechanism. These key techniques are\nexpected to effectively support the application of deep learning in clinical\nbiomedical image analysis, and furtherly improve the analysis performance,\nespecially when large-scale annotated samples are not available. We bulid demos\nat https://github.com/PengyiZhang/MIADeepSSL.", "cat": "cs.CV", "authors": ["Pengyi Zhang", "Yunxin Zhong", "Yulin Deng", "Xiaoying Tang", "Xiaoqiong Li"]}, "1182": {"id": "1911.00611v1", "title": "The GRAVITY Young Stellar Object survey -- I. Probing the disks of Herbig Ae/Be stars in terrestrial orbits", "url": "http://arxiv.org/pdf/1911.00611v1", "date": "2019-11-01 23:04:45", "abs": "The formation and the evolution of protoplanetary disks are important stages\nin the lifetime of stars. The processes of disk evolution and planet formation\nare intrinsically linked. We spatially resolve with GRAVITY/VLTI in the K-band\nthe sub au-scale region of 27 stars to gain statistical understanding of their\nproperties. We look for correlations with stellar parameters, such as\nluminosity, mass, temperature and age. Our sample also cover a range of various\nproperties in terms of reprocessed flux, flared or flat morphology, and gaps.\nWe developed semi-physical geometrical models to fit our interferometric data.\nOur best models correspond to smooth and wide rings, implying that wedge-shaped\nrims at the dust sublimation edge are favored, as found in the H-band. The\nclosure phases are generally non-null with a median value of ~10 deg,\nindicating spatial asymmetries of the intensity distributions. Multi-size grain\npopulations could explain the closure phase ranges below 20-25 deg but other\nscenarios should be invoked to explain the largest ones. Our measurements\nextend the Radius-Luminosity relation to ~1e4 Lsun and confirm the significant\nspread around the mean relation observed in the H-band. Gapped sources exhibit\na large N-to-K band size ratio and large values of this ratio are only observed\nfor the members of our sample that would be older than 1 Ma, less massive, and\nwith lower luminosity. In the 2 Ms mass range, we observe a correlation in the\nincrease of the relative age with the transition from group II to group I, and\nan increase of the N-to-K size ratio. However, the size of the current sample\ndoes not yet permit us to invoke a clear universal evolution mechanism across\nthe HAeBe mass range. The measured locations of the K-band emission suggest\nthat these disks might be structured by forming young planets, rather than by\ndepletion due to EUV, FUV, and X-ray photo-evaporation.", "cat": "astro-ph.SR", "authors": ["K. Perraut", "L. Labadie", "B. Lazareff", "L. Klarmann", "D. Segura-Cox", "M. Benisty", "J. Bouvier", "W. Brandner", "A. Caratti o Garatti", "P. Caselli", "C. Dougados", "P. Garcia", "R. Garcia-Lopez", "S. Kendrew", "M. Koutoulaki", "P. Kervella", "C. -C. Lin", "J. Pineda", "J. Sanchez-Bermudez", "E. van Dishoeck", "R. Abuter", "A. Amorim", "J. -P. Berger", "H. Bonnet", "A. Buron", "F. Cantalloube", "Y. Cl\u00e9net", "V. Coud\u00e9 du Foresto", "J. Dexter", "P. T. de Zeeuw", "G. Duvert", "A. Eckart", "F. Eisenhauer", "F. Eupen", "F. Gao", "E. Gendron", "R. Genzel", "S. Gillessen", "P. Gordo", "R. Grellmann", "X. Haubois", "F. Haussmann", "T. Henning", "S. Hippler", "M. Horrobin", "Z. Hubert", "L. Jocou", "S. Lacour", "J. -B. Le Bouquin", "P. L\u00e9na", "A. M\u00e9rand", "T. Ott", "T. Paumard", "G. Perrin", "O. Pfuhl", "S. Rabien", "T. Ray", "C. Rau", "G. Rousset", "S. Scheithauer", "O. Straub", "C. Straubmeier", "E. Sturm", "F. Vincent", "I. Waisberg", "I. Wank", "F. Widmann", "E. Wieprecht", "M. Wiest", "E. Wiezorrek", "J. Woillez", "S. Yazici"]}, "1183": {"id": "2104.07720v2", "title": "Ontology-based Feature Selection: A Survey", "url": "http://arxiv.org/pdf/2104.07720v2", "date": "2021-04-30 14:17:37", "abs": "The SemanticWeb emerged as an extension to the traditional Web, towards\nadding meaning to a distributed Web of structured and linked data. At its core,\nthe concept of ontology provides the means to semantically describe and\nstructure information and data and expose it to software and human agents in a\nmachine and human-readable form. For software agents to be realized, it is\ncrucial to develop powerful artificial intelligence and machine learning\ntechniques, able to extract knowledge from information and data sources and\nrepresent it in the underlying ontology. This survey aims to provide insight\ninto key aspects of ontology-based knowledge extraction, from various sources\nsuch as text, images, databases and human expertise, with emphasis on the task\nof feature selection. First, some of the most common classification and feature\nselection algorithms are briefly presented. Then, selected methodologies, which\nutilize ontologies to represent features and perform feature selection and\nclassification, are described. The presented examples span diverse application\ndomains, e.g., medicine, tourism, mechanical and civil engineering, and\ndemonstrate the feasibility and applicability of such methods.", "cat": "cs.AI", "authors": ["Konstantinos Sikelis", "George E Tsekouras", "Konstantinos I Kotis"]}, "1184": {"id": "2208.00173v1", "title": "A Survey on Masked Autoencoder for Self-supervised Learning in Vision and Beyond", "url": "http://arxiv.org/pdf/2208.00173v1", "date": "2022-07-30 09:59:28", "abs": "Masked autoencoders are scalable vision learners, as the title of MAE\n\\cite{he2022masked}, which suggests that self-supervised learning (SSL) in\nvision might undertake a similar trajectory as in NLP. Specifically, generative\npretext tasks with the masked prediction (e.g., BERT) have become a de facto\nstandard SSL practice in NLP. By contrast, early attempts at generative methods\nin vision have been buried by their discriminative counterparts (like\ncontrastive learning); however, the success of mask image modeling has revived\nthe masking autoencoder (often termed denoising autoencoder in the past). As a\nmilestone to bridge the gap with BERT in NLP, masked autoencoder has attracted\nunprecedented attention for SSL in vision and beyond. This work conducts a\ncomprehensive survey of masked autoencoders to shed insight on a promising\ndirection of SSL. As the first to review SSL with masked autoencoders, this\nwork focuses on its application in vision by discussing its historical\ndevelopments, recent progress, and implications for diverse applications.", "cat": "cs.CV", "authors": ["Chaoning Zhang", "Chenshuang Zhang", "Junha Song", "John Seon Keun Yi", "Kang Zhang", "In So Kweon"]}, "1185": {"id": "0706.1564v2", "title": "The First Survey of X-ray Flares from Gamma Ray Bursts Observed by Swift: Spectral Properties and Energetics", "url": "http://arxiv.org/pdf/0706.1564v2", "date": "2007-09-07 20:25:42", "abs": "Observations of gamma ray bursts (GRBs) with Swift produced the initially\nsurprising result that many bursts have large X-ray flares superimposed on the\nunderlying afterglow. The flares were sometimes intense, had rapid rise and\ndecay phases, and occurred late relative to the ``prompt'' phase. Some\nremarkable flares are observed with fluence comparable to the prompt GRB\nfluence. Many GRBs have several flares, which are sometimes overlapping. Short,\nintense, repetitive, and late flaring can be most easily understood within the\ncontext of the standard fireball model with the internal engine that powers the\nprompt GRB emission in an active state at late times. However, other models for\nflares have been proposed. Flare origin can be investigated by comparing the\nflare spectra to that of the afterglow and the initial prompt emission. In this\nwork, we have analyzed all significant X-ray flares from the first 110 GRBs\nobserved by Swift. From this sample 33 GRBs were found to have significant\nX-ray flares, with 77 flares that were detected above the 3$\\sigma$ level. In\naddition to temporal analysis presented in a companion paper, a variety of\nspectral models have been fit to each flare. In some cases, we find that the\nspectral fits favor a Band function model, which is more akin to the prompt\nemission than to that of an afterglow. We find that the average fluence of the\nflares is 2.4e-7 erg/cm^2/s in the 0.2-10 keV energy band, which is\napproximately a factor of ten below the average prompt GRB fluence. These\nresults, when combined with those presented in the companion paper on temporal\nproperties of flares, supports the hypothesis that most X-ray flares are\nlate-time activity of the internal engine that spawned the initial GRB; not an\nafterglow related effect.", "cat": "astro-ph", "authors": ["A. D. Falcone", "D. Morris", "J. Racusin", "G. Chincarini", "A. Moretti", "P. Romano", "D. N. Burrows", "C. Pagani", "M. Stroh", "D. Grupe", "S. Campana", "S. Covino", "G. Tagliaferri", "R. Willingale", "N. Gehrels"]}, "1186": {"id": "2402.12451v2", "title": "The Revolution of Multimodal Large Language Models: A Survey", "url": "http://arxiv.org/pdf/2402.12451v2", "date": "2024-06-06 16:13:43", "abs": "Connecting text and visual modalities plays an essential role in generative\nintelligence. For this reason, inspired by the success of large language\nmodels, significant research efforts are being devoted to the development of\nMultimodal Large Language Models (MLLMs). These models can seamlessly integrate\nvisual and textual modalities, while providing a dialogue-based interface and\ninstruction-following capabilities. In this paper, we provide a comprehensive\nreview of recent visual-based MLLMs, analyzing their architectural choices,\nmultimodal alignment strategies, and training techniques. We also conduct a\ndetailed analysis of these models across a wide range of tasks, including\nvisual grounding, image generation and editing, visual understanding, and\ndomain-specific applications. Additionally, we compile and describe training\ndatasets and evaluation benchmarks, conducting comparisons among existing\nmodels in terms of performance and computational requirements. Overall, this\nsurvey offers a comprehensive overview of the current state of the art, laying\nthe groundwork for future MLLMs.", "cat": "cs.CV", "authors": ["Davide Caffagni", "Federico Cocchi", "Luca Barsellotti", "Nicholas Moratelli", "Sara Sarto", "Lorenzo Baraldi", "Lorenzo Baraldi", "Marcella Cornia", "Rita Cucchiara"]}, "1187": {"id": "2011.12247v1", "title": "Classification supporting COVID-19 diagnostics based on patient survey data", "url": "http://arxiv.org/pdf/2011.12247v1", "date": "2020-11-24 17:44:01", "abs": "Distinguishing COVID-19 from other flu-like illnesses can be difficult due to\nambiguous symptoms and still an initial experience of doctors. Whereas, it is\ncrucial to filter out those sick patients who do not need to be tested for\nSARS-CoV-2 infection, especially in the event of the overwhelming increase in\ndisease. As a part of the presented research, logistic regression and XGBoost\nclassifiers, that allow for effective screening of patients for COVID-19, were\ngenerated. Each of the methods was tuned to achieve an assumed acceptable\nthreshold of negative predictive values during classification. Additionally, an\nexplanation of the obtained classification models was presented. The\nexplanation enables the users to understand what was the basis of the decision\nmade by the model. The obtained classification models provided the basis for\nthe DECODE service (decode.polsl.pl), which can serve as support in screening\npatients with COVID-19 disease. Moreover, the data set constituting the basis\nfor the analyses performed is made available to the research community. This\ndata set consisting of more than 3,000 examples is based on questionnaires\ncollected at a hospital in Poland.", "cat": "cs.LG", "authors": ["Joanna Henzel", "Joanna Tobiasz", "Micha\u0142 Kozielski", "Ma\u0142gorzata Bach", "Pawe\u0142 Foszner", "Aleksandra Gruca", "Mateusz Kania", "Justyna Mika", "Anna Papiez", "Aleksandra Werner", "Joanna Zyla", "Jerzy Jaroszewicz", "Joanna Polanska", "Marek Sikora"]}, "1188": {"id": "2403.13368v1", "title": "Computational Models to Study Language Processing in the Human Brain: A Survey", "url": "http://arxiv.org/pdf/2403.13368v1", "date": "2024-03-20 08:01:22", "abs": "Despite differing from the human language processing mechanism in\nimplementation and algorithms, current language models demonstrate remarkable\nhuman-like or surpassing language capabilities. Should computational language\nmodels be employed in studying the brain, and if so, when and how? To delve\ninto this topic, this paper reviews efforts in using computational models for\nbrain research, highlighting emerging trends. To ensure a fair comparison, the\npaper evaluates various computational models using consistent metrics on the\nsame dataset. Our analysis reveals that no single model outperforms others on\nall datasets, underscoring the need for rich testing datasets and rigid\nexperimental control to draw robust conclusions in studies involving\ncomputational models.", "cat": "cs.CL", "authors": ["Shaonan Wang", "Jingyuan Sun", "Yunhao Zhang", "Nan Lin", "Marie-Francine Moens", "Chengqing Zong"]}, "1189": {"id": "2404.03944v1", "title": "The MeerKAT Massive Distant Clusters Survey: A Radio Halo in a Massive Galaxy Cluster at z = 1.23", "url": "http://arxiv.org/pdf/2404.03944v1", "date": "2024-04-05 08:18:17", "abs": "In the current paradigm, high redshift radio halos are expected to be scarce\ndue to inverse Compton energy losses and redshift dimming, which cause them to\nbe intrinsically faint. This low occurrence fraction is predicted by cosmic ray\nelectron turbulent re-acceleration models. To date, only a handful of radio\nhalos have been detected at redshift z > 0.8. We report the MeerKAT detection\nof a radio halo hosted by a galaxy cluster ACT-CL J0329.2-2330 at z = 1.23,\nmaking it the highest redshift halo detected thus far. Using L-band and\nUHF-band observations, we derive a radio halo spectral index of\n$\\alpha^{1.3GHz}_{0.8GHz}$ = 1.3 $\\pm$ 0.4 and a radio power of P$_{1.4GHz}$ =\n(4.4 $\\pm$ 1.5) $\\times$ 10$^{24}$ W Hz$^{-1}$. This result further confirms\nthat there is rapid magnetic field amplification in galaxy clusters at high\nredshift.", "cat": "astro-ph.HE", "authors": ["S. P. Sikhosana", "M. Hilton", "G. Bernardi", "K. Kesebonye", "D. Y. Klutse", "K. Knowles", "K. Moodley", "T. Mroczkowski", "B. Partridge", "C. Sif\u00f3n", "C. Vargas", "E. Wollack"]}, "1190": {"id": "2105.07391v2", "title": "Survey of Visual-Semantic Embedding Methods for Zero-Shot Image Retrieval", "url": "http://arxiv.org/pdf/2105.07391v2", "date": "2021-09-28 08:51:47", "abs": "Visual-semantic embedding is an interesting research topic because it is\nuseful for various tasks, such as visual question answering (VQA), image-text\nretrieval, image captioning, and scene graph generation. In this paper, we\nfocus on zero-shot image retrieval using sentences as queries and present a\nsurvey of the technological trends in this area. First, we provide a\ncomprehensive overview of the history of the technology, starting with a\ndiscussion of the early studies of image-to-text matching and how the\ntechnology has evolved over time. In addition, a description of the datasets\ncommonly used in experiments and a comparison of the evaluation results of each\nmethod are presented. We also introduce the implementation available on github\nfor use in confirming the accuracy of experiments and for further improvement.\nWe hope that this survey paper will encourage researchers to further develop\ntheir research on bridging images and languages.", "cat": "cs.CV", "authors": ["Kazuya Ueki"]}, "1191": {"id": "2305.00241v2", "title": "When Deep Learning Meets Polyhedral Theory: A Survey", "url": "http://arxiv.org/pdf/2305.00241v2", "date": "2023-08-31 13:36:21", "abs": "In the past decade, deep learning became the prevalent methodology for\npredictive modeling thanks to the remarkable accuracy of deep neural networks\nin tasks such as computer vision and natural language processing. Meanwhile,\nthe structure of neural networks converged back to simpler representations\nbased on piecewise constant and piecewise linear functions such as the\nRectified Linear Unit (ReLU), which became the most commonly used type of\nactivation function in neural networks. That made certain types of network\nstructure $\\unicode{x2014}$such as the typical fully-connected feedforward\nneural network$\\unicode{x2014}$ amenable to analysis through polyhedral theory\nand to the application of methodologies such as Linear Programming (LP) and\nMixed-Integer Linear Programming (MILP) for a variety of purposes. In this\npaper, we survey the main topics emerging from this fast-paced area of work,\nwhich bring a fresh perspective to understanding neural networks in more detail\nas well as to applying linear optimization techniques to train, verify, and\nreduce the size of such networks.", "cat": "math.OC", "authors": ["Joey Huchette", "Gonzalo Mu\u00f1oz", "Thiago Serra", "Calvin Tsay"]}, "1192": {"id": "2104.03432v2", "title": "The Low-redshift Lyman-continuum Survey: [S II]-deficiency and the leakage of ionizing radiation", "url": "http://arxiv.org/pdf/2104.03432v2", "date": "2021-07-22 00:37:09", "abs": "The relationship between galaxy characteristics and the reionization of the\nuniverse remains elusive, mainly due to the observational difficulty in\naccessing the Lyman continuum (LyC) at these redshifts. It is thus important to\nidentify low-redshift LyC-leaking galaxies that can be used as laboratories to\ninvestigate the physical processes that allow LyC photons to escape. The\nweakness of the [S II] nebular emission lines relative to typical star-forming\ngalaxies has been proposed as a LyC predictor. In this paper, we show that the\n[S II]-deficiency is an effective method to select LyC-leaking candidates using\ndata from the Low-redshift LyC Survey, which has detected flux below the Lyman\nedge in 35 out of 66 star-forming galaxies with the Cosmic Origins Spectrograph\nonboard the Hubble Space Telescope. We show that LyC leakers tend to be more [S\nII]-deficient and that the fraction of their detections increases as [S\nII]-deficiency becomes more prominent. Correlational studies suggest that [S\nII]-deficiency complements other LyC diagnostics (such as strong Lyman-$\\alpha$\nemission and high [O III]/[O II]). Our results verify an additional technique\nby which reionization-era galaxies could be studied.", "cat": "astro-ph.GA", "authors": ["Bingjie Wang", "Timothy M. Heckman", "Ricardo Amor\u00edn", "Sanchayeeta Borthakur", "John Chisholm", "Harry Ferguson", "Sophia Flury", "Mauro Giavalisco", "Andrea Grazian", "Matthew Hayes", "Alaina Henry", "Anne Jaskot", "Zhiyuan Ji", "Kirill Makan", "Stephan McCandliss", "M. S. Oey", "G\u00f6ran \u00d6stlin", "Alberto Saldana-Lopez", "Daniel Schaerer", "Trinh Thuan", "G\u00e1bor Worseck", "Xinfeng Xu"]}, "1193": {"id": "2302.05184v2", "title": "Rates and properties of type Ia supernovae in galaxy clusters within the Dark Energy Survey", "url": "http://arxiv.org/pdf/2302.05184v2", "date": "2023-09-28 13:45:06", "abs": "We identify 66 photometrically classified type Ia supernovae (SNe Ia) from\nthe Dark Energy Survey (DES) that have occurred within red-sequence selected\ngalaxy clusters. We compare light-curve and host galaxy properties of the\ncluster SNe to 1024 DES SNe Ia located in field galaxies, the largest\ncomparison of two such samples at high redshift (z > 0.1). We find that cluster\nSN light curves decline faster than those in the field (97.7 per cent\nconfidence). However, when limiting these samples to host galaxies of similar\ncolour and mass, there is no significant difference in the SN light curve\nproperties. Motivated by previous detections of a higher-normalised SN Ia delay\ntime distribution in galaxy clusters, we measure the intrinsic rate of SNe Ia\nin cluster and field environments. We find the average ratio of the SN Ia rate\nper galaxy between high mass ($10\\leq\\log\\mathrm{(M_{*}/M_{\\odot})} \\leq\n11.25$) cluster and field galaxies to be $0.594 \\pm0.068$. This difference is\nmass-dependent, with the ratio declining with increasing mass, which suggests\nthat the stellar populations in cluster hosts are older than those in field\nhosts. We show that the mass-normalised rate (or SNe per unit mass) in\nmassive-passive galaxies is consistent between cluster and field environments.\nAdditionally, both of these rates are consistent with rates previously measured\nin clusters at similar redshifts. We conclude that in massive-passive galaxies,\nwhich are the dominant hosts of cluster SNe, the cluster DTD is comparable to\nthe field.", "cat": "astro-ph.HE", "authors": ["M. Toy", "P. Wiseman", "M. Sullivan", "C. Frohmaier", "O. Graur", "A. Palmese", "B. Popovic", "T. M. Davis", "L. Galbany", "L. Kelsey", "C. Lidman", "D. Scolnic", "S. Allam", "S. Desai", "T. M. C. Abbott", "M. Aguena", "O. Alves", "J. Annis", "D. Bacon", "E. Bertin", "D. Brooks", "D. L. Burke", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "F. J. Castander", "C. Conselice", "L. N. da Costa", "M. E. S. Pereira", "J. De Vicente", "H. T. Diehl", "P. Doel", "S. Everett", "I. Ferrero", "J. Frieman", "D. W. Gerdes", "D. Gruen", "R. A. Gruendl", "G. Gutierrez", "S. R. Hinton", "D. L. Hollowood", "K. Honscheid", "D. J. James", "K. Kuehn", "N. Kuropatkin", "J. L. Marshall", "P. Melchior", "J. Mena-Fern\u00e1ndez", "F. Menanteau", "R. Miquel", "A. Pieres", "A. A. Plazas Malag\u00f3n", "A. K. Romer", "E. Sanchez", "V. Scarpine", "I. Sevilla-Noarbe", "M. Smith", "M. Soares-Santos", "E. Suchyta", "G. Tarle", "C. To", "N. Weaverdyck"]}, "1194": {"id": "2303.07293v1", "title": "GPU-based framework for detecting small Solar System bodies in targeted exoplanet surveys", "url": "http://arxiv.org/pdf/2303.07293v1", "date": "2023-03-13 17:15:08", "abs": "Small Solar System bodies are pristine remnants of Solar System formation,\nwhich provide valuable insights for planetary science and astronomy. Their\ndiscovery and cataloging also have strong practical implications to life on\nEarth as the nearest asteroids could pose a serious impact threat. Concurrently\nwith dedicated observational projects, searches for small bodies have been\nperformed on numerous archival data sets from different facilities. Here, we\npresent a framework to increase the scientific return of an exoplanet\ntransit-search survey by recovering serendipitous detections of small bodies in\nits daily and archival data using a GPU-based synthetic tracking algorithm. As\na proof of concept, we analysed $12 \\times 12 \\mathrm{arcmin^2}$ sky fields\nobserved by the 1-m telescopes of the SPECULOOS survey. We analysed 90 sky\nfields distributed uniformly across the sky as part of the daily search for\nsmall bodies and 21 archival fields located within 5 deg from the ecliptic\nplane as part of the archival search (4.4 deg$^2$ in total). Overall, we\nidentified 400 known objects of different dynamical classes from Inner\nMain-belt Asteroids to Jupiter Trojans and 43 potentially new small bodies with\nno priors on their motion. We were able to reach limiting magnitude for unknown\nobjects of $V$=23.8 mag, and a retrieval rate of $\\sim$80% for objects with\n$V<$22 mag and $V<$23.5 mag for the daily and archival searches, respectively.\nSPECULOOS and similar exoplanet surveys can thus serve as pencil-beam surveys\nfor small bodies and probe parameter space beyond $V$=22 mag.", "cat": "astro-ph.EP", "authors": ["Artem Burdanov", "Samantha Hasler", "Julien de Wit"]}, "1195": {"id": "1410.7401v2", "title": "The Subaru high-z quasar survey: discovery of faint z~6 quasars", "url": "http://arxiv.org/pdf/1410.7401v2", "date": "2014-11-28 00:46:51", "abs": "We present the discovery of one or two extremely faint z~6 quasars in 6.5\ndeg^2 utilizing a unique capability of the wide-field imaging of the\nSubaru/Suprime-Cam. The quasar selection was made in (i'-z_B) and (z_B-z_R)\ncolors, where z_B and z_R are bandpasses with central wavelengths of 8842A and\n9841A, respectively. The color selection can effectively isolate quasars at z~6\nfrom M/L/T dwarfs without the J-band photometry down to z_R<24.0, which is 3.5\nmag. deeper than SDSS. We have selected 17 promising quasar candidates. The\nfollow-up spectroscopy for seven targets identified one apparent quasar at\nz=6.156 with M_1450=-23.10. We also identified one possible quasar at z=6.041\nwith a faint continuum of M_1450=-22.58 and a narrow Lyman-alpha emission with\nHWHM=427 km/s, which cannot be distinguished from Lyman-alpha emitters. We\nderive the quasar luminosity function at z~6 by combining our faint quasar\nsample with the bright quasar samples by SDSS and CFHQS. Including our data\npoints invokes a higher number density in the faintest bin of the quasar\nluminosity function than the previous estimate employed. This suggests a\nsteeper faint-end slope than lower-z, though it is yet uncertain based on a\nsmall number of spectroscopically identified faint quasars and several quasar\ncandidates are still remain to be diagnosed. The steepening of the quasar\nluminosity function at the faint-end does increase the expected emission rate\nof the ionizing photon, however, it only changes by a factor of ~2-6. This was\nfound to be still insufficient for the required photon budget of reionization\nat z~6.", "cat": "astro-ph.GA", "authors": ["Nobunari Kashikawa", "Yoshifumi Ishizaki", "Chris J. Willott", "Masafusa Onoue", "Myungshin Im", "Hisanori Furusawa", "Jun Toshikawa", "Shogo Ishikawa", "Yuu Niino", "Kazuhiro Shimasaku", "Masami Ouchi", "Pascale Hibon"]}, "1196": {"id": "2202.02059v2", "title": "The Hydrogen-Poor Superluminous Supernovae from the Zwicky Transient Facility Phase-I Survey: I. Light Curves and Measurements", "url": "http://arxiv.org/pdf/2202.02059v2", "date": "2022-11-03 06:46:51", "abs": "During the Zwicky Transient Facility (ZTF) Phase-I operation, 78\nhydrogen-poor superluminous supernovae (SLSNe-I) were discovered in less than\nthree years, making up the largest sample from a single survey. This paper\n(Paper I) presents the data, including the optical/ultraviolet light curves and\nclassification spectra, while Paper II in this series will focus on the\ndetailed analysis of the light curves and modeling. Our photometry is primarily\ntaken by the ZTF in the $g,r,i$ bands, and with additional data from other\nground-based facilities and Swift. The events of our sample cover a redshift\nrange of $z = 0.06 - 0.67$, with a median and $1\\sigma$ error (16\\% and 84\\%\npercentiles) $z_{\\rm med} = 0.265^{+0.143}_{-0.135}$. The peak luminosity\ncovers $-22.8\\,{\\rm mag} \\leq M_{g,\\rm peak} \\leq -19.8$\\,mag, with a median\nvalue of $-21.48^{+1.13}_{-0.61}$\\,mag. Their light curves evolve slowly with\nthe mean rest-frame rise time of $t_{\\rm rise} = 41.9\\pm17.8$\\,days. The\nluminosity and time scale distributions suggest that low luminosity SLSNe-I\nwith peak luminosity $\\sim -20$\\,mag or extremely fast rising events\n($<10$\\,days) exist but are rare. We confirm previous findings that slowly\nrising SLSNe-I also tend to fade slowly. The rest-frame color and temperature\nevolution show large scatters, suggesting that the SLSN-I population may have\ndiverse spectral energy distributions. The peak rest-frame color shows a\nmoderate correlation with the peak absolute magnitude, i.e. brighter SLSNe-I\ntend to have bluer colors. With optical and ultraviolet photometry, we\nconstruct bolometric luminosity and derive a bolometric correction relation\ngenerally applicable for converting $g,r$-band photometry to bolometric\nluminosity for SLSNe-I.", "cat": "astro-ph.HE", "authors": ["Z. H. Chen", "Lin Yan", "T. Kangas", "R. Lunnan", "S. Schulze", "J. Sollerman", "D. A. Perley", "T. -W. Chen", "K. Taggart", "K. R. Hinds", "A. Gal-Yam", "X. F. Wang", "I. Andreoni", "E. Bellm", "J. S. Bloom", "K. Burdge", "A. Burgos", "D. Cook", "A. Dahiwale", "K. De", "R. Dekany", "A. Dugas", "S. Frederik", "C. Fremling", "M. Graham", "M. Hankins", "A. Ho", "J. Jencson", "V. Karambelkar", "M. Kasliwal", "S. Kulkarni", "R. Laher", "B. Rusholme", "Y. Sharma", "F. Taddia", "L. Tartaglia", "B. P. Thomas", "A. Tzanidakis", "J. Van Roestel", "R. Walter", "Y. Yang", "Y. H. Yao", "O. Yaron"]}, "1197": {"id": "1409.1308v1", "title": "Kiso Supernova Survey (KISS): Survey Strategy", "url": "http://arxiv.org/pdf/1409.1308v1", "date": "2014-09-04 03:07:27", "abs": "The Kiso Supernova Survey (KISS) is a high-cadence optical wide-field\nsupernova (SN) survey. The primary goal of the survey is to catch the very\nearly light of a SN, during the shock breakout phase. Detection of SN shock\nbreakouts combined with multi-band photometry obtained with other facilities\nwould provide detailed physical information on the progenitor stars of SNe. The\nsurvey is performed using a 2.2x2.2 deg field-of-view instrument on the 1.05-m\nKiso Schmidt telescope, the Kiso Wide Field Camera (KWFC). We take a\nthree-minute exposure in g-band once every hour in our survey, reaching\nmagnitude g~20-21. About 100 nights of telescope time per year have been spent\non the survey since April 2012. The number of the shock breakout detections is\nestimated to be of order of 1 during our 3-year project. This paper summarizes\nthe KISS project including the KWFC observing setup, the survey strategy, the\ndata reduction system, and CBET-reported SNe discovered so far by KISS.", "cat": "astro-ph.SR", "authors": ["Tomoki Morokuma", "Nozomu Tominaga", "Masaomi Tanaka", "Kensho Mori", "Emiko Matsumoto", "Yuki Kikuchi", "Takumi Shibata", "Shigeyuki Sako", "Tsutomu Aoki", "Mamoru Doi", "Naoto Kobayashi", "Hiroyuki Maehara", "Noriyuki Matsunaga", "Hiroyuki Mito", "Takashi Miyata", "Yoshikazu Nakada", "Takao Soyano", "Ken'ichi Tarusawa", "Satoshi Miyazaki", "Fumiaki Nakata", "Norio Okada", "Yuki Sarugaku", "Michael W. Richmond", "Hiroshi Akitaya", "Greg Aldering", "Ko Arimatsu", "Carlos Contreras", "Takashi Horiuchi", "Eric Y. Hsiao", "Ryosuke Itoh", "Ikuru Iwata", "Koji", "S. Kawabata", "Nobuyuki Kawai", "Yutaro Kitagawa", "Mitsuru Kokubo", "Daisuke Kuroda", "Paolo", "Mazzali", "Toru Misawa", "Yuki Moritani", "Nidia Morrell", "Rina Okamoto", "Nikolay Pavlyuk", "Mark M. Phillips", "Elena Pian", "Devendra Sahu", "Yoshihiko Saito", "Kei Sano", "Maximilian D. Stritzinger", "Yutaro Tachibana", "Francesco Taddia", "Katsutoshi Takaki", "Ken Tateuchi", "Akihiko Tomita", "Dmitry Tsvetkov", "Takahiro Ui", "Nobuharu Ukita", "Yuji Urata", "Emma S. Walker", "Taketoshi Yoshii"]}, "1198": {"id": "1412.4153v1", "title": "The Gaia-ESO Survey: Chromospheric Emission, Accretion Properties, and Rotation in $\u03b3$ Velorum and Chamaeleon I", "url": "http://arxiv.org/pdf/1412.4153v1", "date": "2014-12-12 22:34:43", "abs": "We use the fundamental parameters delivered by the GES consortium in the\nfirst internal data release to select the members of $\\gamma$ Vel and Cha I\namong the UVES and GIRAFFE spectroscopic observations. A total of 140 $\\gamma$\nVel members and 74 Cha I members were studied. We calculated stellar\nluminosities through spectral energy distributions, while stellar masses were\nderived by comparison with evolutionary tracks. The spectral subtraction of\nlow-activity and slowly rotating templates, which are rotationally broadened to\nmatch the $v\\sin i$ of the targets, enabled us to measure the equivalent widths\n(EWs) and the fluxes in the H$\\alpha$ and H$\\beta$ lines. The H$\\alpha$ line\nwas also used for identifying accreting objects and for evaluating the mass\naccretion rate ($\\dot M_{\\rm acc}$). The distribution of $v\\sin i$ for the\nmembers of $\\gamma$ Vel displays a peak at about 10 km s$^{-1}$ with a tail\ntoward faster rotators. There is also some indication of a different $v\\sin i$\ndistribution for the members of its two kinematical populations. Only a handful\nof stars in $\\gamma$ Vel display signatures of accretion, while many more\naccretors were detected in the younger Cha~I. Accreting and active stars occupy\ntwo different regions in a $T_{\\rm eff}$-flux diagram and we propose a\ncriterion for distinguishing them. We derive $\\dot M_{\\rm acc}$ in the ranges\n$10^{-11}$-$10^{-9} M_\\odot$yr$^{-1}$ and $10^{-10}$-$10^{-7} M_\\odot$yr$^{-1}$\nfor $\\gamma$ Vel and Cha I accretors, respectively. We find less scatter in the\n$\\dot M_{\\rm acc}-M_\\star$ relation derived through the H$\\alpha$ EWs, when\ncompared to the H$\\alpha$ $10\\%W$ diagnostics, in agreement with other authors.", "cat": "astro-ph.SR", "authors": ["A. Frasca", "K. Biazzo", "A. C. Lanzafame", "J. M. Alcal\u00e1", "E. Brugaletta", "A. Klutsch", "B. Stelzer", "G. G. Sacco", "L. Spina", "R. D. Jeffries", "D. Montes", "E. J. Alfaro", "G. Barentsen", "R. Bonito", "J. F. Gameiro", "J. Lopez-Santiago", "G. Pace", "L. Pasquini", "L. Prisinzano", "S. G. Sousa", "G. Gilmore", "S. Randich", "G. Micela", "A. Bragaglia", "E. Flaccomio", "A. Bayo", "M. T. Costado", "E. Franciosini", "V. Hill", "A. Hourihane", "P. Jofre'", "C. Lardo", "E. Maiorca", "T. Masseron", "L. Morbidelli", "C. C. Worley"]}, "1199": {"id": "0805.0813v1", "title": "A Large Population of High Redshift Galaxy Clusters in the IRAC Shallow Cluster Survey", "url": "http://arxiv.org/pdf/0805.0813v1", "date": "2008-05-06 23:22:45", "abs": "We have identified 335 galaxy cluster and group candidates spanning 01, and over 60 at z < 0.5 have been\nspectroscopically confirmed. The mean I-[3.6] color for cluster galaxies up to\nz~1 is well matched by a z_f=3 passively evolving model. At z>1, a wider range\nof formation histories is needed, but higher formation redshifts (i.e. z_f \\ge\n4-5) are favored for most clusters. The cluster autocorrelation function,\nmeasured for the first time out to z=1.5, is found not to have evolved over the\nlast 10 Gyr, in agreement with the prediction from LCDM. The average mass of\nthe IRAC Shallow Cluster Survey sample, inferred from its clustering, is ~\n10^14 Msun.", "cat": "astro-ph", "authors": ["Mark Brodwin", "Peter R. Eisenhardt", "Anthony H. Gonzalez", "Adam Stanford", "Daniel Stern", "Leonidas A. Moustakas", "Michael J. I. Brown", "Ranga-Ram Chary", "Audrey Galametz"]}, "1200": {"id": "2207.10682v1", "title": "Probing the Diffuse Lyman-alpha Emission on Cosmological Scales: Ly\u03b1 Emission Intensity Mapping Using the Complete SDSS-IV eBOSS Survey", "url": "http://arxiv.org/pdf/2207.10682v1", "date": "2022-07-21 18:00:03", "abs": "Based on the Sloan Digital Sky Survey Data Release 16, we have detected the\nlarge-scale structure of Ly$\\alpha$ emission in the Universe at redshifts $z =\n2$--3.5 by cross-correlating quasar positions and Ly$\\alpha$ emission imprinted\nin the residual spectra of luminous red galaxies. We apply an analytical model\nto fit the corresponding Ly$\\alpha$ surface brightness profile and multipoles\nof the redshift-space quasar-Ly$\\alpha$ emission cross-correlation function.\nThe model suggests an average cosmic Ly$\\alpha$ luminosity density of\n${6.6_{-3.1}^{+3.3}}\\times 10^{40} {\\rm erg\\, s^{-1} cMpc^{-3}}$, a $\\sim\n2\\sigma$ detection with a median value about 8--9 times those estimated from\ndeep narrowband surveys of Ly$\\alpha$ emitters at similar redshifts. Although\nthe low signal-to-noise ratio prevents us from a significant detection of the\nLy$\\alpha$ forest-Ly$\\alpha$ emission cross-correlation, the measurement is\nconsistent with the prediction of our best-fit model from quasar-Ly$\\alpha$\nemission cross-correlation within current uncertainties. We rule out the\nscenario that these Ly$\\alpha$ photons mainly originate from quasars. We find\nthat Ly$\\alpha$ emission from star-forming galaxies, including contributions\nfrom that concentrated around the galaxy centers and that in the diffuse\nLy$\\alpha$ emitting halos, is able to explain the bulk of the the Ly$\\alpha$\nluminosity density inferred from our measurements. Ongoing and future surveys\ncan further improve the measurements and advance our understanding of the\ncosmic Ly$\\alpha$ emission field.", "cat": "astro-ph.GA", "authors": ["Xiaojing Lin", "Zheng Zheng", "Zheng Cai"]}, "1201": {"id": "2404.00938v2", "title": "How Can Large Language Models Enable Better Socially Assistive Human-Robot Interaction: A Brief Survey", "url": "http://arxiv.org/pdf/2404.00938v2", "date": "2024-04-05 21:55:47", "abs": "Socially assistive robots (SARs) have shown great success in providing\npersonalized cognitive-affective support for user populations with special\nneeds such as older adults, children with autism spectrum disorder (ASD), and\nindividuals with mental health challenges. The large body of work on SAR\ndemonstrates its potential to provide at-home support that complements\nclinic-based interventions delivered by mental health professionals, making\nthese interventions more effective and accessible. However, there are still\nseveral major technical challenges that hinder SAR-mediated interactions and\ninterventions from reaching human-level social intelligence and efficacy. With\nthe recent advances in large language models (LLMs), there is an increased\npotential for novel applications within the field of SAR that can significantly\nexpand the current capabilities of SARs. However, incorporating LLMs introduces\nnew risks and ethical concerns that have not yet been encountered, and must be\ncarefully be addressed to safely deploy these more advanced systems. In this\nwork, we aim to conduct a brief survey on the use of LLMs in SAR technologies,\nand discuss the potentials and risks of applying LLMs to the following three\nmajor technical challenges of SAR: 1) natural language dialog; 2) multimodal\nunderstanding; 3) LLMs as robot policies.", "cat": "cs.HC", "authors": ["Zhonghao Shi", "Ellen Landrum", "Amy O' Connell", "Mina Kian", "Leticia Pinto-Alva", "Kaleen Shrestha", "Xiaoyuan Zhu", "Maja J Matari\u0107"]}, "1202": {"id": "0907.3704v1", "title": "Entropic uncertainty relations - A survey", "url": "http://arxiv.org/pdf/0907.3704v1", "date": "2009-07-21 19:05:25", "abs": "Uncertainty relations play a central role in quantum mechanics. Entropic\nuncertainty relations in particular have gained significant importance within\nquantum information, providing the foundation for the security of many quantum\ncryptographic protocols. Yet, rather little is known about entropic uncertainty\nrelations with more than two measurement settings. In this note we review known\nresults and open questions.", "cat": "quant-ph", "authors": ["Stephanie Wehner", "Andreas Winter"]}, "1203": {"id": "2008.08358v1", "title": "Spatiotemporal mapping of malaria prevalence in Madagascar using routine surveillance and health survey data", "url": "http://arxiv.org/pdf/2008.08358v1", "date": "2020-08-19 10:06:41", "abs": "Malaria transmission in Madagascar is highly heterogeneous, exhibiting\nspatial, seasonal and long-term trends. Previous efforts to map malaria risk in\nMadagascar used prevalence data from Malaria Indicator Surveys. These\ncross-sectional surveys, conducted during the high transmission season most\nrecently in 2013 and 2016, provide nationally representative prevalence data\nbut cover relatively short time frames. Conversely, monthly case data are\ncollected at health facilities but suffer from biases, including incomplete\nreporting.\n We combined survey and case data to make monthly maps of prevalence between\n2013 and 2016. Health facility catchments were estimated and incidence\nsurfaces, environmental and socioeconomic covariates, and survey data informed\na Bayesian prevalence model. Prevalence estimates were consistently high in the\ncoastal regions and low in the highlands. Prevalence was lowest in 2014 and\npeaked in 2015, highlighting the importance of estimates between survey years.\nSeasonality was widely observed. Similar multi-metric approaches may be\napplicable across sub-Saharan Africa.", "cat": "stat.AP", "authors": ["Rohan Arambepola", "Suzanne H. Keddie", "Emma L. Collins", "Katherine A. Twohig", "Punam Amratia", "Amelia Bertozzi-Villa", "Elisabeth G. Chestnutt", "Joseph Harris", "Justin Millar", "Jennifer Rozier", "Susan F. Rumisha", "Tasmin L. Symons", "Camilo Vargas-Ruiz", "Mauricette Andriamananjara", "Saraha Rabeherisoa", "Ars\u00e8ne C. Ratsimbasoa", "Rosalind E. Howes", "Daniel J. Weiss", "Peter W. Gething", "Ewan Cameron"]}, "1204": {"id": "1610.02057v1", "title": "The SINFONI survey of powerful radio galaxies at z~2: Jet-driven AGN feedback during the Quasar Era", "url": "http://arxiv.org/pdf/1610.02057v1", "date": "2016-10-06 20:27:55", "abs": "We present VLT/SINFONI imaging spectroscopy of the warm ionized gas in 33\npowerful radio galaxies at redshifts z>~2, which are excellent sites to study\nthe interplay of rapidly accreting active galactic nuclei and the interstellar\nmedium of the host galaxy in the very late formation stages of massive\ngalaxies. Our targets span two orders of magnitude in radio size (2-400 kpc)\nand kinetic jet energy (a few 10^46 to almost 10^48 erg s^-1). All sources have\ncomplex gas kinematics with broad line widths up to ~1300 km s^-1. About half\nhave bipolar velocity fields with offsets up to 1500 km s^-1 and are consistent\nwith global back-to-back outflows. The others have complex velocity\ndistributions, often with multiple abrupt velocity jumps far from the nucleus\nof the galaxy, and are not associated with a major merger in any obvious way.\nWe present several empirical constraints that show why gas kinematics and radio\njets seem to be physically related. The gas kinetic energy from large scale\nbulk and local outflow or turbulent motion corresponds to a few 10^-3 to 10^-2\nof the kinetic energy of the jet. In galaxies with jet power >~10^47 erg s^-1,\nthe bulk kinetic energy dominates the total energy budget of the gas,\nsuggesting that the outflows encompasses the global interstellar medium,\nperhaps facilitated by the strong gas turbulence. We compare with recent\nhydrodynamic simulations, and discuss the potential consequences for the\nsubsequent evolution of massive high-z galaxies. The gas-phase metallicities in\nour galaxies are lower than in most low-z AGN, but nonetheless solar or even\nsuper-solar, suggesting that the ISM in these galaxies is very similar to the\ngas from which massive low-redshift galaxies formed most of their gas. This\nfurther highlights that we are seeing these galaxies near the end of their\nactive formation phase.", "cat": "astro-ph.GA", "authors": ["N. Nesvadba", "C. De Breuck", "M. D. Lehnert", "P. N. Best", "C. Collet"]}, "1205": {"id": "2302.08210v1", "title": "A Survey of Geometric Optimization for Deep Learning: From Euclidean Space to Riemannian Manifold", "url": "http://arxiv.org/pdf/2302.08210v1", "date": "2023-02-16 10:50:15", "abs": "Although Deep Learning (DL) has achieved success in complex Artificial\nIntelligence (AI) tasks, it suffers from various notorious problems (e.g.,\nfeature redundancy, and vanishing or exploding gradients), since updating\nparameters in Euclidean space cannot fully exploit the geometric structure of\nthe solution space. As a promising alternative solution, Riemannian-based DL\nuses geometric optimization to update parameters on Riemannian manifolds and\ncan leverage the underlying geometric information. Accordingly, this article\npresents a comprehensive survey of applying geometric optimization in DL. At\nfirst, this article introduces the basic procedure of the geometric\noptimization, including various geometric optimizers and some concepts of\nRiemannian manifold. Subsequently, this article investigates the application of\ngeometric optimization in different DL networks in various AI tasks, e.g.,\nconvolution neural network, recurrent neural network, transfer learning, and\noptimal transport. Additionally, typical public toolboxes that implement\noptimization on manifold are also discussed. Finally, this article makes a\nperformance comparison between different deep geometric optimization methods\nunder image recognition scenarios.", "cat": "cs.LG", "authors": ["Yanhong Fei", "Xian Wei", "Yingjie Liu", "Zhengyu Li", "Mingsong Chen"]}, "1206": {"id": "0710.1345v1", "title": "GHASP : an H alpha kinematic survey of spiral and irregular galaxies. V. Dark matter distribution in 36 nearby spiral galaxies", "url": "http://arxiv.org/pdf/0710.1345v1", "date": "2007-10-06 08:13:49", "abs": "The results obtained from a study of the mass distribution of 36 spiral\ngalaxies are presented. The galaxies were observed using Fabry-Perot\ninterferometry as part of the GHASP survey. The main aim of obtaining high\nresolution H alpha 2D velocity fields is to define more accurately the rising\npart of the rotation curves which should allow to better constrain the\nparameters of the mass distribution. The H alpha velocities were combined with\nlow resolution HI data from the literature, when available. Combining the\nkinematical data with photometric data, mass models were derived from these\nrotation curves using two different functional forms for the halo: an\nisothermal sphere and an NFW profile. For the galaxies already modeled by other\nauthors, the results tend to agree. Our results point at the existence of a\nconstant density core in the center of the dark matter halos rather than a\ncuspy core, whatever the type of the galaxy from Sab to Im. This extends to all\ntypes the result already obtained by other authors studying dwarf and LSB\ngalaxies but would necessitate a larger sample of galaxies to conclude more\nstrongly. Whatever model is used (ISO or NFW), small core radius halos have\nhigher central densities, again for all morphological types. We confirm\ndifferent halo scaling laws, such as the correlations between the core radius\nand the central density of the halo with the absolute magnitude of a galaxy:\nlow luminosity galaxies have small core radius and high central density. We\nfind that the product of the central density with the core radius of the dark\nmatter halo is nearly constant, whatever the model and whatever the absolute\nmagnitude of the galaxy. This suggests that the halo surface density is\nindependent from the galaxy type.", "cat": "astro-ph", "authors": ["M. Spano", "M. Marcelin", "P. Amram", "C. Carignan", "B. Epinat", "O. Hernandez"]}, "1207": {"id": "2007.15951v4", "title": "An Empirical Survey of Data Augmentation for Time Series Classification with Neural Networks", "url": "http://arxiv.org/pdf/2007.15951v4", "date": "2021-07-02 09:15:08", "abs": "In recent times, deep artificial neural networks have achieved many successes\nin pattern recognition. Part of this success can be attributed to the reliance\non big data to increase generalization. However, in the field of time series\nrecognition, many datasets are often very small. One method of addressing this\nproblem is through the use of data augmentation. In this paper, we survey data\naugmentation techniques for time series and their application to time series\nclassification with neural networks. We propose a taxonomy and outline the four\nfamilies in time series data augmentation, including transformation-based\nmethods, pattern mixing, generative models, and decomposition methods.\nFurthermore, we empirically evaluate 12 time series data augmentation methods\non 128 time series classification datasets with six different types of neural\nnetworks. Through the results, we are able to analyze the characteristics,\nadvantages and disadvantages, and recommendations of each data augmentation\nmethod. This survey aims to help in the selection of time series data\naugmentation for neural network applications.", "cat": "cs.LG", "authors": ["Brian Kenji Iwana", "Seiichi Uchida"]}, "1208": {"id": "1503.02083v2", "title": "A Periodically Varying Luminous Quasar at z=2 from the Pan-STARRS1 Medium Deep Survey: A Candidate Supermassive Black Hole Binary in the Gravitational Wave-Driven Regime", "url": "http://arxiv.org/pdf/1503.02083v2", "date": "2015-05-21 21:41:20", "abs": "Supermassive black hole binaries (SMBHBs) should be an inevitable consequence\nof the hierarchical growth of massive galaxies through mergers, and the\nstrongest sirens of gravitational waves (GWs) in the cosmos. And yet, their\ndirect detection has remained elusive due to the compact (sub-parsec) orbital\nseparations of gravitationally bound SMBHBs. Here we exploit a theoretically\npredicted signature of a SMBHB in the time domain: periodic variability caused\nby a mass accretion rate that is modulated by the binary's orbital motion. We\nreport our first significant periodically varying quasar detection from the\nsystematic search in the Pan-STARRS1 (PS1) Medium Deep Survey. Our SMBHB\ncandidate, PSO J334.2028+01.4075, is a luminous radio-loud quasar at $z=2.060$,\nwith extended baseline photometry from the Catalina Real-Time Transient Survey,\nas well as archival spectroscopy from the FIRST Bright Quasar Survey. The\nobserved period ($542 \\pm 15$ days) and estimated black hole mass ($\\log\n(M_{\\rm BH}/M_\\odot) = 9.97 \\pm 0.50$), correspond to an orbital separation of\n$7^{+8}_{-4}$ Schwarzschild radii ($\\sim 0.006^{+0.007}_{-0.003}$ pc), assuming\nthe rest-frame period of the quasar variability traces the orbital period of\nthe binary. This SMBHB candidate, discovered at the peak redshift for SMBH\nmergers, is in a physically stable configuration for a circumbinary accretion\ndisk, and within the regime of GW-driven orbital decay. Our search with PS1 is\na benchmark study for the exciting capabilities of LSST, which will have orders\nof magnitude larger survey power, and will potentially pinpoint the locations\nof thousands of SMBHBs in the variable night sky.", "cat": "astro-ph.HE", "authors": ["Tingting Liu", "Suvi Gezari", "Sebastien Heinis", "Eugene A. Magnier", "William S. Burgett", "Kenneth Chambers", "Heather Flewelling", "Mark Huber", "Klaus W. Hodapp", "Nicholas Kaiser", "Rolf-Peter Kudritzki", "John L. Tonry", "Richard J. Wainscoat", "Christopher Waters"]}, "1209": {"id": "0804.1604v1", "title": "Pair Analysis of Field Galaxies from the Red-Sequence Cluster Survey", "url": "http://arxiv.org/pdf/0804.1604v1", "date": "2008-04-10 03:34:51", "abs": "We study the evolution of the number of close companions of similar\nluminosities per galaxy (Nc) by choosing a volume-limited subset of the\nphotometric redshift catalog from the Red-Sequence Cluster Survey (RCS-1). The\nsample contains over 157,000 objects with a moderate redshift range of 0.25 < z\n< 0.8 and absolute magnitude in Rc (M_Rc) < -20. This is the largest sample\nused for pair evolution analysis, providing data over 9 redshift bins with\nabout 17,500 galaxies in each. After applying incompleteness and projection\ncorrections, Nc shows a clear evolution with redshift. The Nc value for the\nwhole sample grows with redshift as (1+z)^m, where m = 2.83 +/- 0.33 in good\nagreement with N-body simulations in a LCDM cosmology. We also separate the\nsample into two different absolute magnitude bins: -25 < M_Rc < -21 and -21 <\nM_Rc < -20, and find that the brighter the absolute magnitude, the smaller the\nm value. Furthermore, we study the evolution of the pair fraction for different\nprojected separation bins and different luminosities. We find that the m value\nbecomes smaller for larger separation, and the pair fraction for the fainter\nluminosity bin has stronger evolution. We derive the major merger remnant\nfraction f_rem = 0.06, which implies that about 6% of galaxies with -25 < M_Rc\n< -20 have undergone major mergers since z = 0.8.", "cat": "astro-ph", "authors": ["B. C. Hsieh", "H. K. C. Yee", "H. Lin", "M. D. Gladders", "D. G. Gilbank"]}, "1210": {"id": "1104.3914v1", "title": "Cool White Dwarfs Found in the UKIRT Infrared Deep Sky Survey", "url": "http://arxiv.org/pdf/1104.3914v1", "date": "2011-04-20 01:45:45", "abs": "We present the results of a search for cool white dwarfs in the United\nKingdom InfraRed Telescope (UKIRT) Infrared Deep Sky Survey (UKIDSS) Large Area\nSurvey (LAS). The UKIDSS LAS photometry was paired with the Sloan Digital Sky\nSurvey (SDSS) to identify cool hydrogen-rich white dwarf candidates by their\nneutral optical colors and blue near-infrared colors, as well as faint Reduced\nProper Motion magnitudes. Optical spectroscopy was obtained at Gemini\nObservatory, and showed the majority of the candidates to be newly identified\ncool degenerates, with a small number of G- to K-type (sub)dwarf contaminants.\nOur initial search of 280 deg2 of sky resulted in seven new white dwarfs with\neffective temperature T_eff ~ 6000 K. The current followup of 1400 deg2 of sky\nhas produced thirteen new white dwarfs. Model fits to the photometry show that\nseven of the newly identified white dwarfs have 4120 K <= T_eff <= 4480 K, and\ncooling ages between 7.3 Gyr and 8.7 Gyr; they have 40 km/s <= v_tan <= 85 km/s\nand are likely to be thick disk 10-11 Gyr-old objects. The other half of the\nsample has 4610 K <= T_eff <= 5260 K, cooling ages between 4.3 Gyr and 6.9 Gyr,\nand 60 km/s <= v_tan <= 100 km/s. These are either thin disk remnants with\nunusually high velocities, or lower-mass remnants of thick disk or halo late-F\nor G stars.", "cat": "astro-ph.SR", "authors": ["S. K. Leggett", "N. Lodieu", "P. -E. Tremblay", "P. Bergeron", "A. Nitta"]}, "1211": {"id": "0909.3761v2", "title": "The AGN component in deep radio fields: Results from the First Look Survey", "url": "http://arxiv.org/pdf/0909.3761v2", "date": "2010-08-29 12:55:49", "abs": "We are currently exploiting the deep radio/optical/IR information available\nfor the extra-galactic component of the Spitzer First Look Survey (FLS) to\ninvestigate the physical properties of faint radio-selected AGNs, with the aim\nof studying the AGN component of sub-mJy radio fields. One of the key\nunresolved issues is whether, as a function of cosmic epoch, low-power AGNs are\nmore related to efficiently accreting systems (mostly radio-quiet) or to\nsystems with very low accretion rates (mostly radio-loud). Here we present a\nsample of optically identified radio-emitting AGNs extracted from the FLS.\nPreliminary results show that at the flux densities probed by the FLS (S(1.4\nGHz)> 100 microJy) we still have a significant number of radio-loud AGNs,\nsimilarly to what found in 'brighter' sub-mJy radio samples. Very\ninterestingly, however, we have also a clear and direct evidence of a\npopulation of radio-emitting AGNs in the FLS, whose properties are consistent\nwith those expected from existing radio-quiet AGN modeling. Such AGNs could be\nrecognised as such thanks to the availability of IR colors which proved to be\nespecially useful to efficiently separate radio sources triggered by AGNs, from\nsources triggered by star-formation. This latter result supports the idea that\nradio-quiet AGNs are not necessarily radio silent, and very promisingly may\nindicate that the bulk of the radio-quiet AGN population could emerge from\nstudies of deeper radio samples.", "cat": "astro-ph.CO", "authors": ["I. Prandoni", "R. Morganti", "A. Mignano"]}, "1212": {"id": "1410.6212v1", "title": "Sample of optically unidentified X-ray binaries in the Galactic bulge. Constraints on the physical nature from infrared photometric surveys", "url": "http://arxiv.org/pdf/1410.6212v1", "date": "2014-10-22 23:35:16", "abs": "We report on the archival near-infrared and mid-infrared observations of 7\npersistent X-ray sources situated in the Galactic bulge using data from the\nUKIRT Infrared Deep Sky Survey (UKIDSS), Spitzer Galactic Legacy Infrared\nMid-Plane Survey Extraordinaire (GLIMPSE) and the Wide-field Infrared Survey\nExplorer (WISE) all-sky survey. We were able to successfully identify, or\nprovide upper flux limits for the systems SAX J1747.0-2853, IGR J17464-2811, AX\nJ1754.2-2754, IGR J17597-2201, IGR J18134-1636, IGR J18256-1035, Ser X-1 and\nconstrain the nature of these systems. In the case of IGR J17597-2201 we\npresent arguments that the source accretes matter from the stellar wind rather\nthan via Roche lobe overflow of the secondary. We suggest that, at its X-ray\nluminosity of $10^{34-35}$ erg s$^{-1}$, we are probing the poorly known class\nof wind-fed low-mass X-ray binaries (LMXBs).", "cat": "astro-ph.HE", "authors": ["Ivan Zolotukhin", "Mikhail Revnivtsev"]}, "1213": {"id": "1111.6728v1", "title": "A multiwavelength study of the IRAS Deep Survey galaxy sample III. Spectral classification and dynamical properties", "url": "http://arxiv.org/pdf/1111.6728v1", "date": "2011-11-29 08:42:03", "abs": "The infrared deep sample (IDS), in the north ecliptical polar region (NEPR),\nis the first complete, far--IR selected sample, on which numerous studies of\ngalaxy evolution are based. Here we present and analyze the spectral\nclassification of several galaxies in the IDS sample together with rotation\ncurves which allow estimating the lower mass limits of a subsample of objects.\nWe measured fluxes and intensity ratios of the emission lines in the visible\nregion of the spectrum (lambda 4000-9000 A) for 75 galaxy members. Moreover,\nfor some of them (55%), the spectra obtained with the Keck II telescope have\nsufficient wavelength and spatial resolution to derive their rotation curve.\nThese galaxies turn out to be disk like systems, with a high fraction (~50%) of\ninteracting systems. The spectroscopic classification of 42 galaxies, using the\nemission-line ratio diagnostic diagrams, shows that the NEPR sample is\npredominantly composed of starburst galaxies (71%), while the fraction of AGNs\n(7%) and LINERs (21%) is small. The dynamical analysis allows us to estimate\nthe lower mass limits of 39 galaxies. The rest-frame FIR luminosity\ndistribution of these galaxies spans the same range as that of the FIR selected\ncomplete sample, i.e. three orders of magnitude, with the same mean value,\nlog(L_FIR)=10.2. This emphasizes that such galaxies represent FIR properties of\nthe whole sample well. Moreover, their optical properties are typical of the\nsample itself since 62% of these belong to the 60mu selected complete sample.", "cat": "astro-ph.CO", "authors": ["D. Bettoni", "P. Mazzei", "A. della Valle"]}, "1214": {"id": "2404.06234v1", "title": "The Rubin Observatory's Legacy Survey of Space and Time DP0.2 processing campaign at CC-IN2P3", "url": "http://arxiv.org/pdf/2404.06234v1", "date": "2024-04-09 11:53:47", "abs": "The Vera C. Rubin Observatory, currently in construction in Chile, will start\nperforming the Legacy Survey of Space and Time (LSST) in 2025 for 10 years. Its\n8.4-meter telescope will survey the southern sky in less than 4 nights in six\noptical bands, and repeatedly generate about 2 000 exposures per night,\ncorresponding to a data volume of about 20 TiB every night. Three data\nfacilities are preparing to contribute to the production of the annual data\nreleases: the US Data Facility will process 35% of the raw data, the UK data\nfacility will process 25% of the raw data and the French data facility,\noperated by CC-IN2P3, will locally process the remaining 40% of the raw data.\nIn the context of the Data Preview 0.2 (DP0.2), the Data Release Production\npipelines have been executed on the DC-2 simulated dataset (generated by the\nDark Energy Science Collaboration, DESC). This dataset includes 20 000\nsimulated exposures, representing 300 square degrees of Rubin images with a\ntypical depth of 5 years. DP0.2 ran at the Interim Data Facility (based on\nGoogle cloud), and the full exercise was independently replicated at CC-IN2P3.\nDuring this exercise, 3 PiB of data and more than 200 million files were\nproduced. In this contribution we will present a detailed description of the\nsystem that we set up to perform this processing campaign using CC-IN2P3's\ncomputing and storage infrastructure. Several topics will be addressed:\nworkflow generation and execution, batch job submission, memory and I/O\nrequirements, etc. We will focus on the issues that arose during this campaign\nand how we addressed them and will present some perspectives after this\nexercise.", "cat": "astro-ph.IM", "authors": ["Quentin Le Boulc'h", "Fabio Hernandez", "Gabriele Mainetti"]}, "1215": {"id": "1710.06902v1", "title": "The Survey of Water and Ammonia in the Galactic Center (SWAG): Molecular Cloud Evolution in the Central Molecular Zone", "url": "http://arxiv.org/pdf/1710.06902v1", "date": "2017-10-18 19:28:40", "abs": "The Survey of Water and Ammonia in the Galactic Center (SWAG) covers the\nCentral Molecular Zone (CMZ) of the Milky Way at frequencies between 21.2 and\n25.4 GHz obtained at the Australia Telescope Compact Array at $\\sim 0.9$ pc\nspatial and $\\sim 2.0$ km s$^{-1}$ spectral resolution. In this paper, we\npresent data on the inner $\\sim 250$ pc ($1.4^\\circ$) between Sgr C and Sgr B2.\nWe focus on the hyperfine structure of the metastable ammonia inversion lines\n(J,K) = (1,1) - (6,6) to derive column density, kinematics, opacity and kinetic\ngas temperature. In the CMZ molecular clouds, we find typical line widths of\n$8-16$ km s$^{-1}$ and extended regions of optically thick ($\\tau > 1$)\nemission. Two components in kinetic temperature are detected at $25-50$ K and\n$60-100$ K, both being significantly hotter than dust temperatures throughout\nthe CMZ. We discuss the physical state of the CMZ gas as traced by ammonia in\nthe context of the orbital model by Kruijssen et al. (2015) that interprets the\nobserved distribution as a stream of molecular clouds following an open\neccentric orbit. This allows us to statistically investigate the time\ndependencies of gas temperature, column density and line width. We find heating\nrates between $\\sim 50$ and $\\sim 100$ K Myr$^{-1}$ along the stream orbit. No\nstrong signs of time dependence are found for column density or line width.\nThese quantities are likely dominated by cloud-to-cloud variations. Our results\nqualitatively match the predictions of the current model of tidal triggering of\ncloud collapse, orbital kinematics and the observation of an evolutionary\nsequence of increasing star formation activity with orbital phase.", "cat": "astro-ph.GA", "authors": ["Nico Krieger", "J\u00fcrgen Ott", "Henrik Beuther", "Fabian Walter", "J. M. Diederik Kruijssen", "David S. Meier", "Elisabeth A. C. Mills", "Yanett Contreras", "Phil Edwards", "Adam Ginsburg", "Christian Henkel", "Jonathan Henshaw", "James Jackson", "Jens Kauffmann", "Steven Longmore", "Sergio Martin", "Mark R. Morris", "Thushara Pillai", "Matthew Rickert", "Erik Rosolowsky", "Hiroko Shinnaga", "Andrew Walsh", "Farhad Yusef-Zadeh", "Qizhou Zhang"]}, "1216": {"id": "2208.00085v3", "title": "Machine Learning and Computer Vision Techniques in Continuous Beehive Monitoring Applications: A survey", "url": "http://arxiv.org/pdf/2208.00085v3", "date": "2023-09-14 14:45:30", "abs": "Wide use and availability of the machine learning and computer vision\ntechniques allows development of relatively complex monitoring systems in many\ndomains. Besides the traditional industrial domain, new application appears\nalso in biology and agriculture, where we could speak about the detection of\ninfections, parasites and weeds, but also about automated monitoring and early\nwarning systems. This is also connected with the introduction of the easily\naccessible hardware and development kits such as Arduino, or RaspberryPi\nfamily. In this paper, we survey 50 existing papers focusing on the methods of\nautomated beehive monitoring methods using the computer vision techniques,\nparticularly on the pollen and Varroa mite detection together with the bee\ntraffic monitoring. Such systems could also be used for the monitoring of the\nhoneybee colonies and for the inspection of their health state, which could\nidentify potentially dangerous states before the situation is critical, or to\nbetter plan periodic bee colony inspections and therefore save significant\ncosts. Later, we also include analysis of the research trends in this\napplication field and we outline the possible direction of the new\nexplorations. Our paper is aimed also at veterinary and apidology professionals\nand experts, who might not be familiar with machine learning to introduce them\nto its possibilities, therefore each family of applications is opened by a\nbrief theoretical introduction and motivation related to its base method. We\nhope that this paper will inspire other scientists to use machine learning\ntechniques for other applications in beehive monitoring.", "cat": "cs.CV", "authors": ["Simon Bilik", "Tomas Zemcik", "Lukas Kratochvila", "Dominik Ricanek", "Milos Richter", "Sebastian Zambanini", "Karel Horak"]}, "1217": {"id": "2310.18575v1", "title": "The Milky Way Bulge extra-tidal star survey: BH 261 (AL 3)", "url": "http://arxiv.org/pdf/2310.18575v1", "date": "2023-10-28 03:29:13", "abs": "The Milky Way Bulge extra-tidal star survey (MWBest) is a spectroscopic\nsurvey with the goal of identifying stripped globular cluster stars from inner\nGalaxy clusters. In this way, an indication of the fraction of metal-poor bulge\nstars that originated from globular clusters can be determined. We observed and\nanalyzed stars in and around BH 261, an understudied globular cluster in the\nbulge. From seven giants within the tidal radius of the cluster, we measured an\naverage heliocentric radial velocity of = -61 +- 2.6 km/s with a radial\nvelocity dispersion of \\sigma = 6.1 +- 1.9 km/s. The large velocity dispersion\nmay have arisen from tidal heating in the cluster's orbit about the Galactic\ncenter, or because BH 261 has a high dynamical mass as well as a high\nmass-to-light ratio. From spectra of five giants, we measure an average\nmetallicity of <[Fe/H]> = -1.1 +- 0.2 dex. We also spectroscopically confirm an\nRR Lyrae star in BH 261, which yields a distance to the cluster of 7.1 +-\n0.4~kpc. Stars with 3D velocities and metallicities consistent with BH 261\nreaching to ~0.5 degrees from the cluster are identified. A handful of these\nstars are also consistent with the spatial distribution of that potential\ndebris from models focussing on the most recent disruption of the cluster.", "cat": "astro-ph.GA", "authors": ["Andrea Kunder", "Zdenek Prudil", "Kevin Covey", "Joanne Hughes", "Meridith Joyce", "Iulia T. Simion", "Rebekah Kuss", "Carlos Campos", "Christian I. Johnson", "Catherine A. Pilachowski", "Kristen A. Larson", "Andreas J. Koch-Hansen", "Tommaso Marchetti", "Michael R. Rich", "Evan Butler", "William I. Clarkson", "Michael J. Rivet", "Kathryn Devine", "A. Katherina Vivas", "Gabriel I. Perren", "Mario Soto", "Erika Silva"]}, "1218": {"id": "2204.12759v1", "title": "Li-rich Giants in LAMOST Survey. III. The statistical analysis of Li-rich giants", "url": "http://arxiv.org/pdf/2204.12759v1", "date": "2022-04-27 08:16:55", "abs": "The puzzle of Li-rich giant is still unsolved, contradicting the prediction\nof the standard stellar models. Although the exact evolutionary stages play a\nkey role in the knowledge of Li-rich giants, a limited number of Li-rich giants\nhave been taken with high-quality asteroseismic parameters to clearly\ndistinguish the stellar evolutionary stages. Based on the LAMOST Data Release 7\n(DR7), we applied a data-driven neural network method to derive the parameters\nfor giant stars, which contain the largest number of Li-rich giants. The red\ngiant stars are classified into three stages of Red Giant Branch (RGB), Primary\nRed Clump (PRC), and Secondary Red Clump (SRC) relying on the estimated\nasteroseismic parameters. In the statistical analysis of the properties (i.e.\nstellar mass, carbon, nitrogen, Li-rich distribution, and frequency) of Li-rich\ngiants, we found that: (1) Most of the Li-rich RGB stars are suggested to be\nthe descendants of Li-rich pre-RGB stars and/or the result of engulfment of\nplanet or substellar companions; (2) The massive Li-rich SRC stars could be the\nnatural consequence of Li depletion from the high-mass Li-rich RGB stars. (3)\nInternal mixing processes near the helium flash can account for the phenomenon\nof Li-rich on PRC that dominated the Li-rich giants. Based on the comparison of\n[C/N] distributions between Li-rich and normal PRC stars, the Li-enriched\nprocesses probably depend on the stellar mass.", "cat": "astro-ph.SR", "authors": ["Yutao Zhou", "Chun Wang", "Hongliang Yan", "Yang Huang", "Bo Zhang", "Yuan-Sen Ting", "Huawei Zhang", "Jianrong Shi"]}, "1219": {"id": "1803.02373v2", "title": "The SLUGGS Survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to $\\sim$4 effective radii", "url": "http://arxiv.org/pdf/1803.02373v2", "date": "2018-05-25 01:22:20", "abs": "We apply the Jeans Anisotropic MGE (JAM) dynamical modelling method to SAGES\nLegacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type\ngalaxies in the stellar mass range $10^{10}10^{10.7}{\\rm M}_{\\odot}$ in the Magneticum simulations, we\nidentify a significant anticorrelation between total-mass density profile\nslopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas\nthis anticorrelation is weaker for lower stellar masses, implying that the\nmeasured total mass density slopes for low-mass galaxies are less likely to be\ndetermined by merger activity.", "cat": "astro-ph.GA", "authors": ["Sabine Bellstedt", "Duncan A. Forbes", "Aaron J. Romanowsky", "Rhea-Silvia Remus", "Adam R. H. Stevens", "Jean P. Brodie", "Adriano Poci", "Richard McDermid", "Adebusola Alabi", "Leonie Chevalier", "Caitlin Adams", "Anna Ferr\u00e9-Mateu", "Asher Wasserman", "Viraj Pandya"]}, "1220": {"id": "2407.03993v1", "title": "A Survey on Natural Language Counterfactual Generation", "url": "http://arxiv.org/pdf/2407.03993v1", "date": "2024-07-04 15:13:59", "abs": "Natural Language Counterfactual generation aims to minimally modify a given\ntext such that the modified text will be classified into a different class. The\ngenerated counterfactuals provide insight into the reasoning behind a model's\npredictions by highlighting which words significantly influence the outcomes.\nAdditionally, they can be used to detect model fairness issues or augment the\ntraining data to enhance the model's robustness. A substantial amount of\nresearch has been conducted to generate counterfactuals for various NLP tasks,\nemploying different models and methodologies. With the rapid growth of studies\nin this field, a systematic review is crucial to guide future researchers and\ndevelopers. To bridge this gap, this survey comprehensively overview textual\ncounterfactual generation methods, particularly including those based on Large\nLanguage Models. We propose a new taxonomy that categorizes the generation\nmethods into four groups and systematically summarize the metrics for\nevaluating the generation quality. Finally, we discuss ongoing research\nchallenges and outline promising directions for future work.", "cat": "cs.CL", "authors": ["Yongjie Wang", "Xiaoqi Qiu", "Yu Yue", "Xu Guo", "Zhiwei Zeng", "Yuhong Feng", "Zhiqi Shen"]}, "1221": {"id": "0803.2591v1", "title": "The 2dF Redshift Survey II: UGC 8584 - Redshift Periodicity and Rings", "url": "http://arxiv.org/pdf/0803.2591v1", "date": "2008-03-18 10:45:45", "abs": "UGC 8584 was selected by a computer program as having a number of quasars\naround it that obeyed the Karlsson periodicity in its reference frame. On\ncloser examination 9 of the nearest 10 quasars turned out to be extremely close\nto the predicted values. Also it turned out that UGC 8584 was a disturbed\ntriple galaxy and a strong triple radio source as well as being a strong\nmillimeter and infrared source. Evidence for present ejection velocities of\n$z_v \\sim .01$ for the associated quasars is present and some pairing of\nejections is noted.\n A new and important result emerges from this sample of galaxy/quasar\nfamilies, namely that rings and shells of galaxies and quasars tend to surround\ngalaxies which have active nuclei. Test cases suggest obscuration of the\nbackground around these galaxies out to about 20' or beyond. Because incidents\nof strong reddening are not observed, obscuring particles are suggested to be\nlarge compared to optical wavelengths. In principle, material ejected with the\nquasars could be of sizes of gravel or larger.", "cat": "astro-ph", "authors": ["H. Arp", "C. Fulton"]}, "1222": {"id": "1901.07119v2", "title": "Dark Energy Survey Year 1 Results: Calibration of Cluster Mis-centering in the redMaPPer Catalogs", "url": "http://arxiv.org/pdf/1901.07119v2", "date": "2019-06-01 21:52:02", "abs": "The center determination of a galaxy cluster from an optical cluster finding\nalgorithm can be offset from theoretical prescriptions or $N$-body definitions\nof its host halo center. These offsets impact the recovered cluster statistics,\naffecting both richness measurements and the weak lensing shear profile around\nthe clusters. This paper models the centering performance of the \\RM~cluster\nfinding algorithm using archival X-ray observations of \\RM-selected clusters.\nAssuming the X-ray emission peaks as the fiducial halo centers, and through\nanalyzing their offsets to the \\RM~centers, we find that $\\sim 75\\pm 8 \\%$ of\nthe \\RM~clusters are well centered and the mis-centered offset follows a Gamma\ndistribution in normalized, projected distance. These mis-centering offsets\ncause a systematic underestimation of cluster richness relative to the\nwell-centered clusters, for which we propose a descriptive model. Our results\nenable the DES Y1 cluster cosmology analysis by characterizing the necessary\ncorrections to both the weak lensing and richness abundance functions of the\nDES Y1 redMaPPer cluster catalog.", "cat": "astro-ph.CO", "authors": ["Y. Zhang", "T. Jeltema", "D. L. Hollowood", "S. Everett", "E. Rozo", "A. Farahi", "A. Bermeo", "S. Bhargava", "P. Giles", "A. K. Romer", "R. Wilkinson", "E. S. Rykoff", "A. Mantz", "H. T. Diehl", "A. E. Evrard", "C. Stern", "D. Gruen", "A. von der Linden", "M. Splettstoesser", "X. Chen", "M. Costanzi", "S. Allen", "C. Collins", "M. Hilton", "M. Klein", "R. G. Mann", "M. Manolopoulou", "G. Morris", "J. Mayers", "M. Sahlen", "J. Stott", "C. Vergara Cervantes", "P. T. P. Viana", "R. H. Wechsler", "S. Allam", "S. Avila", "K. Bechtol", "E. Bertin", "D. Brooks", "D. L. Burke", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "F. J. Castander", "L. N. da Costa", "J. De Vicente", "S. Desai", "J. P. Dietrich", "P. Doel", "B. Flaugher", "P. Fosalba", "J. Frieman", "J. Garc\u00eda-Bellido", "E. Gaztanaga", "R. A. Gruendl", "J. Gschwend", "G. Gutierrez", "W. G. Hartley", "K. Honscheid", "B. Hoyle", "E. Krause", "K. Kuehn", "N. Kuropatkin", "M. Lima", "M. A. G. Maia", "J. L. Marshall", "P. Melchior", "F. Menanteau", "C. J. Miller", "R. Miquel", "R. L. C. Ogando", "A. A. Plazas", "E. Sanchez", "V. Scarpine", "R. Schindler", "S. Serrano", "I. Sevilla-Noarbe", "M. Smith", "M. Soares-Santos", "E. Suchyta", "M. E. C. Swanson", "G. Tarle", "D. Thomas", "D. L. Tucker", "V. Vikram", "W. Wester"]}, "1223": {"id": "1705.05451v1", "title": "VICS82: the VISTA-CFHT Stripe 82 near-infrared survey", "url": "http://arxiv.org/pdf/1705.05451v1", "date": "2017-05-15 20:57:07", "abs": "We present the VISTA-CFHT Stripe 82 (VICS82) survey: a near-infrared (J+Ks)\nsurvey covering 150 square degrees of the Sloan Digital Sky Survey (SDSS)\nequatorial Stripe 82 to an average depth of J=21.9 AB mag and Ks=21.4 AB mag\n(80% completeness limits; 5-sigma point source depths are approximately 0.5 mag\nbrighter). VICS82 contributes to the growing legacy of multi-wavelength data in\nthe Stripe 82 footprint. The addition of near-infrared photometry to the\nexisting SDSS Stripe 82 coadd ugriz photometry reduces the scatter in stellar\nmass estimates to delta log(M_stellar)~0.3 dex for galaxies with\nM_stellar>10^9M_sun at z~0.5, and offers improvement compared to optical-only\nestimates out to z~1, with stellar masses constrained within a factor of\napproximately 2.5. When combined with other multi-wavelength imaging of the\nStripe, including moderate-to-deep ultraviolet (GALEX), optical and\nmid-infrared (Spitzer IRAC) coverage, as well as tens of thousands of\nspectroscopic redshifts, VICS82 gives access to approximately 0.5 Gpc^3 of\ncomoving volume. Some of the main science drivers of VICS82 include (a)\nmeasuring the stellar mass function of L^star galaxies out to z~1; (b)\ndetecting intermediate redshift quasars at 24$). From these SEDs it is, in principle, through SED fitting\npossible to infer key physical properties, including stellar masses, star\nformation rates, and dust attenuation. These in turn can be compared with the\npredictions of galaxy formation simulations allowing us to validate and refine\nthe incorporated physics. However, the inference of physical properties,\nparticularly from photometry alone, can lead to large uncertainties and\npotential biases. Instead, it is now possible, and common, for simulations to\nbe \\emph{forward-modelled} to yield synthetic observations that can be compared\ndirectly to real observations. In this work, we measure the JWST broadband\nfluxes and colours of a robust sample of $58$ the distributions differ somewhat, though our\nobserved sample size is small and thus susceptible to statistical fluctuations.\nLikewise, the predicted and observed colour evolution show broad agreement, at\nleast at $58$, though, again, the sample\nsize is small here.", "cat": "astro-ph.GA", "authors": ["Stephen M. Wilkins", "Jack C. Turner", "Micaela B. Bagley", "Steven L. Finkelstein", "Ricardo O. Amor\u00edn", "Adrien Aufan Stoffels D Hautefort", "Peter Behroozi", "Rachana Bhatawdekar", "Avishai Dekel", "James Donnellan", "Nicole E. Drakos", "Flaminia Fortuni", "Nimish P. Hathi", "Michaela Hirschmann", "Benne W. Holwerda", "Dimitrios Irodotou", "Anton M. Koekemoer", "Christopher C. Lovell", "Emiliano Merlin", "Will J. Roper", "Louise T. C. Seeyave", "Aswin P. Vijayan", "L. Y. Aaron Yung"]}, "1226": {"id": "0804.4226v3", "title": "Potentially $K_{m}-G$-graphical Sequences: A Survey", "url": "http://arxiv.org/pdf/0804.4226v3", "date": "2009-09-30 00:17:52", "abs": "The set of all non-increasing nonnegative integers sequence $\\pi=$\n ($d(v_1),$ $d(v_2),$ $...,$ $d(v_n)$) is denoted by $NS_n$.\n A sequence $\\pi\\in NS_n$ is said to be graphic if it is the degree sequence\nof a simple graph $G$ on $n$ vertices, and such a graph $G$ is called a\nrealization of $\\pi$. The set of all graphic sequences in $NS_n$ is denoted by\n$GS_n$. A graphical sequence $\\pi$ is potentially $H$-graphical if there is a\nrealization of $\\pi$ containing $H$ as a subgraph, while $\\pi$ is forcibly\n$H$-graphical if every realization of $\\pi$ contains $H$ as a subgraph. Let\n$K_k$ denote a complete graph on $k$ vertices. Let $K_{m}-H$ be the graph\nobtained from $K_{m}$ by removing the edges set $E(H)$ of the graph $H$ ($H$ is\na subgraph of $K_{m}$). This paper summarizes briefly some recent results on\npotentially $K_{m}-G$-graphic sequences and give a useful classification for\ndetermining $\\sigma(H,n)$.", "cat": "math.CO", "authors": ["Chunhui Lai", "Lili Hu"]}, "1227": {"id": "0905.4125v1", "title": "Luminosity Functions of Type Ia Supernovae and their Host Galaxies from the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/0905.4125v1", "date": "2009-05-26 06:53:38", "abs": "The sample of 137 low-redshift type Ia supernovae with 0.05 < z < 0.3\nobtained from the SDSS-II Supernova Survey for the southern equatorial stripe\nof 300 square degrees is used to derive the luminosity functions of type Ia\nsupernovae and of their host galaxies in the gri passbands. We show that the\nluminosity function of type Ia supernova host galaxies matches well with that\nof galaxies in the general field, suggesting that the occurrence of type Ia\nsupernovae does not favour a particular type of galaxies but is predominantly\nproportional to the luminosity of galaxies. The only evidence that points to\npossible correlation between the supernova rate and star formation activity is\nthat the supernova rate in late-type galaxies is higher than that in early-type\ngalaxies by 31+/-35%. The sample contains 8 type Ia supernovae whose host\ngalaxies were not identified, but it is shown that their occurrence is\nconsistent with them occurred in low luminous galaxies beyond the survey. The\nluminosity function of type Ia supernovae is approximately Gaussian with the\nfull-width half maximum being a factor of 1.4 in luminosity. The Gaussian\ndistribution becomes tighter if the ratio of extinction to reddening, R_V, is\nlower than the characteristic value for the Milky Way and if luminosity is\ncorrected for the light curve shape. The colour excess is ~0.07 mag which is\nsignificantly smaller than reddening expected for field galaxies. This colour\nexcess does not vary with the distance of the supernovae from the centre of the\nhost galaxy to 15 kpc. This suggests that the major part of the colour excess\nappears to be either intrinsic or reddening that arises in the immediate\nenvironment of supernova, rather than interstellar reddening in host galaxies.", "cat": "astro-ph.CO", "authors": ["N. Yasuda", "M. Fukugita"]}, "1228": {"id": "1712.04301v2", "title": "Deep Learning for IoT Big Data and Streaming Analytics: A Survey", "url": "http://arxiv.org/pdf/1712.04301v2", "date": "2018-06-05 03:30:38", "abs": "In the era of the Internet of Things (IoT), an enormous amount of sensing\ndevices collect and/or generate various sensory data over time for a wide range\nof fields and applications. Based on the nature of the application, these\ndevices will result in big or fast/real-time data streams. Applying analytics\nover such data streams to discover new information, predict future insights,\nand make control decisions is a crucial process that makes IoT a worthy\nparadigm for businesses and a quality-of-life improving technology. In this\npaper, we provide a thorough overview on using a class of advanced machine\nlearning techniques, namely Deep Learning (DL), to facilitate the analytics and\nlearning in the IoT domain. We start by articulating IoT data characteristics\nand identifying two major treatments for IoT data from a machine learning\nperspective, namely IoT big data analytics and IoT streaming data analytics. We\nalso discuss why DL is a promising approach to achieve the desired analytics in\nthese types of data and applications. The potential of using emerging DL\ntechniques for IoT data analytics are then discussed, and its promises and\nchallenges are introduced. We present a comprehensive background on different\nDL architectures and algorithms. We also analyze and summarize major reported\nresearch attempts that leveraged DL in the IoT domain. The smart IoT devices\nthat have incorporated DL in their intelligence background are also discussed.\nDL implementation approaches on the fog and cloud centers in support of IoT\napplications are also surveyed. Finally, we shed light on some challenges and\npotential directions for future research. At the end of each section, we\nhighlight the lessons learned based on our experiments and review of the recent\nliterature.", "cat": "cs.NI", "authors": ["Mehdi Mohammadi", "Ala Al-Fuqaha", "Sameh Sorour", "Mohsen Guizani"]}, "1229": {"id": "2202.08772v1", "title": "A Survey of Knowledge-Intensive NLP with Pre-Trained Language Models", "url": "http://arxiv.org/pdf/2202.08772v1", "date": "2022-02-17 17:17:43", "abs": "With the increasing of model capacity brought by pre-trained language models,\nthere emerges boosting needs for more knowledgeable natural language processing\n(NLP) models with advanced functionalities including providing and making\nflexible use of encyclopedic and commonsense knowledge. The mere pre-trained\nlanguage models, however, lack the capacity of handling such\nknowledge-intensive NLP tasks alone. To address this challenge, large numbers\nof pre-trained language models augmented with external knowledge sources are\nproposed and in rapid development. In this paper, we aim to summarize the\ncurrent progress of pre-trained language model-based knowledge-enhanced models\n(PLMKEs) by dissecting their three vital elements: knowledge sources,\nknowledge-intensive NLP tasks, and knowledge fusion methods. Finally, we\npresent the challenges of PLMKEs based on the discussion regarding the three\nelements and attempt to provide NLP practitioners with potential directions for\nfurther research.", "cat": "cs.CL", "authors": ["Da Yin", "Li Dong", "Hao Cheng", "Xiaodong Liu", "Kai-Wei Chang", "Furu Wei", "Jianfeng Gao"]}, "1230": {"id": "0808.3400v1", "title": "Comprehensive Two-Point Analyses of Weak Gravitational Lensing Surveys", "url": "http://arxiv.org/pdf/0808.3400v1", "date": "2008-08-25 20:01:55", "abs": "We present a framework for analyzing weak gravitational lensing survey data,\nincluding lensing and source-density observables, plus spectroscopic redshift\ncalibration data. All two-point observables are predicted in terms of\nparameters of a perturbed Robertson-Walker metric, making the framework\nindependent of the models for gravity, dark energy, or galaxy properties. For\nGaussian fluctuations the 2-point model determines the survey likelihood\nfunction and allows Fisher-matrix forecasting. The framework includes nuisance\nterms for the major systematic errors: shear measurement errors, magnification\nbias and redshift calibration errors, intrinsic galaxy alignments, and\ninaccurate theoretical predictions. We propose flexible parameterizations of\nthe many nuisance parameters related to galaxy bias and intrinsic alignment.\nFor the first time we can integrate many different observables and systematic\nerrors into a single analysis. As a first application of this framework, we\ndemonstrate that: uncertainties in power-spectrum theory cause very minor\ndegradation to cosmological information content; nearly all useful information\n(excepting baryon oscillations) is extracted with ~3 bins per decade of angular\nscale; and the rate at which galaxy bias varies with redshift substantially\ninfluences the strength of cosmological inference. The framework will permit\ncareful study of the interplay between numerous observables, systematic errors,\nand spectroscopic calibration data for large weak-lensing surveys.", "cat": "astro-ph", "authors": ["Gary M. Bernstein"]}, "1231": {"id": "1512.07207v1", "title": "A Critical Survey Of Privacy Infrastructures", "url": "http://arxiv.org/pdf/1512.07207v1", "date": "2015-12-20 05:05:20", "abs": "Over the last two decades, the scale and complexity of the Internet and its\nassociated technologies built on the World Wide Web has grown exponentially\nwith access to Internet as a facility occupying a prime place with other\namenities of modern lives. In years to come, usage of Internet may unravel more\npleasant surprises for us as far as novelty in its usage is concerned. As a\ndemocratic function of Internet, and relying on the open model on which it has\nbeen built, there has been concerted efforts in the direction of privacy\nprotection and use of privacy enhancing tools which have gained tangible\ntraction. Innovation in use of VPN, TLS/SSL and cryptographic tools are a\ntestimony to it. Another popular tool is Tor, which has gained widespread\npopularity as it is being increasingly used by anonymity seeking users to\neffectively maintain their discretion while surfing the web.\n However, there is a darker side to increased proliferation of Internet in our\neveryday routine. We are certainly not living in a utopian age and there are\npotentials of misuse of Internet as well. Across every nook and cranny of\nInternet's sprawling virtual world, there are cyber criminals lurking n\ndangerous alleys to use the very same Internet as malevolent tool to abuse it\nand cause financial, physical and social harm to ordinary people. Failing to\nmanage the widespread spawning of World Wide Web has rendered it weak against\nmisuse. In last few decades especially, Internet has been inundated with\nmalware, ransomware, viruses, Trojans, illegal spy tools and what not created\nwith malignant sentiments. In this paper, we will analyze few of the subverting\nprivacy infrastructures.", "cat": "cs.CY", "authors": ["B H Priyanka", "Ravi Prakash"]}, "1232": {"id": "2110.01889v3", "title": "Deep Neural Networks and Tabular Data: A Survey", "url": "http://arxiv.org/pdf/2110.01889v3", "date": "2022-06-29 16:14:08", "abs": "Heterogeneous tabular data are the most commonly used form of data and are\nessential for numerous critical and computationally demanding applications. On\nhomogeneous data sets, deep neural networks have repeatedly shown excellent\nperformance and have therefore been widely adopted. However, their adaptation\nto tabular data for inference or data generation tasks remains challenging. To\nfacilitate further progress in the field, this work provides an overview of\nstate-of-the-art deep learning methods for tabular data. We categorize these\nmethods into three groups: data transformations, specialized architectures, and\nregularization models. For each of these groups, our work offers a\ncomprehensive overview of the main approaches. Moreover, we discuss deep\nlearning approaches for generating tabular data, and we also provide an\noverview over strategies for explaining deep models on tabular data. Thus, our\nfirst contribution is to address the main research streams and existing\nmethodologies in the mentioned areas, while highlighting relevant challenges\nand open research questions. Our second contribution is to provide an empirical\ncomparison of traditional machine learning methods with eleven deep learning\napproaches across five popular real-world tabular data sets of different sizes\nand with different learning objectives. Our results, which we have made\npublicly available as competitive benchmarks, indicate that algorithms based on\ngradient-boosted tree ensembles still mostly outperform deep learning models on\nsupervised learning tasks, suggesting that the research progress on competitive\ndeep learning models for tabular data is stagnating. To the best of our\nknowledge, this is the first in-depth overview of deep learning approaches for\ntabular data; as such, this work can serve as a valuable starting point to\nguide researchers and practitioners interested in deep learning with tabular\ndata.", "cat": "cs.LG", "authors": ["Vadim Borisov", "Tobias Leemann", "Kathrin Se\u00dfler", "Johannes Haug", "Martin Pawelczyk", "Gjergji Kasneci"]}, "1233": {"id": "2308.12113v5", "title": "Advancements in Point Cloud Data Augmentation for Deep Learning: A Survey", "url": "http://arxiv.org/pdf/2308.12113v5", "date": "2024-04-23 05:46:01", "abs": "Deep learning (DL) has become one of the mainstream and effective methods for\npoint cloud analysis tasks such as detection, segmentation and classification.\nTo reduce overfitting during training DL models and improve model performance\nespecially when the amount and/or diversity of training data are limited,\naugmentation is often crucial. Although various point cloud data augmentation\nmethods have been widely used in different point cloud processing tasks, there\nare currently no published systematic surveys or reviews of these methods.\nTherefore, this article surveys these methods, categorizing them into a\ntaxonomy framework that comprises basic and specialized point cloud data\naugmentation methods. Through a comprehensive evaluation of these augmentation\nmethods, this article identifies their potentials and limitations, serving as a\nuseful reference for choosing appropriate augmentation methods. In addition,\npotential directions for future research are recommended. This survey\ncontributes to providing a holistic overview of the current state of point\ncloud data augmentation, promoting its wider application and development.", "cat": "cs.CV", "authors": ["Qinfeng Zhu", "Lei Fan", "Ningxin Weng"]}, "1234": {"id": "2109.01762v2", "title": "(Mis)alignment Between Stance Expressed in Social Media Data and Public Opinion Surveys", "url": "http://arxiv.org/pdf/2109.01762v2", "date": "2021-09-07 16:47:59", "abs": "Stance detection, which aims to determine whether an individual is for or\nagainst a target concept, promises to uncover public opinion from large streams\nof social media data. Yet even human annotation of social media content does\nnot always capture \"stance\" as measured by public opinion polls. We demonstrate\nthis by directly comparing an individual's self-reported stance to the stance\ninferred from their social media data. Leveraging a longitudinal public opinion\nsurvey with respondent Twitter handles, we conducted this comparison for 1,129\nindividuals across four salient targets. We find that recall is high for both\n\"Pro\" and \"Anti\" stance classifications but precision is variable in a number\nof cases. We identify three factors leading to the disconnect between text and\nauthor stance: temporal inconsistencies, differences in constructs, and\nmeasurement errors from both survey respondents and annotators. By presenting a\nframework for assessing the limitations of stance detection models, this work\nprovides important insight into what stance detection truly measures.", "cat": "cs.SI", "authors": ["Kenneth Joseph", "Sarah Shugars", "Ryan Gallagher", "Jon Green", "Alexi Quintana Math\u00e9", "Zijian An", "David Lazer"]}, "1235": {"id": "1505.04288v1", "title": "A short survey on nonlinear models of the classic Costas loop: rigorous derivation and limitations of the classic analysis", "url": "http://arxiv.org/pdf/1505.04288v1", "date": "2015-05-16 16:02:55", "abs": "Rigorous nonlinear analysis of the physical model of Costas loop --- a\nclassic phase-locked loop (PLL) based circuit for carrier recovery, is a\nchallenging task. Thus for its analysis, simplified mathematical models and\nnumerical simulation are widely used. In this work a short survey on nonlinear\nmodels of the BPSK Costas loop, used for pre-design and post-design analysis,\nis presented. Their rigorous derivation and limitations of classic analysis are\ndiscussed. It is shown that the use of simplified mathematical models, and the\napplication of non rigorous methods of analysis (e.g., simulation and\nlinearization) may lead to wrong conclusions concerning the performance of the\nCostas loop physical model.", "cat": "math.DS", "authors": ["R. E. Best", "N. V. Kuznetsov", "O. A. Kuznetsova", "G. A. Leonov", "M. V. Yuldashev", "R. V. Yuldashev"]}, "1236": {"id": "1611.07048v1", "title": "The VIMOS Public Extragalactic Redshift Survey (VIPERS). Full spectroscopic data and auxiliary information release (PDR-2)", "url": "http://arxiv.org/pdf/1611.07048v1", "date": "2016-11-21 21:00:22", "abs": "We present the full public data release (PDR-2) of the VIMOS Public\nExtragalactic Redshift Survey (VIPERS), performed at the ESO VLT. We release\nredshifts, spectra, CFHTLS magnitudes and ancillary information (as masks and\nweights) for a complete sample of 86,775 galaxies (plus 4,732 other objects,\nincluding stars and serendipitous galaxies); we also include their full\nphotometrically-selected parent catalogue. The sample is magnitude limited to\ni_AB < 22.5, with an additional colour-colour pre-selection devised as to\nexclude galaxies at z<0.5. This practically doubles the effective sampling of\nthe VIMOS spectrograph over the range 0.5= 2 are shown to have a confidence level of 96% or larger and\nmake up 88% of all measured galaxy redshifts (76,552 out of 86,775),\nconstituting the VIPERS prime catalogue for statistical investigations. For\nthis sample the rms redshift error, estimated using repeated measurements of\nabout 3,000 galaxies, is found to be sigma_z = 0.00054(1+z). All data are\navailable at http://vipers.inaf.it and on the ESO Archive.", "cat": "astro-ph.GA", "authors": ["M. Scodeggio", "L. Guzzo", "B. Garilli", "B. R. Granett", "M. Bolzonella", "S. de la Torre", "U. Abbas", "C. Adami", "S. Arnouts", "D. Bottini", "A. Cappi", "J. Coupon", "O. Cucciati", "I. Davidzon", "P. Franzetti", "A. Fritz", "A. Iovino", "J. Krywult", "V. Le Brun", "O. Le F\u00e9vre", "D. Maccagni", "K. Malek", "A. Marchetti", "F. Marulli", "M. Polletta", "A. Pollo", "L. A. M. Tasca", "R. Tojeiro", "D. Vergani", "A. Zanichelli", "J. Bel", "E. Branchini", "G. De Lucia", "O. Ilbert", "H. J. McCracken", "T. Moutard", "J. A. Peacock", "G. Zamorani", "A. Burden", "M. Fumana", "E. Jullo", "C. Marinoni", "Y. Mellier", "L. Moscardini", "W. J. Percival"]}, "1237": {"id": "2303.13336v2", "title": "A Survey on Audio Diffusion Models: Text To Speech Synthesis and Enhancement in Generative AI", "url": "http://arxiv.org/pdf/2303.13336v2", "date": "2023-04-02 09:27:20", "abs": "Generative AI has demonstrated impressive performance in various fields,\namong which speech synthesis is an interesting direction. With the diffusion\nmodel as the most popular generative model, numerous works have attempted two\nactive tasks: text to speech and speech enhancement. This work conducts a\nsurvey on audio diffusion model, which is complementary to existing surveys\nthat either lack the recent progress of diffusion-based speech synthesis or\nhighlight an overall picture of applying diffusion model in multiple fields.\nSpecifically, this work first briefly introduces the background of audio and\ndiffusion model. As for the text-to-speech task, we divide the methods into\nthree categories based on the stage where diffusion model is adopted: acoustic\nmodel, vocoder and end-to-end framework. Moreover, we categorize various speech\nenhancement tasks by either certain signals are removed or added into the input\nspeech. Comparisons of experimental results and discussions are also covered in\nthis survey.", "cat": "cs.SD", "authors": ["Chenshuang Zhang", "Chaoning Zhang", "Sheng Zheng", "Mengchun Zhang", "Maryam Qamar", "Sung-Ho Bae", "In So Kweon"]}, "1238": {"id": "2201.07119v5", "title": "A Survey on Code-Based Cryptography", "url": "http://arxiv.org/pdf/2201.07119v5", "date": "2024-07-17 15:45:58", "abs": "The improvements on quantum technology are threatening our daily\ncybersecurity, as a capable quantum computer can break all currently employed\nasymmetric cryptosystems. In preparation for the quantum-era the National\nInstitute of Standards and Technology (NIST) has initiated in 2016 a\nstandardization process for public-key encryption (PKE) schemes,\nkey-encapsulation mechanisms (KEM) and digital signature schemes. In 2023, NIST\nmade an additional call for post-quantum signatures. With this chapter we aim\nat providing a survey on code-based cryptography, focusing on PKEs and\nsignature schemes. We cover the main frameworks introduced in code-based\ncryptography and analyze their security assumptions. We provide the\nmathematical background in a lecture notes style, with the intention of\nreaching a wider audience.", "cat": "cs.CR", "authors": ["Violetta Weger", "Niklas Gassner", "Joachim Rosenthal"]}, "1239": {"id": "1410.6435v1", "title": "Ultraluminous Infrared Galaxies in the AKARI All Sky Survey", "url": "http://arxiv.org/pdf/1410.6435v1", "date": "2014-10-23 18:08:38", "abs": "We present a new catalog of 118 Ultraluminous Infrared Galaxies (ULIRGs) and\none Hyperluminous Infrared Galaxy (HLIRG) by crossmatching AKARI all-sky survey\nwith the Sloan Digital Sky Survey Data Release 10 (SDSS DR10) and the Final\nData Release of the Two-Degree Field Galaxy Redshift Survey (2dFGRS). 40 of the\nULIRGs and one HLIRG are new identifications. We find that ULIRGs are\ninteracting pair galaxies or ongoing/post mergers. This is consistent with the\nwidely accepted view: ULIRGs are major mergers of disk galaxies. We confirm the\npreviously known positive trend between the AGN fraction and IR luminosity. We\nshow that ULIRGs have a large off-set from the 'main sequence' up to z~1; their\noff-set from the z~2 'main sequence' is relatively smaller. We find a\nconsistent result with the previous studies showing that compared to local star\nforming SDSS galaxies of similar mass, local ULIRGs have lower oxygen\nabundances. We for the first time demonstrate that ULIRGs follow the\nfundamental metallicity relation (FMR). The scatter of ULIRGs around the FMR\n(0.09 dex - 0.5 dex) is comparable with the scatter of z~2-3 galaxies. Their\noptical colors show that ULIRGs are mostly blue galaxies and this agrees with\nprevious findings. We provide the largest local (0.050 < z < 0.487) ULIRG\ncatalog with stellar masses, SFRs, gas metallicities and optical colors. Our\ncatalog provides us active galaxies analogous to high-z galaxies in the local\nUniverse where they can be rigorously scrutinized.", "cat": "astro-ph.GA", "authors": ["E. Kilerci Eser", "T. Goto", "Y. Doi"]}, "1240": {"id": "2309.16856v2", "title": "A 9-Month Hubble Space Telescope Near-UV Survey of M87. II. A Strongly Enhanced Nova Rate near the Jet of M87", "url": "http://arxiv.org/pdf/2309.16856v2", "date": "2024-08-14 21:26:58", "abs": "The 135 classical novae that we have discovered in M87 with two\n$\\textit{Hubble Space Telescope}$ imaging surveys appear to be strongly\nconcentrated along that galaxy's jet. Detailed simulations show that the\nlikelihood that this distribution occurred by chance is of order $0.3\\%$. The\nnovae near the jet display outburst characteristics (peak luminosities, colors\nand decline rates) that are indistinguishable from novae far from the jet. We\nexplore whether the remarkable nova distribution could be caused by the jet's\nirradiation of the hydrogen-rich donors in M87's cataclysmic binaries. This\nexplanation, and others extant in the literature which rely on increased binary\nmass transfer rates, fail by orders of magnitude in explaining the enhanced\nnova rate near the jet. An alternate explanation is the presence of a genuine\nsurplus of nova binary systems near the jet, perhaps due to jet-induced star\nformation. This explanation fails to explain the lack of nova enhancement along\nM87's counterjet. The enhanced rate of novae along M87's jet is now firmly\nestablished, and unexplained.", "cat": "astro-ph.HE", "authors": ["Alec M. Lessing", "Michael M. Shara", "Rebekah Hounsell", "Shifra Mandel", "Nava Feder", "William Sparks"]}, "1241": {"id": "2111.00040v1", "title": "A survey of geometric constraints on the blowup of solutions of the Navier--Stokes equation", "url": "http://arxiv.org/pdf/2111.00040v1", "date": "2021-10-29 18:36:49", "abs": "In this survey article, we will discuss some regularity criteria for the\nNavier--Stokes equation that provide geometric constraints on any possible\nfinite-time blowup. We will also discuss the physical significance of such\nregularity criteria.", "cat": "math.AP", "authors": ["Evan Miller"]}, "1242": {"id": "1809.08739v1", "title": "High-mass outflows identified from COHRS CO\\,(3 - 2) Survey", "url": "http://arxiv.org/pdf/1809.08739v1", "date": "2018-09-24 03:32:22", "abs": "An unbiased search of molecular outflows within the region of the COHRS\nsurvey has identified 157 high-mass outflows from a sample of 770 ATLASGAL\nclumps with a detection rate of 20\\%. The detection rate of outflows increases\nfor clumps with higher M$_{clump}$, L$_{bol}$, L$_{bol}$/M$_{clump}$,\nN$_{H_{2}}$, and T$_{dust}$ compared to the clumps with no outflow. The\ndetection rates of the outflow increases from protostellar (8\\%) to YSO clump\n(17\\%) and to MSF clump (29\\%). The detection rate 26\\% for quiescent clump is\npreliminary, because the sample of quiescent clumps is small. A statistical\nrelation between the outflow and clump masses for our sample is\n$\\log(M_{out}/M_{\\bigodot}) = (-1.1\\pm0.21) +\n(0.9\\pm0.07)\\log(M_{clump}/M_{\\bigodot})$. The detection rate of outflows and\nthe outflow mass-loss rate show an increase with increasing M$_{clump}$,\nL$_{bol}$, N$_{H_{2}}$, and T$_{dust}$, which indicates that clumps with\noutflow with higher parameter values are at a more advanced evolutionary stage.\nThe outflow mechanical force increases with increasing bolometric luminosities.\nNo clear evidence has yet been found that higher mass outflows have different\nlaunching conditions than low-mass outflows.", "cat": "astro-ph.GA", "authors": ["Qiang Li", "Jianjun Zhou", "Jarken Esimbek", "Yuxin He", "W. A. Baan", "Dalei Li", "Gang Wu", "Xindi Tang", "Weiguang Ji"]}, "1243": {"id": "1611.01015v2", "title": "The Einstein@Home Gamma-ray Pulsar Survey. I. Search Methods, Sensitivity and Discovery of New Young Gamma-ray Pulsars", "url": "http://arxiv.org/pdf/1611.01015v2", "date": "2017-01-09 16:06:41", "abs": "We report on the results of a recent blind search survey for gamma-ray\npulsars in Fermi Large Area Telescope (LAT) data being carried out on the\ndistributed volunteer computing system, Einstein@Home. The survey has searched\nfor pulsations in 118 unidentified pulsar-like sources, requiring about 10,000\nyears of CPU core time. In total, this survey has resulted in the discovery of\n17 new gamma-ray pulsars, of which 13 are newly reported in this work, and an\naccompanying paper. These pulsars are all young, isolated pulsars with\ncharacteristic ages between 12 kyr and 2 Myr, and spin-down powers between\n$10^{34}$ and $4\\times10^{36}$ erg/s. Two of these are the slowest spinning\ngamma-ray pulsars yet known. One pulsar experienced a very large glitch $\\Delta\nf/f \\approx 3.5\\times10^{-6}$ during the Fermi mission. In this, the first of\ntwo associated papers, we describe the search scheme used in this survey, and\nestimate the sensitivity of our search to pulsations in unidentified Fermi-LAT\nsources. One such estimate results in an upper limit of 57% for the fraction of\npulsed emission from the gamma-ray source associated with the Cas A supernova\nremnant, constraining the pulsed gamma-ray photon flux that can be produced by\nthe neutron star at its center. We also present the results of precise timing\nanalyses for each of the newly detected pulsars.", "cat": "astro-ph.HE", "authors": ["C. J. Clark", "J. Wu", "H. J. Pletsch", "L. Guillemot", "B. Allen", "C. Aulbert", "C. Beer", "O. Bock", "A. Cu\u00e9llar", "H. B. Eggenstein", "H. Fehrmann", "M. Kramer", "B. Machenschalk", "L. Nieder"]}, "1244": {"id": "2301.01705v1", "title": "A Survey on Deep Industrial Transfer Learning in Fault Prognostics", "url": "http://arxiv.org/pdf/2301.01705v1", "date": "2023-01-04 17:01:27", "abs": "Due to its probabilistic nature, fault prognostics is a prime example of a\nuse case for deep learning utilizing big data. However, the low availability of\nsuch data sets combined with the high effort of fitting, parameterizing and\nevaluating complex learning algorithms to the heterogenous and dynamic settings\ntypical for industrial applications oftentimes prevents the practical\napplication of this approach. Automatic adaptation to new or dynamically\nchanging fault prognostics scenarios can be achieved using transfer learning or\ncontinual learning methods. In this paper, a first survey of such approaches is\ncarried out, aiming at establishing best practices for future research in this\nfield. It is shown that the field is lacking common benchmarks to robustly\ncompare results and facilitate scientific progress. Therefore, the data sets\nutilized in these publications are surveyed as well in order to identify\nsuitable candidates for such benchmark scenarios.", "cat": "cs.LG", "authors": ["Benjamin Maschler"]}, "1245": {"id": "2012.06344v2", "title": "Learning from Survey Propagation: a Neural Network for MAX-E-$3$-SAT", "url": "http://arxiv.org/pdf/2012.06344v2", "date": "2021-02-14 09:22:57", "abs": "Many natural optimization problems are NP-hard, which implies that they are\nprobably hard to solve exactly in the worst-case. However, it suffices to get\nreasonably good solutions for all (or even most) instances in practice. This\npaper presents a new algorithm for computing approximate solutions in\n${\\Theta(N})$ for the Maximum Exact 3-Satisfiability (MAX-E-$3$-SAT) problem by\nusing deep learning methodology. This methodology allows us to create a\nlearning algorithm able to fix Boolean variables by using local information\nobtained by the Survey Propagation algorithm. By performing an accurate\nanalysis, on random CNF instances of the MAX-E-$3$-SAT with several Boolean\nvariables, we show that this new algorithm, avoiding any decimation strategy,\ncan build assignments better than a random one, even if the convergence of the\nmessages is not found. Although this algorithm is not competitive with\nstate-of-the-art Maximum Satisfiability (MAX-SAT) solvers, it can solve\nsubstantially larger and more complicated problems than it ever saw during\ntraining.", "cat": "cs.AI", "authors": ["Raffaele Marino"]}, "1246": {"id": "1512.03626v2", "title": "CFHTLenS and RCSLenS: Testing Photometric Redshift Distributions Using Angular Cross-Correlations with Spectroscopic Galaxy Surveys", "url": "http://arxiv.org/pdf/1512.03626v2", "date": "2017-01-05 18:20:00", "abs": "We determine the accuracy of galaxy redshift distributions as estimated from\nphotometric redshift probability distributions $p(z)$. Our method utilises\nmeasurements of the angular cross-correlation between photometric galaxies and\nan overlapping sample of galaxies with spectroscopic redshifts. We describe the\nredshift leakage from a galaxy photometric redshift bin $j$ into a\nspectroscopic redshift bin $i$ using the sum of the $p(z)$ for the galaxies\nresiding in bin $j$. We can then predict the angular cross-correlation between\nphotometric and spectroscopic galaxies due to intrinsic galaxy clustering when\n$i \\neq j$ as a function of the measured angular cross-correlation when $i=j$.\nWe also account for enhanced clustering arising from lensing magnification\nusing a halo model. The comparison of this prediction with the measured signal\nprovides a consistency check on the validity of using the summed $p(z)$ to\ndetermine galaxy redshift distributions in cosmological analyses, as advocated\nby the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). We present an\nanalysis of the photometric redshifts measured by CFHTLenS, which overlaps the\nBaryon Oscillation Spectroscopic Survey (BOSS). We also analyse the\nRed-sequence Cluster Lensing Survey (RCSLenS), which overlaps both BOSS and the\nWiggleZ Dark Energy Survey. We find that the summed $p(z)$ from both surveys\nare generally biased with respect to the true underlying distributions. If\nunaccounted for, this bias would lead to errors in cosmological parameter\nestimation from CFHTLenS by less than $\\sim 4\\%$. For photometric redshift bins\nwhich spatially overlap in 3-D with our spectroscopic sample, we determine\nredshift bias corrections which can be used in future cosmological analyses\nthat rely on accurate galaxy redshift distributions.", "cat": "astro-ph.CO", "authors": ["Ami Choi", "Catherine Heymans", "Chris Blake", "Hendrik Hildebrandt", "Christopher A. J. Duncan", "Thomas Erben", "Reiko Nakajima", "Ludovic Van Waerbeke", "Massimo Viola"]}, "1247": {"id": "2404.05219v1", "title": "Out-of-Distribution Data: An Acquaintance of Adversarial Examples -- A Survey", "url": "http://arxiv.org/pdf/2404.05219v1", "date": "2024-04-08 06:27:38", "abs": "Deep neural networks (DNNs) deployed in real-world applications can encounter\nout-of-distribution (OOD) data and adversarial examples. These represent\ndistinct forms of distributional shifts that can significantly impact DNNs'\nreliability and robustness. Traditionally, research has addressed OOD detection\nand adversarial robustness as separate challenges. This survey focuses on the\nintersection of these two areas, examining how the research community has\ninvestigated them together. Consequently, we identify two key research\ndirections: robust OOD detection and unified robustness. Robust OOD detection\naims to differentiate between in-distribution (ID) data and OOD data, even when\nthey are adversarially manipulated to deceive the OOD detector. Unified\nrobustness seeks a single approach to make DNNs robust against both adversarial\nattacks and OOD inputs. Accordingly, first, we establish a taxonomy based on\nthe concept of distributional shifts. This framework clarifies how robust OOD\ndetection and unified robustness relate to other research areas addressing\ndistributional shifts, such as OOD detection, open set recognition, and anomaly\ndetection. Subsequently, we review existing work on robust OOD detection and\nunified robustness. Finally, we highlight the limitations of the existing work\nand propose promising research directions that explore adversarial and OOD\ninputs within a unified framework.", "cat": "cs.LG", "authors": ["Naveen Karunanayake", "Ravin Gunawardena", "Suranga Seneviratne", "Sanjay Chawla"]}, "1248": {"id": "1403.6309v1", "title": "\"TNOs are Cool\": A survey of the trans-Neptunian region X. Analysis of classical Kuiper belt objects from Herschel and Spitzer observations", "url": "http://arxiv.org/pdf/1403.6309v1", "date": "2014-03-25 11:28:00", "abs": "The classical Kuiper belt contains objects both from a low-inclination,\npresumably primordial, distribution and from a high-inclination dynamically\nexcited population. Based on a sample of classical TNOs with observations at\nthermal wavelengths we determine radiometric sizes, geometric albedos and\nthermal beaming factors as well as study sample properties of dynamically hot\nand cold classicals. Observations near the thermal peak of TNOs using infra-red\nspace telescopes are combined with optical magnitudes using the radiometric\ntechnique with near-Earth asteroid thermal model (NEATM). We have determined\nthree-band flux densities from Herschel/PACS observations at 70.0, 100.0 and\n160.0 $\\mu$m and Spitzer/MIPS at 23.68 and 71.42 $\\mu$m when available. We have\nanalysed 18 classical TNOs with previously unpublished data and re-analysed\npreviously published targets with updated data reduction to determine their\nsizes and geometric albedos as well as beaming factors when data quality\nallows. We have combined these samples with classical TNOs with radiometric\nresults in the literature for the analysis of sample properties of a total of\n44 objects. We find a median geometric albedo for cold classical TNOs of 0.14\nand for dynamically hot classical TNOs, excluding the Haumea family and dwarf\nplanets, 0.085. We have determined the bulk densities of Borasisi-Pabu (2.1\ng/cm^3), Varda-Ilmare (1.25 g/cm^3) and 2001 QC298 (1.14 g/cm^3) as well as\nupdated previous density estimates of four targets. We have determined the\nslope parameter of the debiased cumulative size distribution of dynamically hot\nclassical TNOs as q=2.3 +- 0.1 in the diameter range 1003 with the XRT, of which 60 have observed UV counterparts. We use the\nKepler Input Catalog (KIC) to obtain the optical counterparts of these sources,\nand construct the X-ray to optical flux ratio as a first approximation of the\nclassification of the source. The survey produces a mixture of stellar sources,\nextragalactic sources, and sources which we are not able to classify with\ncertainty. We have obtained optical spectra for thirty of these targets, and\nare conducting an ongoing observing campaign to fully identify the sample. For\nsources classified as stellar or AGN with certainty, we construct SEDs using\nthe 2MASS, UBV and GALEX data supplied for their optical counterparts by the\nKIC, and show that the SEDs differ qualitatively between the source types, and\nso can offer a method of classification in absence of a spectrum. Future papers\nin this series will analyze the timing properties of the stars and AGN in our\nsample separately. Our survey provides the first X-ray and UV data for a number\nof known variable stellar sources, as well as a large number of new X-ray\ndetections in this well-studied portion of the sky. The KSwAGS survey is\ncurrently ongoing in the K2 ecliptic plane fields.", "cat": "astro-ph.HE", "authors": ["Krista Lynne Smith", "Patricia T. Boyd", "Richard F. Mushotzky", "Neil Gehrels", "Rick Edelson", "Steve B. Howell", "Dawn M. Gelino", "Alexander Brown", "Steve Young"]}, "1261": {"id": "1810.12296v1", "title": "Selection functions of large spectroscopic surveys", "url": "http://arxiv.org/pdf/1810.12296v1", "date": "2018-10-29 17:01:24", "abs": "Context. Large spectroscopic surveys open the way to explore our Galaxy. In\norder to use the data from these surveys to understand the Galactic stellar\npopulation, we need to be sure that stars contained in a survey are a\nrepresentative subset of the underlying population. Without the selection\nfunction taken into account, the results might reflect the properties of the\nselection function rather than those of the underlying stellar population.\nAims. In this work, we introduce a method to estimate the selection function\nfor a given spectroscopic survey. We apply this method to a large sample of\npublic spectroscopic surveys. Methods. We apply a median division binning\nalgorithm to bin observed stars in the colour-magnitude space. This approach\nproduces lower uncertainties and lower biases of the selection function\nestimate as compared to traditionally used 2D-histograms. We run a set of\nsimulations to verify the method and calibrate the one free parameter it\ncontains. These simulations allow us to test the precision and accuracy of the\nmethod. Results. We produce and publish estimated values and uncertainties of\nselection functions for a large sample of public spectroscopic surveys. We\npublicly release the code used to produce the selection function estimates.\nConclusions. The effect of the selection function on distance modulus and\nmetallicity distributions of stars in surveys is important for surveys with\nsmall and largely inhomogeneous spatial coverage. For surveys with contiguous\nspatial coverage the effect of the selection function is almost negligible.", "cat": "astro-ph.GA", "authors": ["Alexey Mints", "Saskia Hekker"]}, "1262": {"id": "2202.12956v2", "title": "Agile requirements engineering practices: a survey in Brazilian software development companies", "url": "http://arxiv.org/pdf/2202.12956v2", "date": "2022-03-03 15:57:48", "abs": "Requirements Engineering (RE) is one of the prime areas in software\ndevelopment. Since agile software development englobes several emerging\ntechniques and advocates for continuous improvement, it urges the question of\nwhich agile RE practices are currently most used, their characteristics, and\nthe challenges in their employment. The aim of this work is to investigate and\ncategorize the collection and specification of agile requirements practices\nbased on how professionals perceive their importance for a software project\nthat applies agile methodologies. Thus, a survey was carried out with forty-six\n(46) Brazilian software development professionals, inquiring which methods are\nused for the collection and specification of agile requirements, as well as the\nfeatures, benefits, and difficulties when employing the methods. The responses\nallowed us to perform data analysis and identify the relationships between the\nrespondents' experience and the viewpoints on the collection methods and the\nagile requirements specification. In addition, it was noted that the adoption\nof these methods is still very recent. They have mainly been used for less than\nfive years. Moreover, it was noted that, for most respondents, there are yet\nsignificant challenges and advances to be made for better efficiency in\napplying the informed methods.", "cat": "cs.SE", "authors": ["Juan Carlos Barata", "Diego Lisboa", "Laudelino Cordeiro Bastos", "Adolfo Neto"]}, "1263": {"id": "1308.3216v1", "title": "One more neighbor: The first brown dwarf in the VVV survey", "url": "http://arxiv.org/pdf/1308.3216v1", "date": "2013-08-14 19:29:51", "abs": "Context. The discovery of brown dwarfs (BDs) in the solar neighborhood and\nyoung star clusters has helped to constraint the low-mass end of the stellar\nmass function and the initial mass function. We use data of the Vista Variables\nin the V\\'ia L\\'actea (VVV), a near-infrared (NIR) multiwavelength (Z Y J H Ks)\nmulti-epoch (Ks) ESO Public Survey mapping the Milky Way bulge and southern\nGalactic plane to search for nearby BDs.\n Aims. The ultimate aim of the project is to improve the completeness of the\ncensus of nearby stellar and substellar objects towards the Galactic bulge and\ninner disk regions.\n Methods. Taking advantage of the homogeneous sample of VVV multi-epoch data,\nwe identified stars with high proper motion (> 0.1\"/yr), and then selected\nlow-mass objects using NIR colors. We searched for a possible parallax\nsignature using the all available Ks band epochs. We set some constraints on\nthe month-to-year scale Ks band variability of our candidates, and even\nsearched for possible transiting companions. We obtained NIR spectra to\nproperly classify spectral type and then the physical properties of the final\nlist of candidates.\n Results. We report the discovery of VVV BD001, a new member of the local\nvolume-limited sample (within 20pc from the sun) with well defined proper\nmotion, distance, and luminosity. The spectral type of this new object is an\nL5+-1, unusually blue dwarf. The proper motion for this BD is\nPM(\\alpha)=-0.5455+-0.004 \"/yr, PM(\\delta)=-0.3255+-0.004 \"/yr, and it has a\nparallax of 57+-4 mas which translates into a distance of 17.5 +- 1.1 pc. VVV\nBD001 shows no evidence of variability (\\Delta Ks <0.05mag) over two years,\nespecially constrained on a six month scale during the year 2012.", "cat": "astro-ph.SR", "authors": ["J. C. Beam\u00edn", "D. Minniti", "M. Gromadzki", "R. Kurtev", "V. D. Ivanov", "Y. Beletsky", "P. Lucas", "R. K. Saito", "J. Borissova"]}, "1264": {"id": "0809.1172v2", "title": "The stellar content of the Hamburg/ESO survey. V. The metallicity distribution function of the Galactic halo", "url": "http://arxiv.org/pdf/0809.1172v2", "date": "2009-09-30 16:12:19", "abs": "We determine the metallicity distribution function (MDF) of the Galactic halo\nby means of a sample of 1638 metal-poor stars selected from the Hamburg/ESO\nobjective-prism survey (HES). The sample was corrected for minor biases\nintroduced by the strategy for spectroscopic follow-up observations of the\nmetal-poor candidates, namely \"best and brightest stars first\". [...] We\ndetermined the selection function of the HES, which must be taken into account\nfor a proper comparison between the HES MDF with MDFs of other stellar\npopulations or those predicted by models of Galactic chemical evolution. The\nlatter show a reasonable agreement with the overall shape of the HES MDF for\n[Fe/H] > -3.6, but only a model of Salvadori et al. (2007) with a critical\nmetallicity for low-mass star formation of Z_cr = 10^{-3.4} * Z_Sun reproduces\nthe sharp drop at [Fe/H] ~-3.6 present in the HES MDF. [...] A comparison of\nthe MDF of Galactic globular clusters and of dSph satellites to the Galaxy\nshows qualitative agreement with the halo MDF, derived from the HES, once the\nselection function of the latter is included. However, statistical tests show\nthat the differences between these are still highly significant. [ABSTRACT\nABRIDGED]", "cat": "astro-ph", "authors": ["T. Schoerck", "N. Christlieb", "J. G. Cohen", "T. C. Beers", "S. Shectman", "I. Thompson", "A. McWilliam", "M. S. Bessell", "J. E. Norris", "J. Melendez", "S. Solange Ramirez", "D. Haynes", "P. Cass", "M. Hartley", "K. Russell", "F. Watson", "F. -J. Zickgraf", "B. Behnke", "C. Fechner", "B. Fuhrmeister", "P. S. Barklem", "B. Edvardsson", "A. Frebel", "L. Wisotzki", "D. Reimers"]}, "1265": {"id": "2304.05425v2", "title": "Survey of Gravitationally Lensed Objects in HSC Imaging (SuGOHI). IX. Discovery of Strongly Lensed Quasar Candidates", "url": "http://arxiv.org/pdf/2304.05425v2", "date": "2023-08-10 15:52:18", "abs": "We report the discovery of new lensed quasar candidates in the imaging data\nof the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) DR4, covering\n$1\\,310~{\\rm deg}^2$ of the sky with seeing of $\\approx0.6''$. In addition to\ntwo catalogs of MILLIQUAS and AllWISEAGN, which contain confirmed and candidate\nquasars, we preselect quasar sources using color cuts from the HSC ($grizy$)\nand unWISE ($W1+W2$) photometric data based on SDSS spectroscopic catalogs. We\nsearch for the presence of multiple point sources with similar color through\nthe convolution of the Laplacian of the preselected quasar image cutouts with\nthe Laplacian of the point spread function, resulting in a reduction of lens\ncandidates from $1\\,652\\,329$ to $121\\,511$ ($7.4\\%$). After visual binary\nclassification, we grade $6\\,199$ ($0.4\\%$) potential lenses on a scale of 0 to\n3, with 3 indicating a lens and 0 indicating a non-lens. Finally we obtain 162\nlens candidates with an average grade of $\\geq2$, and among them, we\nsuccessfully recover 18 known lenses. By fitting the light distribution and\nremoving the known contaminants, we discover that 57 new systems contain at\nleast two point sources and a galaxy in between, including 10 possible\nquadruply lensed quasars. This new sample of lens candidates exhibits a median\nseparation of $1.26''$ and a magnitude limit of $i\\approx22$. Spectroscopic or\nhigh-resolution imaging follow up on these newly discovered lensed quasar\ncandidates will further allow their natures to be confirmed.", "cat": "astro-ph.GA", "authors": ["James H. H. Chan", "Kenneth C. Wong", "Xuheng Ding", "Dani Chao", "I-Non Chiu", "Anton T. Jaelani", "Issha Kayo", "Anupreeta More", "Masamune Oguri", "Sherry H. Suyu"]}, "1266": {"id": "1203.2138v1", "title": "Self-Calibration for 3-point Intrinsic Alignment Auto-Correlations in Weak Lensing Surveys", "url": "http://arxiv.org/pdf/1203.2138v1", "date": "2012-03-09 17:05:30", "abs": "The weak lensing signal (cosmic shear) has been shown to be strongly\ncontaminated by the various types of galaxy intrinsic alignment (IA)\ncorrelations, which poses a barrier to precision weak lensing measurements. The\nredshift dependence of the IA signal has been used at the 2-point level to\nreduce this contamination by only measuring cross-correlations between large\nredshift bins, which significantly reduces the galaxy intrinsic ellipticity -\nintrinsic ellipticity (II) correlation. A self-calibration technique based on\nthe redshift dependences of the IA correlations has also been proposed as a\nmeans to remove the 2-point IA contamination from the lensing signal. We\nexplore here the redshift dependences of the IA and lensing bispectra in order\nto propose a self-calibration of the IA auto-correlations at the 3-point level\n(i.e. GGI, GII, and III), which can be well understood without the assumption\nof any particular IA model. We find that future weak lensing surveys will be\nable to measure the distinctive IA redshift dependence over ranges of $|\\Delta\nz^P|\\le 0.2$. Using conservative estimates of photo-z accuracy, we describe the\n3-point self-calibration technique for the total IA signal, which can be\naccomplished through lensing tomography of photo-z bin size $\\sim 0.01$. We\nfind that the 3-point self-calibration can function at the accuracy of the\n2-point technique with modest constraints in redshift separation. This allows\nthe 3-point IA auto-correlation self-calibration technique proposed here to\nsignificantly reduce the contamination of the IA contamination to the weak\nlensing bispectrum.", "cat": "astro-ph.CO", "authors": ["M. A. Troxel", "Mustapha Ishak"]}, "1267": {"id": "2212.01714v1", "title": "A survey on grading format of automated grading tools for programming assignments", "url": "http://arxiv.org/pdf/2212.01714v1", "date": "2022-12-04 00:49:16", "abs": "The prevalence of online platforms and studies has generated the demand for\nautomated grading tools, and as a result, there are plenty in the market. Such\ntools are developed to grade coding assignments quickly, accurately, and\neffortlessly. Since there are varieties of tools available to cater to the\ndiverse options of programming languages and concepts, it is overwhelming for\nany instructor to decide which one suits one's requirements. There are several\nsurveys studying the tools and giving insights into how they function and what\nthey support. However other than knowing the functionality, it is important for\nan instructor to know how the assignments are graded and what is the format of\nthe test cases. This is crucial since the instructor has to design the grading\nformat and therefore requires a learning curve. This survey studies and\nevaluates the automated grading tools based on their evaluation format. This in\nturn helps a reader in deciding which tool to choose and provides an insight\ninto what are the assessment settings and approaches used in grading the coding\nassignment in any specific grading tool.", "cat": "cs.CY", "authors": ["Aditi Agrawal", "Benjamin Reed"]}, "1268": {"id": "1504.00737v4", "title": "An Extragalactic Spectroscopic Survey of the SSA22 Field", "url": "http://arxiv.org/pdf/1504.00737v4", "date": "2015-10-24 23:29:58", "abs": "We present VLT VIMOS, Keck DEIMOS and Keck LRIS multi-object spectra of 367\nsources in the field of the z ~ 3.09 protocluster SSA22. Sources are\nspectroscopically classified via template matching, allowing new\nidentifications for 206 extragalactic sources, including 36 z > 2 Lyman-break\ngalaxies (LBGs) and Lyman-\\alpha\\ emitters (LAEs), 8 protocluster members, and\n94 X-ray sources from the ~ 400 ks Chandra deep survey of SSA22. Additionally,\nin the area covered by our study, we have increased by ~ 4, 13, and 6 times the\nnumber of reliable redshifts of sources at 1.0 < z < 2.0, at z > 3.4, and with\nX-Ray emission, respectively. We compare our results with past spectroscopic\nsurveys of SSA22 to investigate the completeness of the LBGs and the X-Ray\nproperties of the new spectroscopically-classified sources in the SSA22 field.", "cat": "astro-ph.GA", "authors": ["C. Saez", "B. D. Lehmer", "F. E. Bauer", "D. Stern", "A. Gonzales", "I. Rreza", "D. M. Alexander", "Y. Matsuda", "J. E. Geach", "F. A. Harrison", "T. Havashino"]}, "1269": {"id": "0901.3083v1", "title": "Interpreting the yield of transit surveys: Are there groups in the known transiting planets population?", "url": "http://arxiv.org/pdf/0901.3083v1", "date": "2009-01-20 17:35:28", "abs": "Each transiting planet discovered is characterized by 7 measurable\nquantities, that may or may not be linked together (planet mass, radius,\norbital period, and star mass, radius, effective temperature, and metallicity).\nCorrelations between planet mass and period, surface gravity and period, planet\nradius and star temperature have been previously observed among the known\ntransiting giant planets. Two classes of planets have been previously\nidentified based on their Safronov number. We use the CoRoTlux code to compare\nsimulated events to the sample of discovered planets and test the statistical\nsignificance of these correlations. We first generate a stellar field with\nplanetary companions based on radial velocity discoveries and a planetary\nevolution model, then apply a detection criterion that includes both\nstatistical and red noise sources. We compare the yield of our simulated survey\nwith the ensemble of 31 well-characterized giant transiting planets, using a\nmultivariate logistic analysis to assess whether the simulated distribution\nmatches the known transiting planets. Our multivariate analysis shows that our\nsimulated sample and observations are consistent to 76%. The mass vs. period\ncorrelation for giant planets first observed with radial velocity holds with\ntransiting planets. Our model naturally explains the correlation between planet\nsurface gravity and period and the one between planet radius and stellar\neffective temperature. Finally, we are also able to reproduce the previously\nobserved apparent bimodal distribution of Safronov numbers in 10% of our\nsimulated cases, although our model predicts a continuous distribution. This\nshows that the evidence for the existence of two groups of planets with\ndifferent intrinsic properties is not statistically significant.", "cat": "astro-ph.EP", "authors": ["Fressin Francois", "Guillot Tristan", "Nesta Lionel"]}, "1270": {"id": "2008.07568v1", "title": "The Southern Stellar Stream Spectroscopic Survey (S5): Chemical Abundances of Seven Stellar Streams", "url": "http://arxiv.org/pdf/2008.07568v1", "date": "2020-08-17 18:38:25", "abs": "We present high-resolution Magellan/MIKE spectroscopy of 42 red giant stars\nin seven stellar streams confirmed by the Southern Stellar Stream Spectroscopic\nSurvey (S5): ATLAS, Aliqa Uma, Chenab, Elqui, Indus, Jhelum, and Phoenix.\nAbundances of 30 elements have been derived from over 10,000 individual line\nmeasurements or upper limits using photometric stellar parameters and a\nstandard LTE analysis. This is currently the most extensive set of element\nabundances for stars in stellar streams. Three streams (ATLAS, Aliqa Uma, and\nPhoenix) are disrupted metal-poor globular clusters, although only weak\nevidence is seen for the light element anticorrelations commonly observed in\nglobular clusters. Four streams (Chenab, Elqui, Indus, and Jhelum) are\ndisrupted dwarf galaxies, and their stars display abundance signatures that\nsuggest progenitors with stellar masses ranging from $10^6-10^7 M_\\odot$.\nExtensive description is provided for the analysis methods, including the\nderivation of a new method for including the effect of stellar parameter\ncorrelations on each star's abundance and uncertainty.\n This paper includes data gathered with the 6.5 meter Magellan Telescopes\nlocated at Las Campanas Observatory, Chile.", "cat": "astro-ph.SR", "authors": ["Alexander P. Ji", "Ting S. Li", "Terese T. Hansen", "Andrew R. Casey", "Sergey E. Koposov", "Andrew B. Pace", "Dougal Mackey", "Geraint F. Lewis", "Jeffrey D. Simpson", "Joss Bland-Hawthorn", "Lara R. Cullinane", "Gary. S. Da Costa", "Kohei Hattori", "Sarah L. Martell", "Kyler Kuehn", "Denis Erkal", "Nora Shipp", "Zhen Wan", "Daniel B. Zucker"]}, "1271": {"id": "2105.07221v2", "title": "Computational methods for large-scale inverse problems: a survey on hybrid projection methods", "url": "http://arxiv.org/pdf/2105.07221v2", "date": "2021-08-19 18:29:32", "abs": "This paper surveys an important class of methods that combine iterative\nprojection methods and variational regularization methods for large-scale\ninverse problems. Iterative methods such as Krylov subspace methods are\ninvaluable in the numerical linear algebra community and have proved important\nin solving inverse problems due to their inherent regularizing properties and\ntheir ability to handle large-scale problems. Variational regularization\ndescribes a broad and important class of methods that are used to obtain\nreliable solutions to inverse problems, whereby one solves a modified problem\nthat incorporates prior knowledge. Hybrid projection methods combine iterative\nprojection methods with variational regularization techniques in a synergistic\nway, providing researchers with a powerful computational framework for solving\nvery large inverse problems. Although the idea of a hybrid Krylov method for\nlinear inverse problems goes back to the 1980s, several recent advances on new\nregularization frameworks and methodologies have made this field ripe for\nextensions, further analyses, and new applications. In this paper, we provide a\npractical and accessible introduction to hybrid projection methods in the\ncontext of solving large (linear) inverse problems.", "cat": "math.NA", "authors": ["Julianne Chung", "Silvia Gazzola"]}, "1272": {"id": "2307.15732v1", "title": "z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [I] Overview", "url": "http://arxiv.org/pdf/2307.15732v1", "date": "2023-07-28 18:00:01", "abs": "(Abridged) Using the IRAM NOEMA interferometer, we measures the redshifts of\n126 bright galaxies detected in the Herschel H-ATLAS, HeLMS, and HerS surveys.\nWe report reliable spectroscopic redshifts for a total of 124 of the\nHerschel-selected galaxies. The redshifts are estimated from scans of the 3 and\n2-mm bands (and, in one case, the 1-mm band) and are based on the detection of\nat least two emission lines. Together with the Pilot Programme (Neri et al.\n2020), including spectroscopic redshifts of 11 sources, our survey has derived\nprecise redshifts for 135 bright Herschel-selected galaxies, making it the\nlargest sample of high-z galaxies with robust redshifts to date. Most emission\nlines detected are from 12CO (mainly from J=2-1 to 5-4), with some sources seen\nin [CI] and H2O emission lines. The spectroscopic redshifts are in the range\n0.8 2.6 \\times 10^{14}\nM_\\odot h^{-1}_{70}$ and $z > 0.25$ in the survey area. The mass threshold is\napproximately constant above $z = 0.25$, and the complete catalog has a median\nmass of approximately $ M_{500c} = 2.7 \\times 10^{14} M_\\odot h^{-1}_{70}$.\nCompared to previous SPT works, the increased depth of the millimeter-wave data\n(11.2 and 6.5 $\\mu$K-arcmin at 95 and 150 GHz, respectively) makes it possible\nto find more galaxy clusters at high redshift and lower mass.", "cat": "astro-ph.CO", "authors": ["N. Huang", "L. E. Bleem", "B. Stalder", "P. A. R. Ade", "S. W. Allen", "A. J. Anderson", "J. E. Austermann", "J. S. Avva", "J. A. Beall", "A. N. Bender", "B. A. Benson", "F. Bianchini", "S. Bocquet", "M. Brodwin", "J. E. Carlstrom", "C. L. Chang", "H. C. Chiang", "R. Citron", "C. Corbett Moran", "T. M. Crawford", "A. T. Crites", "T. de Haan", "M. A. Dobbs", "W. Everett", "B. Floyd", "J. Gallicchio", "E. M. George", "A. Gilbert", "M. D. Gladders", "S. Guns", "N. Gupta", "N. W. Halverson", "N. Harrington", "J. W. Henning", "G. C. Hilton", "G. P. Holder", "W. L. Holzapfel", "J. D. Hrubes", "J. Hubmayr", "K. D. Irwin", "G. Khullar", "L. Knox", "A. T. Lee", "D. Li", "A. Lowitz", "M. McDonald", "J. J. McMahon", "S. S. Meyer", "L. M. Mocanu", "J. Montgomery", "A. Nadolski", "T. Natoli", "J. P. Nibarger", "G. Noble", "V. Novosad", "S. Padin", "S. Patil", "C. Pryke", "C. L. Reichardt", "J. E. Ruhl", "B. R. Saliwanchik", "A. Saro", "J. T. Sayre", "K. K. Schaffer", "K. Sharon", "C. Sievers", "G. Smecher", "A. A. Stark", "K. T. Story", "C. Tucker", "K. Vanderlinde", "T. Veach", "J. D. Vieira", "G. Wang", "N. Whitehorn", "W. L. K. Wu", "V. Yefremenko"]}, "1275": {"id": "2109.14167v1", "title": "The EDGE-CALIFA survey: The resolved star formation efficiency and local physical conditions", "url": "http://arxiv.org/pdf/2109.14167v1", "date": "2021-09-29 03:23:49", "abs": "We measure the star formation rate (SFR) per unit gas mass and the star\nformation efficiency (SFE$_{\\rm gas}$ for total gas, SFE$_{\\rm mol}$ for the\nmolecular gas) in 81 nearby galaxies selected from the EDGE-CALIFA survey,\nusing $^{12}$CO(J=1-0) and optical IFU data. For this analysis we stack CO\nspectra coherently by using the velocities of H$\\alpha$ detections to detect\nfainter CO emission out to galactocentric radii $r_{\\rm gal} \\sim 1.2 r_{25}$\n($\\sim 3 R_{\\rm e}$), and include the effects of metallicity and high surface\ndensities in the CO-to-H$_2$ conversion. We determine the scale lengths for the\nmolecular and stellar components, finding a close to 1:1 relation between them.\nThis result indicates that CO emission and star formation activity are closely\nrelated. We examine the radial dependence of SFE$_{\\rm gas}$ on physical\nparameters such as galactocentric radius, stellar surface density\n$\\Sigma_{\\star}$, dynamical equilibrium pressure $P_{\\rm DE}$, orbital\ntimescale $\\tau_{\\rm orb}$, and the Toomre $Q$ stability parameter (including\nstar and gas $Q_{\\rm star+gas}$). We observe a generally smooth, continuous\nexponential decline in the SFE$_{\\rm gas}$ with $r_{\\rm gal}$. The SFE$_{\\rm\ngas}$ dependence on most of the physical quantities appears to be well\ndescribed by a power-law. Our results also show a flattening in the SFE$_{\\rm\ngas}$-$\\tau_{\\rm orb}$ relation at $\\log[\\tau_{\\rm orb}]\\sim 7.9-8.1$ and a\nmorphological dependence of the SFE$_{\\rm gas}$ per orbital time, which may\nreflect star formation quenching due to the presence of a bulge component. We\ndo not find a clear correlation between SFE$_{\\rm gas}$ and $Q_{\\rm star+gas}$.", "cat": "astro-ph.GA", "authors": ["V. Villanueva", "A. Bolatto", "S. Vogel", "R. C. Levy", "S. F. Sanchez", "J. Barrera-Ballesteros", "T. Wong", "E. Rosolowsky", "D. Colombo", "M. Rubio", "Y. Cao", "V. Kalinova", "A. Leroy", "D. Utomo", "R. Herrera-Camus", "L. Blitz", "Y. Luo"]}, "1276": {"id": "2307.04120v3", "title": "Toward a stellar population catalog in the Kilo Degree Survey: the impact of stellar recipes on stellar masses and star formation rates", "url": "http://arxiv.org/pdf/2307.04120v3", "date": "2023-12-11 11:04:11", "abs": "The Kilo Degree Survey (KiDS) is currently the only sky survey providing\noptical ($ugri$) plus near-infrared (NIR, $ZYHJK_S$) seeing matched photometry\nover an area larger than 1000 $\\rm deg^2$. This is obtained by incorporating\nthe NIR data from the VISTA Kilo Degree Infrared Galaxy (VIKING) survey,\ncovering the same KiDS footprint. As such, the KiDS multi-wavelength photometry\nrepresents a unique dataset to test the ability of stellar population models to\nreturn robust photometric stellar mass ($M_*$) and star-formation rate (SFR)\nestimates. Here we use a spectroscopic sample of galaxies for which we possess\n$u g r i Z Y J H K_s$ ``gaussianized'' magnitudes from KiDS data release 4. We\nfit the spectral energy distribution from the 9-band photometry using: 1) three\ndifferent popular libraries of stellar {population} templates, 2) single burst,\nsimple and delayed exponential star-formation history models, and 3) a wide\nrange of priors on age and metallicity. As template fitting codes we use two\npopular softwares: LePhare and CIGALE. We investigate the variance of the\nstellar masses and the star-formation rates from the different combinations of\ntemplates, star formation recipes and codes to assess the stability of these\nestimates and define some ``robust'' median quantities to be included in the\nupcoming KiDS data releases. As a science validation test, we derive the mass\nfunction, the star formation rate function, and the SFR-$M_*$ relation for a\nlow-redshift ($z<0.5$) sample of galaxies, that result in excellent agreement\nwith previous literature data. The final catalog, containing $\\sim290\\,000$\ngalaxies with redshift $0.01=5\ndeg (>= 8 deg towards the Galactic bulge) as the input catalog for our survey.\nWe obtained spectroscopic observations for 11,000 galaxies and used\npreviously-obtained velocities for the remainder of the sample to generate a\nredshift catalog that is 97.6% complete to well-defined limits and covers 91%\nof the sky. This provides an unprecedented census of galaxy (baryonic mass)\nconcentrations within 300 Mpc.\n Earlier versions of our survey have been used in a number of publications\nthat have studied the bulk motion of the Local Group, mapped the density and\npeculiar velocity fields out to 50 Mpc, detected galaxy groups, and estimated\nthe values of several cosmological parameters.\n Additionally, we present morphological types for a nearly-complete sub-sample\nof 20,860 galaxies with Ks < 11.25 mag and |b|>= 10 deg.", "cat": "astro-ph.CO", "authors": ["John P. Huchra", "Lucas M. Macri", "Karen L. Masters", "Thomas H. Jarrett", "Perry Berlind", "Michael Calkins", "Aidan C. Crook", "Roc Cutri", "Pirin Erdogdu", "Emilio Falco", "Teddy George", "Conrad M. Hutcheson", "Ofer Lahav", "Jeff Mader", "Jessica D. Mink", "Nathalie Martimbeau", "Stephen Schneider", "Michael Skrutskie", "Susan Tokarz", "Michael Westover"]}, "1299": {"id": "2203.03313v1", "title": "EXORCISM: a spectroscopic survey of young eruptive variables (EXor and candidates)", "url": "http://arxiv.org/pdf/2203.03313v1", "date": "2022-03-07 11:48:10", "abs": "We present an optical/near-IR survey of 11 variable young stars (EXors and\nEXor candidates) aimed at deriving and monitoring their accretion properties.\nAbout 30 optical and near-infrared spectra ($\\Re$ $\\sim$ 1500-2000) were\ncollected between 2014-2019 with the Large Binocular Telescope (LBT). From the\nspectral analysis we have derived the accretion luminosity and mass accretion\nrate, the visual extinction, the temperature and density of the permitted line\nformation region, and the signature of the outflowing matter.\n Two sources (ASASSN-13db and iPTF15afq) have been observed in outburst and\nquiescence, three during a high-level of brightness (XZ Tau, PV Cep, and NY\nOri), and the others in quiescence. These latter have accretion luminosity and\nmass accretion rates in line with the values measured in classical T Tauri\nstars of similar mass. All sources observed more than once present accretion\nvariability. The most extreme case is ASASSN-13db, for which the mass accretion\nrate decreases by two orders of magnitude from the outburst peak in 2015 to\nquiescence in 2017. Also, in NY Ori the accretion luminosity decreases by a\nfactor 25 in one year. In 80% of the sample we detect the [OI]630 nm line, a\ntracer of mass loss. From the variability of the H$\\alpha$/[OI]630, ratio, we\nconclude that mass accretion variations are larger than mass loss variations.\nFrom the analysis of the HI recombination lines a correlation is suggested\nbetween the density of the line formation region and the level of accretion\nactivity of the source.", "cat": "astro-ph.SR", "authors": ["T. Giannini", "A. Giunta", "M. Gangi", "R. Carini", "D. Lorenzetti", "S. Antoniucci", "A. Caratti o Garatti", "L. Cassar\u00e0", "B. Nisini", "A. Rossi", "V. Testa", "F. Vitali"]}, "1300": {"id": "1308.0378v1", "title": "The Northern High Time Resolution Universe Pulsar Survey I: Setup and initial discoveries", "url": "http://arxiv.org/pdf/1308.0378v1", "date": "2013-08-01 23:54:46", "abs": "We report on the setup and initial discoveries of the Northern High Time\nResolution Universe survey for pulsars and fast transients, the first major\npulsar survey conducted with the 100-m Effelsberg radio telescope and the first\nin 20 years to observe the whole northern sky at high radio frequencies. Using\na newly developed 7-beam receiver system combined with a state-of-the-art\npolyphase filterbank, we record an effective bandwidth of 240 MHz in 410\nchannels centred on 1.36 GHz with a time resolution of 54 $\\mu$s. Such fine\ntime and frequency resolution increases our sensitivity to millisecond pulsars\nand fast transients, especially deep inside the Galaxy, where previous surveys\nhave been limited due to intra-channel dispersive smearing. To optimise\nobserving time, the survey is split into three integration regimes dependent on\nGalactic latitude, with 1500-s, 180-s and 90-s integrations for latitude ranges\n$|b|<3.5^{\\circ}$, $|b|<15^{\\circ}$ and $|b|>15^{\\circ}$, respectively. The\nsurvey has so far resulted in the discovery of 15 radio pulsars, including a\npulsar with a characteristic age of $\\sim18$ kyr, {PSR J2004+3429}, and a\nhighly eccentric, binary millisecond pulsar, {PSR J1946+3417}. All newly\ndiscovered pulsars are timed using the 76-m Lovell radio telescope at the\nJodrell Bank Observatory and the Effelsberg radio telescope. We present timing\nsolutions for all newly discovered pulsars and discuss potential supernova\nremnant associations for {PSR J2004+3429}.", "cat": "astro-ph.HE", "authors": ["Ewan D. Barr", "David J. Champion", "Michael Kramer", "Ralph P. Eatough", "Paulo C. C. Freire", "Ramesh Karuppusamy", "K. J. Lee", "Joris P. W. Verbiest", "Cees G. Bassa", "Andrew G. Lyne", "Benjamin Stappers", "Duncan R. Lorimer", "Bernd Klein"]}, "1301": {"id": "2202.07518v1", "title": "HII regions in CALIFA survey: II. The relation between their physical properties and galaxy evolution", "url": "http://arxiv.org/pdf/2202.07518v1", "date": "2022-02-15 15:46:40", "abs": "We present in here the exploration of the physical properties of the sample\nof HII regions and aggregations of the last HII regions catalog of the CALIFA\nsurvey. This sample comprises the optical spectroscopic properties of more than\n~26,000 ionized regions corresponding to 924 galaxies from the Integral Field\nSpectroscopy data, including the flux intensity and equivalent widths and the\nproperties of their underlying stellar population. In the current study we\nderive a set of physical quantities for all these regions based on those\nproperties, including (i) the fraction of young stars; (ii) the ionization\nstrength (using six different estimations); (iii) the oxygen abundance (using\n25 different calibrators); (iv) the nitrogen and nitrogen-to-oxygen abundance;\n(v) the dust extinction and (vi) the electron density. Using this dataset we\nexplore how the loci in the classical diagnostic diagrams are connected with\nthose quantities, the radial distributions of these parameters, and the\ninter-relations between themselves and with the properties of the underlying\nstellar populations. We conclude that many properties of the HII regions are\ntightly related to the galactic stellar evolution at the location where those\nregions are observed. Those properties are modulated only as a second-order\neffect by the properties of the ionizing stars and the ionized nebulae that do\nnot depend on the astrophysical context in which they are formed. Our results\nhighlight the importance of HII regions to explore the chemical evolution in\ngalaxies, clarifying which of their properties can be used as proxies of that\nevolution.", "cat": "astro-ph.GA", "authors": ["C. Espinosa-Ponce", "S. F. S\u00e1nchez", "C. Morisset", "J. K. Barrera-Ballesteros", "L. Galbany", "R. Garc\u00eda-Benito", "E. A. D. Lacerda", "D. Mast"]}, "1302": {"id": "1912.09778v3", "title": "From the bulge to the outer disc: StarHorse stellar parameters, distances, and extinctions for stars in APOGEE DR16 and other spectroscopic surveys", "url": "http://arxiv.org/pdf/1912.09778v3", "date": "2020-04-20 06:34:02", "abs": "We combine high-resolution spectroscopic data from APOGEE-2 Survey Data\nRelease 16 (DR16) with broad-band photometric data from several sources, as\nwell as parallaxes from {\\it Gaia} Data Release 2 (DR2). Using the Bayesian\nisochrone-fitting code {\\tt StarHorse}, we derive distances, extinctions and\nastrophysical parameters for around 388,815 APOGEE stars, achieving typical\ndistance uncertainties of $\\sim 6\\%$ for APOGEE giants, $\\sim 2\\%$ for APOGEE\ndwarfs, as well as extinction uncertainties of $\\sim 0.07$ mag when all\nphotometric information is available, and $\\sim 0.17$ mag if optical photometry\nis missing. {\\tt StarHorse} uncertainties vary with the input spectroscopic\ncatalogue, with the available photometry, and with the parallax uncertainties.\nTo illustrate the impact of our results, we show that, thanks to {\\it Gaia} DR2\nand the now larger sky coverage of APOGEE-2 (including APOGEE-South), we obtain\nan extended map of the Galactic plane, providing unprecedented coverage of the\ndisk close to the Galactic mid-plane ($|Z_{Gal}|<1$ kpc) from the Galactic\nCentre out to $R_{\\rm Gal}\\sim 20$ kpc. The improvements in statistics as well\nas distance and extinction uncertainties unveil the presence of the bar in\nstellar density, as well as the striking chemical duality in the innermost\nregions of the disk, now clearly extending to the inner bulge. We complement\nthis paper with distances and extinctions for stars in other public released\nspectroscopic surveys: 324,999 in GALAH DR2, 4,928,715 in LAMOST DR5, 408,894\nin RAVE DR6, and 6,095 in GES DR3", "cat": "astro-ph.GA", "authors": ["A. B. A. Queiroz", "F. Anders", "C. Chiappini", "A. Khalatyan", "B. X. Santiago", "M. Steinmetz", "M. Valentini", "A. Miglio", "D. Bossini", "B. Barbuy", "I. Minchev", "D. Minniti", "D. A. Garc\u00eda Hern\u00e1ndez", "M. Schultheis", "R. L. Beaton", "T. C. Beers", "D. Bizyaev", "J. R. Brownstein", "K. Cunha", "J. G. Fern\u00e1ndez-Trincado", "P. M. Frinchaboy", "R. R. Lane", "S. R. Majewski", "D. Nataf", "C. Nitschelm", "K. Pan", "A. Roman-Lopes", "J. S. Sobeck", "G. Stringfellow", "O. Zamora"]}, "1303": {"id": "1012.1565v2", "title": "A Survey on Data Warehouse Evolution", "url": "http://arxiv.org/pdf/1012.1565v2", "date": "2010-12-20 20:17:01", "abs": "The data warehouse (DW) technology was developed to integrate heterogeneous\ninformation sources for analysis purposes. Information sources are more and\nmore autonomous and they often change their content due to perpetual\ntransactions (data changes) and may change their structure due to continual\nusers' requirements evolving (schema changes). Handling properly all type of\nchanges is a must. In fact, the DW which is considered as the core component of\nthe modern decision support systems has to be update according to different\ntype of evolution of information sources to reflect the real world subject to\nanalysis. The goal of this paper is to propose an overview and a comparative\nstudy between different works related to the DW evolution problem.", "cat": "cs.DB", "authors": ["wided oueslati", "jalel akaichi"]}, "1304": {"id": "1409.4816v2", "title": "Compression and Encryption of Search Survey Gamma Spectra using Compressive Sensing", "url": "http://arxiv.org/pdf/1409.4816v2", "date": "2015-01-21 22:52:16", "abs": "We have investigated the application of Compressive Sensing (CS)\ncomputational method to simultaneous compression and encryption of gamma\nspectra measured with NaI(Tl) detector during wide area search survey\napplications. Our numerical experiments have demonstrated secure encryption and\nnearly lossless recovery of gamma spectra coded and decoded with CS routines.", "cat": "physics.data-an", "authors": ["Alexander Heifetz", "Sasan Bakhtiari", "Apostolos C. Raptis"]}, "1305": {"id": "1004.1912v2", "title": "Forty seven new T dwarfs from the UKIDSS Large Area Survey", "url": "http://arxiv.org/pdf/1004.1912v2", "date": "2010-04-13 13:15:15", "abs": "We report the discovery of 47 new T dwarfs in the Fourth Data Release (DR4)\nfrom the Large Area Survey (LAS) of the UKIRT Infrared Deep Sky Survey with\nspectral types ranging from T0 to T8.5. These bring the total sample of LAS T\ndwarfs to 80 as of DR4. In assigning spectral types to our objects we have\nidentified 8 new spectrally peculiar objects, and divide 7 of them into two\nclasses. H2O-H-early have a H2O-H index that differs with the H2O-J index by at\nleast 2 sub-types. CH4-J-early have a CH4-J index that disagrees with the H20-J\nindex by at least 2 subtypes. We have ruled out binarity as a sole explanation\nfor both types of peculiarity, and suggest that they may represent hitherto\nunrecognised tracers of composition and/or gravity. Clear trends in z'(AB)-J\nand Y-J are apparent for our sample, consistent with weakening absorption in\nthe red wing of the KI line at 0.77microns with decreasing effective\ntemperature. We have used our sample to estimate space densities for T6-T9\ndwarfs. By comparing our sample to Monte-Carlo simulations of field T dwarfs\nfor various mass functions of the form phi(M) \\propto M^-alpha, we have placed\nweak constraints on the form of the field mass function. Our analysis suggests\nthat the substellar mass function is declining at lower masses, with negative\nvalues of alpha preferred. This is at odds with results for young clusters that\nhave been generally found to have alpha > 0.", "cat": "astro-ph.GA", "authors": ["Ben Burningham", "D. J. Pinfield", "P. W. Lucas", "S. K. Leggett", "N. R. Deacon", "M. Tamura", "C. G. Tinney", "N. Lodieu", "Z. H. Zhang", "N. Huelamo", "H. R. A. Jones", "D. N. Murray", "D. J. Mortlock", "M. Patel", "D. Barrado y Navascues", "M. R. Zapatero Osorio", "M. Ishii", "M. Kuzuhara", "R. L. Smart"]}, "1306": {"id": "2307.04438v1", "title": "Reconfigurable Intelligent Surface Assisted Railway Communications: A survey", "url": "http://arxiv.org/pdf/2307.04438v1", "date": "2023-07-10 09:29:26", "abs": "The number of train passengers and the demand for high data rates to handle\nnew technologies such as video streaming and IoT technologies are continuously\nincreasing. Therefore the exploration of millimeter waves (mmWave) band is a\nkey technology to meet this demand. However, the high penetration loss makes\nmmWave very sensitive to blocking, limiting its coverage area. One promising,\nefficient, and low-cost solution is the reconfigurable intelligent surface\n(RIS). This paper reviews the state of the art of RIS for railway\ncommunications in the mmWave context. First, we present the different types of\nRIS and review some optimization algorithms used in the literature to find the\nRIS phase shift. Then, we review recent works on RIS in the railway domain and\nprovide future directions.", "cat": "eess.SP", "authors": ["Aline Habib", "Ammar El Falou", "Charlotte Langlais", "Marion Berbineau"]}, "1307": {"id": "2205.14815v1", "title": "Influence of the Gaia-Sausage-Enceladus on the density shape of the Galactic stellar halo revealed by halo K giants from the LAMOST survey", "url": "http://arxiv.org/pdf/2205.14815v1", "date": "2022-05-30 02:47:16", "abs": "We present a study of the influence of the Gaia-Sausage-Enceladus (GSE) on\nthe density shape of the Galactic stellar halo using 11624 K giants from the\nLAMOST survey. Every star is assigned a probability of being a member of the\nGSE based on its spherical velocities and metallicity by a Gaussian Mixture\nModel. We divide the stellar halo into two parts by the obtained probabilities,\nof which one is composed of the GSE members and defined as the GSE-related\nhalo, and the other one is referred to as the GSE-removed halo. Using a\nnon-parametric method, the radial number density profiles of the two stellar\nhalos can be well described by a single power law with a variable flattening\n$q$ ($r = \\sqrt{R^2+[(Z/q(r))]^2}, \\nu = {\\nu_0}r^{-\\alpha}$). The index\n$\\alpha$ is $4.92\\pm0.12$ for the GSE-related halo and $4.25\\pm0.14$ for the\nGSE-removed halo. Both the two stellar halos are vertically flattened at\nsmaller radii but become more spherical at larger radii. We find that the\nGSE-related halo is less vertically flattened than the GSE-removed halo, and\nthe difference of $q$ between the two stellar halos ranges from 0.07 to 0.15.\nHowever, after the consideration of the bias, it is thought to be within 0.08\nat most of the radii. Finally, we compare our results with two Milky Way\nanalogues which experience a significant major merger in the TNG50 simulation.\nThe study of the two analogues also shows that the major merger-related stellar\nhalo has a smaller ellipticity than the major merger-removed stellar halo.", "cat": "astro-ph.GA", "authors": ["Wenbo Wu", "Gang Zhao", "Xiang-Xiang Xue", "Wenxiang Pei", "Chengqun Yang"]}, "1308": {"id": "1006.2517v1", "title": "Double-lined Spectroscopic Binary Stars in the Radial Velocity Experiment Survey", "url": "http://arxiv.org/pdf/1006.2517v1", "date": "2010-06-13 08:52:00", "abs": "We devise a new method for the detection of double-lined binary stars in a\nsample of the Radial Velocity Experiment (RAVE) survey spectra. The method is\nboth tested against extensive simulations based on synthetic spectra, and\ncompared to direct visual inspection of all RAVE spectra. It is based on the\nproperties and shape of the cross-correlation function, and is able to recover\n~80% of all binaries with an orbital period of order 1 day. Systems with\nperiods up to 1 year are still within the detection reach. We have applied the\nmethod to 25,850 spectra of the RAVE second data release and found 123\ndouble-lined binary candidates, only eight of which are already marked as\nbinaries in the SIMBAD database. Among the candidates, there are seven that\nshow spectral features consistent with the RS CVn type (solar type with active\nchromosphere) and seven that might be of W UMa type (over-contact binaries).\nOne star, HD 101167, seems to be a triple system composed of three nearly\nidentical G-type dwarfs. The tested classification method could also be\napplicable to the data of the upcoming Gaia mission.", "cat": "astro-ph.SR", "authors": ["G. Matijevic", "T. Zwitter", "U. Munari", "O. Bienayme", "J. Binney", "J. Bland-Hawthorn", "C. Boeche", "R. Campbell", "K. C. Freeman", "B. Gibson", "G. Gilmore", "E. K. Grebel", "A. Helmi", "J. F. Navarro", "Q. A. Parker", "G. M. Seabroke", "A. Siebert", "A. Siviero", "M. Steinmetz", "F. G. Watson", "M. Williams", "R. F. G. Wyse"]}, "1309": {"id": "1511.00883v1", "title": "Allsky NICER and NICEST extinction maps based on the 2MASS near-infrared survey", "url": "http://arxiv.org/pdf/1511.00883v1", "date": "2015-11-03 12:41:09", "abs": "Extinction remains one of the most reliable methods of measuring column\ndensity of nearby Galactic interstellar clouds. The current and ongoing\nnear-infrared surveys enable the mapping of extinction over large sky areas. We\nproduce allsky extinction maps using the 2MASS near-infrared survey. We use the\nNICER and NICEST methods to convert the near-infrared colour excesses to\nextinction estimates. The results are presented in Healpix format at the\nresolutions of 3.0, 4.5, and 12.0 arcmin. The main results of this study are\nthe calculated J-band extinction maps. The comparison with earlier large-scale\nextinction mappings shows good correspondence but also demonstrates the\npresence of resolution-dependent bias. A large fraction of the bias can be\ncorrected by using the NICEST method. For individual regions, best extinction\nestimates are obtained by careful analysis of the local stellar population and\nthe use of the highest resolution afforded by the stellar density. However, the\nuniform allsky maps should still be useful for many global studies and as the\nfirst step into the investigation of individual clouds.", "cat": "astro-ph.GA", "authors": ["M. Juvela", "J. Montillaud"]}, "1310": {"id": "1904.12444v1", "title": "The K2-HERMES Survey: Age and Metallicity of the Thick Disc", "url": "http://arxiv.org/pdf/1904.12444v1", "date": "2019-04-29 04:35:08", "abs": "Asteroseismology is a promising tool to study Galactic structure and\nevolution because it can probe the ages of stars. Earlier attempts comparing\nseismic data from the {\\it Kepler} satellite with predictions from Galaxy\nmodels found that the models predicted more low-mass stars compared to the\nobserved distribution of masses. It was unclear if the mismatch was due to\ninaccuracies in the Galactic models, or the unknown aspects of the selection\nfunction of the stars. Using new data from the K2 mission, which has a\nwell-defined selection function, we find that an old metal-poor thick disc, as\nused in previous Galactic models, is incompatible with the asteroseismic\ninformation. We show that spectroscopic measurements of [Fe/H] and\n[$\\alpha$/Fe] elemental abundances from the GALAH survey indicate a mean\nmetallicity of $\\log (Z/Z_{\\odot})=-0.16$ for the thick disc. Here $Z$ is the\neffective solar-scaled metallicity, which is a function of [Fe/H] and\n[$\\alpha$/Fe]. With the revised disc metallicities, for the first time, the\ntheoretically predicted distribution of seismic masses show excellent agreement\nwith the observed distribution of masses. This provides an indirect\nverification of the asteroseismic mass scaling relation is good to within five\npercent. Using an importance-sampling framework that takes the selection\nfunction into account, we fit a population synthesis model of the Galaxy to the\nobserved seismic and spectroscopic data. Assuming the asteroseismic scaling\nrelations are correct, we estimate the mean age of the thick disc to be about\n10 Gyr, in agreement with the traditional idea of an old $\\alpha$-enhanced\nthick disc.", "cat": "astro-ph.GA", "authors": ["Sanjib Sharma", "Dennis Stello", "Joss Bland-Hawthorn", "Michael R. Hayden", "Joel C. Zinn", "Thomas Kallinger", "Marc Hon", "Martin Asplund", "Sven Buder", "Gayandhi M. De Silva", "Valentina D'Orazi", "Ken Freeman", "Janez Kos", "Geraint F. Lewis", "Jane Lin", "Karin Lind", "Sarah Martell", "Jeffrey D. Simpson", "Rob A. Wittenmyer", "Daniel B. Zucker", "Tomaz Zwitter", "Timothy R. Bedding", "Boquan Chen", "Klemen Cotar", "James Esdaile", "Jonathan Horner", "Daniel Huber", "Prajwal R. Kafle", "Shourya Khanna", "Tanda Li", "Yuan-Sen Ting", "David M. Nataf", "Thomas Nordlander", "Hafiz Saddon", "Gregor Traven", "Duncan Wright", "Rosemary F. G. Wyse"]}, "1311": {"id": "2006.00575v4", "title": "Neural Entity Linking: A Survey of Models Based on Deep Learning", "url": "http://arxiv.org/pdf/2006.00575v4", "date": "2022-04-07 17:56:30", "abs": "This survey presents a comprehensive description of recent neural entity\nlinking (EL) systems developed since 2015 as a result of the \"deep learning\nrevolution\" in natural language processing. Its goal is to systemize design\nfeatures of neural entity linking systems and compare their performance to the\nremarkable classic methods on common benchmarks. This work distills a generic\narchitecture of a neural EL system and discusses its components, such as\ncandidate generation, mention-context encoding, and entity ranking, summarizing\nprominent methods for each of them. The vast variety of modifications of this\ngeneral architecture are grouped by several common themes: joint entity mention\ndetection and disambiguation, models for global linking, domain-independent\ntechniques including zero-shot and distant supervision methods, and\ncross-lingual approaches. Since many neural models take advantage of entity and\nmention/context embeddings to represent their meaning, this work also overviews\nprominent entity embedding techniques. Finally, the survey touches on\napplications of entity linking, focusing on the recently emerged use-case of\nenhancing deep pre-trained masked language models based on the Transformer\narchitecture.", "cat": "cs.CL", "authors": ["Ozge Sevgili", "Artem Shelmanov", "Mikhail Arkhipov", "Alexander Panchenko", "Chris Biemann"]}, "1312": {"id": "2103.00111v5", "title": "Graph Self-Supervised Learning: A Survey", "url": "http://arxiv.org/pdf/2103.00111v5", "date": "2022-05-04 13:18:56", "abs": "Deep learning on graphs has attracted significant interests recently.\nHowever, most of the works have focused on (semi-) supervised learning,\nresulting in shortcomings including heavy label reliance, poor generalization,\nand weak robustness. To address these issues, self-supervised learning (SSL),\nwhich extracts informative knowledge through well-designed pretext tasks\nwithout relying on manual labels, has become a promising and trending learning\nparadigm for graph data. Different from SSL on other domains like computer\nvision and natural language processing, SSL on graphs has an exclusive\nbackground, design ideas, and taxonomies. Under the umbrella of graph\nself-supervised learning, we present a timely and comprehensive review of the\nexisting approaches which employ SSL techniques for graph data. We construct a\nunified framework that mathematically formalizes the paradigm of graph SSL.\nAccording to the objectives of pretext tasks, we divide these approaches into\nfour categories: generation-based, auxiliary property-based, contrast-based,\nand hybrid approaches. We further describe the applications of graph SSL across\nvarious research fields and summarize the commonly used datasets, evaluation\nbenchmark, performance comparison and open-source codes of graph SSL. Finally,\nwe discuss the remaining challenges and potential future directions in this\nresearch field.", "cat": "cs.LG", "authors": ["Yixin Liu", "Ming Jin", "Shirui Pan", "Chuan Zhou", "Yu Zheng", "Feng Xia", "Philip S. Yu"]}, "1313": {"id": "2302.07484v3", "title": "Measurement of the matter-radiation equality scale using the extended Baryon Oscillation Spectroscopic Survey Quasar Sample", "url": "http://arxiv.org/pdf/2302.07484v3", "date": "2023-10-05 16:17:24", "abs": "The position of the peak of the matter power spectrum, the so-called turnover\nscale, is set by the horizon size at the epoch of matter-radiation equality. It\ncan easily be predicted in terms of the physics of the Universe in the\nrelativistic era, and so can be used as a standard ruler, independent of other\nfeatures present in the matter power spectrum, such as baryon acoustic\noscillations (BAO). We use the distribution of quasars measured by the extended\nBaryon Oscillation Spectroscopic Survey (eBOSS) to determine the turnover scale\nin a model-independent fashion statistically. We avoid modelling the BAO by\ndown-weighting affected scales in the covariance matrix using the mode\ndeprojection technique. We measure the wavenumber of the peak to be\n$k_\\mathrm{TO} = \\left( 17.6^{+1.9}_{-1.8} \\right) \\times\n10^{-3}h/\\mathrm{Mpc}$, corresponding to a dilation scale of $\nD_\\mathrm{V}(z_\\mathrm{eff} = 1.48) =\n\\left({36.2^{+4.1}_{-4.4}}\\right)r_\\mathrm{H}$. This is not competitive with\ncurrent BAO distance measures in terms of determining the expansion history but\ndoes provide a useful cross-check. We combine this measurement with\nlow-redshift distance measurements from type-Ia supernova data from Pantheon\nand BAO data from eBOSS to make a sound-horizon free estimate of the\nHubble-Lema\\^itre parameter and find it to be $H_0=\\left({74.7\\pm 9.6}\\right) \\\n\\mathrm{km/s/Mpc}$ with Pantheon, and $H_0=\\left({72.9^{+10.0}_{-8.6}}\\right) \\\n\\mathrm{km/s/Mpc}$ with eBOSS BAO. We make predictions for the measurement of\nthe turnover scale by the Dark Energy Spectroscopic Instrument (DESI) survey,\nthe Maunakea Spectroscopic Explorer (MSE) and MegaMapper, which will make more\nprecise and accurate distance determinations.", "cat": "astro-ph.CO", "authors": ["Benedict Bahr-Kalus", "David Parkinson", "Eva-Maria Mueller"]}, "1314": {"id": "0804.0653v1", "title": "MOA-cam3: a wide-field mosaic CCD camera for a gravitational microlensing survey in New Zealand", "url": "http://arxiv.org/pdf/0804.0653v1", "date": "2008-04-04 05:40:26", "abs": "We have developed a wide-field mosaic CCD camera, MOA-cam3, mounted at the\nprime focus of the Microlensing Observations in Astrophysics (MOA) 1.8-m\ntelescope. The camera consists of ten E2V CCD4482 chips, each having 2kx4k\npixels, and covers a 2.2 deg^2 field of view with a single exposure. The\noptical system is well optimized to realize uniform image quality over this\nwide field. The chips are constantly cooled by a cryocooler at -80C, at which\ntemperature dark current noise is negligible for a typical 1-3 minute exposure.\nThe CCD output charge is converted to a 16-bit digital signal by the GenIII\nsystem (Astronomical Research Cameras Inc.) and readout is within 25 seconds.\nReadout noise of 2--3 ADU (rms) is also negligible. We prepared a wide-band red\nfilter for an effective microlensing survey and also Bessell V, I filters for\nstandard astronomical studies. Microlensing studies have entered into a new\nera, which requires more statistics, and more rapid alerts to catch exotic\nlight curves. Our new system is a powerful tool to realize both these\nrequirements.", "cat": "astro-ph", "authors": ["T. Sako", "T. Sekiguchi", "M. Sasaki", "K. Okajima", "F. Abe", "I. A. Bond", "J. B. Hearnshaw", "Y. Itow", "K. Kamiya", "P. M. Kilmartin", "K. Masuda", "Y. Matsubara", "Y. Muraki", "N. J. Rattenbury", "D. J. Sullivan", "T. Sumi", "P. Tristram", "T. Yanagisawa", "P. C. M. Yock"]}, "1315": {"id": "2309.17192v1", "title": "A Survey of Incremental Transfer Learning: Combining Peer-to-Peer Federated Learning and Domain Incremental Learning for Multicenter Collaboration", "url": "http://arxiv.org/pdf/2309.17192v1", "date": "2023-09-29 12:43:21", "abs": "Due to data privacy constraints, data sharing among multiple clinical centers\nis restricted, which impedes the development of high performance deep learning\nmodels from multicenter collaboration. Naive weight transfer methods share\nintermediate model weights without raw data and hence can bypass data privacy\nrestrictions. However, performance drops are typically observed when the model\nis transferred from one center to the next because of the forgetting problem.\nIncremental transfer learning, which combines peer-to-peer federated learning\nand domain incremental learning, can overcome the data privacy issue and\nmeanwhile preserve model performance by using continual learning techniques. In\nthis work, a conventional domain/task incremental learning framework is adapted\nfor incremental transfer learning. A comprehensive survey on the efficacy of\ndifferent regularization-based continual learning methods for multicenter\ncollaboration is performed. The influences of data heterogeneity, classifier\nhead setting, network optimizer, model initialization, center order, and weight\ntransfer type have been investigated thoroughly. Our framework is publicly\naccessible to the research community for further development.", "cat": "cs.LG", "authors": ["Yixing Huang", "Christoph Bert", "Ahmed Gomaa", "Rainer Fietkau", "Andreas Maier", "Florian Putz"]}, "1316": {"id": "2012.04075v1", "title": "Efficient Attitude Estimators: A Tutorial and Survey", "url": "http://arxiv.org/pdf/2012.04075v1", "date": "2020-12-07 21:41:12", "abs": "Inertial sensors based on micro-electromechanical systems (MEMS) technology,\nsuch as accelerometers and angular rate sensors, are cost-effective solutions\nused in inertial navigation systems in a broad spectrum of applications that\nestimate position, velocity and orientation of a system with respect to an\ninertial reference frame. The task of an orientation filter is to compute an\noptimal solution for the attitude state, consisting of roll, pitch and yaw,\nthrough the fusion of angular rate, accelerometer, and magnetometer\nmeasurements. The aim of this paper is threefold: first, it serves researchers\nand practitioners in the signal processing community seeking the most\nappropriate attitude estimators that fulfills their needs, shedding light on\nthe drawbacks and the advantages of a wide variety of designs. Second, it\nserves as a survey and tutorial for existing estimator designs in the\nliterature, assessing their design aspects and components, and dissecting their\nhidden details for the benefit of researchers. Third, a comprehensive list of\nalgorithms is discussed for a fully functional inertial navigation system,\nstarting from the navigation equations and ending with the filter equations,\nkeeping in mind their suitability for power limited embedded processors. The\nsource code of all algorithms is published, with the aim of it being an\nout-of-box solution for researchers in the field. The reader will take away the\nfollowing concepts from this article: understand the key concepts of an\ninertial navigation system; be able to implement and test a complete stand\nalone solution; be able to evaluate and understand different algorithms;\nunderstand the trade-offs between different filter architectures and\ntechniques; and understand efficient embedded processing techniques, trends and\nopportunities.", "cat": "cs.RO", "authors": ["Hussein Al-Jlailaty", "Mohammad M. Mansour"]}, "1317": {"id": "2306.03446v1", "title": "Computational Agent-based Models in Opinion Dynamics: A Survey on Social Simulations and Empirical Studies", "url": "http://arxiv.org/pdf/2306.03446v1", "date": "2023-06-06 06:56:27", "abs": "Understanding how an individual changes its attitude, belief, and opinion due\nto other people's social influences is vital because of its wide implications.\nA core methodology that is used to study the change of attitude under social\ninfluences is agent-based model (ABM). The goal of this review paper is to\ncompare and contrast existing ABMs, which I classify into two families, the\ndeductive ABMs and the inductive ABMs. The former subsumes social simulation\nstudies, and the latter involves human experiments. To facilitate the\ncomparison between ABMs of different formulations, I propose a general unified\nformulation, in which all ABMs can be viewed as special cases. In addition, I\nshow the connections between deductive ABMs and inductive ABMs, and point out\ntheir strengths and limitations. At the end of the paper, I identify\nunderexplored areas and suggest future research directions.", "cat": "cs.SI", "authors": ["Yun-Shiuan Chuang", "Timothy T. Rogers"]}, "1318": {"id": "2009.02114v1", "title": "Authentication and authorization in microservice-based systems: survey of architecture patterns", "url": "http://arxiv.org/pdf/2009.02114v1", "date": "2020-09-04 11:19:54", "abs": "Context. Service-oriented architecture and its microservice-based approach\nincrease an attack surface of applications. Exposed microservices become a\npivot point for advanced persistent threats and completely change the threat\nlandscape. Correctly implemented authentication and authorization architecture\npatterns are basis of any software maturity program. Objective. The aim of this\nstudy is to provide a helpful resource to application security architect and\ndevelopers on existing architecture patterns to implement authentication and\nauthorization in microservices-based systems. Method. In this paper, we conduct\na review of major electronic databases and libraries as well as security\nstandards and presentations at the major security conferences. Results. In this\nwork based on research papers and major security conferences presentations\nanalysis we identified industry best practices in authentication and\nauthorization patterns and its applicability depending on environment\ncharacteristic. For each described patterns we reviewed its advantages and\ndisadvantages that could be used as decision-making criteria for application\nsecurity architects during architecture design phase.", "cat": "cs.CR", "authors": ["Alexander Barabanov", "Denis Makrushin"]}, "1319": {"id": "2408.00243v1", "title": "A Survey on the Applications of Zero-Knowledge Proofs", "url": "http://arxiv.org/pdf/2408.00243v1", "date": "2024-08-01 02:47:30", "abs": "Zero-knowledge proofs (ZKPs) represent a revolutionary advance in\ncomputational integrity and privacy technology, enabling the secure and private\nexchange of information without revealing underlying private data. ZKPs have\nunique advantages in terms of universality and minimal security assumptions\nwhen compared to other privacy-sensitive computational methods for distributed\nsystems, such as homomorphic encryption and secure multiparty computation.\nTheir application spans multiple domains, from enhancing privacy in blockchain\nto facilitating confidential verification of computational tasks. This survey\nstarts with a high-level overview of the technical workings of ZKPs with a\nfocus on an increasingly relevant subset of ZKPs called zk-SNARKS. While there\nhave been prior surveys on the algorithmic and theoretical aspects of ZKPs, our\nwork is distinguished by providing a broader view of practical aspects and\ndescribing many recently-developed use cases of ZKPs across various domains.\nThese application domains span blockchain privacy, scaling, storage, and\ninteroperability, as well as non-blockchain applications like voting,\nauthentication, timelocks, and machine learning. Aimed at both practitioners\nand researchers, the survey also covers foundational components and\ninfrastructure such as zero-knowledge virtual machines (zkVM), domain-specific\nlanguages (DSLs), supporting libraries, frameworks, and protocols. We conclude\nwith a discussion on future directions, positioning ZKPs as pivotal in the\nadvancement of cryptographic practices and digital privacy across many\napplications.", "cat": "cs.CR", "authors": ["Ryan Lavin", "Xuekai Liu", "Hardhik Mohanty", "Logan Norman", "Giovanni Zaarour", "Bhaskar Krishnamachari"]}, "1320": {"id": "1511.00148v1", "title": "A survey on measuring indirect discrimination in machine learning", "url": "http://arxiv.org/pdf/1511.00148v1", "date": "2015-10-31 16:04:12", "abs": "Nowadays, many decisions are made using predictive models built on historical\ndata.Predictive models may systematically discriminate groups of people even if\nthe computing process is fair and well-intentioned. Discrimination-aware data\nmining studies how to make predictive models free from discrimination, when\nhistorical data, on which they are built, may be biased, incomplete, or even\ncontain past discriminatory decisions. Discrimination refers to disadvantageous\ntreatment of a person based on belonging to a category rather than on\nindividual merit. In this survey we review and organize various discrimination\nmeasures that have been used for measuring discrimination in data, as well as\nin evaluating performance of discrimination-aware predictive models. We also\ndiscuss related measures from other disciplines, which have not been used for\nmeasuring discrimination, but potentially could be suitable for this purpose.\nWe computationally analyze properties of selected measures. We also review and\ndiscuss measuring procedures, and present recommendations for practitioners.\nThe primary target audience is data mining, machine learning, pattern\nrecognition, statistical modeling researchers developing new methods for\nnon-discriminatory predictive modeling. In addition, practitioners and policy\nmakers would use the survey for diagnosing potential discrimination by\npredictive models.", "cat": "cs.CY", "authors": ["Indre Zliobaite"]}, "1321": {"id": "1903.07446v2", "title": "The Road Ahead for Networking: A Survey on ICN-IP Coexistence Solutions", "url": "http://arxiv.org/pdf/1903.07446v2", "date": "2019-10-15 18:29:43", "abs": "In recent years, the current Internet has experienced an unexpected paradigm\nshift in the usage model, which has pushed researchers towards the design of\nthe Information-Centric Networking (ICN) paradigm as a possible replacement of\nthe existing architecture. Even though both Academia and Industry have\ninvestigated the feasibility and effectiveness of ICN, achieving the complete\nreplacement of the Internet Protocol (IP) is a challenging task.\n Some research groups have already addressed the coexistence by designing\ntheir own architectures, but none of those is the final solution to move\ntowards the future Internet considering the unaltered state of the networking.\nTo design such architecture, the research community needs now a comprehensive\noverview of the existing solutions that have so far addressed the coexistence.\nThe purpose of this paper is to reach this goal by providing the first\ncomprehensive survey and classification of the coexistence architectures\naccording to their features (i.e., deployment approach, deployment scenarios,\naddressed coexistence requirements and architecture or technology used) and\nevaluation parameters (i.e., challenges emerging during the deployment and the\nruntime behaviour of an architecture). We believe that this paper will finally\nfill the gap required for moving towards the design of the final coexistence\narchitecture.", "cat": "cs.NI", "authors": ["Mauro Conti", "Ankit Gangwal", "Muhammad Hassan", "Chhagan Lal", "Eleonora Losiouk"]}, "1322": {"id": "1910.02075v2", "title": "The PAU Survey: Background light estimation with deep learning techniques", "url": "http://arxiv.org/pdf/1910.02075v2", "date": "2020-05-05 17:06:27", "abs": "In any imaging survey, measuring accurately the astronomical background light\nis crucial to obtain good photometry. This paper introduces BKGnet, a deep\nneural network to predict the background and its associated error. BKGnet has\nbeen developed for data from the Physics of the Accelerating Universe Survey\n(PAUS), an imaging survey using a 40 narrow-band filter camera (PAUCam). Images\nobtained with PAUCam are affected by scattered light: an optical effect\nconsisting of light multiply that deposits energy in specific detector regions\ncontaminating the science measurements. Fortunately, scattered light is not a\nrandom effect, but it can be predicted and corrected for. We have found that\nBKGnet background predictions are very robust to distorting effects, while\nstill being statistically accurate. On average, the use of BKGnet improves the\nphotometric flux measurements by 7% and up to 20% at the bright end. BKGnet\nalso removes a systematic trend in the background error estimation with\nmagnitude in the i-band that is present with the current PAU data management\nmethod. With BKGnet, we reduce the photometric redshift outlier rate", "cat": "astro-ph.IM", "authors": ["Laura Cabayol-Garcia", "Martin B. Eriksen", "\u00c0lex Alarc\u00f3n", "Adam Amara", "Jorge Carretero", "Ricard Casas", "Francisco Javier Castander", "Enrique Fern\u00e1ndez", "Juan Garc\u00eda-Bellido", "Enrique Gaztanaga", "Henk Hoekstra", "Ramon Miquel", "Christian Neissner", "Cristobal Padilla", "Eusebio S\u00e1nchez", "Santiago Serrano", "Ignacio Sevilla-Noarbe", "Malgorzata Siudek", "Pau Tallada", "Luca Tortorelli"]}, "1323": {"id": "1404.0023v1", "title": "Candidate Clusters of Galaxies at $z>1.3$ Identified in the Spitzer SPT Deep Field Survey", "url": "http://arxiv.org/pdf/1404.0023v1", "date": "2014-03-31 20:11:39", "abs": "We present 279 galaxy cluster candidates at $z > 1.3$ selected from the 94\ndeg$^{2}$ Spitzer South Pole Telescope Deep Field (SSDF) survey. We use a\nsimple algorithm to select candidate high-redshift clusters of galaxies based\non Spitzer/IRAC mid-infrared data combined with shallow all-sky optical data.\nWe identify distant cluster candidates in SSDF adopting an overdensity\nthreshold that results in a high purity (80%) cluster sample based on tests in\nthe Spitzer Deep, Wide-Field Survey of the Bo\\\"otes field. Our simple algorithm\ndetects all three $1.4 < z \\leq 1.75$ X-ray detected clusters in the Bo\\\"otes\nfield. The uniqueness of the SSDF survey resides not just in its area, one of\nthe largest contiguous extragalactic fields observed with Spitzer, but also in\nits deep, multi-wavelength coverage by the South Pole Telescope (SPT),\nHerschel/SPIRE and XMM-Newton. This rich dataset will allow direct or stacked\nmeasurements of Sunyaev-Zel'dovich effect decrements or X-ray masses for many\nof the SSDF clusters presented here, and enable systematic study of the most\ndistant clusters on an unprecedented scale. We measure the angular correlation\nfunction of our sample and find that these candidates show strong clustering.\nEmploying the COSMOS/UltraVista photometric catalog in order to infer the\nredshift distribution of our cluster selection, we find that these clusters\nhave a comoving number density $n_c = (0.7^{+6.3}_{-0.6}) \\times 10^{-7} h^{3}\n\\mathrm{Mpc}^{-3}$ and a spatial clustering correlation scale length $r_0 = (32\n\\pm 7) h^{-1} \\rm{Mpc}$. Assuming our sample is comprised of dark matter halos\nabove a characteristic minimum mass, $M_{{\\rm min}}$, we derive that at $z=1.5$\nthese clusters reside in halos larger than $M_{{\\rm min}} = 1.5^{+0.9}_{-0.7}\n\\times 10^{14} h^{-1} M_{\\odot}$. (abridged)", "cat": "astro-ph.CO", "authors": ["A. Rettura", "J. Martinez-Manso", "D. Stern", "S. Mei", "M. L. N. Ashby", "M. Brodwin", "D. Gettings", "A. H. Gonzalez", "S. A. Stanford", "J. G. Bartlett"]}, "1324": {"id": "1611.05930v2", "title": "Cosmic X-ray surveys of Active Galactic Nuclei: synergy between X-ray and infrared observations", "url": "http://arxiv.org/pdf/1611.05930v2", "date": "2016-11-21 20:50:29", "abs": "We briefly review the synergy between X-ray and infrared observations for\nActive Galactic Nuclei (AGNs) detected in cosmic X-ray surveys, primarily with\nXMM-Newton, Chandra, and NuSTAR. We focus on two complementary aspects of this\nX-ray-infrared synergy (1) the identification of the most heavily obscured AGNs\nand (2) the connection between star formation and AGN activity. We also briefly\ndiscuss future prospects for X-ray-infrared studies over the next decade.", "cat": "astro-ph.HE", "authors": ["D. M. Alexander"]}, "1325": {"id": "1505.06990v1", "title": "A survey of X-ray emission from 100 kpc radio jets", "url": "http://arxiv.org/pdf/1505.06990v1", "date": "2015-05-26 15:01:34", "abs": "We have completed a Chandra snapshot survey of 54 radio jets that are\nextended on arcsec scales. These are associated with flat spectrum radio\nquasars spanning a redshift range z=0.3 to 2.1. X-ray emission is detected from\nthe jet of approximately 60% of the sample objects. We assume minimum energy\nand apply conditions consistent with the original Felten-Morrison calculations\nin order to estimate the Lorentz factors and the apparent Doppler factors. This\nallows estimates of the enthalpy fluxes, which turn out to be comparable to the\nradiative luminosities.", "cat": "astro-ph.HE", "authors": ["Daniel A Schwartz", "Herman L Marshall", "Diana M Worrall", "Mark Birkinshaw", "Eric Perlman", "James E J Lovell", "David Jauncey", "David Murphy", "Jonathan Gelbord", "Leith Godfrey", "Geoffrey Bicknell"]}, "1326": {"id": "1209.0856v1", "title": "A Survey of the Return Times Theorem", "url": "http://arxiv.org/pdf/1209.0856v1", "date": "2012-09-05 03:41:40", "abs": "The goal of this paper is to survey the history, development and current\nstatus of the Return Times Theorem and its many extensions and variations. Let\n$(X, \\mathcal{F}, \\mu)$ be a finite measure space and let $T:X \\rightarrow X$\nbe a measure preserving transformation. Perhaps the oldest result in ergodic\ntheory is that of Poincar\\'e's Recurrence Principle which states: For any set\n$A \\in \\mathcal{F}$, the set of points $x$ of $A$ such that $T^nx$ is not in\nthe set $A$ for all $n > 0$ has zero measure. This says that almost every point\nof $A$ returns to $A$. In fact, almost every point of $A$ returns to $A$\ninfinitely often.\n The return time for a given element $x \\in A$, $r_A(x) = \\inf\\{k \\geq 1: T^kx\n\\in A\\}$, is the first time that the element $x$ returns to the set $A$. By\nPoincar\\'e's Recurrence Principle there is set of full measure in $A$ such that\nall elements of this set have a finite return time. Our study of the Return\nTimes Theorem asks how we can further generalize this notion.\n The paper begins by looking at early work with the concept of weighted\naverages. The second portion of the paper focuses on the historical development\nof the proofs of the Return Times Theorem. Three areas of extension of the\nReturn Times Theorem are then considered: a multiterm version, characteristic\nfactors and breaking the H\\\"olderian duality. The paper concludes with\ndiscussion of some more recent work and open questions to consider.", "cat": "math.DS", "authors": ["Idris Assani", "Kimberly Presser"]}, "1327": {"id": "2301.00394v2", "title": "Deep Learning Technique for Human Parsing: A Survey and Outlook", "url": "http://arxiv.org/pdf/2301.00394v2", "date": "2024-03-14 02:00:19", "abs": "Human parsing aims to partition humans in image or video into multiple\npixel-level semantic parts. In the last decade, it has gained significantly\nincreased interest in the computer vision community and has been utilized in a\nbroad range of practical applications, from security monitoring, to social\nmedia, to visual special effects, just to name a few. Although deep\nlearning-based human parsing solutions have made remarkable achievements, many\nimportant concepts, existing challenges, and potential research directions are\nstill confusing. In this survey, we comprehensively review three core\nsub-tasks: single human parsing, multiple human parsing, and video human\nparsing, by introducing their respective task settings, background concepts,\nrelevant problems and applications, representative literature, and datasets. We\nalso present quantitative performance comparisons of the reviewed methods on\nbenchmark datasets. Additionally, to promote sustainable development of the\ncommunity, we put forward a transformer-based human parsing framework,\nproviding a high-performance baseline for follow-up research through universal,\nconcise, and extensible solutions. Finally, we point out a set of\nunder-investigated open issues in this field and suggest new directions for\nfuture study. We also provide a regularly updated project page, to continuously\ntrack recent developments in this fast-advancing field:\nhttps://github.com/soeaver/awesome-human-parsing.", "cat": "cs.CV", "authors": ["Lu Yang", "Wenhe Jia", "Shan Li", "Qing Song"]}, "1328": {"id": "0909.0095v2", "title": "Online Algorithms for Self-Organizing Sequential Search - A Survey", "url": "http://arxiv.org/pdf/0909.0095v2", "date": "2009-09-02 03:48:38", "abs": "The main objective of this survey is to present the important theoretical and\nexperimental results contributed till date in the area of online algorithms for\nthe self organizing sequential search problem, also popularly known as the List\nUpdate Problem(LUP) in a chronological way. The survey includes competitiveness\nresults of deterministic and randomized online algorithms and complexity\nresults of optimal off line algorithms for the list update problem. We also\npresent the results associated with list update with look ahead, list update\nwith locality of reference and other variants of the list update problem. We\ninvestigate research issues, explore scope of future work associated with each\nissue so that future researchers can find it useful to work on.", "cat": "cs.DS", "authors": ["Rakesh Mohanty", "N. S. Narayanaswamy"]}, "1329": {"id": "1603.06174v1", "title": "Classification of graph algebras: A selective survey", "url": "http://arxiv.org/pdf/1603.06174v1", "date": "2016-03-20 02:41:02", "abs": "This survey reports on current progress of programs to classify graph\nC*-algebras and Leavitt path algebras up to Morita equivalence using K-theory.\nBeginning with an overview and some history, we trace the development of the\nclassification of simple and nonsimple graph C*-algebras and state theorems\nsummarizing the current status of these efforts. We then discuss the much more\nnascent efforts to classify Leavitt path algebras, and we describe the current\nstatus of these efforts as well as outline current impediments that must be\nsolved for this classification program to progress. In particular, we give two\nspecific open problems that must be addressed in order to identify the correct\nK-theoretic invariant for classification of simple Leavitt path algebras, and\nwe discuss the significance of various possible outcomes to these open\nproblems.", "cat": "math.OA", "authors": ["Mark Tomforde"]}, "1330": {"id": "1406.0966v1", "title": "100 deg$^2$ Mock Galaxy Cone for HI Surveys with the Early SKA", "url": "http://arxiv.org/pdf/1406.0966v1", "date": "2014-06-04 08:09:35", "abs": "We distribute an easy-to-use mock catalog of galaxies with detailed neutral\natomic hydrogen (HI) and auxiliary molecular and optical properties. The\ncatalog covers a field of 10-by-10 degrees and a redshift range of z=0-1.2. It\ncontains galaxies with 21cm peak flux densities down to 1uJy and is, within\nthis flux limit, complete for HI masses above 10^8 solar masses. Five random\nrealisations of the catalog in ASCII format (~4GB/file) and subtables with HI\nflux limits of 10u Jy (~500MB/file) and 100uJy$ (~30MB/file) can be downloaded\nat http://ict.icrar.org/store/staff/do/s3sax.", "cat": "astro-ph.GA", "authors": ["Danail Obreschkow", "Martin Meyer"]}, "1331": {"id": "2310.02799v2", "title": "Dissecting Smart Contract Languages: A Survey", "url": "http://arxiv.org/pdf/2310.02799v2", "date": "2023-10-06 15:22:20", "abs": "Blockchain is a distributed ledger technology that gained popularity for\nenabling the transformation of cryptocurrency among peers without mediation by\na centralized third-party authority. Smart contracts expand the applications of\nblockchain technology and have played a role in its widespread adoption. Smart\ncontracts are immutable digital programs that are deployed on blockchains to\ncodify agreements between parties. Existing smart contract implementations have\nfaced challenges, including security vulnerabilities, leading to significant\nlosses and concerns. This has stimulated a wave of attempts to improve Smart\nContract Languages (SCLs) to overcome implementation challenges and ensure code\nquality, producing many languages with diverse features. Scholars have made\nsome attempts to classify SCLs and clarify the process of selecting an SCL, but\nto the best of our knowledge, no comprehensive survey of existing SCLs has been\npublished. Our work surpasses earlier efforts by evaluating a significantly\nlarger set of SCLs, in greater depth, to ease the process of SCL selection for\nblockchain research and implementation. In this paper, we (1) propose a robust\nframework for comparing existing SCLs, (2) analyze and discuss 36 SCLs,\naddressing issues beyond those used to construct the comparison framework, and\n(3) define new parameters for future research and development of SCLs. The\nsurvey provides a guide for those who intend to select or use an SCL to\nimplement smart contracts, develop new SCLs, or add new extensions to the\nexisting SCLs.", "cat": "cs.CR", "authors": ["Majd Soud", "G\u00edsli Hj\u00e1lmt\u00fdsson", "Mohammad Hamdaqa"]}, "1332": {"id": "1801.06628v1", "title": "The SAMI Galaxy Survey: gas content and interaction as the drivers of kinematic asymmetry", "url": "http://arxiv.org/pdf/1801.06628v1", "date": "2018-01-20 05:50:47", "abs": "In order to determine the causes of kinematic asymmetry in the H$\\alpha$ gas\nin the SAMI Galaxy Survey sample, we investigate the comparative influences of\nenvironment and intrinsic properties of galaxies on perturbation. We use\nspatially resolved H$\\alpha$ velocity fields from the SAMI Galaxy Survey to\nquantify kinematic asymmetry ($\\overline{v_{asym}}$) in nearby galaxies and\nenvironmental and stellar mass data from the GAMA survey.\n {We find that local environment, measured as distance to nearest neighbour,\nis inversely correlated with kinematic asymmetry for galaxies with\n$\\mathrm{\\log(M_*/M_\\odot)}>10.0$, but there is no significant correlation for\ngalaxies with $\\mathrm{\\log(M_*/M_\\odot)}<10.0$. Moreover, low mass galaxies\n($\\mathrm{\\log(M_*/M_\\odot)}<9.0$) have greater kinematic asymmetry at all\nseparations, suggesting a different physical source of asymmetry is important\nin low mass galaxies.}\n We propose that secular effects derived from gas fraction and gas mass may be\nthe primary causes of asymmetry in low mass galaxies. High gas fraction is\nlinked to high $\\frac{\\sigma_{m}}{V}$ (where $\\sigma_m$ is H$\\alpha$ velocity\ndispersion and $V$ the rotation velocity), which is strongly correlated with\n$\\overline{v_{asym}}$, and galaxies with $\\log(M_*/M_\\odot)<9.0$ have offset\n$\\overline{\\frac{\\sigma_{m}}{V}}$ from the rest of the sample. Further,\nasymmetry as a fraction of dispersion decreases for galaxies with\n$\\log(M_*/M_\\odot)<9.0$. Gas mass and asymmetry are also inversely correlated\nin our sample. We propose that low gas masses in dwarf galaxies may lead to\nasymmetric distribution of gas clouds, leading to increased relative\nturbulence.", "cat": "astro-ph.GA", "authors": ["J. V. Bloom", "S. M. Croom", "J. J. Bryant", "A. L. Schaefer", "J. Bland-Hawthorn", "S. Brough", "J. Callingham", "L. Cortese", "C. Federrath", "N. Scott", "J. Van de Sande", "F. D'Eugenio", "S. Sweet", "C. Tonini", "J. T. Allen", "M. Goodwin", "A. W. Green", "I. S. Konstantopoulos", "J. Lawrence", "N. Lorente", "A. M. Medling", "M. S. Owers", "S. N. Richards", "R. Sharp"]}, "1333": {"id": "1504.06630v1", "title": "Dusty starbursts and the formation of elliptical galaxies: A SCUBA-2 survey of a z=1.46 cluster", "url": "http://arxiv.org/pdf/1504.06630v1", "date": "2015-04-24 20:05:10", "abs": "We report the results of a deep SCUBA-2 850- and 450-$\\mu$m survey for\ndust-obscured ultra-luminous infrared galaxies (U/LIRGs) in the field of the\nz=1.46 cluster XCS J2215.9-1738. We detect a striking overdensity of\nsub-millimeter sources coincident with the core of this cluster: $\\sim 3-4\n\\times$ higher than expected in a blank field. We use the likely radio and\nmid-infrared counterparts to show that the bulk of these sub-millimeter sources\nhave spectroscopic or photometric redshifts which place them in the cluster and\nthat their multi-wavelength properties are consistent with this association.\nThe average far-infrared luminosities of these galaxies are $(1.0\\pm0.1) \\times\n10^{12} L_{\\odot}$, placing them on the U/LIRG boundary. Using the total star\nformation occurring in the obscured U/LIRG population within the cluster we\nshow that the resulting mass-normalized star-formation rate for this system\nsupports previous claims of a rapid increase in star-formation activity in\ncluster cores out to $z\\sim1.5$, which must be associated with the on-going\nformation of the early-type galaxies which reside in massive clusters today.", "cat": "astro-ph.GA", "authors": ["C. -J. Ma", "I. Smail", "A. M. Swinbank", "J. M. Simpson", "A. P. Thomson", "C. -C. Chen", "A. L. R. Danielson", "M. Hilton", "K. Tadaki", "J. P. Stott", "T. Kodama"]}, "1334": {"id": "1910.10395v2", "title": "Spectral properties of quasars from Sloan Digital Sky Survey data release 14: The catalog", "url": "http://arxiv.org/pdf/1910.10395v2", "date": "2020-06-02 07:48:04", "abs": "We present measurements of the spectral properties for a total of 526,265\nquasars, out of which 63% have continuum S/N$>3$ pixel$^{-1}$, selected from\nthe fourteenth data release of the Sloan Digital Sky Survey (SDSS-DR14) quasar\ncatalog. We performed a careful and homogeneous analysis of the SDSS spectra of\nthese sources, to estimate the continuum and line properties of several\nemission lines such as H${\\alpha}$, H${\\beta}$, H${\\gamma}$, Mg \\textsc{ii}, C\n\\textsc{iii]}, C \\textsc{iv} and Ly${\\alpha}$. From the derived emission line\nparameters, we estimated single-epoch virial black hole masses\n($M_{\\mathrm{BH}}$) for the sample using H${\\beta}$, Mg \\textsc{ii} and C\n\\textsc{iv} emission lines. The sample covers a wide range in bolometric\nluminosity ($\\log L_{\\mathrm{bol}}$; erg s$^{-1}$) between 44.4 and 47.3 and\n$\\log M_{\\mathrm{BH}}$ between 7.1 and 9.9 $M_{\\odot}$. Using the ratio of\n$L_{\\mathrm{bol}}$ to the Eddington luminosity as a measure of the accretion\nrate, the logarithm of the accretion rate is found to be in the range between\n$-$2.06 and 0.43. We performed several correlation analyses between different\nemission line parameters and found them to match with that known earlier using\nsmaller samples. We noticed that strong Fe \\textsc{ii} sources with large\nBalmer line width, and highly accreting sources with large $M_{\\mathrm{BH}}$\nare rare in our sample. We make available online an extended and complete\ncatalog that contains various spectral properties of 526,265 quasars derived in\nthis work along with other properties culled from the SDSS-DR14 quasar catalog.", "cat": "astro-ph.GA", "authors": ["Suvendu Rakshit", "C. S. Stalin", "Jari Kotilainen"]}, "1335": {"id": "1705.01550v1", "title": "The Swift/BAT AGN Spectroscopic Survey (BASS) -- VI. The Gamma_X - L/L_Edd relation", "url": "http://arxiv.org/pdf/1705.01550v1", "date": "2017-05-03 18:00:02", "abs": "We study the observed relation between accretion rate (in terms of L/L_Edd)\nand shape of the hard X-ray spectral energy distribution (namely the photon\nindex Gamma_X) for a large sample of 228 hard X-ray selected, low-redshift\nactive galactic nuclei (AGN), drawn from the Swift/BAT AGN Spectroscopic Survey\n(BASS). This includes 30 AGN for which black hole mass (and therefore L/L_Edd)\nis measured directly through masers, spatially resolved gas or stellar\ndynamics, or reverberation mapping. The high quality and broad energy coverage\nof the data provided through BASS allow us to examine several alternative\ndeterminations of both Gamma_X and L/L_Edd. For the BASS sample as a whole, we\nfind a statistically significant, albeit very weak correlation between Gamma_X\nand L/L_Edd. The best-fitting relations we find, Gamma_X=0.15\nlog(L/L_Edd)+const., are considerably shallower than those reported in previous\nstudies. Moreover, we find no corresponding correlations among the subsets of\nAGN with different M_BH determination methodology. In particular, we find no\nrobust evidence for a correlation when considering only those AGN with direct\nor single-epoch M_BH estimates. This latter finding is in contrast to several\nprevious studies which focused on z>0.5 broad-line AGN. We discuss this tension\nand conclude that it can be partially accounted for if one adopts a simplified,\npower-law X-ray spectral model, combined with L/L_Edd estimates that are based\non the continuum emission and on single-epoch broad line spectroscopy in the\noptical regime. We finally highlight the limitations on using Gamma_X as a\nprobe of supermassive black hole evolution in deep extragalactic X-ray surveys.", "cat": "astro-ph.GA", "authors": ["Benny Trakhtenbrot", "Claudio Ricci", "Michael J. Koss", "Kevin Schawinski", "Richard Mushotzky", "Yoshihiro Ueda", "Sylvain Veilleux", "Isabella Lamperti", "Kyuseok Oh", "Ezequiel Treister", "Daniel Stern", "Fiona Harrison", "Mislav Balokovic", "Neil Gehrels"]}, "1336": {"id": "1805.00488v3", "title": "Evaluating Tests of Virialization and Substructure Using Galaxy Clusters in the ORELSE Survey", "url": "http://arxiv.org/pdf/1805.00488v3", "date": "2018-06-01 00:21:06", "abs": "We evaluated the effectiveness of different indicators of cluster\nvirialization using 12 large-scale structures in the ORELSE survey spanning\nfrom $0.7~1\nsources using a combination of WISE and SDSS-DR8 photometric catalogs. Deeper\nfollow-up imaging data from Subaru and WIYN reveal the cluster to be a rich\nsystem of galaxies, and multi-object spectroscopic observations from Keck\nconfirm five cluster members at z=0.99. The detection and confirmation of this\ncluster represents a first step towards constructing a uniformly-selected\nsample of distant, high-mass galaxy clusters over the full extragalactic sky\nusing WISE data.", "cat": "astro-ph.CO", "authors": ["Daniel P. Gettings", "Anthony H. Gonzalez", "S. Adam Stanford", "Peter R. M. Eisenhardt", "Mark Brodwin", "Conor Mancone", "Daniel Stern", "Gregory R. Zeimann", "Frank J. Masci", "Casey Papovich", "Ichi Tanaka", "Edward L. Wright"]}, "1344": {"id": "2204.13436v2", "title": "A measurement of the Integrated Sachs-Wolfe Effect with the Rapid ASKAP Continuum Survey", "url": "http://arxiv.org/pdf/2204.13436v2", "date": "2022-07-29 00:56:17", "abs": "The evolution of the gravitational potentials on large scales due to the\naccelerated expansion of the Universe is an important and independent probe of\ndark energy, known as the integrated Sachs-Wolfe (ISW) effect. We measure this\nISW effect through cross-correlating the cosmic microwave background maps from\nthe Planck satellite with a radio continuum galaxy distribution map from the\nrecent Rapid ASKAP Continuum Survey (RACS). We detect a positive\ncross-correlation at $\\sim 2.8\\,\\sigma$ relative to the null hypothesis of no\ncorrelation. We parameterise the strength of the ISW effect through an\namplitude parameter and find the constraints to be $A_{\\mathrm{ISW}} =\n0.94^{+0.42}_{-0.41}$, which is consistent with the prediction of an\naccelerating universe within the current concordance cosmological model,\n$\\Lambda$CDM. The credible interval on this parameter is independent of the\ndifferent bias models and redshift distributions that were considered when\nmarginalising over the nuisance parameters. We also detect a power excess in\nthe galaxy auto-correlation angular power spectrum on large scales ($\\ell \\leq\n40$), and investigate possible systematic causes.", "cat": "astro-ph.CO", "authors": ["Benedict Bahr-Kalus", "David Parkinson", "Jacobo Asorey", "Stefano Camera", "Catherine Hale", "Fei Qin"]}, "1345": {"id": "2405.12496v1", "title": "A Survey of Integrating Wireless Technology into Active Noise Control", "url": "http://arxiv.org/pdf/2405.12496v1", "date": "2024-05-21 04:53:39", "abs": "Active Noise Control (ANC) is a widely adopted technology for reducing\nenvironmental noise across various scenarios. This paper focuses on enhancing\nnoise reduction performance, particularly through the refinement of signal\nquality fed into ANC systems. We discuss the main wireless technique integrated\ninto the ANC system, equipped with some innovative algorithms, in diverse\nenvironments. Instead of using microphone arrays, which increase the\ncomputation complexity of the ANC system, to isolate multiple noise sources to\nimprove noise reduction performance, the application of the wireless technique\navoids extra computation demand. Wireless transmissions of reference, error,\nand control signals are also applied to improve the convergence performance of\nthe ANC system. Furthermore, this paper lists some wireless ANC applications,\nsuch as earbuds, headphones, windows, and headrests, underscoring their\nadaptability and efficiency in various settings.", "cat": "eess.AS", "authors": ["Xiaoyi Shen", "Dongyuan Shi", "Zhengding Luo", "Junwei Ji", "Woon-Seng Gan"]}, "1346": {"id": "2107.02850v1", "title": "Survey of Self-Play in Reinforcement Learning", "url": "http://arxiv.org/pdf/2107.02850v1", "date": "2021-07-06 19:33:53", "abs": "In reinforcement learning (RL), the term self-play describes a kind of\nmulti-agent learning (MAL) that deploys an algorithm against copies of itself\nto test compatibility in various stochastic environments. As is typical in MAL,\nthe literature draws heavily from well-established concepts in classical game\ntheory and so this survey quickly reviews some fundamental concepts. In what\nfollows, we present a brief survey of self-play literature, its major themes,\ncriteria, and techniques, and then conclude with an assessment of current\nshortfalls of the literature as well as suggestions for future directions.", "cat": "cs.GT", "authors": ["Anthony DiGiovanni", "Ethan C. Zell"]}, "1347": {"id": "1706.01201v1", "title": "Chandra Survey of Nearby Galaxies: A Significant Population of Candidate Central Black Holes in Late-type Galaxies", "url": "http://arxiv.org/pdf/1706.01201v1", "date": "2017-06-05 06:01:57", "abs": "Based on the Chandra data archive as of March 2016, we have identified 314\ncandidate active galactic nuclei in 719 galaxies located closer than 50 Mpc,\namong them late-type (Hubble types Sc and later) galaxies that previously had\nbeen classified from optical observations as containing star-forming (H II)\nnuclei. These late-type galaxies comprise a valuable subsample to search for\nlow-mass (<~ 10^6 solar masses) central black holes. For the sample as a whole,\nthe overall dependence of the fraction of active nuclei on galaxy type and\nnuclear spectral classification is consistent with previous results based on\noptical surveys. We detect 51 X-ray cores among the 163 H II nuclei and\nestimate that, very conservatively, ~74% of them with luminosities above 10^38\nerg/s are not contaminated by X-ray binaries; the fraction increases to ~92%\nfor X-ray cores with a luminosity of 10^39 erg/s or higher. This allows us to\nestimate a black hole occupation fraction of >~ 21% in these late-type, many\nbulgeless, galaxies.", "cat": "astro-ph.GA", "authors": ["Rui She", "Luis C. Ho", "Hua Feng"]}, "1348": {"id": "1007.2859v1", "title": "A Detailed Model Atmosphere Analysis of Cool White Dwarfs in the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1007.2859v1", "date": "2010-07-16 20:11:34", "abs": "We present optical spectroscopy and near-infrared photometry of 126 cool\nwhite dwarfs in the Sloan Digital Sky Survey (SDSS). Our sample includes high\nproper motion targets selected using the SDSS and USNO-B astrometry and a dozen\npreviously known ultracool white dwarf candidates. Our optical spectroscopic\nobservations demonstrate that a clean selection of large samples of cool white\ndwarfs in the SDSS (and the SkyMapper, Pan-STARRS, and the Large Synoptic\nSurvey Telescope datasets) is possible using a reduced proper motion diagram\nand a tangential velocity cut-off (depending on the proper motion accuracy) of\n30 km/s. Our near-infrared observations reveal eight new stars with significant\nabsorption. We use the optical and near-infrared photometry to perform a\ndetailed model atmosphere analysis. More than 80% of the stars in our sample\nare consistent with either pure hydrogen or pure helium atmospheres. However,\nthe eight stars with significant infrared absorption and the majority of the\npreviously known ultracool white dwarf candidates are best explained with mixed\nhydrogen and helium atmosphere models. The age distribution of our sample is\nconsistent with a Galactic disk age of 8 Gyr. A few ultracool white dwarfs may\nbe as old as 12-13 Gyr, but our models have problems matching the spectral\nenergy distributions of these objects. There are only two halo white dwarf\ncandidates in our sample. However, trigonometric parallax observations are\nrequired for accurate mass and age determinations and to confirm their\nmembership in the halo.", "cat": "astro-ph.GA", "authors": ["Mukremin Kilic", "S. K. Leggett", "P. -E. Tremblay", "Ted von Hippel", "P. Bergeron", "Hugh C. Harris", "Jeffrey A. Munn", "Kurtis A. Williams", "Evalyn Gates", "J. Farihi"]}, "1349": {"id": "1404.3799v2", "title": "The 6dF Galaxy Velocity Survey: Cosmological constraints from the velocity power spectrum", "url": "http://arxiv.org/pdf/1404.3799v2", "date": "2014-10-07 08:14:53", "abs": "We present scale-dependent measurements of the normalised growth rate of\nstructure $f\\sigma_{8}(k, z=0)$ using only the peculiar motions of galaxies. We\nuse data from the 6-degree Field Galaxy Survey velocity sample (6dFGSv)\ntogether with a newly-compiled sample of low-redshift $(z < 0.07)$ type Ia\nsupernovae. We constrain the growth rate in a series of $\\Delta k \\sim 0.03\nh{\\rm Mpc^{-1}}$ bins to $\\sim35\\%$ precision, including a measurement on\nscales $>300 h^{-1}{\\rm Mpc}$, which represents one of the largest-scale growth\nrate measurement to date. We find no evidence for a scale dependence in the\ngrowth rate, or any statistically significant variation from the growth rate as\npredicted by the {\\it Planck} cosmology. Bringing all the scales together, we\ndetermine the normalised growth rate at $z=0$ to $\\sim15\\%$ in a manner {\\it\nindependent} of galaxy bias and in excellent agreement with the constraint from\nthe measurements of redshift-space distortions from 6dFGS. We pay particular\nattention to systematic errors. We point out that the intrinsic scatter present\nin Fundamental-Plane and Tully-Fisher relations is only Gaussian in logarithmic\ndistance units; wrongly assuming it is Gaussian in linear (velocity) units can\nbias cosmological constraints. We also analytically marginalise over zero-point\nerrors in distance indicators, validate the accuracy of all our constraints\nusing numerical simulations, and demonstrate how to combine different\n(correlated) velocity surveys using a matrix `hyper-parameter' analysis.\nCurrent and forthcoming peculiar velocity surveys will allow us to understand\nin detail the growth of structure in the low-redshift universe, providing\nstrong constraints on the nature of dark energy.", "cat": "astro-ph.CO", "authors": ["Andrew Johnson", "Chris Blake", "Jun Koda", "Yin-Zhe Ma", "Matthew Colless", "Martin Crocce", "Tamara M. Davis", "Heath Jones", "John R. Lucey", "Christina Magoulas", "Jeremy Mould", "Morag Scrimgeour", "Christopher M. Springob"]}, "1350": {"id": "2106.07085v4", "title": "Survey: Image Mixing and Deleting for Data Augmentation", "url": "http://arxiv.org/pdf/2106.07085v4", "date": "2023-02-06 19:21:18", "abs": "Neural networks are prone to overfitting and memorizing data patterns. To\navoid over-fitting and enhance their generalization and performance, various\nmethods have been suggested in the literature, including dropout,\nregularization, label smoothing, etc. One such method is augmentation which\nintroduces different types of corruption in the data to prevent the model from\noverfitting and to memorize patterns present in the data. A sub-area of data\naugmentation is image mixing and deleting. This specific type of augmentation\neither deletes image regions or mixes two images to hide or make particular\ncharacteristics of images confusing for the network, forcing it to emphasize\nthe overall structure of the object in an image. Models trained with this\napproach have proven to perform and generalize well compared to those trained\nwithout image mixing or deleting. An added benefit that comes with this method\nof training is robustness against image corruption. Due to its low\ncomputational cost and recent success, researchers have proposed many image\nmixing and deleting techniques. We furnish an in-depth survey of image mixing\nand deleting techniques and provide categorization via their most\ndistinguishing features. We initiate our discussion with some fundamental\nrelevant concepts. Next, we present essentials, such as each category's\nstrengths and limitations, describing their working mechanism, basic\nformulations, and applications. We also discuss the general challenges and\nrecommend possible future research directions for image mixing and deleting\ndata augmentation techniques. Datasets and codes for evaluation are publicly\navailable here.", "cat": "cs.CV", "authors": ["Humza Naveed", "Saeed Anwar", "Munawar Hayat", "Kashif Javed", "Ajmal Mian"]}, "1351": {"id": "2402.03082v1", "title": "Visual Text Meets Low-level Vision: A Comprehensive Survey on Visual Text Processing", "url": "http://arxiv.org/pdf/2402.03082v1", "date": "2024-02-05 15:13:20", "abs": "Visual text, a pivotal element in both document and scene images, speaks\nvolumes and attracts significant attention in the computer vision domain.\nBeyond visual text detection and recognition, the field of visual text\nprocessing has experienced a surge in research, driven by the advent of\nfundamental generative models. However, challenges persist due to the unique\nproperties and features that distinguish text from general objects. Effectively\nleveraging these unique textual characteristics is crucial in visual text\nprocessing, as observed in our study. In this survey, we present a\ncomprehensive, multi-perspective analysis of recent advancements in this field.\nInitially, we introduce a hierarchical taxonomy encompassing areas ranging from\ntext image enhancement and restoration to text image manipulation, followed by\ndifferent learning paradigms. Subsequently, we conduct an in-depth discussion\nof how specific textual features such as structure, stroke, semantics, style,\nand spatial context are seamlessly integrated into various tasks. Furthermore,\nwe explore available public datasets and benchmark the reviewed methods on\nseveral widely-used datasets. Finally, we identify principal challenges and\npotential avenues for future research. Our aim is to establish this survey as a\nfundamental resource, fostering continued exploration and innovation in the\ndynamic area of visual text processing.", "cat": "cs.CV", "authors": ["Yan Shu", "Weichao Zeng", "Zhenhang Li", "Fangmin Zhao", "Yu Zhou"]}, "1352": {"id": "1705.06179v2", "title": "Star formation in galaxies at z~4-5 from the SMUVS survey: a clear starburst/main-sequence bimodality for Halpha emitters on the SFR-M* plane", "url": "http://arxiv.org/pdf/1705.06179v2", "date": "2017-08-18 12:21:19", "abs": "We study a large galaxy sample from the Spitzer Matching Survey of the\nUltraVISTA ultra-deep Stripes (SMUVS) to search for sources with enhanced 3.6\nmicron fluxes indicative of strong Halpha emission at z=3.9-4.9. We find that\nthe percentage of \"Halpha excess\" sources reaches 37-40% for galaxies with\nstellar masses log10(M*/Msun) ~ 9-10, and decreases to <20% at log10(M*/Msun) ~\n10.7. At higher stellar masses, however, the trend reverses, although this is\nlikely due to AGN contamination. We derive star formation rates (SFR) and\nspecific SFR (sSFR) from the inferred Halpha equivalent widths (EW) of our\n\"Halpha excess\" galaxies. We show, for the first time, that the \"Halpha excess\"\ngalaxies clearly have a bimodal distribution on the SFR-M* plane: they lie on\nthe main sequence of star formation (with log10(sSFR/yr^{-1})<-8.05) or in a\nstarburst cloud (with log10(sSFR/yr^{-1}) >-7.60). The latter contains ~15% of\nall the objects in our sample and accounts for >50% of the cosmic SFR density\nat z=3.9-4.9, for which we derive a robust lower limit of 0.066 Msun yr^{-1}\nMpc^{-3}. Finally, we identify an unusual >50sigma overdensity of z=3.9-4.9\ngalaxies within a 0.20 x 0.20 sq. arcmin region. We conclude that the SMUVS\nunique combination of area and depth at mid-IR wavelengths provides an\nunprecedented level of statistics and dynamic range which are fundamental to\nreveal new aspects of galaxy evolution in the young Universe.", "cat": "astro-ph.GA", "authors": ["K. I. Caputi", "S. Deshmukh", "M. L. N. Ashby", "W. I. Cowley", "L. Bisigello", "G. G. Fazio", "J. P. U. Fynbo", "O. Le Fevre", "B. Milvang-Jensen", "O. Ilbert"]}, "1353": {"id": "0906.5424v1", "title": "Carbon abundance in Small Magellanic Cloud planetary nebulae through Advanced Camera for Surveys prism spectroscopy: constraining stellar evolution at low metallicity", "url": "http://arxiv.org/pdf/0906.5424v1", "date": "2009-06-30 07:31:04", "abs": "We perform near ultraviolet ACS prism spectroscopy of 11 Small Magellanic\nCloud (SMC) planetary nebulae (PNe) with the main aim of deriving the abundance\nof carbon. The analysis of the ACS spectra provide reliable atomic carbon\nabundances for all but a couple of our targets; ionic C^(2+) abundances are\ncalculated for all target PNe. With the present paper we more than double the\nnumber of SMC PNe with known carbon abundances, providing a good database to\nstudy the elemental evolution in low- and intermediate-mass stars at low\nmetallicity. We study carbon abundances of Magellanic Cloud PNe in the\nframework of stellar evolution models and the elemental yields. Constraining\nSMC and LMC stellar evolutionary models is now possible with the present data,\nthrough the comparison of the final yields calculated and the CNO abundances\nobserved. We found that SMC PNe are almost exclusively carbon rich, and that\nfor the most part they have not undergone the hot-bottom burning phase,\ncontrary to half of the studied LMC PNe. The yields from stellar evolutionary\nmodels with LMC and SMC metallicities broadly agree with the observations. In\nparticular, evolutionary yields for M$_{\\rm to}<3.5 {\\rm M}_{\\odot}$ well\nencompass the abundances of round and elliptical PNe in the SMC. We found that\nthe carbon emission lines are major coolants for SMC PNe, more so than in their\nLMC counterparts, indicating that metallicity has an effect on the physics of\nPNe, as predicted by Stanghellini et al. (2003).", "cat": "astro-ph.SR", "authors": ["L. Stanghellini", "T. -H. Lee", "R. A. Shaw", "B. Balick", "E. Villaver"]}, "1354": {"id": "2211.09727v1", "title": "A Survey on Evaluation Metrics for Synthetic Material Micro-Structure Images from Generative Models", "url": "http://arxiv.org/pdf/2211.09727v1", "date": "2022-11-03 15:17:42", "abs": "The evaluation of synthetic micro-structure images is an emerging problem as\nmachine learning and materials science research have evolved together. Typical\nstate of the art methods in evaluating synthetic images from generative models\nhave relied on the Fr\\'echet Inception Distance. However, this and other\nsimilar methods, are limited in the materials domain due to both the unique\nfeatures that characterize physically accurate micro-structures and limited\ndataset sizes. In this study we evaluate a variety of methods on scanning\nelectron microscope (SEM) images of graphene-reinforced polyurethane foams. The\nprimary objective of this paper is to report our findings with regards to the\nshortcomings of existing methods so as to encourage the machine learning\ncommunity to consider enhancements in metrics for assessing quality of\nsynthetic images in the material science domain.", "cat": "cond-mat.mtrl-sci", "authors": ["Devesh Shah", "Anirudh Suresh", "Alemayehu Admasu", "Devesh Upadhyay", "Kalyanmoy Deb"]}, "1355": {"id": "2011.01652v1", "title": "A low-frequency radio halo survey of the South Pole Telescope SZ-selected clusters with the GMRT", "url": "http://arxiv.org/pdf/2011.01652v1", "date": "2020-11-03 12:04:28", "abs": "The presence of non-thermal electrons and large scale magnetic fields in the\nintra-cluster medium (ICM) is known through the detection of mega-parsec (Mpc)\nscale diffuse radio synchrotron emission. Although a significant amount of\nprogress in finding new diffuse radio sources has happened in the last decade,\nmost of the investigation has been constrained towards massive low-redshift\nclusters. In this work, we explore clusters with redshift $z>0.3$ in search of\ndiffuse radio emission, at 325 MHz with the Giant Metrewave Radio Telescope\n(GMRT). This campaign has resulted in the discovery of 2 new radio halos\n(SPT-CL J0013-4906 and SPT-CL J0304-4401) along with 2 other detections (SPT-CL\nJ2031-4037 and SPT-CL J2248-4431), previously reported (at 325 MHz) in the\nliterature. In addition, we detect a halo candidate in 1 cluster in our sample,\nand upper limits for halos are placed in 8 clusters where no diffuse emission\nis detected. In the $P_{1.4} - L_\\mathrm{X}$ plane, the detected halos follow\nthe observed correlation, whereas the upper limits lie above the correlation\nline, indicating the possibility of future detection with sensitive\nobservations.", "cat": "astro-ph.HE", "authors": ["Ramij Raja", "Majidul Rahaman", "Abhirup Datta", "Reinout J. van Weeren", "Huib T. Intema", "Surajit Paul"]}, "1356": {"id": "2006.05763v1", "title": "The Gaia-ESO survey: the non-universality of the age-chemical-clocks-metallicity relations in the Galactic disc", "url": "http://arxiv.org/pdf/2006.05763v1", "date": "2020-06-10 10:29:39", "abs": "In the era of large spectroscopic surveys, massive databases of high-quality\nspectra provide tools to outline a new picture of our Galaxy. In this\nframework, an important piece of information is provided by our ability to\ninfer stellar ages. We aim to provide empirical relations between stellar ages\nand abundance ratios for a sample of solar-like stars. We investigate the\ndependence on metallicity, and we apply our relations to Gaia-ESO samples of\nopen clusters and field stars. We analyse high-resolution and high-S/N HARPS\nspectra of a sample of solar-like stars to obtain precise determinations of\ntheir atmospheric parameters and abundances through differential spectral\nanalysis and age through isochrone fitting. We investigate the relations\nbetween ages and abundance ratios. For the abundance ratios with a steeper\ndependence on age, we perform multivariate linear regressions, including the\ndependence on metallicity. We apply our relations to a sample of open clusters\nlocated in 47 kpc. In these clusters, the\ncontent of s-elements is lower than expected from chemical evolution models,\nand consequently the [s/$\\alpha$] are lower than in clusters of the same age\nlocated in the solar neighbourhood. With our chemical evolution model and a set\nof empirical yields, we suggest that a strong dependence on the star formation\nhistory and metallicity-dependent yields of s-elements can substantially modify\nthe slope of the [s/$\\alpha$]-[Fe/H]-age relation in different regions of the\nGalaxy. Our results point towards a non-universal relation\n[s/$\\alpha$]-[Fe/H]-age, indicating the existence of relations at different\nR$_{GC}$ or for different star formation history. A better understanding of the\ns-process at high metallicity is necessary to fully understand the origin of\nthese variations.", "cat": "astro-ph.GA", "authors": ["G. Casali", "L. Spina", "L. Magrini", "A. Karakas", "C. Kobayashi", "A. R. Casey", "S. Feltzing", "M. Van der Swaelmen", "M. Tsantaki", "P. Jofr\u00e9", "A. Bragaglia", "D. Feuillet", "T. Bensby", "K. Biazzo", "A. Gonneau", "G. Tautvaisiene", "M. Baratella", "V. Roccatagliata", "E. Pancino", "S. Sousa", "V. Adibekyan", "S. Martell", "A. Bayo", "R. J. Jackson", "R. D. Jeffries", "G. Gilmore", "S. Randich", "E. Alfaro", "S. E. Koposov", "A. J. Korn", "A. Recio-Blanco", "R. Smiljanic", "E. Franciosini", "A. Hourihane", "L. Monaco", "L. Morbidelli", "G. Sacco", "C. Worley", "S. Zaggia"]}, "1357": {"id": "1204.4726v1", "title": "Submillimetre Photometry of 323 Nearby Galaxies from the Herschel Reference Survey", "url": "http://arxiv.org/pdf/1204.4726v1", "date": "2012-04-20 20:00:04", "abs": "The Herschel Reference Survey (HRS) is a guaranteed time Herschel key project\naimed at studying the physical properties of the interstellar medium in\ngalaxies of the nearby universe. This volume limited, K-band selected sample is\ncomposed of galaxies spanning the whole range of morphological types (from\nellipticals to late-type spirals) and environments (from the field to the\ncentre of the Virgo Cluster). We present flux density measurements of the whole\nsample of 323 galaxies of the HRS in the three bands of the Spectral and\nPhotometric Imaging Receiver (SPIRE), at 250, 350 and 500 microns. Aperture\nphotometry is performed on extended galaxies and point spread function (PSF)\nfitting on timeline data for unresolved objects; we carefully estimate errors\nand upper limits. The flux densities are found to be in good agreement with\nthose of the HeViCS and KINGFISH key projects in all SPIRE bands, and of the\nPlanck consortium at 350 and 550 microns, for the galaxies in common. This\nsubmillimetre catalogue of nearby galaxies is a benchmark for the study of the\ndust properties in the local universe, giving the zero redshift reference for\nany cosmological survey.", "cat": "astro-ph.CO", "authors": ["L. Ciesla", "A. Boselli", "M. W. L. Smith", "G. J. Bendo", "L. Cortese", "S. Eales", "S. Bianchi", "M. Boquien", "V. Buat", "J. Davies", "M. Pohlen", "S. Zibetti", "M. Baes", "A. Cooray", "I. de Looze", "S. di Serego Alighieri", "M. Galametz", "H. L. Gomez", "V. Lebouteiller", "S. C. Madden", "C. Pappalardo", "A. Remy", "L. Spinoglio", "M. Vaccari", "R. Auld", "D. L. Clements"]}, "1358": {"id": "1711.04132v1", "title": "ThunderKAT: The MeerKAT Large Survey Project for Image-Plane Radio Transients", "url": "http://arxiv.org/pdf/1711.04132v1", "date": "2017-11-11 13:09:48", "abs": "ThunderKAT is the image-plane transients programme for MeerKAT. The goal as\noutlined in 2010, and still today, is to find, identify and understand\nhigh-energy astrophysical processes via their radio emission (often in concert\nwith observations at other wavelengths). Through a comprehensive and\ncomplementary programme of surveying and monitoring Galactic synchrotron\ntransients (across a range of compact accretors and a range of other explosive\nphenomena) and exploring distinct populations of extragalactic synchrotron\ntransients (microquasars, supernovae and possibly yet unknown transient\nphenomena) - both from direct surveys and commensal observations - we will\nrevolutionise our understanding of the dynamic and explosive transient radio\nsky. As well as performing targeted programmes of our own, we have made\nagreements with the other MeerKAT large survey projects (LSPs) that we will\nalso search their data for transients. This commensal use of the other surveys,\nwhich remains one of our key programme goals in 2016, means that the combined\nMeerKAT LSPs will produce by far the largest GHz-frequency radio transient\nprogramme to date.", "cat": "astro-ph.HE", "authors": ["R. Fender", "P. A. Woudt", "R. Armstrong", "P. Groot", "V. McBride", "J. Miller-Jones", "K. Mooley", "B. Stappers", "R. Wijers", "M. Bietenholz", "S. Blyth", "M. Bottcher", "D. Buckley", "P. Charles", "L. Chomiuk", "D. Coppejans", "S. Corbel", "M. Coriat", "F. Daigne", "W. J. G. de Blok", "H. Falcke", "J. Girard", "I. Heywood", "A. Horesh", "J. Horrell", "P. Jonker", "T. Joseph", "A. Kamble", "C. Knigge", "E. Koerding", "M. Kotze", "C. Kouveliotou", "C. Lynch", "T. Maccarone", "P. Meintjes", "S. Migliari", "T. Murphy", "T. Nagayama", "G. Nelemans", "G. Nicholson", "T. O'Brien", "A. Oodendaal", "N. Oozeer", "J. Osborne", "M. Perez-Torres", "S. Ratcliffe", "V. Ribeiro", "E. Rol", "A. Rushton", "A. Scaife", "M. Schurch", "G. Sivakoff", "T. Staley", "D. Steeghs", "I. Stewart", "J. Swinbank", "K. van der Heyden", "A. van der Horst", "B. van Soelen", "S. Vergani", "B. Warner", "K. Wiersema"]}, "1359": {"id": "1607.05799v2", "title": "The SLUGGS survey: a new mask design to reconstruct the stellar populations and kinematics of both inner and outer galaxy regions", "url": "http://arxiv.org/pdf/1607.05799v2", "date": "2016-07-24 23:57:06", "abs": "Integral field unit spectrographs allow the 2D exploration of the kinematics\nand stellar populations of galaxies, although they are generally restricted to\nsmall fields-of-view. Using the large field-of-view of the DEIMOS multislit\nspectrograph on Keck and our Stellar Kinematics using Multiple Slits (SKiMS)\ntechnique, we are able to extract sky-subtracted stellar light spectra to large\ngalactocentric radii. Here we present a new DEIMOS mask design named SuperSKiMS\nthat explores large spatial scales without sacrificing high spatial sampling.\nWe simulate a set of observations with such a mask design on the nearby galaxy\nNGC 1023, showing that the kinematic and metallicity measurements can reach\nradii where the galaxy surface brightness is several orders of magnitude\nfainter than the sky. Such a technique is also able to reproduce the kinematic\nand metallicity 2D distributions obtained from literature integral field\nspectroscopy in the innermost galaxy regions. In particular, we use the\nsimulated NGC 1023 kinematics to model its total mass distribution to large\nradii, obtaining comparable results with those from published integral field\nunit observation. Finally, from new spectra of NGC 1023 we obtain stellar 2D\nkinematics and metallicity distributions that show good agreement with integral\nfield spectroscopy results in the overlapping regions. In particular, we do not\nfind a significant offset between our SKiMS and the ATLAS$^\\rm{3D}$ stellar\nvelocity dispersion at the same spatial locations.", "cat": "astro-ph.GA", "authors": ["Nicola Pastorello", "Duncan A. Forbes", "Adriano Poci", "Aaron J. Romanowsky", "Richard McDermid", "Adebusola B. Alabi", "Jean P. Brodie", "Michele Cappellari", "Vincenzo Pota", "Caroline Foster"]}, "1360": {"id": "2303.14571v2", "title": "Fishing for Planets: A Comparative Analysis of EPRV Survey Performance in the Presence of Correlated Noise", "url": "http://arxiv.org/pdf/2303.14571v2", "date": "2024-06-24 18:40:33", "abs": "With dedicated exoplanet surveys underway for multiple extreme precision\nradial velocity (EPRV) instruments, the near-future prospects of RV exoplanet\nscience are promising. These surveys' generous time allocations are expected to\nfacilitate the discovery of Earth analogs around bright, nearby Sun-like stars.\nBut survey success will depend critically on the choice of observing strategy,\nwhich will determine the survey's ability to mitigate known sources of noise\nand extract low-amplitude exoplanet signals. Here, we present an analysis of\nthe Fisher information content of simulated EPRV surveys, accounting for the\nmost recent advances in our understanding of stellar variability on both short\nand long timescales (i.e., oscillations and granulation within individual\nnights, and activity-induced variations across multiple nights). In this\nanalysis, we capture the correlated nature of stellar variability by\nparameterizing these signals with Gaussian Process kernels. We describe the\nunderlying simulation framework as well as the physical interpretation of the\nFisher information content, and we evaluate the efficacy of EPRV survey\nstrategies that have been presented in the literature. We explore and compare\nstrategies for scheduling observations over various timescales and we make\nrecommendations to optimize survey performance for the detection of Earth-like\nexoplanets.", "cat": "astro-ph.EP", "authors": ["Arvind F. Gupta", "Megan Bedell"]}, "1361": {"id": "2204.04101v1", "title": "Dynamical Mahler Measure: A survey and some recent results", "url": "http://arxiv.org/pdf/2204.04101v1", "date": "2022-04-08 14:31:44", "abs": "We study the dynamical Mahler measure of multivariate polynomials and present\ndynamical analogues of various results from the classical Mahler measure as\nwell as examples of formulas allowing the computation of the dynamical Mahler\nmeasure in certain cases. We discuss multivariate analogues of dynamical\nKronecker's Lemma and present some improvements on the result for two variables\ndue to Carter, Lal\\'in, Manes, Miller, and Mocz.", "cat": "math.NT", "authors": ["Annie Carter", "Matilde Lal\u00edn", "Michelle Manes", "Alison Beth Miller"]}, "1362": {"id": "2201.09454v1", "title": "Design of Fieldable Cross-Layer Optimized Network using Embedded Software Defined Radios: Survey and Novel Architecture with Field Trials", "url": "http://arxiv.org/pdf/2201.09454v1", "date": "2022-01-24 04:46:00", "abs": "The proliferation of wireless devices and their ever increasing influence on\nour day-to-day life is very evident and seems irreplaceable. This exponential\ngrowth in demand, both in terms of the number of devices and Quality of Service\n(QoS) had spawned the concept of cross-layer optimization several years ago.\nThe primary goal of the cross-layer approach was to liberate the strict\nboundary between the layers of the traditional Open Systems Interconnection\n(OSI) protocol stack. The initial decade focused on establishing the\ntheoretical feasibility of this revolutionary concept and gauging the\neffectiveness and limits of this idea. During the next phase, the advent of\nsoftware defined radios (SDR) accelerated the growth of this domain due to its\nadded flexibility. Yet, there has been a gaping abyss between solutions\ndesigned in theory and ones deployed in practice. To establish this, we first\npresent an elaborate survey of the cross-layer protocol stack literature. Next,\nwe briefly discuss how a commercial off-the-shelf (COTS), low SWaP (Size,\nWeight, and Power) embedded SDR (e-SDR) was transformed into a standalone,\nfieldable transceiver. Thereafter, we provide the software design ethos that\nfocuses on efficiency and flexibility such that the optimization objectives and\ncross-layer interactions can be reconfigured rapidly. To demonstrate our\nclaims, we provide results from extensive outdoor over-the-air experiments in\nvarious settings with up to 10-node network topologies. The results from the\nfield trials demonstrate high reliability, throughput, and dynamic routing\ncapability. To the best of our knowledge, this is the first time in literature,\na COTS e-SDR has been leveraged to successfully design a cross-layer optimized\ntransceiver that is capable of forming an ad hoc network that provides high\nthroughput and high reliability in a ruggedized, weatherized, and fieldable\nform factor.", "cat": "cs.NI", "authors": ["Jithin Jagannath", "Anu Jagannath", "Justin Henney", "Tyler Gwin", "Zackary Kane", "Noor Biswas", "Andrew Drozd"]}, "1363": {"id": "2005.12518v1", "title": "Survey: Machine Learning in Production Rendering", "url": "http://arxiv.org/pdf/2005.12518v1", "date": "2020-05-26 05:23:32", "abs": "In the past few years, machine learning-based approaches have had some great\nsuccess for rendering animated feature films. This survey summarizes several of\nthe most dramatic improvements in using deep neural networks over traditional\nrendering methods, such as better image quality and lower computational\noverhead. More specifically, this survey covers the fundamental principles of\nmachine learning and its applications, such as denoising, path guiding,\nrendering participating media, and other notoriously difficult light transport\nsituations. Some of these techniques have already been used in the latest\nreleased animations while others are still in the continuing development by\nresearchers in both academia and movie studios. Although learning-based\nrendering methods still have some open issues, they have already demonstrated\npromising performance in multiple parts of the rendering pipeline, and people\nare continuously making new attempts.", "cat": "cs.GR", "authors": ["Shilin Zhu"]}, "1364": {"id": "1906.08452v2", "title": "A Survey of Multi-Access Edge Computing in 5G and Beyond: Fundamentals, Technology Integration, and State-of-the-Art", "url": "http://arxiv.org/pdf/1906.08452v2", "date": "2020-01-02 03:39:56", "abs": "Driven by the emergence of new compute-intensive applications and the vision\nof the Internet of Things (IoT), it is foreseen that the emerging 5G network\nwill face an unprecedented increase in traffic volume and computation demands.\nHowever, end users mostly have limited storage capacities and finite processing\ncapabilities, thus how to run compute-intensive applications on\nresource-constrained users has recently become a natural concern. Mobile edge\ncomputing (MEC), a key technology in the emerging fifth generation (5G)\nnetwork, can optimize mobile resources by hosting compute-intensive\napplications, process large data before sending to the cloud, provide the cloud\ncomputing capabilities within the radio access network (RAN) in close proximity\nto mobile users, and offer context-aware services with the help of RAN\ninformation. Therefore, MEC enables a wide variety of applications, where the\nreal-time response is strictly required, e.g., driverless vehicles, augmented\nreality, robotics, and immerse media. Indeed, the paradigm shift from 4G to 5G\ncould become a reality with the advent of new technological concepts. The\nsuccessful realization of MEC in the 5G network is still in its infancy and\ndemands for constant efforts from both academic and industry communities. In\nthis survey, we first provide a holistic overview of MEC technology and its\npotential use cases and applications. Then, we outline up-to-date researches on\nthe integration of MEC with the new technologies that will be deployed in 5G\nand beyond. We also summarize testbeds and experimental evaluations, and open\nsource activities, for edge computing. We further summarize lessons learned\nfrom state-of-the-art research works as well as discuss challenges and\npotential future directions for MEC research.", "cat": "cs.NI", "authors": ["Quoc-Viet Pham", "Fang Fang", "Vu Nguyen Ha", "Md. Jalil Piran", "Mai Le", "Long Bao Le", "Won-Joo Hwang", "Zhiguo Ding"]}, "1365": {"id": "1901.06546v1", "title": "An unbiased spectral line survey observation toward the low-mass star-forming region L1527", "url": "http://arxiv.org/pdf/1901.06546v1", "date": "2019-01-19 16:10:26", "abs": "An unbiased spectral line survey toward a solar-type Class 0/I protostar,\nIRAS04368+2557, in L1527 has been carried out in the 3 mm band with the\nNobeyama 45 m telescope. L1527 is known as a warm carbon-chain chemistry (WCCC)\nsource, which harbors abundant unsaturated organic species such as C$_n$H ($n =\n3,\\ 4,\\ 5,\\ldots$) in a warm and dense region near the protostar. The\nobservation covers the frequency range from 80 to 116 GHz. A supplementary\nobservation has also been conducted in the 70 GHz band to observe fundamental\ntransitions of deuterated species. In total, 69 molecular species are\nidentified, among which 27 species are carbon-chain species and their isomers,\nincluding their minor isotopologues. This spectral line survey provides us with\na good template of the chemical composition of the WCCC source.", "cat": "astro-ph.GA", "authors": ["Kento Yoshida", "Nami Sakai", "Yuri Nishimura", "Tomoya Tokudome", "Yoshimasa Watanabe", "Takeshi Sakai", "Shuro Takano", "Satoshi Yamamoto"]}, "1366": {"id": "1201.3994v1", "title": "Comparison of potential ASKAP HI survey source finders", "url": "http://arxiv.org/pdf/1201.3994v1", "date": "2012-01-19 09:15:57", "abs": "The large size of the ASKAP HI surveys DINGO and WALLABY necessitates\nautomated 3D source finding. A performance difference of a few percent\ncorresponds to a significant number of galaxies being detected or undetected.\nAs such, the performance of the automated source finding is of paramount\nimportance to both of these surveys. We have analysed the performance of\nvarious source finders to determine which will allow us to meet our survey\ngoals during the DINGO and WALLABY design studies. Here we present a comparison\nof the performance of five different methods of automated source finding. These\nsource finders are Duchamp, the Gamma-finder, CNHI, a 2D-1D Wavelet\nReconstruction and S+C finder, a sigma clipping method. Each source finder was\napplied on the same three-dimensional data cubes containing (a) point sources\nwith a Gaussian velocity profile and (b) spatially extended model-galaxies with\ninclinations and rotation profiles. We focus on the completeness and\nreliability of each algorithm when comparing the performance of the different\nsource finders.", "cat": "astro-ph.IM", "authors": ["Attila Popping", "Russell Jurek", "Tobias Westmeier", "Paolo Serra", "Lars Floer", "Martin Meyer", "Baerbel Koribalski"]}, "1367": {"id": "1408.3585v1", "title": "A Bayesian blind survey for cold molecular gas in the Universe", "url": "http://arxiv.org/pdf/1408.3585v1", "date": "2014-08-15 16:53:29", "abs": "A new Bayesian method for performing an image domain search for line-emitting\ngalaxies is presented. The method uses both spatial and spectral information to\nrobustly determine the source properties, employing either simple Gaussian, or\nother physically motivated models whilst using the evidence to determine the\nprobability that the source is real. In this paper, we describe the method, and\nits application to both a simulated data set, and a blind survey for cold\nmolecular gas using observations of the Hubble Deep Field North taken with the\nPlateau de Bure Interferometer. We make a total of 6 robust detections in the\nsurvey, 5 of which have counterparts in other observing bands. We identify the\nmost secure detections found in a previous investigation, while finding one new\nprobable line source with an optical ID not seen in the previous analysis. This\nstudy acts as a pilot application of Bayesian statistics to future searches to\nbe carried out both for low-$J$ CO transitions of high redshift galaxies using\nthe JVLA, and at millimeter wavelengths with ALMA, enabling the inference of\nrobust scientific conclusions about the history of the molecular gas properties\nof star-forming galaxies in the Universe through cosmic time.", "cat": "astro-ph.IM", "authors": ["Lindley Lentati", "Chris Carilli", "Paul Alexander", "Fabian Walter", "Roberto Decarli"]}, "1368": {"id": "1909.05148v1", "title": "A Survey on Machine Learning for Optical Communication [Machine Learning View]", "url": "http://arxiv.org/pdf/1909.05148v1", "date": "2019-08-21 04:35:17", "abs": "Machine Learning (ML) for Optical Communication (OC) is certainly a hot topic\nemerged recently and will continue to raise interest at least for the next few\nyears. The rate of research development in this area is growing very rapidly.\nNovelty of this research direction resides mainly in the peculiarity of the\napplication field, rather than in the methodological approaches, which are (at\nleast up to now) state-of-the-art ML algorithms. Reviewing the literature shows\nthat many of the ML algorithms have not yet been used in this area, and many of\nthe OC applications are not considered yet, which reflects the fact that the\nresearch topic is pristine. Accordingly, tutorial investigations are quiet\nnecessary in this filed to help researchers be aware about the last\nprogressions and cavities of this field. Although several tutorials have been\nreleased recently, they considered this topic from OC view, and neglected ML\nview. However, it is required to have an investigations about the ML algorithms\nused in this subject. Accordingly, for the first time, this paper reviews ML\nfor OC literature from ML viewpoint. This view could be really helpful because\nonly OC experts work on ML for OC, and they are not ML experts, so it could\nreally help them to have a comprehensive view on the ML subjects implantable in\nOC. It has worth to mention that compared with other works, this survey reviews\nmuch more investigations; therefore, it has more generality, and gives the\nreader to have a comprehensive overview on this topic.", "cat": "eess.SP", "authors": ["M. A. Amirabadi"]}, "1369": {"id": "1608.01807v2", "title": "SIFT Meets CNN: A Decade Survey of Instance Retrieval", "url": "http://arxiv.org/pdf/1608.01807v2", "date": "2017-05-23 08:10:33", "abs": "In the early days, content-based image retrieval (CBIR) was studied with\nglobal features. Since 2003, image retrieval based on local descriptors (de\nfacto SIFT) has been extensively studied for over a decade due to the advantage\nof SIFT in dealing with image transformations. Recently, image representations\nbased on the convolutional neural network (CNN) have attracted increasing\ninterest in the community and demonstrated impressive performance. Given this\ntime of rapid evolution, this article provides a comprehensive survey of\ninstance retrieval over the last decade. Two broad categories, SIFT-based and\nCNN-based methods, are presented. For the former, according to the codebook\nsize, we organize the literature into using large/medium-sized/small codebooks.\nFor the latter, we discuss three lines of methods, i.e., using pre-trained or\nfine-tuned CNN models, and hybrid methods. The first two perform a single-pass\nof an image to the network, while the last category employs a patch-based\nfeature extraction scheme. This survey presents milestones in modern instance\nretrieval, reviews a broad selection of previous works in different categories,\nand provides insights on the connection between SIFT and CNN-based methods.\nAfter analyzing and comparing retrieval performance of different categories on\nseveral datasets, we discuss promising directions towards generic and\nspecialized instance retrieval.", "cat": "cs.CV", "authors": ["Liang Zheng", "Yi Yang", "Qi Tian"]}, "1370": {"id": "2307.04782v2", "title": "Deeper than DEEP: A Spectroscopic Survey of $z>3$ Lyman-$\u03b1$ Emitters in the Extended Groth Strip", "url": "http://arxiv.org/pdf/2307.04782v2", "date": "2024-02-02 01:28:49", "abs": "We present a spectroscopic survey of Ly$\\alpha$ emitters in the Extended\nGroth Strip (EGS) field, targeting the regime near the Epoch of Reionization.\nUsing Keck/DEIMOS, we observed 947 high-$z$ candidates with photometric\nredshifts from 3 $< z_\\text{phot} <$ 7 and down to an $H$-band (HST/WFC3 F160W)\nmagnitude limit of < 27.5. Observations were taken over the course of 8 nights,\nwith integration times ranging from 4 to 7.8 hours. Our survey secured 137\nunique redshifts, 126 of which are Ly$\\alpha$ emitters at 2.8 $< z <$ 6.5 with\na mean redshift of $\\overline{z} = 4.3$. We provide a comprehensive redshift\ncatalog for our targets, as well as the reduced one- and two- dimensional\nspectra for each object. These observations will provide an important auxiliary\ndataset for the JWST Directors Discretionary Early Release Science (DD-ERS)\nprogram the Cosmic Evolution Early Release Science Survey (CEERS), which\nrecently completed near- and mid-IR imaging and spectroscopy of galaxies in the\nEGS field.", "cat": "astro-ph.GA", "authors": ["Stephanie M. Urbano Stawinski", "M. C. Cooper", "Steven L. Finkelstein", "Intae Jung", "Pablo G. P\u00e9rez-Gonz\u00e1lez", "Caitlin M. Casey", "Olivia R. Cooper", "Nimish P. Hathi", "Benne W. Holwerda", "Anton M. Koekemoer", "Vital Fern\u00e1ndez", "Rebecca L. Larson", "Ray A. Lucas", "L. Y. Aaron Yung"]}, "1371": {"id": "2109.07342v1", "title": "Sequential Point Cloud Prediction in Interactive Scenarios: A Survey", "url": "http://arxiv.org/pdf/2109.07342v1", "date": "2021-09-15 14:53:44", "abs": "Point cloud has been widely used in the field of autonomous driving since it\ncan provide a more comprehensive three-dimensional representation of the\nenvironment than 2D images. Point-wise prediction based on point cloud sequence\n(PCS) is an essential part of environment understanding, which can assist in\nthe decision-making and motion-planning of autonomous vehicles. However, PCS\nprediction has not been deeply researched in the literature. This paper\nproposes a brief review of the sequential point cloud prediction methods,\nfocusing on interactive scenarios. Firstly, we define the PCS prediction\nproblem and introduce commonly-used frameworks. Secondly, by reviewing\nnon-predictive problems, we analyze and summarize the spatio-temporal feature\nextraction methods based on PCS. On this basis, we review two types of PCS\nprediction tasks, scene flow estimation (SFE) and point cloud location\nprediction (PCLP), highlighting their connections and differences. Finally, we\ndiscuss some opening issues and point out some potential research directions.", "cat": "cs.RO", "authors": ["Haowen Wang", "Zirui Li", "Jianwei Gong"]}, "1372": {"id": "2210.01472v2", "title": "Monitoring Public Behavior During a Pandemic Using Surveys: Proof-of-Concept Via Epidemic Modelling", "url": "http://arxiv.org/pdf/2210.01472v2", "date": "2023-01-31 09:56:46", "abs": "Implementing a lockdown for disease mitigation is a balancing act:\nNon-pharmaceutical interventions can reduce disease transmission significantly,\nbut interventions also have considerable societal costs. Therefore,\ndecision-makers need near real-time information to calibrate the level of\nrestrictions. We fielded daily surveys in Denmark during the second wave of the\nCOVID-19 pandemic to monitor public response to the announced lockdown. A key\nquestion asked respondents to state their number of close contacts within the\npast 24 hours. Here, we establish a link between survey data, mobility data,\nand hospitalizations via epidemic modelling. Using Bayesian analysis, we then\nevaluate the usefulness of survey responses as a tool to monitor the effects of\nlockdown and then compare the predictive performance to that of mobility data.\nWe find that, unlike mobility, self-reported contacts decreased significantly\nin all regions before the nation-wide implementation of non-pharmaceutical\ninterventions and improved predicting future hospitalizations compared to\nmobility data. A detailed analysis of contact types indicates that contact with\nfriends and strangers outperforms contact with colleagues and family members\n(outside the household) on the same prediction task. Representative surveys\nthus qualify as a reliable, non-privacy invasive monitoring tool to track the\nimplementation of non-pharmaceutical interventions and study potential\ntransmission paths.", "cat": "physics.data-an", "authors": ["Andreas Koher", "Frederik J\u00f8rgensen", "Michael Bang Petersen", "Sune Lehmann"]}, "1373": {"id": "2312.00333v2", "title": "Green Edge AI: A Contemporary Survey", "url": "http://arxiv.org/pdf/2312.00333v2", "date": "2024-07-31 15:17:58", "abs": "Artificial intelligence (AI) technologies have emerged as pivotal enablers\nacross a multitude of industries largely due to their significant resurgence\nover the past decade. The transformative power of AI is primarily derived from\nthe utilization of deep neural networks (DNNs), which require extensive data\nfor training and substantial computational resources for processing.\nConsequently, DNN models are typically trained and deployed on resource-rich\ncloud servers. However, due to potential latency issues associated with cloud\ncommunications, deep learning (DL) workflows are increasingly being\ntransitioned to wireless edge networks in proximity to end-user devices (EUDs).\nThis shift is designed to support latency-sensitive applications and has given\nrise to a new paradigm of edge AI, which will play a critical role in upcoming\nsixth-generation (6G) networks to support ubiquitous AI applications. Despite\nits considerable potential, edge AI faces substantial challenges, mostly due to\nthe dichotomy between the resource limitations of wireless edge networks and\nthe resource-intensive nature of DL. Specifically, the acquisition of\nlarge-scale data, as well as the training and inference processes of DNNs, can\nrapidly deplete the battery energy of EUDs. This necessitates an\nenergy-conscious approach to edge AI to ensure both optimal and sustainable\nperformance. In this paper, we present a contemporary survey on green edge AI.\nWe commence by analyzing the principal energy consumption components of edge AI\nsystems to identify the fundamental design principles of green edge AI. Guided\nby these principles, we then explore energy-efficient design methodologies for\nthe three critical tasks in edge AI systems, including training data\nacquisition, edge training, and edge inference. Finally, we underscore\npotential future research directions to further enhance the energy efficiency\nof edge AI.", "cat": "cs.AI", "authors": ["Yuyi Mao", "Xianghao Yu", "Kaibin Huang", "Ying-Jun Angela Zhang", "Jun Zhang"]}, "1374": {"id": "1712.00606v1", "title": "A survey study on major technical barriers affecting the decision to adopt cloud services", "url": "http://arxiv.org/pdf/1712.00606v1", "date": "2017-12-02 13:03:35", "abs": "In the context of cloud computing, risks associated with underlying\ntechnologies, risks involving service models and outsourcing, and enterprise\nreadiness have been recognized as potential barriers for the adoption. To\naccelerate cloud adoption, the concrete barriers negatively influencing the\nadoption decision need to be identified. Our study aims at understanding the\nimpact of technical and security-related barriers on the organizational\ndecision to adopt the cloud. We analyzed data collected through a web survey of\n352 individuals working for enterprises consisting of decision makers as well\nas employees from other levels within an organization. The comparison of\nadopter and non-adopter sample reveals three potential adoption inhibitor,\nsecurity, data privacy, and portability. The result from our logistic\nregression analysis confirms the criticality of the security concern, which\nresults in an up to 26-fold increase in the non-adoption likelihood. Our study\nunderlines the importance of the technical and security perspectives for\nresearch investigating the adoption of technology.", "cat": "cs.SE", "authors": ["Nattakarn Phaphoom", "Xiaofeng Wang", "Sarah Samuel", "Sven Helmer", "Pekka Abrahamsson"]}, "1375": {"id": "2103.05561v1", "title": "Did Chatbots Miss Their 'Apollo Moment'? A Survey of the Potential, Gaps and Lessons from Using Collaboration Assistants During COVID-19", "url": "http://arxiv.org/pdf/2103.05561v1", "date": "2021-02-27 19:08:54", "abs": "Artificial Intelligence (AI) technologies have long been positioned as a tool\nto provide crucial data-driven decision support to people. In this survey\npaper, we look at how AI in general, and collaboration assistants (CAs or\nchatbots for short) in particular, have been used during a true global exigency\n- the COVID-19 pandemic. The key observation is that chatbots missed their\n\"Apollo moment\" when they could have really provided contextual, personalized,\nreliable decision support at scale that the state-of-the-art makes possible. We\nreview the existing capabilities that are feasible and methods, identify the\npotential that chatbots could have met, the use-cases they were deployed on,\nthe challenges they faced and gaps that persisted, and draw lessons that, if\nimplemented, would make them more relevant in future health emergencies.", "cat": "cs.HC", "authors": ["Biplav Srivastava"]}, "1376": {"id": "1508.01512v1", "title": "The Subaru FMOS Galaxy Redshift Survey (FastSound). III. The mass-metallicity relation and the fundamental metallicity relation at $z\\sim1.4$", "url": "http://arxiv.org/pdf/1508.01512v1", "date": "2015-08-06 20:04:12", "abs": "We present the results from a large near-infrared spectroscopic survey with\nSubaru/FMOS (\\textit{FastSound}) consisting of $\\sim$ 4,000 galaxies at\n$z\\sim1.4$ with significant H$\\alpha$ detection. We measure the gas-phase\nmetallicity from the [N~{\\sc ii}]$\\lambda$6583/H$\\alpha$ emission line ratio of\nthe composite spectra in various stellar mass and star-formation rate bins. The\nresulting mass-metallicity relation generally agrees with previous studies\nobtained in a similar redshift range to that of our sample. No clear dependence\nof the mass-metallicity relation with star-formation rate is found. Our result\nat $z\\sim1.4$ is roughly in agreement with the fundamental metallicity relation\nat $z\\sim0.1$ with fiber aperture corrected star-formation rate. We detect\nsignificant [S~{\\sc ii}]$\\lambda\\lambda$6716,6731 emission lines from the\ncomposite spectra. The electron density estimated from the [S~{\\sc\nii}]$\\lambda\\lambda$6716,6731 line ratio ranges from 10 -- 500 cm$^{-3}$, which\ngenerally agrees with that of local galaxies. On the other hand, the\ndistribution of our sample on [N~{\\sc ii}]$\\lambda$6583/H$\\alpha$ vs. [S~{\\sc\nii}]$\\lambda\\lambda$6716,6731/H$\\alpha$ is different from that found locally.\nWe estimate the nitrogen-to-oxygen abundance ratio (N/O) from the N2S2 index,\nand find that the N/O in galaxies at $z\\sim1.4$ is significantly higher than\nthe local values at a fixed metallicity and stellar mass. The metallicity at\n$z\\sim1.4$ recalculated with this N/O enhancement taken into account decreases\nby 0.1 -- 0.2 dex. The resulting metallicity is lower than the local\nfundamental metallicity relation.", "cat": "astro-ph.GA", "authors": ["Kiyoto Yabe", "Kouji Ohta", "Masayuki Akiyama", "Andrew Bunker", "Gavin Dalton", "Richard Ellis", "Karl Glazebrook", "Tomotsugu Goto", "Masatoshi Imanishi", "Fumihide Iwamuro", "Hiroyuki Okada", "Ikkoh Shimizu", "Naruhisa Takato", "Naoyuki Tamura", "Motonari Tonegawa", "Tomonori Totani"]}, "1377": {"id": "2409.02968v1", "title": "A Comprehensive Survey of Blockchain Scalability: Shaping Inner-Chain and Inter-Chain Perspectives", "url": "http://arxiv.org/pdf/2409.02968v1", "date": "2024-09-04 06:47:50", "abs": "Blockchain is widely applied in logistics, finance, and agriculture. As\nsingle blockchain users grow, scalability becomes crucial. However, existing\nworks lack a comprehensive summary of blockchain scalability. They focus on\nsingle chains or cross-chain technologies. This survey summarizes scalability\nacross the physical and logical layers, as well as inner-chain, inter-chain,\nand technology dimensions. The physical layer covers data and protocols, while\nthe logical layer represents blockchain architecture. Each component is\nanalyzed from inner-chain and inter-chain perspectives, considering\ntechnological factors. The aim is to enhance researchers' understanding of\nblockchain's architecture, data, and protocols to advance scalability research.", "cat": "cs.DB", "authors": ["Baochao Chen", "Liyuan Ma", "Hao Xu", "Juncheng Ma", "Dengcheng Hu", "Xiulong Liu", "Jie Wu", "Jianrong Wang", "Keqiu Li"]}, "1378": {"id": "1403.4935v1", "title": "Spectral Energy Distribution Fitting of HETDEX Pilot Survey Lyman-alpha Emitters in COSMOS and GOODS-N", "url": "http://arxiv.org/pdf/1403.4935v1", "date": "2014-03-19 20:00:14", "abs": "We use broadband photometry extending from the rest-frame UV to the near-IR\nto fit the individual spectral energy distributions (SEDs) of 63 bright\n(L(Ly-alpha) > 10^43 ergs/s) Ly-alpha emitting galaxies (LAEs) in the redshift\nrange 1.9 < z < 3.6. We find that these LAEs are quite heterogeneous, with\nstellar masses that span over three orders of magnitude, from 7.5 < log M <\n10.5. Moreover, although most LAEs have small amounts of extinction, some\nhigh-mass objects have stellar reddenings as large as E(B-V) ~0.4.\nInterestingly, in dusty objects the optical depths for Ly-alpha and the UV\ncontinuum are always similar, indicating that Ly-alpha photons are not\nundergoing many scatters before escaping their galaxy. In contrast, the ratio\nof optical depths in low-reddening systems can vary widely, illustrating the\ndiverse nature of the systems. Finally, we show that in the star formation rate\n(SFR)-log mass diagram, our LAEs fall above the \"main-sequence\" defined by z ~\n3 continuum selected star-forming galaxies. In this respect, they are similar\nto sub-mm-selected galaxies, although most LAEs have much lower mass.", "cat": "astro-ph.GA", "authors": ["Alex Hagen", "Robin Ciardullo", "Caryl Gronwall", "Viviana Acquaviva", "Joanna Bridge", "Gregory R. Zeimann", "Guillermo A. Blanc", "Nicholas A. Bond", "Steven L. Finkelstein", "Mimi Song", "Eric Gawiser", "Derek B. Fox", "Henry Gebhardt", "A. I. Malz", "Donald P. Schneider", "Niv Drory", "Karl Gebhardt", "Gary J. Hill"]}, "1379": {"id": "1208.6572v1", "title": "Ensemble filter techniques for intermittent data assimilation - a survey", "url": "http://arxiv.org/pdf/1208.6572v1", "date": "2012-08-31 18:27:28", "abs": "This survey paper is written with the intention of giving a mathematical\nintroduction to filtering techniques for intermittent data assimilation, and to\nsurvey some recent advances in the field. The paper is divided into three\nparts. The first part introduces Bayesian statistics and its application to\nstatistical inference and estimation. Basic aspects of Markov processes, as\nthey typically arise from scientific models in the form of stochastic\ndifferential and/or difference equations, are covered in the second part. The\nthird and final part describes the filtering approach to estimation of model\nstates by assimilation of observational data into scientific models. While most\nof the material is of survey type, very recent advances in the field of\nnonlinear data assimilation covered in this paper include a discussion of\nBayesian inference in the context of optimal transportation and coupling of\nrandom variables, as well as a discussion of recent advances in ensemble\ntransform filters. References and sources for further reading material will be\nlisted at the end of each section.", "cat": "math.NA", "authors": ["Colin J. Cotter", "Sebastian Reich"]}, "1380": {"id": "2310.09822v1", "title": "Turn Passive to Active: A Survey on Active Intellectual Property Protection of Deep Learning Models", "url": "http://arxiv.org/pdf/2310.09822v1", "date": "2023-10-15 12:54:32", "abs": "The intellectual property protection of deep learning (DL) models has\nattracted increasing serious concerns. Many works on intellectual property\nprotection for Deep Neural Networks (DNN) models have been proposed. The vast\nmajority of existing work uses DNN watermarking to verify the ownership of the\nmodel after piracy occurs, which is referred to as passive verification. On the\ncontrary, we focus on a new type of intellectual property protection method\nnamed active copyright protection, which refers to active authorization control\nand user identity management of the DNN model. As of now, there is relatively\nlimited research in the field of active DNN copyright protection. In this\nreview, we attempt to clearly elaborate on the connotation, attributes, and\nrequirements of active DNN copyright protection, provide evaluation methods and\nmetrics for active copyright protection, review and analyze existing work on\nactive DL model intellectual property protection, discuss potential attacks\nthat active DL model copyright protection techniques may face, and provide\nchallenges and future directions for active DL model intellectual property\nprotection. This review is helpful to systematically introduce the new field of\nactive DNN copyright protection and provide reference and foundation for\nsubsequent work.", "cat": "cs.CR", "authors": ["Mingfu Xue", "Leo Yu Zhang", "Yushu Zhang", "Weiqiang Liu"]}, "1381": {"id": "1312.3192v1", "title": "The Galactic Bulge Survey: completion of the X-ray survey observations", "url": "http://arxiv.org/pdf/1312.3192v1", "date": "2013-12-11 14:44:13", "abs": "We provide the Chandra source list for the last ~quarter of the area covered\nby the Galactic Bulge Survey (GBS). The GBS targets two strips of 6\\degr x\n1\\degr (12 square degrees in total), one above (1\\degr 10^{15} (10^{12}) M_\\odot$, which corresponds to the\ncosmological density parameter $|\\Omega| < 10^{-4}$ at the galaxy-scale mass\nrange $|M|=10^{12-15}M_\\odot$. The number density of the Ellis wormhole is\n$n<10^{-4} h^3 {\\rm Mpc}^{-3}$ for a range of the throat radius $a =\n10^{1-4}$pc, which is much smaller than the Einstein ring radius.", "cat": "astro-ph.CO", "authors": ["Ryuichi Takahashi", "Hideki Asada"]}, "1385": {"id": "2007.08911v3", "title": "Technologies for Trustworthy Machine Learning: A Survey in a Socio-Technical Context", "url": "http://arxiv.org/pdf/2007.08911v3", "date": "2022-01-20 13:42:29", "abs": "Concerns about the societal impact of AI-based services and systems has\nencouraged governments and other organisations around the world to propose AI\npolicy frameworks to address fairness, accountability, transparency and related\ntopics. To achieve the objectives of these frameworks, the data and software\nengineers who build machine-learning systems require knowledge about a variety\nof relevant supporting tools and techniques. In this paper we provide an\noverview of technologies that support building trustworthy machine learning\nsystems, i.e., systems whose properties justify that people place trust in\nthem. We argue that four categories of system properties are instrumental in\nachieving the policy objectives, namely fairness, explainability, auditability\nand safety & security (FEAS). We discuss how these properties need to be\nconsidered across all stages of the machine learning life cycle, from data\ncollection through run-time model inference. As a consequence, we survey in\nthis paper the main technologies with respect to all four of the FEAS\nproperties, for data-centric as well as model-centric stages of the machine\nlearning system life cycle. We conclude with an identification of open research\nproblems, with a particular focus on the connection between trustworthy machine\nlearning technologies and their implications for individuals and society.", "cat": "cs.LG", "authors": ["Ehsan Toreini", "Mhairi Aitken", "Kovila P. L. Coopamootoo", "Karen Elliott", "Vladimiro Gonzalez Zelaya", "Paolo Missier", "Magdalene Ng", "Aad van Moorsel"]}, "1386": {"id": "2209.08987v2", "title": "Combining gravitational lensing and gravitational redshift to measure the anisotropic stress with future galaxy surveys", "url": "http://arxiv.org/pdf/2209.08987v2", "date": "2023-04-25 09:58:59", "abs": "Galaxy surveys provide one of the best ways to constrain the theory of\ngravity at cosmological scales. They can be used to constrain the two\ngravitational potentials encoding time, $\\Psi$, and spatial, $\\Phi$,\ndistortions, which are exactly equal at late time within general relativity.\nHence, any small variation leading to a nonzero anisotropic stress, i.e. a\ndifference between these potentials, would be an indication for modified\ngravity. Current analyses usually consider gravitational lensing and\nredshift-space distortions to constrain the anisotropic stress, but these rely\non certain assumptions like the validity of the weak equivalence principle, and\na specific time evolution of the functions encoding deviations from general\nrelativity. In this work, we propose a reparametrization of the gravitational\nlensing observable, together with the use of the relativistic dipole of the\ncorrelation function of galaxies to directly measure the anisotropic stress\nwith a minimum amount of assumptions. We consider the future Legacy Survey of\nSpace and Time of the Vera C. Rubin Observatory and the future Square Kilometer\nArray, and show that combining gravitational lensing and gravitational redshift\nwith the proposed approach we will achieve model-independent constraints on the\nanisotropic stress at the level of $\\sim 20\\,\\%$.", "cat": "astro-ph.CO", "authors": ["Isaac Tutusaus", "Daniel Sobral-Blanco", "Camille Bonvin"]}, "1387": {"id": "1101.2122v1", "title": "Molecules as tracers of galaxy evolution: an EMIR survey. I. Presentation of the data and first results", "url": "http://arxiv.org/pdf/1101.2122v1", "date": "2011-01-11 13:13:11", "abs": "We investigate the molecular gas properties of a sample of 23 galaxies in\norder to find and test chemical signatures of galaxy evolution and to compare\nthem to IR evolutionary tracers. Observation at 3 mm wavelengths were obtained\nwith the EMIR broadband receiver, mounted on the IRAM 30 m telescope on Pico\nVeleta, Spain. We compare the emission of the main molecular species with\nexisting models of chemical evolution by means of line intensity ratios\ndiagrams and principal component analysis. We detect molecular emission in 19\ngalaxies in two 8 GHz-wide bands centred at 88 and 112 GHz. The main detected\ntransitions are the J=1-0 lines of CO, 13CO, HCN, HNC, HCO+, CN, and C2H. We\nalso detect HC3N J=10-9 in the galaxies IRAS 17208, IC 860, NGC 4418, NGC 7771,\nand NGC 1068. The only HC3N detections are in objects with HCO+/HCN<1 and warm\nIRAS colours. Galaxies with the highest HC3N/HCN ratios have warm IRAS colours\n(60/100 {\\mu}m>0.8). The brightest HC3N emission is found in IC 860, where we\nalso detect the molecule in its vibrationally excited state.We find low HNC/HCN\nline ratios (<0.5), that cannot be explained by existing PDR or XDR chemical\nmodels. Bright HC3N emission in HCO+-faint objects may imply that these are not\ndominated by X-ray chemistry. Thus the HCN/HCO+ line ratio is not, by itself, a\nreliable tracer of XDRs. Bright HC3N and faint HCO+ could be signatures of\nembedded starformation, instead of AGN activity.", "cat": "astro-ph.CO", "authors": ["F. Costagliola", "S. Aalto", "M. I. Rodriguez", "S. Muller", "H. W. W. Spoon", "S. Mart\u00edn", "M. A. Per\u00e9z-Torres", "A. Alberdi", "J. E. Lindberg", "F. Batejat", "E. J\u00fctte", "P. van der Werf", "F. Lahuis"]}, "1388": {"id": "1911.06408v1", "title": "Design Requirements of Generic Hand Exoskeletons and Survey of Hand Exoskeletons for Rehabilitation, Assistive or Haptic Use", "url": "http://arxiv.org/pdf/1911.06408v1", "date": "2019-11-14 22:42:35", "abs": "Most current hand exoskeletons have been designed specifically for\nrehabilitation, assistive or haptic applications to simplify the design\nrequirements. Clinical studies on post-stroke rehabilitation have shown that\nadapting assistive or haptic applications into physical therapy sessions\nsignificantly improves the motor learning and treatment process. The recent\ntechnology can lead to the creation of generic hand exoskeletons that are\napplication-agnostic. In this paper, our motivation is to create guidelines and\nbest practices for generic exoskeletons by reviewing the literature of current\ndevices. First, we describe each application and briefly explain their design\nrequirements, and then list the design selections to achieve these\nrequirements. Then, we detail each selection by investigating the existing\nexoskeletons based on their design choices, and by highlighting their impact on\napplication types. With the motivation of creating efficient generic\nexoskeletons in the future, we finally summarize the best practices in the\nliterature.", "cat": "cs.RO", "authors": ["Mine Sarac", "Massimiliano Solazzi", "Antonio Frisoli"]}, "1389": {"id": "2106.02377v2", "title": "A Survey on Deep Domain Adaptation for LiDAR Perception", "url": "http://arxiv.org/pdf/2106.02377v2", "date": "2021-06-07 06:42:57", "abs": "Scalable systems for automated driving have to reliably cope with an\nopen-world setting. This means, the perception systems are exposed to drastic\ndomain shifts, like changes in weather conditions, time-dependent aspects, or\ngeographic regions. Covering all domains with annotated data is impossible\nbecause of the endless variations of domains and the time-consuming and\nexpensive annotation process. Furthermore, fast development cycles of the\nsystem additionally introduce hardware changes, such as sensor types and\nvehicle setups, and the required knowledge transfer from simulation. To enable\nscalable automated driving, it is therefore crucial to address these domain\nshifts in a robust and efficient manner. Over the last years, a vast amount of\ndifferent domain adaptation techniques evolved. There already exists a number\nof survey papers for domain adaptation on camera images, however, a survey for\nLiDAR perception is absent. Nevertheless, LiDAR is a vital sensor for automated\ndriving that provides detailed 3D scans of the vehicle's surroundings. To\nstimulate future research, this paper presents a comprehensive review of recent\nprogress in domain adaptation methods and formulates interesting research\nquestions specifically targeted towards LiDAR perception.", "cat": "cs.CV", "authors": ["Larissa T. Triess", "Mariella Dreissig", "Christoph B. Rist", "J. Marius Z\u00f6llner"]}, "1390": {"id": "1901.06032v7", "title": "A Survey of the Recent Architectures of Deep Convolutional Neural Networks", "url": "http://arxiv.org/pdf/1901.06032v7", "date": "2020-05-10 12:43:40", "abs": "Deep Convolutional Neural Network (CNN) is a special type of Neural Networks,\nwhich has shown exemplary performance on several competitions related to\nComputer Vision and Image Processing. Some of the exciting application areas of\nCNN include Image Classification and Segmentation, Object Detection, Video\nProcessing, Natural Language Processing, and Speech Recognition. The powerful\nlearning ability of deep CNN is primarily due to the use of multiple feature\nextraction stages that can automatically learn representations from the data.\nThe availability of a large amount of data and improvement in the hardware\ntechnology has accelerated the research in CNNs, and recently interesting deep\nCNN architectures have been reported. Several inspiring ideas to bring\nadvancements in CNNs have been explored, such as the use of different\nactivation and loss functions, parameter optimization, regularization, and\narchitectural innovations. However, the significant improvement in the\nrepresentational capacity of the deep CNN is achieved through architectural\ninnovations. Notably, the ideas of exploiting spatial and channel information,\ndepth and width of architecture, and multi-path information processing have\ngained substantial attention. Similarly, the idea of using a block of layers as\na structural unit is also gaining popularity. This survey thus focuses on the\nintrinsic taxonomy present in the recently reported deep CNN architectures and,\nconsequently, classifies the recent innovations in CNN architectures into seven\ndifferent categories. These seven categories are based on spatial exploitation,\ndepth, multi-path, width, feature-map exploitation, channel boosting, and\nattention. Additionally, the elementary understanding of CNN components,\ncurrent challenges, and applications of CNN are also provided.", "cat": "cs.CV", "authors": ["Asifullah Khan", "Anabia Sohail", "Umme Zahoora", "Aqsa Saeed Qureshi"]}, "1391": {"id": "1905.12117v1", "title": "The Evolution of Brightest Cluster Galaxies in the Nearby Universe I: Colours and Stellar Masses from the Sloan Digital Sky Survey and Wide Infrared Survey Explorer", "url": "http://arxiv.org/pdf/1905.12117v1", "date": "2019-05-28 22:25:19", "abs": "We present a study of the evolution of brightest cluster galaxies (BCGs) in a\nsample of clusters at $0.05 \\leq z<0.35$ from the SDSS and WISE with halo\nmasses in the range $6 \\times 10^{13}M_\\odot$ (massive groups) -\n$10^{15.5}M_\\odot$ (Coma-like clusters). We analyse optical and infrared\ncolours and stellar masses of BCGs as a function of the mass of their host\nhaloes. We find that BCGs are mostly red and quiescent galaxies and that a\nminority ($\\sim 9$\\%) of them are star-forming. We find that the optical $g-r$\ncolours are consistent with those of red sequence galaxies at the same\nredshifts; however, we detect the presence of a tail of blue and mostly\nstar-forming BCGs preferentially located in low-mass clusters and groups.\nAlthough the blue tail is dominated by star-forming galaxies, we find that\nstar-forming BCGs may also have red $g-r$ colours, indicating dust-enshrouded\nstar formation. The fraction of star-forming BCGs increases with redshift and\ndecreases with cluster mass and BCG stellar mass. We find that cool-core\nclusters host both star-forming and quiescent BCGs; however, non cool-core\nclusters are dominated by quiescent BCGs. Star formation appears thus as the\nresult of processes that depend on stellar mass, cluster mass and cooling state\nof the intra-cluster medium. Our results suggest no significant stellar mass\ngrowth at $z<0.35$, supporting the notion that BCGs had accreted most of their\nmass by $z = 0.35$. Overall we find a low (1\\%) AGN fraction detected at IR\nwavelengths.", "cat": "astro-ph.GA", "authors": ["Pierluigi Cerulo", "Gustavo A. Orellana", "Giovanni Covone"]}, "1392": {"id": "2009.03071v2", "title": "The TESS-Keck Survey II: An Ultra-Short Period Rocky Planet and its Siblings Transiting the Galactic Thick-Disk Star TOI-561", "url": "http://arxiv.org/pdf/2009.03071v2", "date": "2020-12-14 19:30:28", "abs": "We report the discovery of TOI-561, a multi-planet system in the galactic\nthick disk that contains a rocky, ultra-short period planet (USP). This bright\n($V=10.2$) star hosts three small transiting planets identified in photometry\nfrom the NASA TESS mission: TOI-561 b (TOI-561.02, P=0.44 days, $R_b =\n1.45\\pm0.11\\,R_\\oplus$), c (TOI-561.01, P=10.8 days,\n$R_c=2.90\\pm0.13\\,R_\\oplus$), and d (TOI-561.03, P=16.3 days,\n$R_d=2.32\\pm0.16\\,R_\\oplus$). The star is chemically ([Fe/H]$=-0.41\\pm0.05$,\n[$\\alpha$/H]$=+0.23\\pm0.05$) and kinematically consistent with the galactic\nthick disk population, making TOI-561 one of the oldest ($10\\pm3\\,$Gyr) and\nmost metal-poor planetary systems discovered yet. We dynamically confirm\nplanets b and c with radial velocities from the W. M. Keck Observatory High\nResolution Echelle Spectrometer. Planet b has a mass and density of\n$3.2\\pm0.8\\,M_\\oplus$ and $5.5^{+2.0}_{-1.6}\\,$g$\\,$cm$^{-3}$, consistent with\na rocky composition. Its lower-than-average density is consistent with an\niron-poor composition, although an Earth-like iron-to-silicates ratio is not\nruled out. Planet c is $7.0\\pm2.3\\,M_\\oplus$ and $1.6\\pm0.6\\,$g$\\,$cm$^{-3}$,\nconsistent with an interior rocky core overlaid with a low-mass volatile\nenvelope. Several attributes of the photometry for planet d (which we did not\ndetect dynamically) complicate the analysis, but we vet the planet with\nhigh-contrast imaging, ground-based photometric follow-up and radial\nvelocities. TOI-561 b is the first rocky world around a galactic thick-disk\nstar confirmed with radial velocities and one of the best rocky planets for\nthermal emission studies.", "cat": "astro-ph.EP", "authors": ["Lauren M. Weiss", "Fei Dai", "Daniel Huber", "John M. Brewer", "Karen A. Collins", "David R. Ciardi", "Elisabeth C. Matthews", "Carl Ziegler", "Steve B. Howell", "Natalie M. Batalha", "Ian J. M> Crossfield", "Courtney Dressing", "Benjamin Fulton", "Andrew W. Howard", "Howard Isaacson", "Stephen R. Kane", "Erik A. Petigura", "Paul Robertson", "Arpita Roy", "Ryan A. Rubenzahl", "Joseph D. Twicken", "Zachary R. Claytor", "Keivan G. Stassun", "Mason G. MacDougall", "Ashley Chontos", "Steven Giacalone", "Paul A. Dalba", "Teo Mocnik", "Michelle L. Hill", "Corey Beard", "Joseph M. Akana Murphy", "Lee J. Rosenthal", "Aida Behmard", "Judan van Zandt", "Jack Lubin", "Molly R. Kosiarek", "Michael B. Lund", "Jessie L. Christiansen", "Rachel A. Matson", "Charles A. Beichman", "Joshua E. Schlieder", "Erica J. Gonzales", "C\u00e9sar Brice\u00f1o", "Nicholas Law", "Andrew W. Mann", "Kevin I. Collins", "Phil Evans", "Akihiko Fukui", "Eric L. N. Jensen", "Felipe Murgas", "Norio Narita", "Eric Palle", "Hannu Parviainen", "Richard P. Schwarz", "Thiam-Guan Tan", "Jack S. Acton", "Edwarf M. Bryant", "Alexander Chaushev", "Philipp Eigm\u00fcller", "Sam Gill", "Jon Jenkins", "George Ricker", "Sara Seager", "Joshua N. Winn"]}, "1393": {"id": "2011.14976v1", "title": "Cloud-Based Video Streaming Services: A Survey", "url": "http://arxiv.org/pdf/2011.14976v1", "date": "2020-11-30 16:48:21", "abs": "Video streaming, in various forms of video on demand (VOD), live, and 360\ndegree streaming, has grown dramatically during the past few years. In\ncomparison to traditional cable broadcasters whose contents can only be watched\non TVs, video streaming is ubiquitous and viewers can flexibly watch the video\ncontents on various devices, ranging from smart-phones to laptops and large TV\nscreens. Such ubiquity and flexibility are enabled by interweaving multiple\ntechnologies, such as video compression, cloud computing, content delivery\nnetworks, and several other technologies. As video streaming gains more\npopularity and dominates the Internet traffic, it is essential to understand\nthe way it operates and the interplay of different technologies involved in it.\nAccordingly, the first goal of this paper is to unveil sophisticated processes\nto deliver a raw captured video to viewers' devices. In particular, we\nelaborate on the video encoding, transcoding, packaging, encryption, and\ndelivery processes. We survey recent efforts in academia and industry to\nenhance these processes. As video streaming industry is increasingly becoming\nreliant on cloud computing, the second goal of this survey is to explore and\nsurvey the ways cloud services are utilized to enable video streaming services.\nThe third goal of the study is to position the undertaken research works in\ncloud-based video streaming and identify challenges that need to be obviated in\nfuture to advance cloud-based video streaming industry to a more flexible and\nuser-centric service.", "cat": "cs.MM", "authors": ["Xiangbo Li", "Mahmoud Darwich", "Magdy Bayoumi", "Mohsen Amini Salehi"]}, "1394": {"id": "1611.00859v2", "title": "The Gaia-ESO Survey: the inner disk, intermediate-age open cluster Trumpler 23", "url": "http://arxiv.org/pdf/1611.00859v2", "date": "2017-01-10 17:11:27", "abs": "Context: Trumpler 23 is a moderately populated, intermediate-age open cluster\nwithin the solar circle at a Rgc ~6 kpc. It is in a crowded field very close to\nthe Galactic plane and the color-magnitude diagram shows significant field\ncontamination and possible differential reddening; it is a relatively\nunderstudied cluster for these reasons, but its location makes it a key object\nfor determining Galactic abundance distributions.\n Aims: New data from the Gaia-ESO Survey enable the first ever radial velocity\nand spectroscopic metallicity measurements for this cluster. We aim to use\nvelocities to isolate cluster members, providing more leverage for determining\ncluster parameters.\n Methods: Gaia-ESO Survey data for 167 potential members have yielded radial\nvelocity measurements, which were used to determine the systemic velocity of\nthe cluster and membership of individual stars. Atmospheric parameters were\nalso used as a check on membership when available. Literature photometry was\nused to re-determine cluster parameters based on radial velocity member stars\nonly; theoretical isochrones are fit in the V, V-I diagram. Cluster abundance\nmeasurements of ten radial-velocity member stars with high-resolution\nspectroscopy are presented for 24 elements. These abundances have been compared\nto local disk stars, and where possible placed within the context of literature\ngradient studies.\n Results: We find Trumpler 23 to have an age of 0.80 +/- 0.10 Gyr, significant\ndifferential reddening with an estimated mean cluster E(V-I) of 1.02\n+0.14/-0.09, and an apparent distance modulus of 14.15 +/- 0.20. We find an\naverage cluster metallicity of [Fe/H] = 0.14 +/- 0.03 dex, a solar [alpha/Fe]\nabundance, and notably subsolar [s-process/Fe] abundances.", "cat": "astro-ph.SR", "authors": ["J. C. Overbeek", "E. D. Friel", "P. Donati", "R. Smiljanic", "H. R. Jacobson", "D. Hatzidimitriou", "E. V. Held", "L. Magrini", "A. Bragaglia", "S. Randich", "A. Vallenari", "T. Cantat-Gaudin", "G. Tautvaisiene", "F. Jimenez-Esteban", "A. Frasca", "D. Geisler", "S. Villanova", "B. Tang", "C. Munoz", "G. Marconi", "G. Carraro", "I. San Roman", "A. Drazdauskas", "R. Zenoviene", "G. Gilmore", "R. D. Jeffries", "E. Flaccomio", "E. Pancino", "A. Bayo", "M. T. Costado", "F. Damiani", "P. Jofre", "L. Monaco", "L. Prisinzano", "S. G. Sousa", "S. Zaggia"]}, "1395": {"id": "1610.06175v1", "title": "HI4PI: A full-sky HI survey based on EBHIS and GASS", "url": "http://arxiv.org/pdf/1610.06175v1", "date": "2016-10-19 20:00:01", "abs": "Measurement of the Galactic neutral atomic hydrogen (HI) column density, NHI,\nand brightness temperatures, Tb, is of high scientific value for a broad range\nof astrophysical disciplines. In the past two decades, one of the most-used\nlegacy HI datasets has been the Leiden/Argentine/Bonn Survey (LAB). We release\nthe HI 4$\\pi$ survey (HI4PI), an all-sky database of Galactic HI, which\nsupersedes the LAB survey. The HI4PI survey is based on data from the recently\ncompleted first coverage of the Effelsberg-Bonn HI Survey (EBHIS) and from the\nthird revision of the Galactic All-Sky Survey (GASS). EBHIS and GASS share\nsimilar angular resolution and match well in sensitivity. Combined, they are\nideally suited to be a successor to LAB. The new HI4PI survey outperforms the\nLAB in angular resolution (16.2', FWHM) and sensitivity (RMS: 43 mK). Moreover,\nit has full spatial sampling and thus overcomes a major drawback of LAB, which\nseverely undersamples the sky. We publish all-sky column density maps of the\nneutral atomic hydrogen in the Milky Way, along with full spectroscopic data,\nin several map projections including HEALPix.", "cat": "astro-ph.GA", "authors": ["HI4PI Collaboration", "N. Ben Bekhti", "L. Fl\u00f6er", "R. Keller", "J. Kerp", "D. Lenz", "B. Winkel", "J. Bailin", "M. R. Calabretta", "L. Dedes", "H. A. Ford", "B. K. Gibson", "U. Haud", "S. Janowiecki", "P. M. W. Kalberla", "F. J. Lockman", "N. M. McClure-Griffiths", "T. Murphy", "H. Nakanishi", "D. J. Pisano", "L. Staveley-Smith"]}, "1396": {"id": "1502.07041v1", "title": "Describing Colors, Textures and Shapes for Content Based Image Retrieval - A Survey", "url": "http://arxiv.org/pdf/1502.07041v1", "date": "2015-02-25 03:51:43", "abs": "Visual media has always been the most enjoyed way of communication. From the\nadvent of television to the modern day hand held computers, we have witnessed\nthe exponential growth of images around us. Undoubtedly it's a fact that they\ncarry a lot of information in them which needs be utilized in an effective\nmanner. Hence intense need has been felt to efficiently index and store large\nimage collections for effective and on- demand retrieval. For this purpose\nlow-level features extracted from the image contents like color, texture and\nshape has been used. Content based image retrieval systems employing these\nfeatures has proven very successful. Image retrieval has promising applications\nin numerous fields and hence has motivated researchers all over the world. New\nand improved ways to represent visual content are being developed each day.\nTremendous amount of research has been carried out in the last decade. In this\npaper we will present a detailed overview of some of the powerful color,\ntexture and shape descriptors for content based image retrieval. A comparative\nanalysis will also be carried out for providing an insight into outstanding\nchallenges in this field.", "cat": "cs.IR", "authors": ["Jamil Ahmad", "Muhammad Sajjad", "Irfan Mehmood", "Seungmin Rho", "Sung Wook Baik"]}, "1397": {"id": "1704.06043v2", "title": "X-Ray bright optically faint active galactic nuclei in the Subaru Hyper Suprime-Cam wide survey", "url": "http://arxiv.org/pdf/1704.06043v2", "date": "2017-09-05 07:31:17", "abs": "We construct a sample of X-ray bright optically faint active galactic nuclei\nby combining Subaru Hyper Suprime-Cam, XMM-Newton, and infrared source\ncatalogs. 53 X-ray sources satisfying i band magnitude fainter than 23.5 mag\nand X-ray counts with EPIC-PN detector larger than 70 are selected from 9.1\ndeg^2, and their spectral energy distributions (SEDs) and X-ray spectra are\nanalyzed. 44 objects with an X-ray to i-band flux ratio F_X/F_i>10 are\nclassified as extreme X-ray-to-optical flux sources. SEDs of 48 among 53 are\nrepresented by templates of type 2 AGNs or starforming galaxies and show\nsignature of stellar emission from host galaxies in the optical in the source\nrest frame. Infrared/optical SEDs indicate significant contribution of emission\nfrom dust to infrared fluxes and that the central AGN is dust obscured.\nPhotometric redshifts determined from the SEDs are in the range of 0.6-2.5.\nX-ray spectra are fitted by an absorbed power law model, and the intrinsic\nabsorption column densities are modest (best-fit log N_H = 20.5-23.5 cm^-2 in\nmost cases). The absorption corrected X-ray luminosities are in the range of\n6x10^42 - 2x10^45 erg s^-1. 20 objects are classified as type 2 quasars based\non X-ray luminsosity and N_H. The optical faintness is explained by a\ncombination of redshifts (mostly z>1.0), strong dust extinction, and in part a\nlarge ratio of dust/gas.", "cat": "astro-ph.GA", "authors": ["Yuichi Terashima", "Makoto Suganuma", "Masayuki Akiyama", "Jenny. E. Greene", "Toshihiro Kawaguchi", "Kazushi Iwasawa", "Tohru Nagao", "Hirofumi Noda", "Yoshiki Toba", "Yoshihiro Ueda", "Takuji Yamashita"]}, "1398": {"id": "1706.00427v2", "title": "Source Selection for Cluster Weak Lensing Measurements in the Hyper Suprime-Cam Survey", "url": "http://arxiv.org/pdf/1706.00427v2", "date": "2018-01-10 19:22:47", "abs": "We present optimized source galaxy selection schemes for measuring cluster\nweak lensing (WL) mass profiles unaffected by cluster member dilution from the\nSubaru Hyper Suprime-Cam Strategic Survey Program (HSC-SSP). The ongoing\nHSC-SSP survey will uncover thousands of galaxy clusters to $z\\lesssim1.5$. In\nderiving cluster masses via WL, a critical source of systematics is\ncontamination and dilution of the lensing signal by cluster {members, and by\nforeground galaxies whose photometric redshifts are biased}. Using the\nfirst-year CAMIRA catalog of $\\sim$900 clusters with richness larger than 20\nfound in $\\sim$140 deg$^2$ of HSC-SSP data, we devise and compare several\nsource selection methods, including selection in color-color space (CC-cut),\nand selection of robust photometric redshifts by applying constraints on their\ncumulative probability distribution function (PDF; P-cut). We examine the\ndependence of the contamination on the chosen limits adopted for each method.\nUsing the proper limits, these methods give mass profiles with minimal dilution\nin agreement with one another. We find that not adopting either the CC-cut or\nP-cut methods results in an underestimation of the total cluster mass\n($13\\pm4\\%$) and the concentration of the profile ($24\\pm11\\%$). The level of\ncluster contamination can reach as high as $\\sim10\\%$ at $R\\approx 0.24$\nMpc/$h$ for low-z clusters without cuts, while employing either the P-cut or\nCC-cut results in cluster contamination consistent with zero to within the 0.5%\nuncertainties. Our robust methods yield a $\\sim60\\sigma$ detection of the\nstacked CAMIRA surface mass density profile, with a mean mass of\n$M_\\mathrm{200c} = (1.67\\pm0.05({\\rm {stat}}))\\times 10^{14}\\,M_\\odot/h$.", "cat": "astro-ph.CO", "authors": ["Elinor Medezinski", "Masamune Oguri", "Atsushi J. Nishizawa", "Joshua S. Speagle", "Hironao Miyatake", "Keiichi Umetsu", "Alexie Leauthaud", "Ryoma Murata", "Rachel Mandelbaum", "Crist\u00f3bal Sif\u00f3n", "Michael A. Strauss", "Song Huang", "Melanie Simet", "Nobuhiro Okabe", "Masayuki Tanaka", "Yutaka Komiyama"]}, "1399": {"id": "1810.03828v1", "title": "AKARI/IRC Near-Infrared Asteroid Spectroscopic Survey: AcuA-spec", "url": "http://arxiv.org/pdf/1810.03828v1", "date": "2018-10-09 06:23:11", "abs": "Knowledge of water in the solar system is important for understanding of a\nwide range of evolutionary processes and the thermal history of the solar\nsystem. To explore the existence of water in the solar system, it is\nindispensable to investigate hydrated minerals and/or water ice on asteroids.\nThese water-related materials show absorption features in the 3-$\\micron$ band\n(wavelengths from 2.7 to 3.1 $\\micron$). We conducted a spectroscopic survey of\nasteroids in the 3-$\\micron$ band using the Infrared Camera (IRC) on board the\nJapanese infrared satellite AKARI. In the warm mission period of AKARI, 147\npointed observations were performed for 66 asteroids in the grism mode for\nwavelengths from 2.5 to 5 $\\micron$. According to these observations, most\nC-complex asteroids have clear absorption features ($> 10\\%$ with respect to\nthe continuum) related to hydrated minerals at a peak wavelength of\napproximately 2.75 $\\micron$, while S-complex asteroids have no significant\nfeature in this wavelength range. The present data are released to the public\nas the Asteroid Catalog using AKARI Spectroscopic Observations (AcuA-spec).", "cat": "astro-ph.EP", "authors": ["Fumihiko Usui", "Sunao Hasegawa", "Takafumi Ootsubo", "Takashi Onaka"]}, "1400": {"id": "1901.05983v2", "title": "Stellar populations of galaxies in the ALHAMBRA survey up to $z \\sim 1$. IV. Properties of quiescent galaxies on the stellar mass$-$size plane", "url": "http://arxiv.org/pdf/1901.05983v2", "date": "2019-10-03 12:25:18", "abs": "We perform a comprehensive study of the stellar population properties of\nquiescent galaxies as a function of size and stellar mass to constrain the\nphysical mechanism governing the stellar mass assembly and the likely evolutive\nscenarios that explain their growth in size. After selecting all the quiescent\ngalaxies from the ALHAMBRA survey by the dust-corrected stellar mass$-$colour\ndiagram, we built a shared sample of $\\sim850$ quiescent galaxies with reliable\nsizes from the HST. The stellar population properties were retrieved using the\nSED-fitting code MUFFIT with various sets of composite stellar population\nmodels. Age, formation epoch, metallicity, and extinction were studied on the\nstellar mass$-$size plane as function of size through a Monte Carlo approach.\nThis accounted for uncertainties and degeneracy effects amongst stellar\npopulation properties. The stellar population properties of quiescent galaxies\nand their stellar mass and size since $z\\sim1$ are correlated. At fixed stellar\nmass, the more compact the quiescent galaxy, the older and richer in metals it\nis ($1$Gyr and $0.1$dex, respectively). In addition, more compact galaxies may\npresent slight lower extinctions than their more extended counterparts at the\nsame stellar mass ($<0.1$ mag). By means of studying constant regions of\nstellar population properties across the stellar mass$-$size plane, we obtained\nempirical relations to constrain the physical mechanism that governs the\nstellar mass assembly of the form $M_\\star \\propto r_\\mathrm{c}^\\alpha$, where\n$\\alpha$ amounts to $0.50-0.55 \\pm 0.09$. There are indications that support\nthe idea that the velocity dispersion is tightly correlated with the stellar\ncontent of galaxies. The mechanisms driving the evolution of stellar\npopulations can therefore be partly linked to the dynamical properties of\ngalaxies, along with their gravitational potential.", "cat": "astro-ph.GA", "authors": ["L. A. D\u00edaz-Garc\u00eda", "A. J. Cenarro", "C. L\u00f3pez-Sanjuan", "L. Peralta de Arriba", "I. Ferreras", "M. Cervi\u00f1o", "I. M\u00e1rquez", "J. Masegosa", "A. del Olmo", "J. Perea"]}, "1401": {"id": "2303.03885v1", "title": "AI Risk Skepticism, A Comprehensive Survey", "url": "http://arxiv.org/pdf/2303.03885v1", "date": "2023-02-16 16:32:38", "abs": "In this thorough study, we took a closer look at the skepticism that has\narisen with respect to potential dangers associated with artificial\nintelligence, denoted as AI Risk Skepticism. Our study takes into account\ndifferent points of view on the topic and draws parallels with other forms of\nskepticism that have shown up in science. We categorize the various skepticisms\nregarding the dangers of AI by the type of mistaken thinking involved. We hope\nthis will be of interest and value to AI researchers concerned about the future\nof AI and the risks that it may pose. The issues of skepticism and risk in AI\nare decidedly important and require serious consideration. By addressing these\nissues with the rigor and precision of scientific research, we hope to better\nunderstand the objections we face and to find satisfactory ways to resolve\nthem.", "cat": "cs.CY", "authors": ["Vemir Michael Ambartsoumean", "Roman V. Yampolskiy"]}, "1402": {"id": "1905.10081v1", "title": "The Baum-Connes conjecture: an extended survey", "url": "http://arxiv.org/pdf/1905.10081v1", "date": "2019-05-24 08:14:21", "abs": "We present a history of the Baum-Connes conjecture, the methods involved, the\ncurrent status, and the mathematics it generated.", "cat": "math.OA", "authors": ["Maria Paula Gomez Aparicio", "Pierre Julg", "Alain Valette"]}, "1403": {"id": "1102.0831v1", "title": "Intelligent Semantic Web Search Engines: A Brief Survey", "url": "http://arxiv.org/pdf/1102.0831v1", "date": "2011-02-04 03:56:09", "abs": "The World Wide Web (WWW) allows the people to share the information (data)\nfrom the large database repositories globally. The amount of information grows\nbillions of databases. We need to search the information will specialize tools\nknown generically search engine. There are many of search engines available\ntoday, retrieving meaningful information is difficult. However to overcome this\nproblem in search engines to retrieve meaningful information intelligently,\nsemantic web technologies are playing a major role. In this paper we present\nsurvey on the search engine generations and the role of search engines in\nintelligent web and semantic search technologies.", "cat": "cs.AI", "authors": ["G. Madhu", "Dr. A. Govardhan", "Dr. T. V. Rajinikanth"]}, "1404": {"id": "1605.05792v1", "title": "Chemical tagging in the SDSS-III/APOGEE survey: new identifications of halo stars with globular cluster origins", "url": "http://arxiv.org/pdf/1605.05792v1", "date": "2016-05-19 01:31:47", "abs": "We present new identifications of five red giant stars in the Galactic halo\nwith chemical abundance patterns that indicate they originally formed in\nglobular clusters. Using data from the Apache Point Observatory Galactic\nEvolution Experiment (APOGEE) Survey available through Sloan Digital Sky Survey\nData Release 12 (DR12), we first identify likely halo giants, and then search\nthose for the well-known chemical tags associated with globular clusters,\nspecifically enrichment in nitrogen and aluminum. We find that 2% of the halo\ngiants in our sample have this chemical signature, in agreement with previous\nresults. Following the interpretation in our previous work on this topic, this\nwould imply that at least 13% of halo stars originally formed in globular\nclusters. Recent developments in the theoretical understanding of globular\ncluster formation raise questions about that interpretation, and we concede the\npossibility that these migrants represent a small fraction of the halo field.\nThere are roughly as many stars with the chemical tags of globular clusters in\nthe halo field as there are in globular clusters, whether or not they are\naccompanied by a much larger chemically untaggable population of former\nglobular cluster stars.", "cat": "astro-ph.GA", "authors": ["Sarah Martell", "Matthew Shetrone", "Sara Lucatello", "Ricardo Schiavon", "Szabolcs Meszaros", "Carlos Allende Prieto", "Anibal Garcia Hernandez", "Tim Beers", "David Nidever"]}, "1405": {"id": "1611.07722v1", "title": "A Survey on Privacy-preserving Schemes for Smart Grid Communications", "url": "http://arxiv.org/pdf/1611.07722v1", "date": "2016-11-23 10:20:34", "abs": "In this paper, we present a comprehensive survey of privacy-preserving\nschemes for Smart Grid communications. Specifically, we select and in-detail\nexamine thirty privacy preserving schemes developed for or applied in the\ncontext of Smart Grids. Based on the communication and system models, we\nclassify these schemes that are published between 2013 and 2016, in five\ncategories, including, 1) Smart grid with the advanced metering infrastructure,\n2) Data aggregation communications, 3) Smart grid marketing architecture, 4)\nSmart community of home gateways, and 5) Vehicle-to grid architecture. For each\nscheme, we survey the attacks of leaking privacy, countermeasures, and game\ntheoretic approaches. In addition, we review the survey articles published in\nthe recent years that deal with Smart Grids communications, applications,\nstandardization, and security. Based on the current survey, several\nrecommendations for further research are discussed at the end of this paper.", "cat": "cs.CR", "authors": ["Mohamed Amine Ferrag", "Leandros A. Maglaras", "Helge Janicke", "Jianmin Jiang"]}, "1406": {"id": "2404.18897v1", "title": "Neural network prediction of model parameters for strong lensing samples from Hyper Suprime-Cam Survey", "url": "http://arxiv.org/pdf/2404.18897v1", "date": "2024-04-29 17:34:24", "abs": "Galaxies that cause the strong gravitational lensing of background galaxies\nprovide us crucial information about the distribution of matter around them.\nTraditional modelling methods that analyse such strong lenses are both time and\nresource consuming, require sophisticated lensing codes and modelling\nexpertise. To study the large lens population expected from imaging surveys\nsuch as LSST, we need fast and automated analysis methods. In this work, we\nbuild and train a simple convolutional neural network with an aim to rapidly\npredict model parameters of gravitational lenses. We focus on the most\nimportant lens mass model parameters, namely, the Einstein radius, the axis\nratio and the position angle of the major axis of the mass distribution. The\nnetwork is trained on a variety of simulated data with an increasing degree of\nrealism and shows satisfactory performance on simulated test data. The trained\nnetwork is then applied to the real sample of galaxy-scale candidate lenses\nfrom the Subaru HSC, a precursor survey to LSST. Unlike the simulated lenses,\nwe do not have the ground truth for the real lenses. Therefore, we have\ncompared our predictions with those from YattaLens, a lens modelling pipeline.\nAdditionally, we also compare the parameter predictions for 10 HSC lenses that\nwere also studied by other conventional modelling methods. These comparisons\nshow a fair quantitative agreement on the Einstein radius, although the axis\nratio and the position angle from the network as well as the individual\nmodelling methods, seem to have systematic uncertainties beyond the quoted\nerrors.", "cat": "astro-ph.CO", "authors": ["Priyanka Gawade", "Anupreeta More", "Surhud More", "Akisato Kimura", "Alessandro Sonnenfeld", "Masamune Oguri", "Naoki Yoshida"]}, "1407": {"id": "2109.10787v1", "title": "DHT-based Communications Survey: Architectures and Use Cases", "url": "http://arxiv.org/pdf/2109.10787v1", "date": "2021-09-22 15:18:04", "abs": "Several distributed system paradigms utilize Distributed Hash Tables (DHTs)\nto realize structured peer-to-peer (P2P) overlays. DHT structures arise as the\nmost commonly used organizations for peers that can efficiently perform crucial\nservices such as data storage, replication, query resolution, and load\nbalancing. With the advances in various distributed system technologies, novel\nand efficient solutions based on DHTs emerge and play critical roles in system\ndesign. DHT-based methods and communications have been proposed to address\nchallenges such as scalability, availability, reliability and performance, by\nconsidering unique characteristics of these technologies. In this article, we\npropose a classification of the state-of-the-art DHT-based methods focusing on\ntheir system architecture, communication, routing and technological aspects\nacross various system domains. To the best of our knowledge, there is no\ncomprehensive survey on DHT-based applications from system architecture and\ncommunication perspectives that spans various domains of recent distributed\nsystem technologies. We investigate the recently emerged DHT-based solutions in\nthe seven key domains of edge and fog computing, cloud computing, blockchain,\nthe Internet of Things (IoT), Online Social Networks (OSNs), Mobile Ad Hoc\nNetworks (MANETs), and Vehicular Ad Hoc Networks (VANETs). In contrast to the\nexisting surveys, our study goes beyond the commonly known DHT methods such as\nstorage, routing, and lookup, and identifies diverse DHT-based solutions\nincluding but not limited to aggregation, task scheduling, resource management\nand discovery, clustering and group management, federation, data dependency\nmanagement, and data transmission. Furthermore, we identify open problems and\ndiscuss future research guidelines for each domain.", "cat": "cs.DC", "authors": ["Yahya Hassanzadeh-Nazarabadi", "Sanaz Taheri-Boshrooyeh", "Safa Otoum", "Seyhan Ucar", "\u00d6znur \u00d6zkasap"]}, "1408": {"id": "1812.09628v1", "title": "Intelligent Tutoring Systems: A Comprehensive Historical Survey with Recent Developments", "url": "http://arxiv.org/pdf/1812.09628v1", "date": "2018-12-23 00:40:44", "abs": "This paper provides interested beginners with an updated and detailed\nintroduction to the field of Intelligent Tutoring Systems (ITS). ITSs are\ncomputer programs that use artificial intelligence techniques to enhance and\npersonalize automation in teaching. This paper is a literature review that\nprovides the following: First, a review of the history of ITS along with a\ndiscussion on the interface between human learning and computer tutors and how\neffective ITSs are in contemporary education. Second, the traditional\narchitectural components of an ITS and their functions are discussed along with\napproaches taken by various ITSs. Finally, recent innovative ideas in ITS\nsystems are presented. This paper concludes with some of the author's views\nregarding future work in the field of intelligent tutoring systems.", "cat": "cs.HC", "authors": ["Ali Alkhatlan", "Jugal Kalita"]}, "1409": {"id": "2311.08474v2", "title": "The ALMA-ALPINE [CII] survey: Kennicutt-Schmidt relation in four massive main-sequence galaxies at z~4.5", "url": "http://arxiv.org/pdf/2311.08474v2", "date": "2023-11-17 10:47:11", "abs": "The Kennicutt-Schmidt (KS) relation between the gas and the star formation\nrate (SFR) surface density ($\\Sigma_{\\rm gas}$-$\\Sigma_{\\rm SFR}$) is essential\nto understand star formation processes in galaxies. So far, it has been\nmeasured up to z~2.5 in main-sequence galaxies. In this letter, we aim to put\nconstraints at z~4.5 using a sample of four massive main-sequence galaxies\nobserved by ALMA at high resolution. We obtained ~0.3\"-resolution [CII] and\ncontinuum maps of our objects, which we then converted into gas and obscured\nSFR surface density maps. In addition, we produced unobscured SFR surface\ndensity maps by convolving Hubble ancillary data in the rest-frame UV. We then\nderived the average $\\Sigma_{\\rm SFR}$ in various $\\Sigma_{\\rm gas}$ bins, and\nestimated the uncertainties using a Monte Carlo sampling. Our galaxy sample\nfollows the KS relation measured in main-sequence galaxies at lower redshift\nand is slightly lower than predictions from simulations. Our data points probe\nthe high end both in terms of $\\Sigma_{\\rm gas}$ and $\\Sigma_{\\rm gas}$, and\ngas depletion timescales (285-843 Myr) remain similar to z~2 objects. However,\nthree of our objects are clearly morphologically disturbed, and we could have\nexpected shorter gas depletion timescales (~100 Myr) similar to merger-driven\nstarbursts at lower redshifts. This suggests that the mechanisms triggering\nstarbursts at high redshift may be different than in the low- and\nintermediate-z Universe.", "cat": "astro-ph.GA", "authors": ["M. B\u00e9thermin", "C. Accard", "C. Guillaume", "M. Dessauges-Zavadsky", "E. Ibar", "P. Cassata", "T. Devereaux", "A. Faisst", "J. Freundlich", "G. C. Jones", "K. Kraljic", "H. Algera", "R. O. Amorin", "S. Bardelli", "M. Boquien", "V. Buat", "E. Donghia", "Y. Dubois", "A. Ferrara", "Y. Fudamoto", "M. Ginolfi", "P. Guillard", "M. Giavalisco", "C. Gruppioni", "G. Gururajan", "N. Hathi", "C. C. Hayward", "A. M. Koekemoer", "B. C. Lemaux", "G. E. Magdis", "J. Molina", "D. Narayanan", "L. Mayer", "F. Pozzi", "F. Rizzo", "M. Romano", "L. Tasca", "P. Theul\u00e9", "D. Vergani", "L. Vallini", "G. Zamorani", "A. Zanella", "E. Zucca"]}, "1410": {"id": "1512.00318v1", "title": "A Proper Motion Survey Using the First Sky Pass of NEOWISE-Reactivation Data", "url": "http://arxiv.org/pdf/1512.00318v1", "date": "2015-12-01 16:10:59", "abs": "The Wide-field Infrared Survey Explorer (WISE) was reactivated in December of\n2013 (NEOWISE) to search for potentially hazardous near-Earth objects. We have\nconducted a survey using the first sky pass of NEOWISE data and the AllWISE\ncatalog to identify nearby stars and brown dwarfs with large proper motions\n($\\mu_{\\rm total}$ $\\gtrsim$ 250 mas yr$^{-1}$). A total of 20,548 high proper\nmotion objects were identified, 1,006 of which are new discoveries. This survey\nhas uncovered a significantly larger sample of fainter objects (W2 $\\gtrsim$13\nmag) than the previous WISE motion surveys of Luhman (2014a) and Kirkpatrick et\nal. (2014). Many of these objects are predicted to be new L and T dwarfs based\non near- and mid-infrared colors. Using estimated spectral types along with\ndistance estimates, we have identified several objects likely belonging to the\nnearby Solar neighborhood (d $<$ 25 pc). We have followed up 19 of these new\ndiscoveries with near-infrared or optical spectroscopy, focusing on potentially\nnearby objects, objects with the latest predicted spectral types, and potential\nlate-type subdwarfs. This subset includes 6 M dwarfs, 5 of which are likely\nsubdwarfs, as well as 8 L dwarfs and 5 T dwarfs, many of which have blue\nnear-infrared colors. As an additional supplement, we provide 2MASS and AllWISE\npositions and photometry for every object found in our search, as well as\n2MASS/AllWISE calculated proper motions.", "cat": "astro-ph.SR", "authors": ["Adam C. Schneider", "Jennifer Greco", "Michael C. Cushing", "J. Davy Kirkpatrick", "Amy Mainzer", "Christopher R. Gelino", "Sergio B. Fajardo-Acosta", "James Bauer"]}, "1411": {"id": "1605.09331v1", "title": "Clues to the Structure of AGN through massive variability surveys", "url": "http://arxiv.org/pdf/1605.09331v1", "date": "2016-05-30 17:15:35", "abs": "Variability studies hold information on otherwise unresolvable regions in\nActive Galactic Nuclei (AGN). Population studies of large samples likewise have\nbeen very productive for our understanding of AGN. These two themes are coming\ntogether in the idea of systematic variability studies of large samples - with\nSDSS, PanSTARRS, and soon, LSST. I summarise what we have learned about the\noptical and UV variability of AGN, and what it tells us about accretion discs\nand the BLR. The most exciting recent results have focused on rare large-scale\noutbursts and collapses - Tidal Disruption Events, changing-look AGN, and large\namplitude microlensing. All of these promise to give us new insight into AGN\nphysics.", "cat": "astro-ph.HE", "authors": ["Andy Lawrence"]}, "1412": {"id": "2408.08915v1", "title": "A Survey on Blockchain-based Supply Chain Finance with Progress and Future directions", "url": "http://arxiv.org/pdf/2408.08915v1", "date": "2024-08-14 15:08:51", "abs": "Supply Chain Finance is very important for supply chain competition, which is\nan important tool to activate the capital flow in the supply chain. Supply\nChain Finance-related research can support multiple applications and services,\nsuch as providing accounts receivable financing, enhancing risk management, and\noptimizing supply chain management. For more than a decade, the development of\nBlockchain has attracted widely attention in various fields, especially in\nfinance. With the characteristics of data tamper-proof, forgery-proof,\ncryptography, consensus verification, and decentralization, Blockchain fits\nwell with the realistic needs of Supply Chain Finance, which requires data\nintegrity, authenticity, privacy, and information sharing. Therefore, it is\ntime to summarize the applications of Blockchain technology in the field of\nSupply Chain Finance. What Blockchain technology brings to Supply Chain Finance\nis not only to alleviate the problems of information asymmetry, credit\ndisassembly, and financing cost, but also to improve Supply Chain Finance\noperations through smart contracts to intelligent Supply Chain Finance and in\ncombination with other technologies, such as artificial intelligence, cloud\ncomputing, and data mining, jointly. So there has been some work in\nBlockchain-based Supply Chain Finance research for different Supply Chain\nFinance oriented applications, but most of these work are at the management\nlevel to propose conceptual frameworks or simply use Blockchain without\nexploiting its deep applications. Moreover, there are few systematic reviews\nproviding a comprehensive summary of current work in the area of\nBlockchain-based Supply Chain Finance. In this paper, we ...", "cat": "cs.CR", "authors": ["Zhengdong Luo"]}, "1413": {"id": "2406.10696v1", "title": "Mining comorbidities: a brief survey", "url": "http://arxiv.org/pdf/2406.10696v1", "date": "2024-06-15 17:31:43", "abs": "In this manuscript we will present a brief overview of the comorbidity\nconcept. We will start by laying its foundations and its definitions and then\ndescribing the role that machine learning can hold in mining and defining it.\nThe purpose of this short survey is to present a brief overview of the\ndefinition of comorbidity as a concept, and showing some of the latest\napplications and potentialities for the application of natural language\nprocessing and text mining techniques.", "cat": "q-bio.OT", "authors": ["Giovanna Maria Dimitri"]}, "1414": {"id": "1501.06650v2", "title": "MALT-45: A 7 mm survey of the southern Galaxy - I. Techniques and spectral line data", "url": "http://arxiv.org/pdf/1501.06650v2", "date": "2015-02-01 10:02:58", "abs": "We present the first results from the MALT-45 (Millimetre Astronomer's Legacy\nTeam - 45 GHz) Galactic Plane survey. We have observed 5 square-degrees ($l =\n330 - 335$, $b = \\pm0.5$) for spectral lines in the 7 mm band (42-44 and 48-49\nGHz), including $\\text{CS}$ $(1-0)$, class I $\\text{CH}_3\\text{OH}$ masers in\nthe $7(0,7)-6(1,6)$ $\\text{A}^{+}$ transition and $\\text{SiO}$ $(1-0)$\n$v=0,1,2,3$. MALT-45 is the first unbiased, large-scale, sensitive spectral\nline survey in this frequency range. In this paper, we present data from the\nsurvey as well as a few intriguing results; rigorous analyses of these science\ncases are reserved for future publications. Across the survey region, we\ndetected 77 class I $\\text{CH}_3\\text{OH}$ masers, of which 58 are new\ndetections, along with many sites of thermal and maser $\\text{SiO}$ emission\nand thermal $\\text{CS}$. We found that 35 class I $\\text{CH}_3\\text{OH}$ masers\nwere associated with the published locations of class II\n$\\text{CH}_3\\text{OH}$, $\\text{H}_2\\text{O}$ and $\\text{OH}$ masers but 42 have\nno known masers within 60 arcsec. We compared the MALT-45 $\\text{CS}$ with\n$\\text{NH}_3$ (1,1) to reveal regions of $\\text{CS}$ depletion and high\nopacity, as well as evolved star-forming regions with a high ratio of\n$\\text{CS}$ to $\\text{NH}_3$. All $\\text{SiO}$ masers are new detections, and\nappear to be associated with evolved stars from the $\\it{Spitzer}$ Galactic\nLegacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE). Generally, within\n$\\text{SiO}$ regions of multiple vibrational modes, the intensity decreases as\n$v=1,2,3$, but there are a few exceptions where $v=2$ is stronger than $v=1$.", "cat": "astro-ph.SR", "authors": ["Christopher H. Jordan", "Andrew J. Walsh", "Vicki Lowe", "Maxim A. Voronkov", "Simon P. Ellingsen", "Shari L. Breen", "Cormac R. Purcell", "Peter J. Barnes", "Michael G. Burton", "Maria R. Cunningham", "Tracey Hill", "James M. Jackson", "Steven N. Longmore", "Nicolas Peretto", "James S. Urquhart"]}, "1415": {"id": "1507.02286v1", "title": "The VLT-FLAMES Tarantula Survey XXI. Stellar spin rates of O-type spectroscopic binaries", "url": "http://arxiv.org/pdf/1507.02286v1", "date": "2015-07-08 20:00:43", "abs": "The initial distribution of spin rates of massive stars is a fingerprint of\ntheir elusive formation process. It also sets a key initial condition for\nstellar evolution and is thus an important ingredient in stellar population\nsynthesis. So far, most studies have focused on single stars. Most O stars are\nhowever found in multiple systems. By establishing the spin-rate distribution\nof a sizeable sample of O-type spectroscopic binaries and by comparing the\ndistributions of binary sub-populations with one another as well as with that\nof presumed single stars in the same region, we aim to constrain the initial\nspin distribution of O stars in binaries, and to identify signatures of the\nphysical mechanisms that affect the evolution of the massive stars spin rates.\nWe use ground-based optical spectroscopy obtained in the framework of the\nVLT-FLAMES Tarantula Survey (VFTS) to establish the projected equatorial\nrotational velocities (\\vrot) for components of 114 spectroscopic binaries in\n30 Doradus. The \\vrot\\ values are derived from the full-width at half-maximum\n(FWHM) of a set of spectral lines, using a FWHM vs. \\vrot\\ calibration that we\nderive based on previous line analysis methods applied to single O-type stars\nin the VFTS sample. The overall \\vrot\\ distribution of the primary stars\nresembles that of single O-type stars in the VFTS, featuring a low-velocity\npeak (at $\\vrot < 200$ kms) and a shoulder at intermediate velocities ($200 <\n\\vrot < 300$ kms). The distributions of binaries and single stars however\ndiffer in two ways. First, the main peak at $\\vrot \\sim$100 kms is broader and\nslightly shifted toward higher spin rates in the binary distribution compared\nto that of the presumed-single stars. Second, the \\vrot distribution of\nprimaries lacks a significant population of stars spinning faster than 300 kms\nwhile such a population is clearly present in the single star sample.", "cat": "astro-ph.SR", "authors": ["O. H. Ram\u00edrez-Agudelo", "H. Sana", "S. E. de Mink", "V. H\u00e9nault-Brunet", "A. de Koter", "N. Langer", "F. Tramper", "G. Gr\u00e4fener", "C. J. Evans", "J. S. Vink", "P. L. Dufton", "W. D. Taylor"]}, "1416": {"id": "1009.4131v1", "title": "A Comprehensive Survey of Hydrogen Chloride in the Galaxy", "url": "http://arxiv.org/pdf/1009.4131v1", "date": "2010-09-21 16:09:11", "abs": "We report new observations of the fundamental $J=1-0$ transition of HCl (at\n625.918GHz) toward a sample of 25 galactic star-forming regions, molecular\nclouds, and evolved stars, carried out using the Caltech Submillimeter\nObservatory. Fourteen sources in the sample are also observed in the\ncorresponding H\\tscl\\ $J=1-0$ transition (at 624.978GHz). We have obtained\nclear detections in all but four of the targets, often in emission. Absorptions\nagainst bright background continuum sources are also seen in nine cases,\nusually involving a delicate balance between emission and absorption features.\nFrom RADEX modeling, we derive gas densities and HCl column densities for\nsources with HCl emission. HCl is found in a wide range of environments, with\ngas densities ranging from $10^5$ to $10^7$~cm$^{-3}$. The HCl abundance\nrelative to H$_2$ is in the range of $(3-30)\\times10^{-10}$. Comparing with the\nchlorine abundance in the solar neighborhood, this corresponds to a chlorine\ndepletion factor of up to $\\sim$400, assuming that HCl accounts for one third\nof the total chlorine in the gas phase. The [\\tfcl]/[\\tscl] isotopic ratio is\nrather varied, from unity to $\\sim$5, mostly lower than the terrestrial value\nof 3.1. Such variation is highly localized, and could be generated by the\nnucleosynthesis in supernovae, which predicts a \\tscl\\ deficiency in most\nmodels. The lower ratios seen in W3IRS4 and W3IRS5 likely confine the\nprogenitors of the supernovae to stars with relatively large mass\n($\\ga$25M$_\\sun$) and high metallicity (Z$\\sim$0.02).", "cat": "astro-ph.GA", "authors": ["Ruisheng Peng", "Hiroshige Yoshida", "Richard A. Chamberlin", "Thomas G. Phillips", "Dariusz C. Lis", "Maryvonne Gerin"]}, "1417": {"id": "2208.08532v1", "title": "Survey of Methods for Solving Systems of Nonlinear Equations, Part II: Optimization Based Approaches", "url": "http://arxiv.org/pdf/2208.08532v1", "date": "2022-08-17 20:58:11", "abs": "This paper presents a comprehensive survey of methods which can be utilized\nto search for solutions to systems of nonlinear equations (SNEs). Our\nobjectives with this survey are to synthesize pertinent literature in this\nfield by presenting a thorough description and analysis of the known methods\ncapable of finding one or many solutions to SNEs, and to assist interested\nreaders seeking to identify solution techniques which are well suited for\nsolving the various classes of SNEs which one may encounter in real world\napplications.\n To accomplish these objectives, we present a multi-part survey. In part one,\nwe focused on root-finding approaches which can be used to search for solutions\nto a SNE without transforming it into an optimization problem. In part two, we\nintroduce the various transformations which have been utilized to transform a\nSNE into an optimization problem, and we discuss optimization algorithms which\ncan then be used to search for solutions. We emphasize the important\ncharacteristics of each method, and we discuss promising directions for future\nresearch. In part three, we will present a robust quantitative comparative\nanalysis of methods capable of searching for solutions to SNEs.", "cat": "cs.MS", "authors": ["Ilias S. Kotsireas", "Panos M. Pardalos", "Alexander Semenov", "William T. Trevena", "Michael N. Vrahatis"]}, "1418": {"id": "1806.00172v1", "title": "Discovery of OH absorption from a galaxy at z~0.05: implications for large surveys with SKA pathfinders", "url": "http://arxiv.org/pdf/1806.00172v1", "date": "2018-06-01 02:38:22", "abs": "We present the first detection of OH absorption in diffuse gas at $z>0$,\nalong with another eight stringent limits on OH column densities for cold\natomic gas in galaxies at $0$13.6)\nto be $n_{\\rm OH}$ = $0.008^{+0.018}_{-0.008}$ at $z\\sim0.1$. Based on this we\nexpect to detect 10$^{+20}_{-10}$ such OH absorbers from the MeerKAT Absorption\nLine Survey. Using HI 21-cm and OH 1667 MHz absorption lines detected towards\nQ0248+430, we estimate ($\\Delta F/F$) = (5.2$\\pm$4.5)$\\times 10^{-6}$, where $F\n\\equiv g_p (\\alpha^2/\\mu)^{1.57}$, $\\alpha$ $-$ the fine structure constant,\n$\\mu$ $-$ the electron-proton mass ratio and $g_p$ $-$ the proton gyromagnetic\nratio. This corresponds to $\\Delta\\alpha/\\alpha$($z=0.0519$) = (1.7 $\\pm$\n1.4)$\\times 10^{-6}$, which is among the stringent constraints on the\nfractional variation of $\\alpha$.", "cat": "astro-ph.GA", "authors": ["N. Gupta", "E. Momjian", "R. Srianand", "P. Petitjean", "P. Noterdaeme", "D. Gyanchandani", "R. Sharma", "S. Kulkarni"]}, "1419": {"id": "2112.11393v3", "title": "A Survey on Perfectly-Secure Verifiable Secret-Sharing", "url": "http://arxiv.org/pdf/2112.11393v3", "date": "2022-02-04 12:43:12", "abs": "Verifiable Secret-Sharing (VSS) is a fundamental primitive in secure\ndistributed computing. It is used as a building block in several distributed\ncomputing tasks, such as Byzantine agreement and secure multi-party\ncomputation. In this article, we consider VSS schemes with perfect security,\ntolerating computationally unbounded adversaries. We comprehensively survey the\nexisting perfectly-secure VSS schemes in three different communication\nsettings, namely synchronous, asynchronous and hybrid setting and provide full\ndetails of the existing schemes in these settings. The aim of this survey is to\nprovide a clear knowledge and foundation to researchers who are interested in\nknowing and extending the state-of-the-art perfectly-secure VSS schemes.", "cat": "cs.CR", "authors": ["Anirudh Chandramouli", "Ashish Choudhury", "Arpita Patra"]}, "1420": {"id": "2008.06803v2", "title": "Parsec-scale properties of steep and flat spectrum extragalactic radio sources from a VLBA survey of a complete north polar cap sample", "url": "http://arxiv.org/pdf/2008.06803v2", "date": "2020-12-03 09:37:59", "abs": "We observed with the VLBA at 2.3 and 8.6 GHz a complete flux-density limited\nsample of 482 radio sources with declination >+75 degrees brighter than 200 mJy\nat 1.4 GHz drawn from the NVSS catalog. 34% of the sources show parsec-scale\nemission above the flux density detection limit of 30 mJy; their accurate\npositions and parsec-scale structure parameters are determined. Among all the\nsources detected at least at the shortest VLBA baselines, the majority, or 72%,\nhas a steep single-dish spectrum. The fraction of the sources with a detectable\nparsec-scale structure is above 95% among the flat-spectrum and close to 25%\namong the steep-spectrum objects. We identified 82 compact steep-spectrum\nsource candidates, which make up 17% of the sample; most of them are reported\nfor the first time. The compactness and the brightness temperature of the\nsources in our sample show a positive correlation with single-dish and VLBA\nspectral indices. All the sources with a significant 8 GHz variability were\ndetected by the VLBA snapshot observations, which independently confirmed their\ncompactness. We demonstrated that 54% of the sources detected by the VLBA at\n2.3 GHz in our sample have a steep VLBA spectrum. The compact radio emission of\nthese sources is likely dominated by optically thin jets or mini-lobes, not by\nan opaque jet core. These results show that future VLBI surveys aimed to search\nfor new sources with parsec-scale structure should include not only\nflat-spectrum sources, but also steep-spectrum ones in order to reach an\nacceptable level of completeness.", "cat": "astro-ph.GA", "authors": ["Alexander V. Popkov", "Yuri Y. Kovalev", "Leonid Y. Petrov", "Yuri A. Kovalev"]}, "1421": {"id": "2105.04387v5", "title": "Recent Advances in Deep Learning Based Dialogue Systems: A Systematic Survey", "url": "http://arxiv.org/pdf/2105.04387v5", "date": "2022-03-30 02:37:38", "abs": "Dialogue systems are a popular natural language processing (NLP) task as it\nis promising in real-life applications. It is also a complicated task since\nmany NLP tasks deserving study are involved. As a result, a multitude of novel\nworks on this task are carried out, and most of them are deep learning based\ndue to the outstanding performance. In this survey, we mainly focus on the deep\nlearning based dialogue systems. We comprehensively review state-of-the-art\nresearch outcomes in dialogue systems and analyze them from two angles: model\ntype and system type. Specifically, from the angle of model type, we discuss\nthe principles, characteristics, and applications of different models that are\nwidely used in dialogue systems. This will help researchers acquaint these\nmodels and see how they are applied in state-of-the-art frameworks, which is\nrather helpful when designing a new dialogue system. From the angle of system\ntype, we discuss task-oriented and open-domain dialogue systems as two streams\nof research, providing insight into the hot topics related. Furthermore, we\ncomprehensively review the evaluation methods and datasets for dialogue systems\nto pave the way for future research. Finally, some possible research trends are\nidentified based on the recent research outcomes. To the best of our knowledge,\nthis survey is the most comprehensive and up-to-date one at present for deep\nlearning based dialogue systems, extensively covering the popular techniques.\nWe speculate that this work is a good starting point for academics who are new\nto the dialogue systems or those who want to quickly grasp up-to-date\ntechniques in this area.", "cat": "cs.CL", "authors": ["Jinjie Ni", "Tom Young", "Vlad Pandelea", "Fuzhao Xue", "Erik Cambria"]}, "1422": {"id": "1405.0398v1", "title": "Symmetric Algorithm Survey: A Comparative Analysis", "url": "http://arxiv.org/pdf/1405.0398v1", "date": "2014-05-02 13:32:50", "abs": "Information Security has become an important issue in modern world as the\npopularity and infiltration of internet commerce and communication technologies\nhas emerged, making them a prospective medium to the security threats. To\nsurmount these security threats modern data communications uses cryptography an\neffective, efficient and essential component for secure transmission of\ninformation by implementing security parameter counting Confidentiality,\nAuthentication, accountability, and accuracy. To achieve data security\ndifferent cryptographic algorithms (Symmetric & Asymmetric) are used that\njumbles data in to scribbled format that can only be reversed by the user that\nhave to desire key. This paper presents a comprehensive comparative analysis of\ndifferent existing cryptographic algorithms (symmetric) based on their\nArchitecture, Scalability, Flexibility, Reliability, Security and Limitation\nthat are essential for secure communication (Wired or Wireless).", "cat": "cs.CR", "authors": ["Mansoor Ebrahim", "Shujaat Khan", "Umer Bin Khalid"]}, "1423": {"id": "2307.09590v3", "title": "The FENIKS Survey: Spectroscopic Confirmation of Massive Quiescent Galaxies at z ~ 3-5", "url": "http://arxiv.org/pdf/2307.09590v3", "date": "2024-05-01 13:35:16", "abs": "The measured ages of massive, quiescent galaxies at $z\\sim 3-4$ imply that\nmassive galaxies quench as early as $z\\sim 6$. While the number of\nspectroscopic confirmations of quiescent galaxies at $z < 3$ has increased over\nthe years, there are only a handful at $z > 3.5$. We report spectroscopic\nredshifts of one secure ($z=3.757$) and two tentative ($z = 3.336$, $z=4.673$)\nmassive ($\\log(M_\\ast/M_\\odot) > 10.3$) quiescent galaxies with 11 hours of\nKeck/MOSFIRE $K$-band observations. Our candidates were selected from the\nFENIKS survey, which uses deep Gemini/Flamingos-2 $K_b$ $K_r$ imaging optimized\nfor increased sensitivity to the characteristic red colors of galaxies at $z >\n3$ with strong Balmer/4000 \\AA\\ breaks. The rest-frame $UVJ$ and $(ugi)_s$\ncolors of 3/4 quiescent candidates are consistent with $1-2$ Gyr old stellar\npopulations. This places these galaxies as the oldest objects at these\nredshifts, and challenges the notion that quiescent galaxies at $z > 3$ are all\nrecently-quenched, \"post-starburst\" galaxies. Our spectroscopy shows that the\nother quiescent-galaxy candidate is a broad-line AGN ($z = 3.594$) with strong,\nredshifted $H\\beta$+[O III] emission with a velocity offset $>1000$ km/s,\nindicative of a powerful outflow. The star-formation history of our highest\nredshift candidate suggests that its progenitor was already in place by $z \\sim\n7-11$, reaching $\\sim$ 10$^{11} M_{\\odot}$ by $z \\simeq 8$. These observations\nreveal the limit of what is possible with deep near-infrared photometry and\ntargeted spectroscopy from the ground and demonstrate that secure spectroscopic\nconfirmation of quiescent galaxies at $z > 4$ is only feasible with JWST.", "cat": "astro-ph.GA", "authors": ["Jacqueline Antwi-Danso", "Casey Papovich", "James Esdaile", "Themiya Nanayakkara", "Karl Glazebrook", "Taylor A. Hutchison", "Katherine E. Whitaker", "Z. Cemile Marsan", "Ruben J. Diaz", "Danilo Marchesini", "Adam Muzzin", "Kim-Vy H. Tran", "David J. Setton", "Yasha Kaushal", "Joshua S. Speagle", "Justin Cole"]}, "1424": {"id": "2404.12343v1", "title": "Gemini Near Infrared Spectrograph -- Distant Quasar Survey: Rest-Frame Ultraviolet-Optical Spectral Properties of Broad Absorption Line Quasars", "url": "http://arxiv.org/pdf/2404.12343v1", "date": "2024-04-18 17:16:52", "abs": "We present the rest-frame ultraviolet-optical spectral properties of 65 broad\nabsorption line (BAL) quasars from the Gemini Near Infrared\nSpectrograph-Distant Quasar Survey (GNIRS-DQS). These properties are compared\nwith those of 195 non-BAL quasars from GNIRS-DQS in order to identify the\ndrivers for the appearance of BALs in quasar spectra. In particular, we compare\nequivalent widths and velocity widths, as well as velocity offsets from\nsystemic redshifts, of principal emission lines. In spite of the differences\nbetween their rest-frame ultraviolet spectra, we find that luminous BAL quasars\nare generally indistinguishable from their non-BAL counterparts in the\nrest-frame optical band at redshifts $1.55 \\lesssim z \\lesssim 3.50$. We do not\nfind any correlation between BAL trough properties and the H$\\beta$-based\nsupermassive black hole masses and normalized accretion rates in our sample.\nConsidering the Sloan Digital Sky Survey quasar sample, which includes the\nGNIRS-DQS sample, we find that a monochromatic luminosity at rest-frame 2500 A\nof $\\gtrsim 10^{45}$ erg s$^{-1}$ is a necessary condition for launching BAL\noutflows in quasars. We compare our findings with other BAL quasar samples and\ndiscuss the roles that accretion rate and orientation play in the appearance of\nBAL troughs in quasar spectra.", "cat": "astro-ph.GA", "authors": ["Harum Ahmed", "Ohad Shemmer", "Brandon Matthews", "Cooper Dix", "Trung Ha", "Gordon T. Richards", "Michael S. Brotherton", "Adam D. Myers", "W. N. Brandt", "Sarah C. Gallagher", "Richard Green", "Paulina Lira", "Jacob N. McLane", "Richard M. Plotkin", "Donald P. Schneider"]}, "1425": {"id": "2310.01315v1", "title": "Cosmology with imaging galaxy surveys: the impact of evolving galaxy bias and magnification", "url": "http://arxiv.org/pdf/2310.01315v1", "date": "2023-10-02 16:21:19", "abs": "The joint analysis of galaxy clustering and galaxy-shear cross-correlations\n(galaxy-galaxy lensing) in imaging surveys constitutes one of the main avenues\nto obtain cosmological information. Analyses from Stage III surveys have\nassumed constant galaxy bias and weak lensing magnification coefficients within\nredshift bins. We use simple models of bias and magnification evolution to show\nthat plausible levels of evolution impact cosmological parameter inference\nsignificantly for Stage IV surveys and possibly for current datasets as well.\nThe distance weighting factors in galaxy-galaxy lensing cause it to have a\ndifferent effective mean redshift within a lens bin than galaxy clustering. If\nthe evolution is not included carefully in the theory modeling, this produces\nan apparent de-correlation of clustering and lensing even on large scales and\nleads to biased cosmological constraints. The level of bias is sensitive to the\nredshift and the width of the lens redshift distributions: for\nmagnitude-limited-like samples it is comparable to the statistical precision\neven for the full DES survey, and exceeds it for Rubin-LSST. We find that\nignoring the evolution can lead to approximately $1\\sigma$ biases in the\ncosmological constraints in future Rubin-LSST analyses. We describe how these\neffects can be mitigated from the modeling and data sides, in particular by\nusing cross-correlations to constrain the evolution parameters. We also\ndemonstrate that the combination of galaxy clustering and CMB lensing does not\nsuffer from this problem, due to the different distance weighting.", "cat": "astro-ph.CO", "authors": ["Shivam Pandey", "Carles S\u00e1nchez", "Bhuvnesh Jain", "The LSST Dark Energy Science Collaboration"]}, "1426": {"id": "1101.0001v2", "title": "MOIRCS Deep Survey. X. Evolution of Quiescent Galaxies as a Function of Stellar Mass at 0.56 by performing SED fitting of the\nmulti broad-band photometry from the U to Spitzer 5.8um bands with the\npopulation synthesis model of Bruzual & Charlot (2003) where exponentially\ndecaying star formation histories are assumed. The number density of quiescent\ngalaxies increases by a factor of ~3 from 1.0~ 1-1.5.", "cat": "astro-ph.CO", "authors": ["Masaru Kajisawa", "Takashi Ichikawa", "Tomohiro Yoshikawa", "Toru Yamada", "Masato Onodera", "Masayuki Akiyama", "Ichi Tanaka"]}, "1427": {"id": "2005.09266v2", "title": "The POlarised GLEAM Survey (POGS) II: Results from an All-Sky Rotation Measure Synthesis Survey at Long Wavelengths", "url": "http://arxiv.org/pdf/2005.09266v2", "date": "2020-11-12 10:30:35", "abs": "The low-frequency linearly-polarised radio source population is largely\nunexplored. However, a renaissance in low-frequency polarimetry has been\nenabled by pathfinder and precursor instruments for the Square Kilometre Array.\nIn this second paper from the POlarised GaLactic and Extragalactic All-Sky\nMurchison Widefield Array (MWA) Survey -- the POlarised GLEAM Survey, or POGS\n-- we present the results from our all-sky MWA Phase I Faraday Rotation Measure\nsurvey. Our survey covers nearly the entire Southern sky in the Declination\nrange $-82^{\\circ}$ to $+30^{\\circ}$ at a resolution between around three and\nseven arcminutes (depending on Declination) using data in the frequency range\n169$-$231 MHz. We have performed two targeted searches: the first covering\n25,489 square degrees of sky, searching for extragalactic polarised sources;\nthe second covering the entire sky South of Declination $+30^{\\circ}$,\nsearching for known pulsars. We detect a total of 517 sources with 200 MHz\nlinearly-polarised flux densities between 9.9 mJy and 1.7 Jy, of which 33 are\nknown radio pulsars. All sources in our catalogues have Faraday rotation\nmeasures in the range $-328.07$ rad m$^{-2}$ to $+279.62$ rad m$^{-2}$. The\nFaraday rotation measures are broadly consistent with results from\nhigher-frequency surveys, but with typically more than an order of magnitude\nimprovement in the precision, highlighting the power of low-frequency\npolarisation surveys to accurately study Galactic and extragalactic magnetic\nfields. We discuss the properties of our extragalactic and known-pulsar source\npopulation, how the sky distribution relates to Galactic features, and identify\na handful of new pulsar candidates among our nominally extragalactic source\npopulation.", "cat": "astro-ph.GA", "authors": ["C. J. Riseley", "T. J. Galvin", "C. Sobey", "T. Vernstrom", "S. V. White", "X. Zhang", "B. M. Gaensler", "G. Heald", "C. S. Anderson", "T. M. O. Franzen", "P. J. Hancock", "N. Hurley-Walker", "E. Lenc", "C. L. Van Eck"]}, "1428": {"id": "2405.10936v1", "title": "A Survey on Large Language Models with Multilingualism: Recent Advances and New Frontiers", "url": "http://arxiv.org/pdf/2405.10936v1", "date": "2024-05-17 17:47:39", "abs": "The rapid development of Large Language Models (LLMs) demonstrates remarkable\nmultilingual capabilities in natural language processing, attracting global\nattention in both academia and industry. To mitigate potential discrimination\nand enhance the overall usability and accessibility for diverse language user\ngroups, it is important for the development of language-fair technology.\nDespite the breakthroughs of LLMs, the investigation into the multilingual\nscenario remains insufficient, where a comprehensive survey to summarize recent\napproaches, developments, limitations, and potential solutions is desirable. To\nthis end, we provide a survey with multiple perspectives on the utilization of\nLLMs in the multilingual scenario. We first rethink the transitions between\nprevious and current research on pre-trained language models. Then we introduce\nseveral perspectives on the multilingualism of LLMs, including training and\ninference methods, model security, multi-domain with language culture, and\nusage of datasets. We also discuss the major challenges that arise in these\naspects, along with possible solutions. Besides, we highlight future research\ndirections that aim at further enhancing LLMs with multilingualism. The survey\naims to help the research community address multilingual problems and provide a\ncomprehensive understanding of the core concepts, key techniques, and latest\ndevelopments in multilingual natural language processing based on LLMs.", "cat": "cs.CL", "authors": ["Kaiyu Huang", "Fengran Mo", "Hongliang Li", "You Li", "Yuanchi Zhang", "Weijian Yi", "Yulong Mao", "Jinchen Liu", "Yuzhuang Xu", "Jinan Xu", "Jian-Yun Nie", "Yang Liu"]}, "1429": {"id": "2311.00415v2", "title": "Geophysical survey based on Hybrid Gravimetry using Relative Measurements and an Atomic Gravimeter as an Absolute Reference", "url": "http://arxiv.org/pdf/2311.00415v2", "date": "2024-03-25 15:07:38", "abs": "Gravimetry is a versatile metrological approach in geophysics to accurately\nmap subterranean mass and density anomalies. There is a broad diversification\nregarding the working principle of gravimeters, wherein atomic gravimeters are\none of the most technologically progressive class of gravimeters which can\nmonitor gravity at an absolute scale with a high-repetition without exhibiting\ndrift. Despite the apparent utility for geophysical surveys, atomic gravimeters\nare (currently) laboratory-bound devices due to the vexatious task of\ntransportation. Here, we demonstrated the utility of an atomic gravimeter\non-site during a gravity survey, where the issue of immobility was circumvented\nwith a relative spring gravimeter. The atomic gravimeter served as a means to\nmap the relative data from the spring gravimeter to an absolute measurement\nwith an effective precision of 7.7$\\mu$Gal. Absolute measurements provide a\nrobust and feasible method to define and control gravity data taken at\ndifferent sites, or a later date, which is critical to analyze underground\ngeological units, in particular when it is combined with other geophysical\napproaches.", "cat": "physics.atom-ph", "authors": ["Nathan Shettell", "Kai Sheng Lee", "Fong En Oon", "Elizaveta Maksimova", "Christoph Hufnagel", "Shengji Wei", "Rainer Dumke"]}, "1430": {"id": "2212.00051v2", "title": "Morphological Parameters and Associated Uncertainties for 8 Million Galaxies in the Hyper Suprime-Cam Wide Survey", "url": "http://arxiv.org/pdf/2212.00051v2", "date": "2024-03-01 19:00:08", "abs": "We use the Galaxy Morphology Posterior Estimation Network (GaMPEN) to\nestimate morphological parameters and associated uncertainties for $\\sim 8$\nmillion galaxies in the Hyper Suprime-Cam (HSC) Wide survey with $z \\leq 0.75$\nand $m \\leq 23$. GaMPEN is a machine learning framework that estimates Bayesian\nposteriors for a galaxy's bulge-to-total light ratio ($L_B/L_T$), effective\nradius ($R_e$), and flux ($F$). By first training on simulations of galaxies\nand then applying transfer learning using real data, we trained GaMPEN with\n$<1\\%$ of our dataset. This two-step process will be critical for applying\nmachine learning algorithms to future large imaging surveys, such as the\nRubin-Legacy Survey of Space and Time (LSST), the Nancy Grace Roman Space\nTelescope (NGRST), and Euclid. By comparing our results to those obtained using\nlight-profile fitting, we demonstrate that GaMPEN's predicted posterior\ndistributions are well-calibrated ($\\lesssim 5\\%$ deviation) and accurate. This\nrepresents a significant improvement over light profile fitting algorithms\nwhich underestimate uncertainties by as much as $\\sim60\\%$. For an overlapping\nsub-sample, we also compare the derived morphological parameters with values in\ntwo external catalogs and find that the results agree within the limits of\nuncertainties predicted by GaMPEN. This step also permits us to define an\nempirical relationship between the S\\'ersic index and $L_B/L_T$ that can be\nused to convert between these two parameters. The catalog presented here\nrepresents a significant improvement in size ($\\sim10 \\times $), depth ($\\sim4$\nmagnitudes), and uncertainty quantification over previous state-of-the-art\nbulge+disk decomposition catalogs. With this work, we also release GaMPEN's\nsource code and trained models, which can be adapted to other datasets.", "cat": "astro-ph.GA", "authors": ["Aritra Ghosh", "C. Megan Urry", "Aayush Mishra", "Laurence Perreault-Levasseur", "Priyamvada Natarajan", "David B. Sanders", "Daisuke Nagai", "Chuan Tian", "Nico Cappelluti", "Jeyhan S. Kartaltepe", "Meredith C. Powell", "Amrit Rau", "Ezequiel Treister"]}, "1431": {"id": "2202.11412v2", "title": "The Modular Isomorphism Problem: a survey", "url": "http://arxiv.org/pdf/2202.11412v2", "date": "2022-04-08 09:54:33", "abs": "The Modular Isomorphism Problem asks if an isomorphism of group algebras of\ntwo finite p-groups G and H over a field of characteristic p, implies an\nisomorhism of the groups G and H. We survey the history of the problem, explain\nstrategies which were developed to study it and present the recent negative\nsolution of the problem. The problem is also compared to other isomorphism\nproblems for group rings and various question remaining open are included.", "cat": "math.RA", "authors": ["Leo Margolis"]}, "1432": {"id": "1609.07150v1", "title": "The Gaia-ESO Survey: Lithium depletion in the Gamma Velorum cluster and inflated radii in low-mass pre-main-sequence stars", "url": "http://arxiv.org/pdf/1609.07150v1", "date": "2016-09-22 20:00:26", "abs": "We show that non-magnetic models for the evolution of pre-main-sequence (PMS)\nstars *cannot* simultaneously describe the colour-magnitude diagram (CMD) and\nthe pattern of lithium depletion seen in the cluster of young, low-mass stars\nsurrounding $\\gamma^2$ Velorum. The age of 7.5+/-1 Myr inferred from the CMD is\nmuch younger than that implied by the strong Li depletion seen in the cluster\nM-dwarfs and the Li depletion occurs at much redder colours than predicted. The\nepoch at which a star of a given mass depletes its Li and the surface\ntemperature of that star are both dependent on its radius. We demonstrate that\nif the low-mass stars have radii ~10 per cent larger at a given mass and age,\nthen both the CMD and Li depletion pattern of the Gamma Vel cluster are\nexplained at a common age of 18-21 Myr. This radius inflation could be produced\nby some combination of magnetic suppression of convection and extensive cool\nstarspots. Models that incorporate radius inflation suggest that PMS stars\nsimilar to those in the Gamma Vel cluster, in the range 0.230 per cent) than inferred from\nconventional, non-magnetic models in the Hertzsprung-Russell diagram.\nSystematic changes of this size may be of great importance in understanding the\nevolution of young stars, disc lifetimes and the formation of planetary\nsystems.", "cat": "astro-ph.SR", "authors": ["R. D. Jeffries", "R. J. Jackson", "E. Franciosini", "S. Randich", "D. Barrado", "A. Frasca", "A. Klutsch", "A. C. Lanzafame", "L. Prisinzano", "G. G. Sacco", "G. Gilmore", "A. Vallenari", "E. J. Alfaro", "S. E. Koposov", "E. Pancino", "A. Bayo", "A. R. Casey", "M. T. Costado", "F. Damiani", "A. Hourihane", "J. Lewis", "P. Jofre", "L. Magrini", "L. Monaco", "L. Morbidelli", "C. C. Worley", "S. Zaggia", "T. Zwitter"]}, "1433": {"id": "2006.16259v3", "title": "The Ophiuchus DIsc Survey Employing ALMA (ODISEA). II. The effect of stellar multiplicity on disc properties", "url": "http://arxiv.org/pdf/2006.16259v3", "date": "2021-01-29 13:37:54", "abs": "We present Adaptive Optics (AO) near infrared (NIR) observations using\nVLT/NACO and Keck/NIRC2 of ODISEA targets. ODISEA is an ALMA survey of the\nentire population of circumstellar discs in the Ophiuchus molecular cloud. From\nthe whole sample of ODISEA we select all the discs that are not already\nobserved in the NIR with AO and that are observable with NACO or NIRC2. The\nNIR-ODISEA survey consists of 147 stars observed in NIR AO imaging for the\nfirst time, as well as revisiting almost all the binary systems of Ophiuchus\npresent in the literature (20 out of 21). In total, we detect 20 new binary\nsystems and one triple system. For each of them we calculate the projected\nseparation and position angle of the companion, as well as their NIR and\nmillimeter flux ratios. From the NIR contrast we derived the masses of the\nsecondaries, finding that 9 of them are in the sub-stellar regime (30-50\n\\MJup). Discs in multiple systems reach a maximum total dust mass of $\\sim$ 50\nM$_{\\oplus}$, while discs in single stars can reach a dust mass of 200\nM$_{\\oplus}$. Discs with masses above 10 M$_{\\oplus}$ are found only around\nbinaries with projected separations larger than $\\sim$ 110 au. The maximum disc\nsize is also larger around single star than binaries. However, since most discs\nin Ophiuchus are very small and low-mass, the effect of visual binaries is\nrelatively weak in the general disc population.", "cat": "astro-ph.SR", "authors": ["Alice Zurlo", "Lucas A. Cieza", "Sebasti\u00e1n P\u00e9rez", "Valentin Christiaens", "Jonathan P. Williams", "Greta Guidi", "Hector C\u00e1novas", "Simon Casassus", "Antonio Hales", "David A. Principe", "Dary Ru\u00edz-Rodr\u00edguez", "Antonia Fernandez-Figueroa"]}, "1434": {"id": "1810.04846v1", "title": "Regulatory Options and Technical Challenges for the 5.9 GHz Spectrum: Survey and Analysis", "url": "http://arxiv.org/pdf/1810.04846v1", "date": "2018-10-11 05:27:44", "abs": "In 1999, the Federal Communications Commission (FCC) allocated 75 MHz in the\n5.9 GHz ITS Band (5850-5925 MHz) for use by Dedicated Short Range\nCommunications (DSRC) to facilitate information transfer between equipped\nvehicles and roadside systems. This allocation for DSRC in the ITS band has\nbeen a co-primary allocation while the band is shared with the Fixed Satellite\nService (FSS), fixed microwave service, amateur radio services and other\nFederal users authorized by the National Telecommunications and Information\nAdministration (NTIA). In recent time, Cellular V2X (C-V2X), introduced in 3GPP\nRelease 14 LTE standard, has received significant attention due to its\nperceived ability to deliver superior performance with respect to vehicular\nsafety applications. There is a strong momentum in the industry for C-V2X to be\nconsidered as a viable alternative to DSRC and accordingly, to operate in the\nITS spectrum. In another recent notice, the FCC is soliciting input for a\nproposed rulemaking to open up more bandwidth for unlicensed Wi-Fi devices,\nmainly based on the 802.11ac standard. The FCC plans to work with the\nDepartment of Transportation (DoT), and the automotive and communications\nindustries to evaluate potential sharing techniques in the ITS band between\nDSRC and Wi-Fi devices. This paper analyzes the expected scenarios that might\nemerge from FCC and the National Highway Traffic Safety Administration (NHTSA)\nregulation options and identifies the technical challenge associated with each\nscenario. We also provide a literature survey and find that many of resulting\ntechnical challenges remain open research problems that need to be addressed.\nWe conclude that the most challenging issue is related to the interoperability\nbetween DSRC and C-V2X in the 5.9 GHz band and the detection and avoidance of\nharmful adjacent and co-channel interference.", "cat": "eess.SP", "authors": ["Junsung Choi", "Vuk Marojevic", "Mina Labib", "Siddharth Kabra", "Jayanthi Rao", "Sushanta Das", "Jeffery H. Reed", "Carl B. Dietrich"]}, "1435": {"id": "2110.10141v2", "title": "Dark Energy Survey Year 3 results: cosmology with moments of weak lensing mass maps", "url": "http://arxiv.org/pdf/2110.10141v2", "date": "2022-09-09 07:25:32", "abs": "We present a cosmological analysis using the second and third moments of the\nweak lensing mass (convergence) maps from the first three years of data (Y3)\ndata of the Dark Energy Survey (DES). The survey spans an effective area of\n4139 square degrees and uses the images of over 100 million galaxies to\nreconstruct the convergence field. The second moment of the convergence as a\nfunction of smoothing scale contains information similar to standard shear\n2-point statistics. The third moment, or the skewness, contains additional\nnon-Gaussian information. The data is analysed in the context of the\n$\\Lambda$CDM model, varying 5 cosmological parameters and 19 nuisance\nparameters modelling astrophysical and measurement systematics. Our modelling\nof the observables is completely analytical, and has been tested with\nsimulations in our previous methodology study. We obtain a 1.7\\% measurement of\nthe amplitude of fluctuations parameter $S_8\\equiv \\sigma_8\n(\\Omega_m/0.3)^{0.5} = 0.784\\pm 0.013$. The measurements are shown to be\ninternally consistent across redshift bins, angular scales, and between second\nand third moments. In particular, the measured third moment is consistent with\nthe expectation of gravitational clustering under the $\\Lambda$CDM model. The\naddition of the third moment improves the constraints on $S_8$ and $\\Omega_{\\rm\nm}$ by $\\sim$15\\% and $\\sim$25\\% compared to an analysis that only uses second\nmoments. We compare our results with {\\it Planck} constraints from the Cosmic\nMicrowave Background (CMB), finding a $2.2$ \\textendash $2.8\\sigma$ tension in\nthe full parameter space, depending on the combination of moments considered.\nThe third moment independently is in $2.8\\sigma$ tension with {\\it Planck}, and\nthus provides a cross-check on analyses of 2-point correlations.", "cat": "astro-ph.CO", "authors": ["M. Gatti", "B. Jain", "C. Chang", "M. Raveri", "D. Z\u00fcrcher", "L. Secco", "L. Whiteway", "N. Jeffrey", "C. Doux", "T. Kacprzak", "D. Bacon", "P. Fosalba", "A. Alarcon", "A. Amon", "K. Bechtol", "M. Becker", "G. Bernstein", "J. Blazek", "A. Campos", "A. Choi", "C. Davis", "J. Derose", "S. Dodelson", "F. Elsner", "J. Elvin-Poole", "S. Everett", "A. Ferte", "D. Gruen", "I. Harrison", "D. Huterer", "M. Jarvis", "E. Krause", "P. F. Leget", "P. Lemos", "N. Maccrann", "J. Mccullough", "J. Muir", "J. Myles", "A. Navarro", "S. Pandey", "J. Prat", "R. P. Rollins", "A. Roodman", "C. Sanchez", "E. Sheldon", "T. Shin", "M. Troxel", "I. Tutusaus", "B. Yin", "M. Aguena", "S. Allam", "F. Andrade-Oliveira", "J. Anni", "E. Bertin", "D. Brooks", "D. L. Burke", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "R. Cawthon", "M. Costanzi", "L. N. da Costa", "M. E. S. Pereira", "J. De Vicente", "S. Desai", "H. T. Diehl", "J. P. Dietrich", "P. Doel", "A. Drlica-Wagner", "K. Eckert", "A. E. Evrard", "I. Ferrero", "J. Garc\u00eda-Bellido", "E. Gaztanaga", "T. Giannantonio", "R. A. Gruendl", "J. Gschwend", "G. Gutierrez", "S. R. Hinton", "D. L. Hollowood", "K. Honscheid", "D. J. James", "K. Kuehn", "N. Kuropatkin", "O. Laha", "C. Lidman", "M. A. G. Maia", "J. L. Marshall", "P. Melchior", "F. Menanteau", "R. Miquel", "R. Morgan", "A. Palmese", "F. Paz-Chinch\u00f3n", "A. Pieres", "A. A. Plazas Malag\u00f3n", "K. Reil", "M. Rodriguez-Monroyv", "A. K. Romer", "E. Sanchez", "M. Schubnell", "S. Serrano", "I. Sevilla-Noarbe", "M. Smith", "M. Soares-Santos", "E. Suchyta", "G. Tarle", "D. Thomas", "C. To", "T. N. Varga"]}, "1436": {"id": "0711.1059v2", "title": "Photometric Redshifts for the Dark Energy Survey and VISTA and Implications for Large Scale Structure", "url": "http://arxiv.org/pdf/0711.1059v2", "date": "2008-02-13 22:49:34", "abs": "We conduct a detailed analysis of the photometric redshift requirements for\nthe proposed Dark Energy Survey (DES) using two sets of mock galaxy simulations\nand an artificial neural network code - ANNz. In particular, we examine how\noptical photometry in the DES grizY bands can be complemented with near\ninfra-red photometry from the planned VISTA Hemisphere Survey (VHS) in the\nJHK_s bands. We find that the rms scatter on the photometric redshift estimate\nover 1 1 - 2% Eddington Luminosity\nfor a typical 1.4M neutron star compact object. This sensitivity, combined with\nthe high cadence, and the fact that the survey can be performed all year round,\nmake it a powerful discovery tool for outbursting accreting X-ray pulsars in\nthe SMC. In this paper describe results from the first year of observations of\nS-CUBED, which includes the 1SCUBEDX catalog of 265 X-ray sources, 160 of which\nare not identified with any previously cataloged X-ray source. We report on\nbulk properties of sources in the 1SCUBEDX catalog. Finally we focus on results\nof S-CUBED observations of several interesting sources, which includes\ndiscovery of three Type II outbursts from BeXRBs, and the detection of Type I\noutbursts and orbital periods in 6 BeXRB systems.", "cat": "astro-ph.HE", "authors": ["J. A. Kennea", "M. J. Coe", "P. A. Evans", "J. Waters", "R. E. Jasko"]}, "1440": {"id": "1708.02449v1", "title": "The extended ROSAT-ESO Flux-Limited X-ray Galaxy Cluster Survey (REFLEX II) VII The Mass Function of Galaxy Clusters", "url": "http://arxiv.org/pdf/1708.02449v1", "date": "2017-08-08 11:21:58", "abs": "The mass function of galaxy clusters is a sensitive tracer of the\ngravitational evolution of the cosmic large-scale structure and serves as an\nimportant census of the fraction of matter bound in large structures. We obtain\nthe mass function by fitting the observed cluster X-ray luminosity distribution\nfrom the REFLEX galaxy cluster survey to models of cosmological structure\nformation. We marginalise over uncertainties in the cosmological parameters as\nwell as those of the relevant galaxy cluster scaling relations. The mass\nfunction is determined with an uncertainty less than 10% in the mass range 3 x\n10^12 to 5 x 10^14 M$_\\odot$. For the cumulative mass function we find a slope\nat the low mass end consistent with a value of -1, while the mass rich end\ncut-off is milder than a Schechter function with an exponential term exp($-\nM^\\delta$) with $\\delta$ smaller than 1. Changing the Hubble parameter in the\nrange $H_0 = 67 - 73 km s^-1 Mpc^{-1}$ or allowing the total neutrino mass to\nhave a value between 0 - 0.4 eV causes variations less than the uncertainties.\nWe estimate the fraction of mass locked up in galaxy clusters: about 4.4% of\nthe matter in the Universe is bound in clusters (inside $r_200$) with a mass\nlarger than 10^14 M$_\\odot$ and 14% to clusters and groups with a mass larger\nthan 10^13 M$_\\odot$ at the present Universe. We also discuss the evolution of\nthe galaxy cluster population with redshift. Our results imply that there is\nhardly any clusters with a mass > 10^15 M$_\\odot$ above a redshift of z = 1.", "cat": "astro-ph.CO", "authors": ["Hans Boehringer", "Gayoung Chon", "Masataka Fukugita"]}, "1441": {"id": "2104.11271v2", "title": "A Systematic Survey on Android API Usage for Data-Driven Analytics with Smartphones", "url": "http://arxiv.org/pdf/2104.11271v2", "date": "2022-06-06 18:53:54", "abs": "Recent industrial and academic research has focused on data-driven analytics\nwith smartphones by collecting user interaction, context, and device systems\ndata through Application Programming interfaces (APIs) and sensors. The Android\nOS provides various APIs to collect such mobile usage and sensor data for\nthird-party developers. Usage Statistics API (US API) and Accessibility Service\nAPI (AS API) are representative Android APIs for collecting app usage data and\nare used for various research purposes as they can collect fine-grained\ninteraction data (e.g., app usage history, user interaction type). Furthermore,\nother sensor APIs help to collect a user's context and device state data, along\nwith AS/US APIs. This review investigates mobile usage and sensor data-driven\nresearch using AS/US APIs, by categorizing the research purposes and the data\ntypes. In this paper, the surveyed studies are classified as follows: five\nthemes and 21 subthemes, and a four-layer hierarchical data classification\nstructure. This allows us to identify a data usage trend and derive insight\ninto data collection according to research purposes. Several limitations and\nfuture research directions of mobile usage and sensor data-driven analytics\nresearch are discussed, including the impact of changes in the Android API\nversions on research, the privacy and data quality issues, and the mitigation\nof reproducibility risks with standardized data typology.", "cat": "cs.HC", "authors": ["Hansoo Lee", "Joonyoung Park", "Uichin Lee"]}, "1442": {"id": "2404.10407v1", "title": "Comprehensive Survey of Model Compression and Speed up for Vision Transformers", "url": "http://arxiv.org/pdf/2404.10407v1", "date": "2024-04-16 09:19:11", "abs": "Vision Transformers (ViT) have marked a paradigm shift in computer vision,\noutperforming state-of-the-art models across diverse tasks. However, their\npractical deployment is hampered by high computational and memory demands. This\nstudy addresses the challenge by evaluating four primary model compression\ntechniques: quantization, low-rank approximation, knowledge distillation, and\npruning. We methodically analyze and compare the efficacy of these techniques\nand their combinations in optimizing ViTs for resource-constrained\nenvironments. Our comprehensive experimental evaluation demonstrates that these\nmethods facilitate a balanced compromise between model accuracy and\ncomputational efficiency, paving the way for wider application in edge\ncomputing devices.", "cat": "cs.CV", "authors": ["Feiyang Chen", "Ziqian Luo", "Lisang Zhou", "Xueting Pan", "Ying Jiang"]}, "1443": {"id": "1904.08434v1", "title": "The Herschel Dwarf Galaxy Survey: II. Physical conditions, origin of [CII] emission, and porosity of the multiphase low-metallicity ISM", "url": "http://arxiv.org/pdf/1904.08434v1", "date": "2019-04-17 18:00:12", "abs": "The sensitive infrared telescopes, Spitzer and Herschel, have been used to\ntarget low-metallicity star-forming galaxies, allowing us to investigate the\nproperties of their interstellar medium (ISM) in unprecedented detail.\nInterpretation of the observations in physical terms relies on careful modeling\nof those properties. We have employed a multiphase approach to model the ISM\nphases (HII region and photodissociation region) with the spectral synthesis\ncode Cloudy. Our goal is to characterize the physical conditions (gas\ndensities, radiation fields, etc.) in the ISM of the galaxies from the Herschel\nDwarf Galaxy Survey. We are particularly interested in correlations between\nthose physical conditions and metallicity or star-formation rate. Other key\nissues we have addressed are the contribution of different ISM phases to the\ntotal line emission, especially of the [CII]157um line, and the\ncharacterization of the porosity of the ISM. We find that the lower-metallicity\ngalaxies of our sample tend to have higher ionization parameters and galaxies\nwith higher specific star-formation rates have higher gas densities. The [CII]\nemission arises mainly from PDRs and the contribution from the ionized gas\nphases is small, typically less than 30% of the observed emission. We also find\ncorrelation - though with scatter - between metallicity and both the PDR\ncovering factor and the fraction of [CII] from the ionized gas. Overall, the\nlow metal abundances appear to be driving most of the changes in the ISM\nstructure and conditions of these galaxies, and not the high specific\nstar-formation rates. These results demonstrate in a quantitative way the\nincrease of ISM porosity at low metallicity. Such porosity may be typical of\ngalaxies in the young Universe.", "cat": "astro-ph.GA", "authors": ["D. Cormier", "N. P. Abel", "S. Hony", "V. Lebouteiller", "S. C. Madden", "F. L. Polles", "F. Galliano", "I. De Looze", "M. Galametz", "A. Lambert-Huyghe"]}, "1444": {"id": "1208.5592v3", "title": "Predictions for ASKAP Neutral Hydrogen Surveys", "url": "http://arxiv.org/pdf/1208.5592v3", "date": "2012-10-05 02:30:19", "abs": "The Australian Square Kilometer Array Pathfinder (ASKAP) will revolutionise\nour knowledge of gas-rich galaxies in the Universe. Here we present predictions\nfor two proposed extragalactic ASKAP neutral hydrogen (HI) emission-line\nsurveys, based on semi-analytic models applied to cosmological N-body\nsimulations. The ASKAP HI All-Sky Survey, known as WALLABY, is a shallow 3 Pi\nsurvey (z = 0 - 0.26) which will probe the mass and dynamics of over 600,000\ngalaxies. A much deeper small-area HI survey, called DINGO, aims to trace the\nevolution of HI from z = 0 - 0.43, a cosmological volume of 40 million Mpc^3,\ndetecting potentially 100,000 galaxies. The high-sensitivity 30 antenna ASKAP\ncore (diameter ~2 km) will provide an angular resolution of 30 arcsec (at z=0).\nOur simulations show that the majority of galaxies detected in WALLABY (87.5%)\nwill be resolved. About 5000 galaxies will be well resolved, i.e. more than\nfive beams (2.5 arcmin) across the major axis, enabling kinematic studies of\ntheir gaseous disks. This number would rise to 160,000 galaxies if all 36 ASKAP\nantennas could be used; the additional six antennas provide baselines up to 6\nkm, resulting in an angular resolution of 10 arcsec. For DINGO this increased\nresolution is highly desirable to minimise source confusion; reducing confusion\nrates from a maximum of 10% of sources at the survey edge to 3%. We estimate\nthat the sources detected by WALLABY and DINGO will span four orders of\nmagnitude in total halo mass (from 10^{11} to 10^{15} Msol) and nearly seven\norders of magnitude in stellar mass (from 10^{5} to 10^{12} Msol), allowing us\nto investigate the process of galaxy formation across the last four billion\nyears.", "cat": "astro-ph.CO", "authors": ["Alan R. Duffy", "Martin J. Meyer", "Lister Staveley-Smith", "Maksym Bernyk", "Darren J. Croton", "Barbel S. Koribalski", "Derek Gerstmann", "Stefan Westerlund"]}, "1445": {"id": "1905.11835v1", "title": "Analysis of the physical nature of 22 New VVV Survey Globular Cluster candidates in the Milky Way Bulge", "url": "http://arxiv.org/pdf/1905.11835v1", "date": "2019-05-27 15:54:29", "abs": "In order to characterize 22 new globular cluster (GC) candidates in the\nGalactic bulge, we present their colour-magnitude diagrams (CMDs) and Ks-band\nluminosity functions (LFs) using the near-infrared VVV database as well as\nGaia-DR2 proper motion dataset. CMDs were obtained, on one hand, after properly\ndecontaminating the observed diagrams from background/foreground disc stars and\nother sources. On the other hand, CMDs were also obtained based upon star\nselection in proper motion diagrams. Taking into account our deep CMDs and LFs\nanalyses, we find that 17 out of 22 new GC candidates may be real and should\ntherefore be followed-up, while 5 candidates were discarded from the original\nsample. We also search for RR Lyrae and Mira variable stars in the fields of\nthese new GC candidates. In particular, we confirm that Minni 40 may be a real\ncluster. If confirmed by further follow-up analysis, it would be the closest GC\nto the Galactic centre in projected angular distance, located only 0.5 deg away\nfrom it. We consider that it is very difficult to confirm the physical reality\nof these small, poorly-populated bulge GCs so in many cases alternative\ntechniques are needed to corroborate our findings.", "cat": "astro-ph.GA", "authors": ["Tali Palma", "Dante Minniti", "Javier Alonso-Garc\u00eda", "Juliana Crestani", "Henryka Netzel", "Juan J. Clari\u00e1", "Roberto K. Saito", "Bruno Dias", "Jos\u00e9 G. Fern\u00e1ndez-Trincado", "Roberto Kammers", "Douglas Geisler", "Mat\u00edas G\u00f3mez", "Maren Hempel", "Joyce Pullen"]}, "1446": {"id": "1802.02239v2", "title": "Spectrophotometric Redshifts In The Faint Infrared Grism Survey: Finding Overdensities Of Faint Galaxies", "url": "http://arxiv.org/pdf/1802.02239v2", "date": "2018-03-05 20:00:58", "abs": "We improve the accuracy of photometric redshifts by including low-resolution\nspectral data from the G102 grism on the Hubble Space Telescope, which assists\nin redshift determination by further constraining the shape of the broadband\nSpectral Energy Disribution (SED) and identifying spectral features. The\nphotometry used in the redshift fits includes near-IR photometry from\nFIGS+CANDELS, as well as optical data from ground-based surveys and HST ACS,\nand mid-IR data from Spitzer. We calculated the redshifts through the\ncomparison of measured photometry with template galaxy models, using the EAZY\nphotometric redshift code. For objects with F105W $< 26.5$ AB mag with a\nredshift range of $0 < z < 6$, we find a typical error of $\\Delta z = 0.03 *\n(1+z)$ for the purely photometric redshifts; with the addition of FIGS spectra,\nthese become $\\Delta z = 0.02 * (1+z)$, an improvement of 50\\%. Addition of\ngrism data also reduces the outlier rate from 8\\% to 7\\% across all fields.\nWith the more-accurate spectrophotometric redshifts (SPZs), we searched the\nFIGS fields for galaxy overdensities. We identified 24 overdensities across the\n4 fields. The strongest overdensity, matching a spectroscopically identified\ncluster at $z=0.85$, has 28 potential member galaxies, of which 8 have previous\nspectroscopic confirmation, and features a corresponding X-ray signal. Another\ncorresponding to a cluster at $z=1.84$ has 22 members, 18 of which are\nspectroscopically confirmed. Additionally, we find 4 overdensities that are\ndetected at an equal or higher significance in at least one metric to the two\nconfirmed clusters.", "cat": "astro-ph.GA", "authors": ["John Pharo", "Sangeeta Malhotra", "James Rhoads", "Russell Ryan", "Vithal Tilvi", "Norbert Pirzkal", "Steven Finkelstein", "Rogier Windhorst", "Norman Grogin", "Anton Koekemoer", "Zhenya Zheng", "Nimish Hathi", "Keunho Kim", "Bhavin Joshi", "Huan Yang", "Lise Christensen", "Andrea Cimatti", "Jon Gardner", "Nadia Zakamska", "Ignacio Ferreras", "Pascale Hibon", "Anna Pasquali"]}, "1447": {"id": "2402.13149v1", "title": "Choosing a Suitable Requirement Prioritization Method: A Survey", "url": "http://arxiv.org/pdf/2402.13149v1", "date": "2024-02-20 17:05:16", "abs": "Software requirements prioritization plays a crucial role in software\ndevelopment. It can be viewed as the process of ordering requirements by\ndetermining which requirements must be done first and which can be done later.\nPowerful requirements prioritization techniques are of paramount importance to\nfinish the implementation on time and within budget. Many factors affect\nrequirement prioritization such as stakeholder expectations, complexity,\ndependency, scalability, risk, and cost. Therefore, finding the proper order of\nrequirements is a challenging process. Hence, different types of requirements\nprioritization techniques have been developed to support this task. In this\nsurvey, we propose a novel classification that can classify the prioritization\ntechniques under two major classes: relative and exact prioritization\ntechniques class, where each class is divided into two subclasses. We depend in\nour classification on the way the value of ranking is given to the requirement,\neither explicitly as a specific value in the case of the exact prioritization\ntechniques class, or implicitly in the case of the Relative prioritization\ntechnique class. An overview of fifteen different requirements prioritization\ntechniques are presented and organized according to the proposed classification\ncriteria's. Moreover, we make a comparison between methods that are related to\nthe same subclass to analyze their strengths and weaknesses. Based on the\ncomparison results, the properties for each proposed subclass of techniques are\nidentified. Depending on these properties, we present some recommendations to\nhelp project managers in the process of selecting the most suitable technique\nto prioritize requirements based on their project characteristics (number of\nrequirements, time, cost, and accuracy).", "cat": "cs.SE", "authors": ["Esraa Alhenawi", "Shatha Awawdeh", "Ruba Abu Khurma", "Maribel Garc\u00eda-Arenas", "Pedro A. Castillo", "Amjad Hudaib"]}, "1448": {"id": "2406.05575v1", "title": "A Survey on Hybrid Motion Planning Methods for Automated Driving Systems", "url": "http://arxiv.org/pdf/2406.05575v1", "date": "2024-06-08 21:15:14", "abs": "Motion planning is an essential element of the modular architecture of\nautonomous vehicles, serving as a bridge between upstream perception modules\nand downstream low-level control signals. Traditional motion planners were\ninitially designed for specific Automated Driving Functions (ADFs), yet the\nevolving landscape of highly automated driving systems (ADS) requires motion\nfor a wide range of ADFs, including unforeseen ones. This need has motivated\nthe development of the ``hybrid\" approach in the literature, seeking to enhance\nmotion planning performance by combining diverse techniques, such as\ndata-driven (learning-based) and logic-driven (analytic) methodologies. Recent\nresearch endeavours have significantly contributed to the development of more\nefficient, accurate, and safe hybrid methods for Tactical Decision Making (TDM)\nand Trajectory Generation (TG), as well as integrating these algorithms into\nthe motion planning module. Owing to the extensive variety and potential of\nhybrid methods, a timely and comprehensive review of the current literature is\nundertaken in this survey article. We classify the hybrid motion planners based\non the types of components they incorporate, such as combinations of\nsampling-based with optimization-based/learning-based motion planners. The\ncomparison of different classes is conducted by evaluating the addressed\nchallenges and limitations, as well as assessing whether they focus on TG\nand/or TDM. We hope this approach will enable the researchers in this field to\ngain in-depth insights into the identification of current trends in hybrid\nmotion planning and shed light on promising areas for future research.", "cat": "cs.RO", "authors": ["MReza Alipour Sormoli", "Konstantinos Koufos", "Mehrdad Dianati", "Roger Woodman"]}, "1449": {"id": "0911.0523v1", "title": "Properties and environment of Radio Emitting Galaxies in the VLA-zCOSMOS survey", "url": "http://arxiv.org/pdf/0911.0523v1", "date": "2009-11-03 09:44:09", "abs": "We investigate the properties and the environment of radio sources with\noptical counterpart from the combined VLA-COSMOS and zCOSMOS samples. The\nadvantage of this sample is the availability of optical spectroscopic\ninformation, high quality redshifts, and accurate density determination.\n By comparing the star formation rates estimated from the optical spectral\nenergy distribution with those based on the radio luminosity, we divide the\nradio sources in three families, passive AGN, non-passive AGN and star forming\ngalaxies. These families occupy specific regions of the 8.0-4.5 $\\mu$m infrared\ncolor--specific star formation plane, from which we extract the corresponding\ncontrol samples.\n Only the passive AGN have a significantly different environment distribution\nfrom their control sample. The fraction of radio-loud passive AGN increases\nfrom ~2% in underdense regions to ~15% for overdensities (1+delta) greater than\n10. This trend is also present as a function of richness of the groups hosting\nthe radio sources. Passive AGN in overdensities tend to have higher radio\nluminosities than those in lower density environments. Since the black hole\nmass distribution is similar in both environments, we speculate that, for low\nradio luminosities, the radio emission is controlled (through fuel\ndisponibility or confinement of radio jet by local gas pressure) by the\ninterstellar medium of the host galaxy, while in other cases it is determined\nby the structure (group or cluster) in which the galaxy resides.", "cat": "astro-ph.CO", "authors": ["S. Bardelli", "E. Schinnerer", "V. Smolcic", "G. Zamorani", "E. Zucca", "M. Mignoli", "C. Halliday", "K. Kovac", "P. Ciliegi", "K. Caputi", "A. M. Koekemoer", "A. Bongiorno", "M. Bondi", "M. Bolzonella", "D. Vergani", "L. Pozzetti", "C. M. Carollo", "T. Contini", "J. -P. Kneib", "O. LeFevre", "S. Lilly", "V. Mainieri", "A. Renzini", "M. Scodeggio", "G. Coppa", "O. Cucciati", "S. delaTorre", "L. deRavel", "P. Franzetti", "B. Garilli", "A. Iovino", "P. Kampczyk", "C. Knobel", "F. Lamareille", "J. -F. LeBorgne", "V. LeBrun", "C. Maier", "R. Pello`", "Y. Peng", "E. Perez-Montero", "E. Ricciardelli", "J. D. Silverman", "M. Tanaka", "L. Tasca", "L. Tresse", "U. Abbas", "D. Bottini", "A. Cappi", "P. Cassata", "A. Cimatti", "L. Guzzo", "A. Leauthaud", "D. Maccagni", "C. Marinoni", "H. J. McCracken", "P. Memeo", "B. Meneux", "P. Oesch", "C. Porciani", "R. Scaramella", "P. Capak", "D. Sanders", "N. Scoville", "Y. Taniguchi", "K. Jahnke"]}, "1450": {"id": "1610.00918v1", "title": "The properties of the Malin 1 galaxy giant disk: A panchromatic view from the NGVS and GUViCS surveys", "url": "http://arxiv.org/pdf/1610.00918v1", "date": "2016-10-04 10:14:27", "abs": "Low surface brightness galaxies (LSBGs) represent a significant percentage of\nlocal galaxies but their formation and evolution remain elusive. They may hold\ncrucial information for our understanding of many key issues (i.e., census of\nbaryonic and dark matter, star formation in the low density regime, mass\nfunction). The most massive examples - the so called giant LSBGs - can be as\nmassive as the Milky Way, but with this mass being distributed in a much larger\ndisk. Malin 1 is an iconic giant LSBG, perhaps the largest disk galaxy known.\nWe attempt to bring new insights on its structure and evolution on the basis of\nnew images covering a wide range in wavelength. We have computed surface\nbrightness profiles (and average surface brightnesses in 16 regions of\ninterest), in six photometric bands (FUV, NUV, u, g, i, z). We compared these\ndata to various models, testing a variety of assumptions concerning the\nformation and evolution of Malin 1. We find that the surface brightness and\ncolor profiles can be reproduced by a long and quiet star-formation history due\nto the low surface density; no significant event, such as a collision, is\nnecessary. Such quiet star formation across the giant disk is obtained in a\ndisk model calibrated for the Milky Way, but with an angular momentum\napproximately 20 times larger. Signs of small variations of the star-formation\nhistory are indicated by the diversity of ages found when different regions\nwithin the galaxy are intercompared.For the first time, panchromatic images of\nMalin 1 are used to constrain the stellar populations and the history of this\niconic example among giant LSBGs. Based on our model, the extreme disk of Malin\n1 is found to have a long history of relatively low star formation (about 2\nMsun/yr). Our model allows us to make predictions on its stellar mass and\nmetallicity.", "cat": "astro-ph.GA", "authors": ["S. Boissier", "A. Boselli", "L. Ferrarese", "P. Cote", "Y. Roehlly", "S. D. J. Gwyn", "J. -C. Cuillandre", "J. Roediger", "J. Koda", "J. C. Munos Mateos", "A. Gil de Paz", "B. F. Madore"]}, "1451": {"id": "1905.06036v1", "title": "Robust profile decomposition for large extragalactic spectral-line surveys", "url": "http://arxiv.org/pdf/1905.06036v1", "date": "2019-05-15 09:01:16", "abs": "We present a novel algorithm that is based on a Bayesian Markov Chain Monte\nCarlo (MCMC) technique for performing robust profile analysis of a data cube\nfrom either single-dish or interferometric radio telescopes. It fits a set of\nmodels comprised of a number of Gaussian components given by the user to\nindividual line-of-sight velocity profiles, then compares them and finds an\noptimal model based on the Bayesian Inference Criteria computed for each\nmodel.The decomposed Gaussian components are then classified into bulk or\nnon-circular motions as well as kinematically cold or warm components. The\nfitting based on the Bayesian MCMC technique is insensitive to initial\nestimates of the parameters, and suffers less from finding the global minimum\nin models given enough sampling points and a wide range of priors for the\nparameters. It is found to provide reliable profile decomposition and\nclassification of the decomposed components in a fully automated way, together\nwith robust error estimation of the parameters as shown by performance tests\nusing artificial data cubes. We apply the newly developed algorithm to the HI\ndata cubes of sample galaxies from the Local Volume HI galaxy Survey (LVHIS).\nWe also compare the kinematically cold and warm components, and bulk velocity\nfields with previous analyses made in a classical method.", "cat": "astro-ph.GA", "authors": ["Se-Heon Oh", "Lister Staveley-Smith", "Bi-Qing For"]}, "1452": {"id": "1301.2774v3", "title": "Crowd Labeling: a survey", "url": "http://arxiv.org/pdf/1301.2774v3", "date": "2014-09-03 06:37:23", "abs": "Recently, there has been a burst in the number of research projects on human\ncomputation via crowdsourcing. Multiple choice (or labeling) questions could be\nreferred to as a common type of problem which is solved by this approach. As an\napplication, crowd labeling is applied to find true labels for large machine\nlearning datasets. Since crowds are not necessarily experts, the labels they\nprovide are rather noisy and erroneous. This challenge is usually resolved by\ncollecting multiple labels for each sample, and then aggregating them to\nestimate the true label. Although the mechanism leads to high-quality labels,\nit is not actually cost-effective. As a result, efforts are currently made to\nmaximize the accuracy in estimating true labels, while fixing the number of\nacquired labels.\n This paper surveys methods to aggregate redundant crowd labels in order to\nestimate unknown true labels. It presents a unified statistical latent model\nwhere the differences among popular methods in the field correspond to\ndifferent choices for the parameters of the model. Afterwards, algorithms to\nmake inference on these models will be surveyed. Moreover, adaptive methods\nwhich iteratively collect labels based on the previously collected labels and\nestimated models will be discussed. In addition, this paper compares the\ndistinguished methods, and provides guidelines for future work required to\naddress the current open issues.", "cat": "cs.AI", "authors": ["Jafar Muhammadi", "Hamid Reza Rabiee", "Abbas Hosseini"]}, "1453": {"id": "1111.2487v3", "title": "First spectro-interferometric survey of Be stars I. Observations and constraints on the disks geometry and kinematics", "url": "http://arxiv.org/pdf/1111.2487v3", "date": "2011-12-08 20:21:52", "abs": "Context. Classical Be stars are hot non-supergiant stars surrounded by a\ngaseous circumstellar disk that is responsible for the observed infrared-excess\nand emission lines. The phenomena involved in the disk formation still remain\nhighly debated. Aims. To progress in the understanding of the physical process\nor processes responsible for the mass ejections and test the hypothesis that\nthey depend on the stellar parameters, we initiated a survey on the\ncircumstellar environment of the brightest Be stars. Methods. To achieve this\ngoal, we used spectro-interferometry, the only technique that combines high\nspectral (R=12000) and high spatial ($\\theta_{\\rm min}$=4\\,mas) resolutions.\nObservations were carried out at the Paranal observatory with the VLTI/AMBER\ninstrument. We concentrated our observations on the Br$\\gamma$ emission line to\nbe able to study the kinematics within the circumstellar disk. Our sample is\ncomposed of eight bright classical Be stars : $\\alpha$ Col, $\\kappa$ CMa,\n$\\omega$ Car, p Car, $\\delta$ Cen, $\\mu$ Cen, $\\alpha$ Ara, and \\textit{o} Aqr.\nResults. We managed to determine the disk extension in the line and the nearby\ncontinuum for most targets. We also constrained the disk kinematics, showing\nthat it is dominated by rotation with a rotation law close to the Keplerian\none. Our survey also suggests that these stars are rotating at a mean velocity\nof V/V$_{\\rm c}$\\,=\\,0.82\\,$\\pm$\\,0.08. This corresponds to a rotational rate\nof $\\Omega/\\Omega_{\\rm c}$\\,=\\,0.95\\,$\\pm$\\,0.02 Conclusions. We did not detect\nany correlation between the stellar parameters and the structure of the\ncircumstellar environment. Moreover, it seems that a simple model of a\ngeometrically thin Keplerian disk can explain most of our spectrally resolved\nK-band data. Nevertheless, some small departures from this model have been\ndetected for at least two objects (i.e, $\\kappa$ CMa and $\\alpha$ Col).\nFinally, our Be stars sample suggests that rotation is the main physical\nprocess driving the mass-ejection. Nevertheless, smaller effects from other\nmechanisms have to be taken into account to fully explain how the residual\ngravity is compensated.", "cat": "astro-ph.SR", "authors": ["Anthony Meilland", "Florentin Millour", "Samer Kanaan", "Philippe Stee", "Romain G. Petrov", "Karl-Heinz Hofmann", "Antonella Natta", "Karine Perraut"]}, "1454": {"id": "1905.06167v4", "title": "A Survey of Blocking and Filtering Techniques for Entity Resolution", "url": "http://arxiv.org/pdf/1905.06167v4", "date": "2020-08-21 15:40:39", "abs": "Efficiency techniques are an integral part of Entity Resolution, since its\ninfancy. In this survey, we organized the bulk of works in the field into\nBlocking, Filtering and hybrid techniques, facilitating their understanding and\nuse. We also provided an in-dept coverage of each category, further classifying\nthe corresponding works into novel sub-categories. Lately, the efficiency\ntechniques have received more attention, due to the rise of Big Data. This\nincludes large volumes of semi-structured data, which pose challenges not only\nto the scalability of efficiency techniques, but also to their core\nassumptions: the requirement of Blocking for schema knowledge and of Filtering\nfor high similarity thresholds. The former led to the introduction of\nschema-agnostic Blocking in conjunction with Block Processing techniques, while\nthe latter led to more relaxed criteria of similarity. Our survey covers these\nnew fields in detail, putting in context all relevant works.", "cat": "cs.DB", "authors": ["George Papadakis", "Dimitrios Skoutas", "Emmanouil Thanos", "Themis Palpanas"]}, "1455": {"id": "2203.04264v2", "title": "A Survey on Privacy for B5G/6G: New Privacy Challenges, and Research Directions", "url": "http://arxiv.org/pdf/2203.04264v2", "date": "2022-12-14 00:34:10", "abs": "Massive developments in mobile wireless telecommunication networks have been\nmade during the last few decades. At present, mobile users are getting familiar\nwith the latest 5G networks, and the discussion for the next generation of\nBeyond 5G (B5G)/6G networks has already been initiated. It is expected that\nB5G/6G will push the existing network capabilities to the next level, with\nhigher speeds, enhanced reliability and seamless connectivity. To make these\nexpectations a reality, research is progressing on new technologies,\narchitectures, and intelligence-based decision-making processes related to\nB5G/6G. Privacy considerations are a crucial aspect that requires further\nattention in such developments, as billions of people and devices will be\ntransmitting data through the upcoming network. However, the main recognition\nremains biased towards the network security. A discussion focused on privacy of\nB5G/6G is lacking at the moment. To address the gap, this paper provides a\ncomprehensive survey on privacy-related aspects of B5G/6G networks. First, it\ndiscusses a taxonomy of different privacy perspectives. Based on the taxonomy,\nthe paper then conceptualizes a set of challenges that appear as barriers to\nreach privacy preservation. Next, this work provides a set of solutions\napplicable to the proposed architecture of B5G/6G networks to mitigate the\nchallenges. It also provides an overview of standardization initiatives for\nprivacy preservation. Finally, the paper concludes with a roadmap of future\ndirections, which will be an arena for new research towards privacy-enhanced\nB5G/6G networks. This work provides a basis for privacy aspects that will\nsignificantly impact peoples' daily lives when using these future networks.", "cat": "cs.CR", "authors": ["Chamara Sandeepa", "Bartlomiej Siniarski", "Nicolas Kourtellis", "Shen Wang", "Madhusanka Liyanage"]}, "1456": {"id": "2403.02901v1", "title": "A Comprehensive Survey on Process-Oriented Automatic Text Summarization with Exploration of LLM-Based Methods", "url": "http://arxiv.org/pdf/2403.02901v1", "date": "2024-03-05 12:11:07", "abs": "Automatic Text Summarization (ATS), utilizing Natural Language Processing\n(NLP) algorithms, aims to create concise and accurate summaries, thereby\nsignificantly reducing the human effort required in processing large volumes of\ntext. ATS has drawn considerable interest in both academic and industrial\ncircles. Many studies have been conducted in the past to survey ATS methods;\nhowever, they generally lack practicality for real-world implementations, as\nthey often categorize previous methods from a theoretical standpoint. Moreover,\nthe advent of Large Language Models (LLMs) has altered conventional ATS\nmethods. In this survey, we aim to 1) provide a comprehensive overview of ATS\nfrom a ``Process-Oriented Schema'' perspective, which is best aligned with\nreal-world implementations; 2) comprehensively review the latest LLM-based ATS\nworks; and 3) deliver an up-to-date survey of ATS, bridging the two-year gap in\nthe literature. To the best of our knowledge, this is the first survey to\nspecifically investigate LLM-based ATS methods.", "cat": "cs.AI", "authors": ["Hanlei Jin", "Yang Zhang", "Dan Meng", "Jun Wang", "Jinghua Tan"]}, "1457": {"id": "2305.08515v3", "title": "Physics lab courses under digital transformation: A tri-national survey among university lab instructors about the role of new digital technologies and learning objectives", "url": "http://arxiv.org/pdf/2305.08515v3", "date": "2023-09-19 10:19:10", "abs": "Physics lab courses permanently undergo transformations, in recent times\nespecially to adapt to the emergence of new digital technologies and the\nCovid-19 pandemic in which digital technologies facilitated distance learning.\nSince these transformations often occur within individual institutions, it is\nuseful to get an overview of these developments by capturing the status quo of\ndigital technologies and the related acquisition of digital competencies in\nphysics lab courses. Thus, we conducted a survey among physics lab instructors\n(N=79) at German, Finnish, and Croatian universities. The findings reveal that\nlab instructors already use a variety of digital technologies and that the\npandemic particularly boosted the use of smartphones/tablets, simulations, and\ndigital tools for communication/collaboration/organization. The participants\ngenerally showed a positive attitude toward using digital technologies in\nphysics lab courses, especially due to their potential for experiments and\nstudents' competence acquisition, motivational effects, and contemporaneity.\nAcquiring digital competencies is rated as less important than established\nlearning objectives, however, collecting and processing data with digital tools\nwas rated as an important competency that students should acquire. The\ninstructors perceived open forms of labwork and particular digital technologies\nfor specific learning objectives (e.g., microcontrollers for experimental\nskills) as useful for reaching their learning objectives. Our survey\ncontributes to the reflection of what impact the emergence of digital\ntechnologies in our society and the Covid-19 pandemic had on physics lab\ncourses and reveals first indications for the future transformation of hands-on\nuniversity physics education.", "cat": "physics.ed-ph", "authors": ["Simon Zacharias Lahme", "Pascal Klein", "Antti Lehtinen", "Andreas M\u00fcller", "Pekka Pirinen", "Lucija Ron\u010devi\u0107", "Ana Su\u0161ac"]}, "1458": {"id": "1806.05661v1", "title": "Modeling of a stepped Luneburg lens for all-sky surveys", "url": "http://arxiv.org/pdf/1806.05661v1", "date": "2018-06-14 17:39:41", "abs": "We investigate the scattered light properties of a Luneburg lens approximated\nas a series of concentric shells with discrete refractive indices. The stepped\nLuneburg lens has been previously modeled at microwave wavelengths with full\nsolutions for the electromagnetic field equations when the lens is of\ncomparable size to the wavelength. We investigate the properties of a Luneburg\nlens at optical wavelengths using a geometric ray tracing technique. We develop\na stack-based ray tracing algorithm with the Python programming language that\ntracks all reflected and refracted rays generated at each optical interface.\nThe code shows that a Luneburg lens with 40 steps and a refractive index\npower-law exponent of 0.55 will produce images of nearly all naked eye (<6)\nmagnitude stars with an enclosed energy of 50% at a spatial resolution of 3.2\ndegrees. We find 72 cases of blended stars where a star with magnitude <6 falls\nwithin 3 degrees of angular separation from a star with magnitude <1. The\noptical stepped Luneburg lens has promising applications for low-cost,\ncontinuous all-sky monitoring to obtain transit light curves of bright, nearby\nstars.", "cat": "astro-ph.IM", "authors": ["Mason Carney", "Matthew A. Kenworthy"]}, "1459": {"id": "2310.04697v5", "title": "Optical system for extremely large spectroscopic survey telescope", "url": "http://arxiv.org/pdf/2310.04697v5", "date": "2024-03-19 05:24:49", "abs": "This article presents research work on a spectroscopic survey telescope. Our\nidea is as follows: for such a telescope, a pure reflecting optical system is\ndesigned, which should have an aperture and a field of view (FOV) both as large\nas possible and excellent image quality, and then a strip lensm (lens-prism)\natmospheric dispersion corrector (S-ADC) is added, only for correcting the\natmospheric dispersion. Given the fund limitation and the simplicity of scaling\nup, some 12-m telescopes are designed as examples. Su, Korsch, and Meinel put\nforward the four-mirror Nasmyth systems I and II, which are used in this paper.\nFOVs of 1.5{\\deg}, 2{\\deg}, and 2.5{\\deg} are selected. For all systems, the\nimage qualities are excellent. Because the S-ADC relaxes the optical glass size\nrestriction, this 12-m telescope with a FOV of 2.5{\\deg} can be magnified in\nproportion to a 16-m telescope. Its etendue (from French \\'etendue) and focal\nsurface will now be the largest in the world. In such a telescope, a pure\nreflecting optical system can also be obtained. A subsequent coud\\'e system is\ndesigned with excellent image quality.", "cat": "astro-ph.IM", "authors": ["Ding-qiang Su", "Hua Bai", "Xiangyan Yuan", "Xiangqun Cui"]}, "1460": {"id": "0802.3146v1", "title": "Infrared Properties Of AGB Stars: from Existing Databases to Antarctic Surveys", "url": "http://arxiv.org/pdf/0802.3146v1", "date": "2008-02-21 16:15:54", "abs": "We present here a study of the Infrared properties of Asymptotic Giant Branch\nstars (hereafter AGB) based on existing databases, mainly from space-borne\nexperiments. Preliminary results about C and S stars are discussed, focusing on\nthe topics for which future Infrared surveys from Antarctica will be crucial.\nThis kind of surveys will help in making more quantitative our knowledge of the\nlast evolutionary stages of low mass stars, especially for what concerns\nluminosities and mass loss.", "cat": "astro-ph", "authors": ["R. Guandalini", "M. Busso"]}, "1461": {"id": "0906.3691v1", "title": "IR imaging surveys of AGB stars in the Magellanic Clouds", "url": "http://arxiv.org/pdf/0906.3691v1", "date": "2009-06-19 15:09:34", "abs": "AGB stars are ideal IR targets because they are cool and bright. Most of them\nescaped detection in optical or shallow IR surveys in the eighties contributing\nto the puzzling missing number of AGB stars with respect to theoretical\npredictions and former stages of evolution. Observations and AGB models have\nadvanced steadily in the following decades providing us with an almost complete\nview of the AGB stars in the Magellanic Clouds. Their properties are tracers of\nstructure and chemistry across galaxies. New surveys will be able to fill-in\nthe gaps, in terms of sensitivity and monitoring, providing new constraints for\nthe formation and evolution of the Magellanic Clouds.", "cat": "astro-ph.CO", "authors": ["Maria-Rosa L. Cioni"]}, "1462": {"id": "1909.06418v1", "title": "Towards A Robot Explanation System: A Survey and Our Approach to State Summarization, Storage and Querying, and Human Interface", "url": "http://arxiv.org/pdf/1909.06418v1", "date": "2019-09-13 19:40:23", "abs": "As robot systems become more ubiquitous, developing understandable robot\nsystems becomes increasingly important in order to build trust. In this paper,\nwe present an approach to developing a holistic robot explanation system, which\nconsists of three interconnected components: state summarization, storage and\nquerying, and human interface. To find trends towards and gaps in the\ndevelopment of such an integrated system, a literature review was performed and\ncategorized around those three components, with a focus on robotics\napplications. After the review of each component, we discuss our proposed\napproach for robot explanation. Finally, we summarize the system as a whole and\nreview its functionality.", "cat": "cs.RO", "authors": ["Zhao Han", "Jordan Allspaw", "Adam Norton", "Holly A. Yanco"]}, "1463": {"id": "2407.21222v1", "title": "A survey of asymptotics of determinants for structured matrices", "url": "http://arxiv.org/pdf/2407.21222v1", "date": "2024-07-30 22:22:34", "abs": "In this survey we show how to produce asymptotics of determinants of\nstructured matrices using operator theory methods. We describe the asymptotics\nfor finite Toeplitz matrices, finite Toeplitz plus Hankel matrices and\ngeneralizations of these, and also finite sections of functions of Toeplitz\noperators, all with smooth matrix-valued symbols. Many of these results are\nwell-known. However, the results for certain Toeplitz plus Hankel operators\nwith matrix-valued symbol are presented for the first time and the result for\nthe finite sections of functions of Toeplitz operators is new.", "cat": "math.FA", "authors": ["E. Basor", "T. Ehrhardt", "J. A. Virtanen"]}, "1464": {"id": "1702.05107v2", "title": "Systematic Survey for [OII], [OIII], and H$\u03b1$ Blobs at $z=0.1-1.5$: The Implication for Evolution of Galactic-Scale Outflow", "url": "http://arxiv.org/pdf/1702.05107v2", "date": "2017-05-03 03:56:12", "abs": "We conduct a systematic search for galaxies at $z=0.1-1.5$ with\n[OII]$\\lambda3727$, [OIII]$\\lambda5007$, or H$\\alpha\\lambda6563$ emission lines\nextended over at least 30 kpc by using deep narrowband and broadband imaging in\nSubaru-XMM Deep Survey (SXDS) field. These extended emission-line galaxies are\ndubbed [OII], [OIII], or H$\\alpha$ blobs. Based on a new selection method that\nsecurely selects extended emission-line galaxies, we find 77 blobs at\n$z=0.40-1.46$ with the isophotal area of emission lines down to\n$1.2\\times10^{-18}$ erg s$^{-1}$ cm$^{-2}$ kpc$^{-2}$. Four of them are\nspectroscopically confirmed to be [OIII] blobs at $z=0.83$. We identify AGN\nactivities in 8 blobs with X-ray and radio data and find that the fraction of\nAGN contribution increases with increasing isophotal area of the extended\nemission. With the Kolmogorov-Smirnov (KS) and Anderson-Darling tests, we\nconfirm that the stellar-mass distributions of H$\\alpha$ and [OII] blobs are\nnot drawn from those of the emitters at the $>90$% confidence level in that\nH$\\alpha$ and [OII] blobs are located at the massive end of the distributions,\nbut cannot reject null hypothesis of being the same distributions in terms of\nthe specific star formation rates. It is suggested that galactic-scale outflows\ntend to be more prominent in more massive star-forming galaxies. Exploiting our\nsample homogeneously selected over the large area, we derive the number\ndensities of blobs at each epoch. The number densities of blobs decrease\ndrastically with redshifts at the rate that is larger than that of the decrease\nof cosmic star formation densities.", "cat": "astro-ph.GA", "authors": ["Suraphong Yuma", "Masami Ouchi", "Alyssa B. Drake", "Seiji Fujimoto", "Takashi Kojima", "Yuma Sugahara"]}, "1465": {"id": "1009.3182v2", "title": "Precision cosmology with a wide area XMM cluster survey", "url": "http://arxiv.org/pdf/1009.3182v2", "date": "2011-07-06 15:19:24", "abs": "We explore the cosmological constraints expected from wide area XMM-type\ncluster surveys covering 50-200 deg2, under realistic observing conditions. We\nperform a Fisher matrix analysis based on cluster number counts in combination\nwith estimates of the 2-point cluster correlation function. The effect of the\nsurvey design is implemented through an observationally well tested cluster\nselection function. Special attention is given to the modelling of the shot\nnoise and sample variance, which we estimate by applying our selection function\nto numerically simulated surveys. We then infer the constraints on the equation\nof state of the dark energy considering various survey configurations. We\nquantitatively investigate the respective impact of the cluster mass\nmeasurements, of the correlation function and of the 1 1.0 mag. show\ndouble-peaked spectral energy distribution, indicating the existence of the\ncircumstellar envelopes around them. 26 N-type stars have IRAS Point Source\nCatalog(PSC) associations. For FBS 1812+455 IRAS Low-Resolution Spectra in the\nwavelength range 7.7 - 22.6micron and Spitzer Space Telescope Spectra in the\nrange 5 - 38micro are presented clearly showing absorption features of\nC2H2(acetylene) molecule at 7.5 and 13.7micron , and the SiC(silicone carbide)\nemission at 11.3micron. The mass-loss rates for eight Mira-type variables are\nderived from the K-[12] color and from the pulsation periods. The reddest\nobject among the targets is N-type C star FBS 2213+421, which belong to the\ngroup of the cold post-AGB R Coronae Borealis(R CrB) variables.", "cat": "astro-ph.SR", "authors": ["K. S. Gigoyan", "A. Sarkissian", "C. Rossi", "D. Russeil", "G. Kostandyan", "M. Calabresi", "F. Zamkotsian", "M. Meftah"]}, "1470": {"id": "1902.08944v2", "title": "Hypotheses Testing from Complex Survey Data Using Bootstrap Weights: A Unified Approach", "url": "http://arxiv.org/pdf/1902.08944v2", "date": "2021-03-03 00:55:03", "abs": "Standard statistical methods that do not take proper account of the\ncomplexity of survey design can lead to erroneous inferences when applied to\nsurvey data due to unequal selection probabilities, clustering, and other\ndesign features. In particular, the actual type I error rates of tests of\nhypotheses using standard methods can be much bigger than the nominal\nsignificance level. Methods that take account of survey design features in\ntesting hypotheses have been proposed, including Wald tests and quasi-score\ntests that involve the estimated covariance matrices of parameter estimates. In\nthis paper, we present a unified approach to hypothesis testing that does not\nrequire computing the covariance matrices by constructing bootstrap\napproximations to weighted likelihood ratio statistics and weighted quasi-score\nstatistics and establish the asymptotic validity of the proposed bootstrap\ntests. In addition, we also consider hypothesis testing from categorical data\nand present a bootstrap procedure for testing simple goodness of fit and\nindependence in a two-way table. In the simulation studies, the type I error\nrates of the proposed approach are much closer to their nominal significance\nlevel compared with the naive likelihood-ratio test and quasi-score test. An\napplication to data from an educational survey under a logistic regression\nmodel is also presented.", "cat": "stat.ME", "authors": ["Jae-kwang Kim", "J. N. K. Rao", "Zhonglei Wang"]}, "1471": {"id": "1702.08023v6", "title": "A survey on difference hierarchies of regular languages", "url": "http://arxiv.org/pdf/1702.08023v6", "date": "2018-03-28 17:01:28", "abs": "Difference hierarchies were originally introduced by Hausdorff and they play\nan important role in descriptive set theory. In this survey paper, we study\ndifference hierarchies of regular languages. The first sections describe\nstandard techniques on difference hierarchies, mostly due to Hausdorff. We\nillustrate these techniques by giving decidability results on the difference\nhierarchies based on shuffle ideals, strongly cyclic regular languages and the\npolynomial closure of group languages.", "cat": "cs.FL", "authors": ["Olivier Carton", "Dominique Perrin", "Jean-\u00c9ric Pin"]}, "1472": {"id": "1801.01882v1", "title": "The 105 month Swift-BAT all-sky hard X-ray survey", "url": "http://arxiv.org/pdf/1801.01882v1", "date": "2018-01-05 19:00:01", "abs": "We present a catalog of hard X-ray sources detected in the first 105 months\nof observations with the Burst Alert Telescope (BAT) coded mask imager on board\nthe Swift observatory. The 105 month Swift-BAT survey is a uniform hard X-ray\nall-sky survey with a sensitivity of $8.40\\times 10^{-12}\\ {\\rm erg\\ s^{-1}\\\ncm^{-2}}$ over 90% of the sky and $7.24\\times 10^{-12}\\ {\\rm erg\\ s^{-1}\\\ncm^{-2}}$ over 50% of the sky in the 14-195 keV band. The Swift-BAT 105 month\ncatalog provides 1632 (422 new detections) hard X-ray sources in the 14-195 keV\nband above the 4.8{\\sigma} significance level. Adding to the previously known\nhard X-ray sources, 34% (144/422) of the new detections are identified as\nSeyfert AGN in nearby galaxies (z<0.2). The majority of the remaining\nidentified sources are X-ray binaries (7%, 31) and blazars/BL Lac objects (10%,\n43). As part of this new edition of the Swift-BAT catalog, we release\neight-channel spectra and monthly sampled light curves for each object in the\nonline journal and at the Swift-BAT 105 month Web site.", "cat": "astro-ph.HE", "authors": ["Kyuseok Oh", "Michael Koss", "Craig B. Markwardt", "Kevin Schawinski", "Wayne H. Baumgartner", "Scott D. Barthelmy", "S. Bradley Cenko", "Neil Gehrels", "Richard Mushotzky", "Abigail Petulante", "Claudio Ricci", "Amy Lien", "Benny Trakhtenbrot"]}, "1473": {"id": "2304.12480v1", "title": "Towards Addressing Training Data Scarcity Challenge in Emerging Radio Access Networks: A Survey and Framework", "url": "http://arxiv.org/pdf/2304.12480v1", "date": "2023-04-24 22:33:54", "abs": "The future of cellular networks is contingent on artificial intelligence (AI)\nbased automation, particularly for radio access network (RAN) operation,\noptimization, and troubleshooting. To achieve such zero-touch automation, a\nmyriad of AI-based solutions are being proposed in literature for modeling and\noptimizing network behavior to achieve the zero-touch automation goal. However,\nto work reliably, AI based automation, requires a deluge of training data.\nConsequently, the success of AI solutions is limited by a fundamental challenge\nfaced by cellular network research community: scarcity of training data. We\npresent an extensive review of classic and emerging techniques to address this\nchallenge. We first identify the common data types in RAN and their known\nuse-cases. We then present a taxonomized survey of techniques to address\ntraining data scarcity for various data types. This is followed by a framework\nto address the training data scarcity. The framework builds on available\ninformation and combination of techniques including interpolation,\ndomain-knowledge based, generative adversarial neural networks, transfer\nlearning, autoencoders, few-shot learning, simulators, and testbeds. Potential\nnew techniques to enrich scarce data in cellular networks are also proposed,\nsuch as by matrix completion theory, and domain knowledge-based techniques\nleveraging different network parameters and geometries. An overview of\nstate-of-the art simulators and testbeds is also presented to make readers\naware of current and emerging platforms for real data access. The extensive\nsurvey of training data scarcity addressing techniques combined with proposed\nframework to select a suitable technique for given type of data, can assist\nresearchers and network operators in choosing appropriate methods to overcome\nthe data scarcity challenge in leveraging AI to radio access network\nautomation.", "cat": "eess.SY", "authors": ["Haneya Naeem Qureshi", "Usama Masood", "Marvin Manalastas", "Syed Muhammad Asad Zaidi", "Hasan Farooq", "Julien Forgeat", "Maxime Bouton", "Shruti Bothe", "Per Karlsson", "Ali Rizwan", "Ali Imran"]}, "1474": {"id": "1401.3759v1", "title": "The PdBI Arcsecond Whirlpool Survey (PAWS): Multi-phase cold gas kinematic of M51", "url": "http://arxiv.org/pdf/1401.3759v1", "date": "2014-01-15 21:15:54", "abs": "The kinematic complexity and the favorable position of M51 on the sky make\nthis galaxy an ideal target to test different theories of spiral arm dynamics.\nTaking advantage of the new high resolution PdBI Arcsecond Whirlpool Survey\n(PAWS) data, we undertake a detailed kinematic study of M51 to characterize and\nquantify the origin and nature of the non-circular motions. Using a tilted-ring\nanalysis supported by several other archival datasets we update the estimation\nof M51's position angle (PA=(173 +/- 3) deg) and inclination (i=(22 +/- 5)\ndeg). Harmonic decomposition of the high resolution (40 pc) CO velocity field\nshows the first kinematic evidence of an m=3 wave in the inner disk of M51 with\na corotation at R(CR,m=3)=1.1 +/- 0.1 kpc and a pattern speed of Omega_p(m=3) =\n140 km/(s kpc). This mode seems to be excited by the nuclear bar, while the\nbeat frequencies generated by the coupling between the m=3 mode and the main\nspiral structure confirm its density-wave nature. We observe also a signature\nof an m=1 mode that is likely responsible for the lopsidedness of M51 at small\nand large radii. We provide a simple method to estimate the radial variation of\nthe amplitude of the spiral perturbation (Vsp) attributed to the different\nmodes. The main spiral arm structure has =50-70 km/s, while the streaming\nvelocity associated with the m=1 and m=3 modes is, in general, 2 times lower.\nOur joint analysis of HI and CO velocity fields at low and high spatial\nresolution reveals that the atomic and molecular gas phases respond differently\nto the spiral perturbation due to their different vertical distribution and\nemission morphology.", "cat": "astro-ph.GA", "authors": ["Dario Colombo", "Sharon E. Meidt", "Eva Schinnerer", "Santiago Garcia-Burillo", "Annie Hughes", "Jerome Pety", "Adam K. Leroy", "Clare L. Dobbs", "Gaelle Dumas", "Todd A. Thompson", "Karl F. Schuster", "Carsten Kramer"]}, "1475": {"id": "0908.3948v2", "title": "Will the Large Synoptic Survey Telescope detect extra-solar planetesimals entering the solar system?", "url": "http://arxiv.org/pdf/0908.3948v2", "date": "2009-09-14 18:56:12", "abs": "Planetesimal formation is a common by-product of the star formation process.\nTaking the dynamical history of the Solar system as a guideline -- in which the\nplanetesimal belts were heavily depleted due to graviational perburbation with\nthe giant planets -- and assuming similar processes have take place in other\nplanetary systems, one would expect the interestellar space to be filled with\nextra-solar planetesimals. However, not a single one of these objects has been\ndetected so far entering the Solar system, even though it would clearly be\ndistinguishable from a Solar system comet due to its highly hyperbolic orbit.\nThe Large Synoptic Survey Telescope (LSST) will provide wide coverage maps of\nthe sky to a very high sensitivity, ideal to detect moving objects like comets,\nboth active and inactive. In anticipation of these observations, we estimate\nhow many inactive \"interstellar comets\" might be detected during the duration\nof the survey. The calculation takes into account estimates (from observations\nand models) of the number density of stars, the amount of solids available to\nform planetesimals, the frequency of planet and planetesimal formation, the\nefficiency of planetesimal ejection, and the possible size distribution of\nthese small bodies.", "cat": "astro-ph.EP", "authors": ["Amaya Moro-Martin", "Edwin L. Turner", "Abraham Loeb"]}, "1476": {"id": "1205.3231v1", "title": "Survey on Distributed Data Mining in P2P Networks", "url": "http://arxiv.org/pdf/1205.3231v1", "date": "2012-05-15 01:00:07", "abs": "The exponential increase of availability of digital data and the necessity to\nprocess it in business and scientific fields has literally forced upon us the\nneed to analyze and mine useful knowledge from it. Traditionally data mining\nhas used a data warehousing model of gathering all data into a central site,\nand then running an algorithm upon that data. Such a centralized approach is\nfundamentally inappropriate due to many reasons like huge amount of data,\ninfeasibility to centralize data stored at multiple sites, bandwidth limitation\nand privacy concerns. To solve these problems, Distributed Data Mining (DDM)\nhas emerged as a hot research area. Careful attention in the usage of\ndistributed resources of data, computing, communication, and human factors in a\nnear optimal fashion are paid by distributed data mining. DDM is gaining\nattention in peer-to-peer (P2P) systems which are emerging as a choice of\nsolution for applications such as file sharing, collaborative movie and song\nscoring, electronic commerce, and surveillance using sensor networks. The main\nintension of this draft paper is to provide an overview of DDM and P2P Data\nMining. The paper discusses the need for DDM, taxonomy of DDM architectures,\nvarious DDM approaches, DDM related works in P2P systems and issues and\nchallenges in P2P data mining.", "cat": "cs.DB", "authors": ["Rekha Sunny T", "Sabu M. Thampi"]}, "1477": {"id": "0901.2587v2", "title": "The WiggleZ Dark Energy Survey: small-scale clustering of Lyman Break Galaxies at z < 1", "url": "http://arxiv.org/pdf/0901.2587v2", "date": "2009-02-25 07:48:47", "abs": "The WiggleZ Dark Energy Survey is a large-scale structure survey of\nintermediate-redshift UV-selected emission-line galaxies scheduled to cover\n1000 sq deg, spanning a broad redshift range 0.2 < z < 1.0. The main scientific\ngoal of the survey is the measurement of baryon acoustic oscillations (BAO) in\nthe galaxy clustering pattern at a significantly higher redshift than previous\nstudies. The BAO may be applied as a standard cosmological ruler to constrain\ndark energy models. Based on the first 20% of the dataset, we present initial\nresults concerning the small-scale clustering of the WiggleZ targets, together\nwith survey forecasts. The WiggleZ galaxy population possesses a clustering\nlength r_0 = 4.40 +/- 0.12 Mpc/h, which is significantly larger than z=0\nUV-selected samples, with a slope gamma = 1.92 +/- 0.08. This clustering length\nis comparable to z=3 Lyman Break Galaxies with similar UV luminosities. The\nfull survey, scheduled for completion in 2010, will map an effective volume\nV_eff ~ 1 Gpc^3 (evaluated at a scale k = 0.15 h/Mpc) and will measure the\nangular-diameter distance and Hubble expansion rates in three redshift bins\nwith accuracies ~ 5%. We will determine the value of a constant dark energy\nequation-of-state parameter, w, with a higher precision than existing\nsupernovae observations using an entirely independent technique. The WiggleZ\nand supernovae measurements lie in highly complementary directions in the plane\nof w and the matter density Omega_m. The forecast using the full combination of\nWiggleZ, supernovae and CMB datasets is a marginalized error sigma(w) = 0.07,\nproviding a robust and precise measurement of the properties of dark energy\nincluding cross-checking of systematic errors.", "cat": "astro-ph.CO", "authors": ["Chris Blake", "Russell Jurek", "Sarah Brough", "Matthew Colless", "Warrick Couch", "Scott Croom", "Tamara Davis", "Michael Drinkwater", "Duncan Forbes", "Karl Glazebrook", "Barry Madore", "Chris Martin", "Kevin Pimbblet", "Greg Poole", "Michael Pracy", "Rob Sharp", "Todd Small", "David Woods"]}, "1478": {"id": "2103.13285v1", "title": "The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries", "url": "http://arxiv.org/pdf/2103.13285v1", "date": "2021-03-24 15:56:10", "abs": "The See Change survey was designed to make $z>1$ cosmological measurements by\nefficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving\ncluster mass measurements through weak lensing. This survey observed twelve\ngalaxy clusters with the Hubble Space Telescope spanning the redshift range\n$z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at\n$z\\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this\nproved to be a highly efficient use of HST for SN observations; the See Change\nsurvey additionally tested the feasibility of maintaining, or further\nincreasing, the efficiency at yet higher redshifts, where we have less detailed\ninformation on the expected cluster masses and star-formation rates. We find\nthat the resulting number of SNe Ia per orbit is a factor of $\\sim 8$ higher\nthan for a field search, and 45% of our orbits contained an active SN Ia within\n22 rest-frame days of peak, with one of the clusters by itself yielding 6 of\nthe SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel\nfeatures include fully blinded SN searches, the first random forest candidate\nclassifier for undersampled IR data (with a 50% detection threshold within 0.05\nmagnitudes of human searchers), real-time forward-modeling photometry of\ncandidates, and semi-automated photometric classifications and follow-up\nforecasts. We also describe the spectroscopic follow-up, instrumental in\nmeasuring host-galaxy redshifts. The cosmology analysis of our sample will be\npresented in a companion paper.", "cat": "astro-ph.CO", "authors": ["Brian Hayden", "David Rubin", "Kyle Boone", "Greg Aldering", "Jakob Nordin", "Mark Brodwin", "Susana Deustua", "Sam Dixon", "Parker Fagrelius", "Andy Fruchter", "Peter Eisenhardt", "Anthony Gonzalez", "Ravi Gupta", "Isobel Hook", "Chris Lidman", "Kyle Luther", "Adam Muzzin", "Zachary Raha", "Pilar Ruiz-Lapuente", "Clare Saunders", "Caroline Sofiatti", "Adam Stanford", "Nao Suzuki", "Tracy Webb", "Steven C. Williams", "Gillian Wilson", "Mike Yen", "Rahman Amanullah", "Kyle Barbary", "Hans Bohringer", "Greta Chappell", "Carlos Cunha", "Miles Currie", "Rene Fassbender", "Michael Gladders", "Ariel Goobar", "Hendrik Hildenrandt", "Henk Hoekstra", "Xiaosheng Huang", "Dragan Huterer", "M. James Jee", "Alex Kim", "Marek Kowalski", "Eric Linder", "Joshua E. Meyers", "Reynald Pain", "Saul Perlmutter", "Johan Richard", "Piero Rosati", "Eduardo Rozo", "Eli Rykoff", "Joana Santos", "Anthony Spadafora", "Daniel Stern", "Risa Wechsler", "The Supernova Cosmology Project"]}, "1479": {"id": "1702.06083v1", "title": "The Gaia-ESO Survey. Mg-Al anti-correlation in iDR4 globular clusters", "url": "http://arxiv.org/pdf/1702.06083v1", "date": "2017-02-20 17:56:54", "abs": "We use Gaia-ESO Survey iDR4 data to explore the Mg-Al anti-correlation in\nglobular clusters, that were observed as calibrators, as a demonstration of the\nquality of Gaia-ESO Survey data and analysis. The results compare well with the\navailable literature, within 0.1 dex or less, after a small (compared to the\ninternal spreads) offset between the UVES and the GIRAFFE data of 0.10-0.15 dex\nwas taken into account. In particular, we present for the first time data for\nNGC 5927, one of the most metal-rich globular clusters studied in the\nliterature so far with [Fe/H]=-0.49 dex, that was included to connect with the\nopen cluster regime in the Gaia-ESO Survey internal calibration. The extent and\nshape of the Mg-Al anti-correlation provide strong constraints on the multiple\npopulation phenomenon in globular clusters. In particular, we studied the\ndependency of the Mg-Al anti-correlation extension with metallicity,\npresent-day mass, and age of the clusters, using GES data in combination with a\nlarge set of homogenized literature measurements. We find a dependency with\nboth metallicity and mass, that is evident when fitting for the two parameters\nsimultaneously, but no significant dependency with age. We confirm that the\nMg-Al anti-correlation is not seen in all clusters, but disappears for the less\nmassive or most metal-rich ones. We also use our dataset to see whether a\nnormal anti-correlation would explain the low [Mg/$\\alpha$] observed in some\nextragalactic globular clusters, but find that none of the clusters in our\nsample can reproduce it, and more extreme chemical compositions (like the one\nof NGC 2419) would be required. We conclude that GES iDR4 data already meet the\nrequirements set by the main survey goals, and can be used to study in detail\nglobular clusters even if the analysis procedures were not specifically\ndesigned for them.", "cat": "astro-ph.SR", "authors": ["E. Pancino", "the GES collaboration"]}, "1480": {"id": "1805.10456v1", "title": "Photometric survey of 67 near-Earth objects", "url": "http://arxiv.org/pdf/1805.10456v1", "date": "2018-05-26 10:11:14", "abs": "The near-Earth object (NEO) population is a window into the original\nconditions of the protosolar nebula, and has the potential to provide a key\npathway for the delivery of water and organics to the early Earth. In addition\nto delivering the crucial ingredients for life, NEOs can pose a serious hazard\nto humanity since they can impact the Earth. To properly quantify the impact\nrisk, physical properties of the NEO population need to be studied.\nUnfortunately, NEOs have a great variation in terms of mitigation-relevant\nquantities (size, albedo, composition, etc.) and less than 15% of them have\nbeen characterized to date. There is an urgent need to undertake a\ncomprehensive characterization of smaller NEOs (D<300m) given that there are\nmany more of them than larger objects. One of the main aims of the NEOShield-2\nproject (2015--2017), financed by the European Community in the framework of\nthe Horizon 2020 program, is therefore to retrieve physical properties of a\nwide number of NEOs in order to design impact mitigation missions and assess\nthe consequences of an impact on Earth. We carried out visible photometry of\nNEOs, making use of the DOLORES instrument at the Telescopio Nazionale Galileo\n(TNG, La Palma, Spain) in order to derive visible color indexes and the\ntaxonomic classification for each target in our sample. We attributed for the\nfirst time the taxonomical complex of 67 objects obtained during the first year\nof the project. While the majority of our sample belong to the S-complex,\ncarbonaceous C-complex NEOs deserve particular attention. These NEOs can be\nlocated in orbits that are challenging from a mitigation point of view, with\nhigh inclination and low minimum orbit intersection distance (MOID). In\naddition, the lack of carbonaceous material we see in the small NEO population\nmight not be due to an observational bias alone.", "cat": "astro-ph.EP", "authors": ["S. Ieva", "E. Dotto", "E. Mazzotta Epifani", "D. Perna", "A. Rossi", "M. A. Barucci", "A. Di Paola", "R. Speziali", "M. Micheli", "E. Perozzi", "M. Lazzarin", "I. Bertini"]}, "1481": {"id": "1607.06772v2", "title": "ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Search for [CII] line and dust emission in 66$ using ASPECS, our ALMA Spectroscopic Survey in the\nHubble Ultra-Deep Field (UDF). Our observations, which cover the frequency\nrange $212-272$ GHz, encompass approximately the range $6$4.5\n$\\sigma$, two of which correspond to blind detections with no optical\ncounterparts. At this significance level, our statistical analysis shows that\nabout 60\\% of our candidates are expected to be spurious. For one of our\nblindly selected [CII] line candidates, we tentatively detect the CO(6-5) line\nin our parallel 3-mm line scan. None of the line candidates are individually\ndetected in the 1.2 mm continuum. A stack of all [CII] candidates results in a\ntentative detection with $S_{1.2mm}=14\\pm5\\mu$Jy. This implies a dust-obscured\nstar formation rate (SFR) of $(3\\pm1)$ M$_\\odot$ yr$^{-1}$. We find that the\ntwo highest--SFR objects have candidate [CII] lines with luminosities that are\nconsistent with the low-redshift $L_{\\rm [CII]}$ vs. SFR relation. The other\ncandidates have significantly higher [CII] luminosities than expected from\ntheir UV--based SFR. At the current sensitivity it is unclear whether the\nmajority of these sources are intrinsically bright [CII] emitters, or spurious\nsources. If only one of our line candidates was real (a scenario greatly\nfavored by our statistical analysis), we find a source density for [CII]\nemitters at $66). The\nprime high level science product of CLASSY is accurately coadded UV spectra,\nranging from ~1000-2000A, derived from a combination of archival and new data\nobtained with HST's Cosmic Origins Spectrograph (COS). This paper details the\nmulti-stage technical processes of creating this prime data product, and the\nmethodologies involved in extracting, reducing, aligning, and coadding\nfar-ultraviolet (FUV) and near-ultraviolet (NUV) spectra. We provide guidelines\non how to successfully utilize COS observations of extended sources, despite\nCOS being optimized for point sources, and best-practice recommendations for\nthe coaddition of UV spectra in general. Moreover, we discuss the effects of\nour reduction and coaddition techniques in the scientific application of the\nCLASSY data. In particular, we find that accurately accounting for flux\ncalibration offsets can affect the derived properties of the stellar\npopulations, while customized extractions of NUV spectra for extended sources\nare essential for correctly diagnosing the metallicity of galaxies via CIII]\nnebular emission. Despite changes in spectral resolution of up to ~25% between\nindividual datasets (due to changes in the COS line spread function), no\nadverse affects were observed on the difference in velocity width and outflow\nvelocities of isolated absorption lines when measured in the final combined\ndata products, owing in-part to our signal-to-noise regime of S/N<20.", "cat": "astro-ph.GA", "authors": ["Bethan L. James", "Danielle A. Berg", "Teagan King", "David J. Sahnow", "Matilde Mingozzi", "John Chisholm", "Timothy Heckman", "Crystal L. Martin", "Dan P. Stark", "The Classy Team", ":", "Alessandra Aloisi", "Ricardo O. Amor\u00edn", "Karla Z. Arellano-C\u00f3rdova", "Matthew Bayliss", "Rongmon Bordoloi", "Jarle Brinchmann", "St\u00e9phane Charlot", "Jacopo Chevallard", "Ilyse Clark", "Dawn K. Erb", "Anna Feltre", "Matthew Hayes", "Alaina Henry", "Svea Hernandez", "Anne Jaskot", "Tucker Jones", "Lisa J. Kewley", "Nimisha Kumari", "Claus Leitherer", "Mario Llerena", "Michael Maseda", "Themiya Nanayakkara", "Masami Ouchi", "Adele Plat", "Richard W. Pogge", "Swara Ravindranath", "Jane R. Rigby", "Ryan Sanders", "Claudia Scarlata", "Peter Senchyna", "Evan D. Skillman", "Charles C. Steidel", "Allison L. Strom", "Yuma Sugahara", "Stephen M. Wilkins", "Aida Wofford", "Xinfeng Xu"]}, "1494": {"id": "2003.05459v2", "title": "Beyond Gaia: Asteroseismic Distances of M giants using Ground-Based Transient Surveys", "url": "http://arxiv.org/pdf/2003.05459v2", "date": "2020-05-09 03:06:56", "abs": "Evolved stars near the tip of the red giant branch (TRGB) show solar-like\noscillations with periods spanning hours to months and amplitudes ranging from\n$\\sim$1 mmag to $\\sim$100 mmag. The systematic detection of the resulting\nphotometric variations with ground-based telescopes would enable the\napplication of asteroseismology to a much larger and more distant sample of\nstars than is currently accessible with space-based telescopes such as\n\\textit{Kepler} or the ongoing Transiting Exoplanet Survey Satellite\n(\\textit{TESS}) mission. We present an asteroseismic analysis of 493 M giants\nusing data from two ground-based surveys: the Asteroid Terrestrial-impact Last\nAlert System (ATLAS) and the All-Sky Automated Survey for Supernovae (ASAS-SN).\nBy comparing the extracted frequencies with constraints from \\textit{Kepler},\nthe Sloan Digital Sky Survey Apache Point Observatory Galaxy Evolution\nExperiment (APOGEE), and Gaia we demonstrate that ground-based transient\nsurveys allow accurate distance measurements to oscillating M giants with a\nprecision of $\\sim$15$\\%$. Using stellar population synthesis models we predict\nthat ATLAS and ASAS-SN can provide asteroseismic distances to\n$\\sim$2$\\times$10$^{6}$ galactic M giants out to typical distances of $20-50 \\;\n\\rm{kpc}$, vastly improving the reach of Gaia and providing critical\nconstraints for Galactic archaeology and galactic dynamics.", "cat": "astro-ph.SR", "authors": ["Connor Auge", "Daniel Huber", "Aren Heinze", "B. J. Shappee", "John Tonry", "Sukanya Chakrabarti", "Robyn E. Sanderson", "Larry Denneau", "Heather Flewelling", "Thomas W. -S. Holoien", "C. S. Kochanek", "Giuliano Pignata", "Amanda Sickafoose", "Brian Stalder", "K. Z. Stanek", "Dennis Stello", "Todd A. Thompson"]}, "1495": {"id": "1005.4013v1", "title": "Sensors Lifetime Enhancement Techniques in Wireless Sensor Networks - A Survey", "url": "http://arxiv.org/pdf/1005.4013v1", "date": "2010-05-21 17:15:08", "abs": "Wireless Sensor Networks are basically used for gathering information needed\nby smart environments but they are particularly useful in unattended situations\nwhere terrain, climate and other environmental constraints may hinder in the\ndeployment of wired/conventional networks. Unlike traditional networks, these\nsensor networks do not have a continuous power supply at their disposal. Rather\nthe individual sensors are battery operated and the lifetime of the individual\nsensors and thus the overall network depend heavily on duty cycle of these\nsensors. Analysis on WSNs shows that communication module is the main part\nwhich consumes most of the sensor energy and that is why energy conservation is\nthe major optimization goal. Since routing protocols and MAC protocols directly\naccess the communication module therefore the design of protocols in these two\ndomains should take into account the energy conservation goal. In this paper,\nwe discuss different state-of-the-art protocols both in MAC and routing domains\nthat have been proposed for WSNs to achieve the overall goal of prolonging the\nnetwork lifetime. The routing protocols in WSNs are generally categorized into\nthree groups - data centric, hierarchical and location-based but we focus on\nonly the first two categories because location-based routing protocols\ngenerally require a prior knowledge about sensors location which most of the\ntimes is not available due to random deployment of the sensors. We then discuss\nhow schedule-based and contention-based MAC protocols can contribute to achieve\noptimal utilization of the limited energy resource by avoiding or reducing the\nchances of collisions and thus the need for retransmission.", "cat": "cs.NI", "authors": ["Sami Halawani", "Abdul Waheed Khan"]}, "1496": {"id": "2308.13702v3", "title": "Extending the Chemical Reach of the H3 Survey: Detailed Abundances of the Dwarf-galaxy Stellar Stream Wukong/LMS-1", "url": "http://arxiv.org/pdf/2308.13702v3", "date": "2024-04-05 15:43:15", "abs": "We present the first detailed chemical-abundance analysis of stars from the\ndwarf-galaxy stellar stream Wukong/LMS-1 covering a wide metallicity range\n($-3.5 < \\rm[Fe/H] \\lesssim -1.3$). We find abundance patterns that are\neffectively indistinguishable from the bulk of Indus and Jhelum, a pair of\nsmaller stellar streams proposed to be dynamically associated with\nWukong/LMS-1. We confirmed a carbon-enhanced metal-poor star ($\\rm[C/Fe] >\n+0.7$ and $\\rm[Fe/H] \\sim -2.9$) in Wukong/LMS-1 with strong enhancements in\nSr, Y, and Zr, which is peculiar given its solar-level [Ba/Fe]. Wukong/LMS-1\nstars have high abundances of $\\alpha$ elements up to $\\rm[Fe/H] \\gtrsim -2$,\nwhich is expected for relatively massive dwarfs. Towards the high-metallicity\nend, Wukong/LMS-1 becomes $\\alpha$-poor, revealing that it probably experienced\nfairly standard chemical evolution. We identified a pair of N- and Na-rich\nstars in Wukong/LMS-1, reminiscent of multiple populations in globular\nclusters. This indicates that this dwarf galaxy contained at least one globular\ncluster that was completely disrupted in addition to two intact ones previously\nknown to be associated with Wukong/LMS-1, which is possibly connected to\nsimilar evidence found in Indus. From these $\\geq$3 globular clusters, we\nestimate the total mass of Wukong/LMS-1 to be ${\\approx}10^{10} M_\\odot$,\nrepresenting ${\\sim}1$% of the present-day Milky Way. Finally, the [Eu/Mg]\nratio in Wukong/LMS-1 continuously increases with metallicity, making this the\nfirst example of a dwarf galaxy where the production of $r$-process elements is\nclearly dominated by delayed sources, presumably neutron-star mergers.", "cat": "astro-ph.GA", "authors": ["Guilherme Limberg", "Alexander P. Ji", "Rohan P. Naidu", "Anirudh Chiti", "Silvia Rossi", "Sam A. Usman", "Yuan-Sen Ting", "Dennis Zaritsky", "Ana Bonaca", "Lais Borbolato", "Joshua S. Speagle", "Vedant Chandra", "Charlie Conroy"]}, "1497": {"id": "1709.07604v3", "title": "A Comprehensive Survey of Graph Embedding: Problems, Techniques and Applications", "url": "http://arxiv.org/pdf/1709.07604v3", "date": "2018-02-02 07:01:22", "abs": "Graph is an important data representation which appears in a wide diversity\nof real-world scenarios. Effective graph analytics provides users a deeper\nunderstanding of what is behind the data, and thus can benefit a lot of useful\napplications such as node classification, node recommendation, link prediction,\netc. However, most graph analytics methods suffer the high computation and\nspace cost. Graph embedding is an effective yet efficient way to solve the\ngraph analytics problem. It converts the graph data into a low dimensional\nspace in which the graph structural information and graph properties are\nmaximally preserved. In this survey, we conduct a comprehensive review of the\nliterature in graph embedding. We first introduce the formal definition of\ngraph embedding as well as the related concepts. After that, we propose two\ntaxonomies of graph embedding which correspond to what challenges exist in\ndifferent graph embedding problem settings and how the existing work address\nthese challenges in their solutions. Finally, we summarize the applications\nthat graph embedding enables and suggest four promising future research\ndirections in terms of computation efficiency, problem settings, techniques and\napplication scenarios.", "cat": "cs.AI", "authors": ["Hongyun Cai", "Vincent W. Zheng", "Kevin Chen-Chuan Chang"]}, "1498": {"id": "1710.08930v2", "title": "The Reionization Lensing Cluster Survey (RELICS) and the Brightest High-z Galaxies", "url": "http://arxiv.org/pdf/1710.08930v2", "date": "2018-04-20 19:02:06", "abs": "Massive foreground galaxy clusters magnify and distort the light of objects\nbehind them, permitting a view into both the extremely distant and\nintrinsically faint galaxy populations. We present here the z ~ 6 - 8 candidate\nhigh-redshift galaxies from the Reionization Lensing Cluster Survey (RELICS), a\nHubble and Spitzer Space Telescope survey of 41 massive galaxy clusters\nspanning an area of ~200 arcmin^2. These clusters were selected to be excellent\nlenses and we find similar high-redshift sample sizes and magnitude\ndistributions as CLASH. We discover 321 candidate galaxies with photometric\nredshifts between z ~ 6 to z ~ 8, including extremely bright objects with\nH-band magnitudes of m_AB ~ 23 mag. As a sample, the observed (lensed)\nmagnitudes of these galaxies are among the brightest known at z> 6, comparable\nto much wider, blank-field surveys. RELICS demonstrates the efficiency of using\nstrong gravitational lenses to produce high-redshift samples in the epoch of\nreionization. These brightly observed galaxies are excellent targets for\nfollow-up study with current and future observatories, including the James Webb\nSpace Telescope.", "cat": "astro-ph.GA", "authors": ["Brett Salmon", "Dan Coe", "Larry Bradley", "Rychard Bouwens", "Marusa Bradac", "Kuang-Han Huang", "Pascal Oesch", "Daniel Stark", "Keren Sharon", "Michele Trenti", "Roberto J. Avila", "Sara Ogaz", "Felipe Andrade-Santos", "Daniela Carrasco", "Catherine Cerny", "William Dawson", "Brenda L. Frye", "Austin Hoag", "Traci Lin Johnson", "Christine Jones", "Daniel Lam", "Lorenzo Lovisari", "Ramesh Mainali", "Matt Past", "Rachel Paterno-Mahler", "Avery Peterson", "Adam Riess", "Steven A. Rodney", "Russel Ryan", "Irene Sendra-Server", "Lou Strolger", "Keiichi Umetsu", "Benedetta Vulcani", "Adi Zitrin"]}, "1499": {"id": "0905.3995v1", "title": "The Westerbork SINGS Survey II. Polarization, Faraday Rotation, and Magnetic Fields", "url": "http://arxiv.org/pdf/0905.3995v1", "date": "2009-05-25 11:09:59", "abs": "A sample of large northern Spitzer Infrared Nearby Galaxies Survey (SINGS)\ngalaxies has recently been observed with the Westerbork Synthesis Radio\nTelescope (WSRT). We present observations of the linearly polarized radio\ncontinuum emission in this WSRT-SINGS galaxy sample. Of the 28 galaxies treated\nin this paper, 21 are detected in polarized radio continuum at 18- and 22-cm\nwavelengths. We utilize the rotation measure synthesis (RM-Synthesis) method,\nas implemented by Brentjens & de Bruyn, to coherently detect polarized emission\nfrom a large fractional bandwidth, while simultaneously assessing the degree of\nFaraday rotation experienced by the radiation along each line-of-sight. This\nrepresents the first time that the polarized emission and its Faraday rotation\nhave been systematically probed down to ~10 microJy/beam RMS for a large sample\nof galaxies. Non-zero Faraday rotation is found to be ubiquitous in all of the\ntarget fields, from both the Galactic foreground and the target galaxies\nthemselves. In this paper, we present an overview of the polarized emission\ndetected in each of the WSRT-SINGS galaxies. The most prominent trend is a\nsystematic modulation of the polarized intensity with galactic azimuth, such\nthat a global minimum in the polarized intensity is seen toward the\nkinematically receding major axis. The implied large-scale magnetic field\ngeometry is discussed in a companion paper. A second novel result is the\ndetection of multiple nuclear Faraday depth components that are offset to both\npositive and negative RM by 100-200 rad/m^2 in all targets that host polarized\n(circum-)nuclear emission.", "cat": "astro-ph.GA", "authors": ["G. Heald", "R. Braun", "R. Edmonds"]}, "1500": {"id": "1701.08156v2", "title": "A Comprehensive Survey on Bengali Phoneme Recognition", "url": "http://arxiv.org/pdf/1701.08156v2", "date": "2018-04-26 18:17:00", "abs": "Hidden Markov model based various phoneme recognition methods for Bengali\nlanguage is reviewed. Automatic phoneme recognition for Bengali language using\nmultilayer neural network is reviewed. Usefulness of multilayer neural network\nover single layer neural network is discussed. Bangla phonetic feature table\nconstruction and enhancement for Bengali speech recognition is also discussed.\nComparison among these methods is discussed.", "cat": "cs.SD", "authors": ["Sadia Tasnim Swarna", "Shamim Ehsan", "Md. Saiful Islam", "Marium E Jannat"]}, "1501": {"id": "1601.04385v1", "title": "Real-Time Data Mining of Massive Data Streams from Synoptic Sky Surveys", "url": "http://arxiv.org/pdf/1601.04385v1", "date": "2016-01-18 02:06:45", "abs": "The nature of scientific and technological data collection is evolving\nrapidly: data volumes and rates grow exponentially, with increasing complexity\nand information content, and there has been a transition from static data sets\nto data streams that must be analyzed in real time. Interesting or anomalous\nphenomena must be quickly characterized and followed up with additional\nmeasurements via optimal deployment of limited assets. Modern astronomy\npresents a variety of such phenomena in the form of transient events in digital\nsynoptic sky surveys, including cosmic explosions (supernovae, gamma ray\nbursts), relativistic phenomena (black hole formation, jets), potentially\nhazardous asteroids, etc. We have been developing a set of machine learning\ntools to detect, classify and plan a response to transient events for astronomy\napplications, using the Catalina Real-time Transient Survey (CRTS) as a\nscientific and methodological testbed. The ability to respond rapidly to the\npotentially most interesting events is a key bottleneck that limits the\nscientific returns from the current and anticipated synoptic sky surveys.\nSimilar challenge arise in other contexts, from environmental monitoring using\nsensor networks to autonomous spacecraft systems. Given the exponential growth\nof data rates, and the time-critical response, we need a fully automated and\nrobust approach. We describe the results obtained to date, and the possible\nfuture developments.", "cat": "astro-ph.IM", "authors": ["S. G. Djorgovski", "M. J. Graham", "C. Donalek", "A. A. Mahabal", "A. J. Drake", "M. Turmon", "T. Fuchs"]}, "1502": {"id": "1009.5905v1", "title": "TASTE: The Asiago Survey for Timing transit variations of Exoplanets", "url": "http://arxiv.org/pdf/1009.5905v1", "date": "2010-09-29 14:59:31", "abs": "A promising method to detect earth-sized exoplanets is the timing analysis of\na known transit. The technique allows a search for variations in transit\nduration or center induced by the perturbation of a third body, e.g. a second\nplanet or an exomoon. To this aim, TASTE (The Asiago Survey for Timing transit\nvariations of Exoplanets) project will collect high-precision, short-cadence\nlight curves for a selected sample of transits by using imaging differential\nphotometry at the Asiago 1.82m telescope. The first light curves show that our\nproject can already provide a competitive timing accuracy, as well as a\nsignificant improvement over the orbital parameters. We derived refined\nephemerides for HAT-P-3b and HAT-P-14b with only one transit each, thanks to a\ntiming accuracy of 11 and 25 s, respectively.", "cat": "astro-ph.EP", "authors": ["V. Nascimbeni", "G. Piotto", "L. R. Bedin", "M. Damasso"]}, "1503": {"id": "2304.09003v1", "title": "Elliptic curve over totally real fields: A Survey", "url": "http://arxiv.org/pdf/2304.09003v1", "date": "2023-04-18 14:12:55", "abs": "In this survey article, we summarise the known results towards the\nconjecture: elliptic curves over totally real number fields are modular. For\nunderstanding these recent results in the literature, we present some necessary\nbackground along with certain applications.", "cat": "math.NT", "authors": ["Bidisha Roy", "Lalit Vaishya"]}, "1504": {"id": "2403.14496v1", "title": "How Human-Centered Explainable AI Interface Are Designed and Evaluated: A Systematic Survey", "url": "http://arxiv.org/pdf/2403.14496v1", "date": "2024-03-21 15:44:56", "abs": "Despite its technological breakthroughs, eXplainable Artificial Intelligence\n(XAI) research has limited success in producing the {\\em effective\nexplanations} needed by users. In order to improve XAI systems' usability,\npractical interpretability, and efficacy for real users, the emerging area of\n{\\em Explainable Interfaces} (EIs) focuses on the user interface and user\nexperience design aspects of XAI. This paper presents a systematic survey of 53\npublications to identify current trends in human-XAI interaction and promising\ndirections for EI design and development. This is among the first systematic\nsurvey of EI research.", "cat": "cs.HC", "authors": ["Thu Nguyen", "Alessandro Canossa", "Jichen Zhu"]}, "1505": {"id": "1510.00916v1", "title": "On the Atmospheric Extinction Reduction Procedure in Multiband Wide-Field Photometric Surveys", "url": "http://arxiv.org/pdf/1510.00916v1", "date": "2015-10-04 08:33:50", "abs": "We propose an improved method for the atmospheric extinction reduction within\noptical photometry. Our method is based on the simultaneous multicolor\nobservations of photometric standards. Such data are now available within the\nmodern wide-field sky surveys and contain a large amount of information about\ninstant atmospheric conditions. So, it became possible to estimate the\nextinction parameters on the basis of a quite short observational dataset and,\nhence, to trace the rapid stars twinkling accurately. Having been developed for\na new MiniMegaTORTORA observational system, the proposed method can be adopted\nfor a wide range of modern observational programs.", "cat": "astro-ph.IM", "authors": ["A. Zakharov", "A. Mironov", "A. Biryukov", "N. Kroussanova", "M. Prokhorov", "G. Beskin", "S. Karpov", "S. Bondar", "E. Ivanov", "A. Perkov", "V. Sasyuk"]}, "1506": {"id": "2101.11174v4", "title": "Graph Neural Network for Traffic Forecasting: A Survey", "url": "http://arxiv.org/pdf/2101.11174v4", "date": "2022-02-22 05:46:58", "abs": "Traffic forecasting is important for the success of intelligent\ntransportation systems. Deep learning models, including convolution neural\nnetworks and recurrent neural networks, have been extensively applied in\ntraffic forecasting problems to model spatial and temporal dependencies. In\nrecent years, to model the graph structures in transportation systems as well\nas contextual information, graph neural networks have been introduced and have\nachieved state-of-the-art performance in a series of traffic forecasting\nproblems. In this survey, we review the rapidly growing body of research using\ndifferent graph neural networks, e.g. graph convolutional and graph attention\nnetworks, in various traffic forecasting problems, e.g. road traffic flow and\nspeed forecasting, passenger flow forecasting in urban rail transit systems,\nand demand forecasting in ride-hailing platforms. We also present a\ncomprehensive list of open data and source resources for each problem and\nidentify future research directions. To the best of our knowledge, this paper\nis the first comprehensive survey that explores the application of graph neural\nnetworks for traffic forecasting problems. We have also created a public GitHub\nrepository where the latest papers, open data, and source resources will be\nupdated.", "cat": "cs.LG", "authors": ["Weiwei Jiang", "Jiayun Luo"]}, "1507": {"id": "1312.0793v1", "title": "A Survey for Ground-State OH Masers Toward a Sample of Herbig-Haro Objects", "url": "http://arxiv.org/pdf/1312.0793v1", "date": "2013-12-03 12:17:40", "abs": "Herbig-Haro objects are regions of shocked gas and dust which are produced\nwhen collimated outflows from a protostar interact with the surrounding dense\ngas. They have many similarities to supernova remnants which are interacting\nwith molecular clouds. 1720-MHz OH masers have been identified towards a number\nof interacting supernova remnants. Observations and models indicate that these\nmasers are shock excited and are produced behind C-type shocks. If conditions\nbehind the shock fronts of Herbig-Haro objects are similarly able to support\n1720-MHz OH masers they could be a useful diagnostic tool for star formation.\nWe therefore searched for 1720-MHz OH maser emission towards a sample of 97\nHerbig-Haro objects using the Green Bank radio telescope. We detected 1720-MHz\nOH lines in emission in 17 of them, but neither their spectral signature nor\nfollow-up observations with the Very Large Array showed any conclusive evidence\nof maser emission. We conclude that the emission detected from our single-dish\nobservations must be extended and most likely originates from thermal or\nquasi-thermal excitation processes. We also investigated the properties of\nHerbig-Haro shocks more closely and conclude that despite the overall\nsimilarities to supernova remnants, the conditions required for maser emission,\nin particular, a sufficient velocity-coherent column density, are not likely to\noccur in Herbig-Haro objects.", "cat": "astro-ph.GA", "authors": ["A. de Witt", "M. Bietenholz", "R. Booth", "M. Gaylard"]}, "1508": {"id": "2010.09858v3", "title": "Vehicular Visible Light Positioning for Collision Avoidance and Platooning: A Survey", "url": "http://arxiv.org/pdf/2010.09858v3", "date": "2023-11-02 18:12:35", "abs": "Relative vehicle positioning methods can contribute to safer and more\nefficient autonomous driving by enabling collision avoidance and platooning\napplications. For full automation, these applications require cm-level\npositioning accuracy and greater than 50 Hz update rate. Since sensor-based\nmethods (e.g., LIDAR, cameras) have not been able to reliably satisfy these\nrequirements under all conditions so far, complementary methods are sought.\nRecently, positioning based on visible light communication signals from vehicle\nhead/tail LED lights (VLP) has shown significant promise as a complementary\nmethod attaining cm-level accuracy and near-kHz rate in realistic driving\nscenarios. Vehicular VLP methods measure relative bearing (angle) or range\n(distance) of transmitters (i.e., head/tail lights) based on received signals\nfrom on-board photodiodes and estimate transmitter relative positions based on\nthose measurements. In this survey, we first review existing vehicular VLP\nmethods and propose a new method that advances the state-of-the-art in\npositioning performance. Next, we analyze the theoretical and simulated\nperformance of all methods in realistic driving scenarios under challenging\nnoise and weather conditions, real asymmetric light beam patterns and different\nvehicle dimensions and light placements. Our simulation results show that the\nnewly proposed VLP method is the overall best performer, and can indeed satisfy\nthe accuracy and rate requirements for localization in collision avoidance and\nplatooning applications within practical constraints. Finally, we discuss\nremaining open challenges that are faced for the deployment of VLP solutions in\nthe automotive sector and further research questions.", "cat": "eess.SP", "authors": ["Burak Soner", "Merve Karakas", "Utku Noyan", "Furkan Sahbaz", "Sinem Coleri"]}, "1509": {"id": "1805.00477v1", "title": "A simultaneous search for High-$z$ LAEs and LBGs in the SHARDS survey", "url": "http://arxiv.org/pdf/1805.00477v1", "date": "2018-05-01 18:00:01", "abs": "We have undertaken a comprehensive search for both Lyman Alpha Emitters\n(LAEs) and Lyman Break Galaxies (LBGs) in the SHARDS Survey of the GOODS-N\nfield. SHARDS is a deep imaging survey, made with the 10.4 m Gran Telescopio\nCanarias (GTC), employing 25 medium band filters in the range from 500 to 941\nnm. This is the first time that both LAEs and LBGs are surveyed simultaneously\nin a systematic way in a large field. We draw a sample of 1558 sources; 528 of\nthem are LAEs. Most of the sources (1434) show rest-frame UV continua. A\nminority of them (124) are pure LAEs with virtually no continuum detected in\nSHARDS. We study these sources from $z\\sim3.35$ up to $z\\sim6.8$, well into the\nepoch of reionization. Note that surveys done with just one or two narrow band\nfilters lack the possibility to spot the rest-frame UV continuum present in\nmost of our LAEs. We derive redshifts, Star Formation Rates (SFRs), Ly$\\alpha$\nEquivalent Widths (EWs) and Luminosity Functions (LFs). Grouping within our\nsample is also studied, finding 92 pairs or small groups of galaxies at the\nsame redshift separated by less than 60 comoving kpc. In addition, we relate 87\nand 55 UV-selected objects with two known overdensities at $z=4.05$ and\n$z=5.198$, respectively. Finally, we show that surveys made with broad band\nfilters are prone to introduce many unwanted sources ($\\sim20$% interlopers),\nwhich means that previous studies may be overestimating the calculated LFs,\nspecially at the faint end.", "cat": "astro-ph.GA", "authors": ["P. Arrabal Haro", "J. M. Rodr\u00edguez Espinosa", "C. Mu\u00f1oz-Tu\u00f1\u00f3n", "P. G. P\u00e9rez-Gonz\u00e1lez", "H. Dannerbauer", "\u00c1. Bongiovanni", "G. Barro", "A. Cava", "A. Lumbreras-Calle", "A. Hern\u00e1n-Caballero", "M. C. Eliche-Moral", "H. Dom\u00ednguez S\u00e1nchez", "C. J. Conselice", "L. Tresse", "B. Alcalde Pampliega", "M. Balcells", "E. Daddi", "G. Rodighiero"]}, "1510": {"id": "1011.5360v2", "title": "The SINS survey of z~2 galaxy kinematics: properties of the giant star forming clumps", "url": "http://arxiv.org/pdf/1011.5360v2", "date": "2011-02-09 20:46:52", "abs": "We have studied the properties of giant star forming clumps in five z~2\nstar-forming disks with deep SINFONI AO spectroscopy at the ESO VLT. The clumps\nreside in disk regions where the Toomre Q-parameter is below unity, consistent\nwith their being bound and having formed from gravitational instability. Broad\nH{\\alpha}/[NII] line wings demonstrate that the clumps are launching sites of\npowerful outflows. The inferred outflow rates are comparable to or exceed the\nstar formation rates, in one case by a factor of eight. Typical clumps may lose\na fraction of their original gas by feedback in a few hundred million years,\nallowing them to migrate into the center. The most active clumps may lose much\nof their mass and disrupt in the disk. The clumps leave a modest imprint on the\ngas kinematics. Velocity gradients across the clumps are 10-40 km/s/kpc,\nsimilar to the galactic rotation gradients. Given beam smearing and clump\nsizes, these gradients may be consistent with significant rotational support in\ntypical clumps. Extreme clumps may not be rotationally supported; either they\nare not virialized, or they are predominantly pressure supported. The velocity\ndispersion is spatially rather constant and increases only weakly with star\nformation surface density. The large velocity dispersions may be driven by the\nrelease of gravitational energy, either at the outer disk/accreting streams\ninterface, and/or by the clump migration within the disk. Spatial variations in\nthe inferred gas phase oxygen abundance are broadly consistent with inside-out\ngrowing disks, and/or with inward migration of the clumps.", "cat": "astro-ph.CO", "authors": ["R. Genzel", "S. Newman", "T. Jones", "N. M. F\u00f6rster Schreiber", "K. Shapiro", "S. Genel", "S. J. Lilly", "A. Renzini", "L. J. Tacconi", "N. Bouch\u00e9", "A. Burkert", "G. Cresci", "P. Buschkamp", "C. M. Carollo", "D. Ceverino", "R. Davies", "A. Dekel", "F. Eisenhauer", "E. Hicks", "J. Kurk", "D. Lutz", "C. Mancini", "T. Naab", "Y. Peng", "A. Sternberg", "D. Vergani", "G. Zamorani"]}, "1511": {"id": "2404.13586v1", "title": "The PEPSI Exoplanet Transit Survey (PETS). V: New Na D transmission spectra indicate a quieter atmosphere on HD 189733b", "url": "http://arxiv.org/pdf/2404.13586v1", "date": "2024-04-21 08:53:57", "abs": "Absorption lines from exoplanet atmospheres observed in transmission allow us\nto study atmospheric characteristics such as winds. We present a new\nhigh-resolution transit time-series of HD 189733b, acquired with the PEPSI\ninstrument at the LBT and analyze the transmission spectrum around the Na D\nlines. We model the spectral signature of the RM-CLV-effect using synthetic\nPHOENIX spectra based on spherical LTE atmospheric models. We find a Na D\nabsorption signature between the second and third contact but not during the\ningress and egress phases, which casts doubt on the planetary origin of the\nsignal. Presupposing a planetary origin of the signal, the results suggest a\nweak day-to-nightside streaming wind in the order of 0.7 km/s and a moderate\nsuper-rotational streaming wind in the order of 3 - 4 km/s, challenging claims\nof prevailing strong winds on HD 189733b.", "cat": "astro-ph.EP", "authors": ["E. Keles", "S. Czesla", "K. Poppenhaeger", "P. Hauschildt", "T. A. Carroll", "I. Ilyin", "M. Baratella", "M. Steffen", "K. G. Strassmeier", "A. S. Bonomo", "B. S. Gaudi", "T. Henning", "M. C. Johnson", "K. Molaverdikhani", "V. Nascimbeni", "J. Patience", "A. Reiners", "G. Scandariato", "E. Schlawin", "E. Shkolnik", "D. Sicilia", "A. Sozzetti", "M. Mallonn", "C. Veillet", "J. Wang", "F. Yan"]}, "1512": {"id": "1807.11840v1", "title": "Open Source Android Vulnerability Detection Tools: A Survey", "url": "http://arxiv.org/pdf/1807.11840v1", "date": "2018-07-31 14:37:18", "abs": "Since last decade, smartphones have become an integral part of everyone's\nlife. Having the ability to handle many useful and attractive applications,\nsmartphones sport flawless functionality and small sizes leading to their\nexponential growth. Additionally, due to the huge user base and a wide range of\nfunctionalities, these mobile platforms have become a popular source of\ninformation to the public through several Apps provided by the DHS Citizen\nApplication Directory. Such wide audience to this platform is also making it a\nhuge target for cyber- attacks. While Android, the most popular open source\nmobile platform, has its base set of permissions to protect the device and\nresources, it does not provide a security framework to defend against any\nattack. This paper surveys threat, vulnerability and security analysis tools,\nwhich are open source in nature, for the Android platform and systemizes the\nknowledge of Android security mechanisms. Additionally, a comparison of three\npopular tools is presented.", "cat": "cs.CR", "authors": ["Keyur Kulkarni", "Ahmad Y Javaid"]}, "1513": {"id": "1810.10597v1", "title": "The speaker-independent lipreading play-off; a survey of lipreading machines", "url": "http://arxiv.org/pdf/1810.10597v1", "date": "2018-10-24 20:06:19", "abs": "Lipreading is a difficult gesture classification task. One problem in\ncomputer lipreading is speaker-independence. Speaker-independence means to\nachieve the same accuracy on test speakers not included in the training set as\nspeakers within the training set. Current literature is limited on\nspeaker-independent lipreading, the few independent test speaker accuracy\nscores are usually aggregated within dependent test speaker accuracies for an\naveraged performance. This leads to unclear independent results. Here we\nundertake a systematic survey of experiments with the TCD-TIMIT dataset using\nboth conventional approaches and deep learning methods to provide a series of\nwholly speaker-independent benchmarks and show that the best\nspeaker-independent machine scores 69.58% accuracy with CNN features and an SVM\nclassifier. This is less than state of the art speaker-dependent lipreading\nmachines, but greater than previously reported in independence experiments.", "cat": "cs.CV", "authors": ["Jake Burton", "David Frank", "Madhi Saleh", "Nassir Navab", "Helen L. Bear"]}, "1514": {"id": "1109.5698v1", "title": "The DEEP3 Galaxy Redshift Survey: The Impact of Environment on the Size Evolution of Massive Early-type Galaxies at Intermediate Redshift", "url": "http://arxiv.org/pdf/1109.5698v1", "date": "2011-09-26 20:00:02", "abs": "Using data drawn from the DEEP2 and DEEP3 Galaxy Redshift Surveys, we\ninvestigate the relationship between the environment and the structure of\ngalaxies residing on the red sequence at intermediate redshift. Within the\nmassive (10 < log(M*/Msun) < 11) early-type population at 0.4 < z <1.2, we find\na significant correlation between local galaxy overdensity (or environment) and\ngalaxy size, such that early-type systems in higher-density regions tend to\nhave larger effective radii (by ~0.5 kpc or 25% larger) than their counterparts\nof equal stellar mass and Sersic index in lower-density environments. This\nobserved size-density relation is consistent with a model of galaxy formation\nin which the evolution of early-type systems at z < 2 is accelerated in\nhigh-density environments such as groups and clusters and in which dry, minor\nmergers (versus mechanisms such as quasar feedback) play a central role in the\nstructural evolution of the massive, early-type galaxy population.", "cat": "astro-ph.CO", "authors": ["Michael C. Cooper", "Roger L. Griffith", "Jeffrey A. Newman", "Alison L. Coil", "Marc Davis", "Aaron A. Dutton", "S. M. Faber", "Puragra Guhathakurta", "David C. Koo", "Jennifer M. Lotz", "Benjamin J. Weiner", "Christopher N. A. Willmer", "Renbin Yan"]}, "1515": {"id": "1608.06483v1", "title": "The Sloan Digital Sky Survey Quasar Catalog: twelfth data release", "url": "http://arxiv.org/pdf/1608.06483v1", "date": "2016-08-23 12:31:44", "abs": "We present the Data Release 12 Quasar catalog (DR12Q) from the Baryon\nOscillation Spectroscopic Survey (BOSS) of the SDSS-III. This catalog includes\nall SDSS-III/BOSS objects that were spectroscopically targeted as quasar\ncandidates during the full survey and that are confirmed as quasars via visual\ninspection of the spectra, have luminosities Mi[z=2]<-20.5 (in a LCDM cosmology\nwith H_0 = 70 km/s/Mpc, Omega_M = 0.3, and Omega _L=0.7), and either display at\nleast one emission line with a full width at half maximum (FWHM)larger than 500\nkm/s or, if not, have interesting/complex absorption features. The catalog also\nincludes previously known quasars (mostly from SDSS-I and II) that were\nreobserved by BOSS. The catalog contains 297,301 quasars detected over 9,376\nsquare degrees with robust identification and redshift measured by a\ncombination of principal component eigenspectra. The number of quasars with\nz>2.15 is about an order of magnitude greater than the number of z>2.15 quasars\nknown prior to BOSS. Redshifts and FWHMs are provided for the strongest\nemission lines (CIV, CIII], MgII). The catalog identifies 29,580 broad\nabsorption line quasars and lists their characteristics. For each object, the\ncatalog presents five-band (u, g, r, i, z) CCD-based photometry together with\nsome information on the optical morphology and the selection criteria. When\navailable, the catalog also provides information on the optical variability of\nquasars using SDSS and PTF multi-epoch photometry. The catalog also contains\nX-ray, ultraviolet, near-infrared, and radio emission properties of the\nquasars, when available, from other large-area surveys. The calibrated digital\nspectra, covering the wavelength region 3,600-10,500A at a spectral resolution\nin the range 1,3005~\\mathrm{Gyr}$ to as high as $10~\\mathrm{Gyr}$. We combine MUSE data with\nliterature data to obtain an overall velocity dispersion of $\\sigma_{v} =\n7.07^{+1.29}_{-1.12}~\\mathrm{km\\ s^{-1}}$ for Leo T. When we divide the sample\nof stars into young and old populations, we find that they have distinct\nkinematics. Specifically, the young population has a velocity dispersion of\n$2.31^{+2.68}_{-1.65}\\,\\mathrm{km\\ s^{-1}}$, contrasting with that of the old\npopulation, of $8.14^{+1.66}_{-1.38}\\,\\mathrm{km\\ s^{-1}}$. The fact that the\nkinematics of the cold neutral gas is in good agreement with the kinematics of\nthe young population suggests that the recent star formation in Leo T is linked\nwith the cold neutral gas. We assess the existence of extended emission-line\nregions and find none to a surface brightness limit of~$< 1\\times\n10^{-20}\\,\\mathrm{erg}\\,\\mathrm{s}^{-1}\\,\\mathrm{cm}^{-2}~\\mathrm{arcsec}^{-2}$\nwhich corresponds to an upper limit on star formation of $\\sim\n10^{-11}~\\mathrm{M_\\odot~yr^{-1}~pc^{-2}}$, implying that the star formation in\nLeo T has ended.", "cat": "astro-ph.GA", "authors": ["Daniel Vaz", "Jarle Brinchmann", "Sebastiaan L. Zoutendijk", "Leindert A. Boogaard", "Sebastian Kamann", "Justin I. Read", "Martin M. Roth", "Peter M. Weilbacher", "Matthias Steinmetz"]}, "1520": {"id": "2109.06057v2", "title": "Unsupervised Person Re-Identification: A Systematic Survey of Challenges and Solutions", "url": "http://arxiv.org/pdf/2109.06057v2", "date": "2021-10-02 00:51:15", "abs": "Person re-identification (Re-ID) has been a significant research topic in the\npast decade due to its real-world applications and research significance. While\nsupervised person Re-ID methods achieve superior performance over unsupervised\ncounterparts, they can not scale to large unlabelled datasets and new domains\ndue to the prohibitive labelling cost. Therefore, unsupervised person Re-ID has\ndrawn increasing attention for its potential to address the scalability issue\nin person Re-ID. Unsupervised person Re-ID is challenging primarily due to\nlacking identity labels to supervise person feature learning. The corresponding\nsolutions are diverse and complex, with various merits and limitations.\nTherefore, comprehensive surveys on this topic are essential to summarise\nchallenges and solutions to foster future research. Existing person Re-ID\nsurveys have focused on supervised methods from classifications and\napplications but lack detailed discussion on how the person Re-ID solutions\naddress the underlying challenges. This survey review recent works on\nunsupervised person Re-ID from the perspective of challenges and solutions.\nSpecifically, we provide an in-depth analysis of highly influential methods\nconsidering the four significant challenges in unsupervised person Re-ID: 1)\nlacking ground-truth identity labels to supervise person feature learning; 2)\nlearning discriminative person features with pseudo-supervision; 3) learning\ncross-camera invariant person feature, and 4) the domain shift between\ndatasets. We summarise and analyse evaluation results and provide insights on\nthe effectiveness of the solutions. Finally, we discuss open issues and suggest\nsome promising future research directions.", "cat": "cs.CV", "authors": ["Xiangtan Lin", "Pengzhen Ren", "Chung-Hsing Yeh", "Lina Yao", "Andy Song", "Xiaojun Chang"]}, "1521": {"id": "2311.03731v2", "title": "A Survey of Large Language Models Attribution", "url": "http://arxiv.org/pdf/2311.03731v2", "date": "2023-12-14 09:31:50", "abs": "Open-domain generative systems have gained significant attention in the field\nof conversational AI (e.g., generative search engines). This paper presents a\ncomprehensive review of the attribution mechanisms employed by these systems,\nparticularly large language models. Though attribution or citation improve the\nfactuality and verifiability, issues like ambiguous knowledge reservoirs,\ninherent biases, and the drawbacks of excessive attribution can hinder the\neffectiveness of these systems. The aim of this survey is to provide valuable\ninsights for researchers, aiding in the refinement of attribution methodologies\nto enhance the reliability and veracity of responses generated by open-domain\ngenerative systems. We believe that this field is still in its early stages;\nhence, we maintain a repository to keep track of ongoing studies at\nhttps://github.com/HITsz-TMG/awesome-llm-attributions.", "cat": "cs.CL", "authors": ["Dongfang Li", "Zetian Sun", "Xinshuo Hu", "Zhenyu Liu", "Ziyang Chen", "Baotian Hu", "Aiguo Wu", "Min Zhang"]}, "1522": {"id": "1412.3209v1", "title": "The Structure and Stellar Content of the Outer Disks of Galaxies: A New View from the Pan-STARRS1 Medium Deep Survey", "url": "http://arxiv.org/pdf/1412.3209v1", "date": "2014-12-10 06:23:22", "abs": "We present the results of an analysis of Pan-STARRS1 Medium Deep Survey\nmulti-band (g,r,i,z,y) images of a sample of 698 low-redshift disk galaxies\nthat span broad ranges in stellar mass, star-formation rate, and bulge/disk\nratio. We use population synthesis SED fitting techniques to explore the radial\ndistribution of the light, color, surface mass density, mass/light ratio, and\nage of the stellar populations. We characterize the structure and stellar\ncontent of the galaxy disks out to radii of about twice Petrosian r90, beyond\nwhich the halo light becomes significant. We measure normalized radial profiles\nfor sub-samples of galaxies in three bins each of stellar mass and\nconcentration. We also fit radial profiles to each galaxy. The majority of\ngalaxies have down-bending radial surface brightness profiles in the bluer\nbands with a break radius at roughly r90. However, they typically show single\nunbroken exponentials in the reddest bands and in the stellar surface mass\ndensity. We find that the mass/light ratio and stellar age radial profiles have\na characteristic \"U-shape\". There is a good correlation between the amplitude\nof the down-bend in the surface brightness profile and the rate of the increase\nin the M/L ratio in the outer disk. As we move from late- to early-type\ngalaxies, the amplitude of the down-bend and the radial gradient in M/L both\ndecrease. Our results imply a combination of stellar radial migration and\nsuppression of recent star formation can account for the stellar populations of\nthe outer disk.", "cat": "astro-ph.GA", "authors": ["Z. Zheng", "D. Thilker", "T. Heckman", "G. Meurer", "W. Burgett", "K. Chambers", "M. Huber", "N. Kaiser", "E. Magnier", "N. Metcalfe", "P. Price", "J. Tonry", "R. Wainscoat", "C. Waters"]}, "1523": {"id": "1407.2970v1", "title": "Survey on counting special types of polynomials", "url": "http://arxiv.org/pdf/1407.2970v1", "date": "2014-07-10 21:25:48", "abs": "Most integers are composite and most univariate polynomials over a finite\nfield are reducible. The Prime Number Theorem and a classical result of\nGau{\\ss} count the remaining ones, approximately and exactly.\n For polynomials in two or more variables, the situation changes dramatically.\nMost multivariate polynomials are irreducible. This survey presents counting\nresults for some special classes of multivariate polynomials over a finite\nfield, namely the the reducible ones, the s-powerful ones (divisible by the\ns-th power of a nonconstant polynomial), the relatively irreducible ones\n(irreducible but reducible over an extension field), the decomposable ones, and\nalso for reducible space curves. These come as exact formulas and as\napproximations with relative errors that essentially decrease exponentially in\nthe input size.\n Furthermore, a univariate polynomial f is decomposable if f = g o h for some\nnonlinear polynomials g and h. It is intuitively clear that the decomposable\npolynomials form a small minority among all polynomials. The tame case, where\nthe characteristic p of Fq does not divide n = deg f, is fairly\nwell-understood, and we obtain closely matching upper and lower bounds on the\nnumber of decomposable polynomials. In the wild case, where p does divide n,\nthe bounds are less satisfactory, in particular when p is the smallest prime\ndivisor of n and divides n exactly twice. The crux of the matter is to count\nthe number of collisions, where essentially different (g, h) yield the same f.\nWe present a classification of all collisions at degree n = p^2 which yields an\nexact count of those decomposable polynomials.", "cat": "math.AC", "authors": ["Joachim von zur Gathen", "Konstantin Ziegler"]}, "1524": {"id": "2006.16867v2", "title": "Boosting Deep Neural Networks with Geometrical Prior Knowledge: A Survey", "url": "http://arxiv.org/pdf/2006.16867v2", "date": "2023-03-03 15:36:34", "abs": "Deep Neural Networks achieve state-of-the-art results in many different\nproblem settings by exploiting vast amounts of training data. However,\ncollecting, storing and - in the case of supervised learning - labelling the\ndata is expensive and time-consuming. Additionally, assessing the networks'\ngeneralization abilities or predicting how the inferred output changes under\ninput transformations is complicated since the networks are usually treated as\na black box. Both of these problems can be mitigated by incorporating prior\nknowledge into the neural network. One promising approach, inspired by the\nsuccess of convolutional neural networks in computer vision tasks, is to\nincorporate knowledge about symmetric geometrical transformations of the\nproblem to solve that affect the output in a predictable way. This promises an\nincreased data efficiency and more interpretable network outputs. In this\nsurvey, we try to give a concise overview about different approaches that\nincorporate geometrical prior knowledge into neural networks. Additionally, we\nconnect those methods to 3D object detection for autonomous driving, where we\nexpect promising results when applying those methods.", "cat": "cs.CV", "authors": ["Matthias Rath", "Alexandru Paul Condurache"]}, "1525": {"id": "1601.06513v1", "title": "The Gaia-ESO Survey: membership and Initial Mass Function of the Gamma Velorum cluster", "url": "http://arxiv.org/pdf/1601.06513v1", "date": "2016-01-25 08:51:05", "abs": "Understanding the properties of young open clusters, such as the Initial Mass\nFunction (IMF), star formation history and dynamic evolution, is crucial to\nobtain reliable theoretical predictions of the mechanisms involved in the star\nformation process. We want to obtain a list, as complete as possible, of\nconfirmed members of the young open cluster Gamma Velorum, with the aim of\nderiving general cluster properties such as the IMF. We used all available\nspectroscopic membership indicators within the Gaia-ESO public archive together\nwith literature photometry and X-ray data and, for each method, we derived the\nmost complete list of candidate cluster members. Then, we considered\nphotometry, gravity and radial velocities as necessary conditions to select a\nsubsample of candidates whose membership was confirmed by using the lithium and\nH$\\alpha$ lines and X-rays as youth indicators. We found 242 confirmed and 4\npossible cluster members for which we derived masses using very recent stellar\nevolutionary models. The cluster IMF in the mass range investigated in this\nstudy shows a slope of $\\alpha=2.6\\pm0.5$ for $0.521.0. These abundance\ndiscrepancies are independent of their line-of-sight velocity separation from\nthe host quasar, and the velocity width of the metal lines (v90). Contrary to\nprevious studies, MDLAs show no difference in [alpha/Fe] relative to single\nDLAs matched in metallicity and redshift. In addition, we present follow-up\nUVES data of J0034+1639, a sightline containing three DLAs, including a\nmetal-poor DLA with [Fe/H]=-2.82 (the third lowest [Fe/H] in DLAs identified to\ndate) at z=4.25. Lastly we study the dust-corrected [Zn/Fe], emphasizing that\nnear-IR coverage of X-Shooter provides unprecedented access to MgII, CaII and\nTiII lines (at redshifts 3-4) to provide additional evidence for subsolar\n[Zn/Fe] ratio in DLAs.", "cat": "astro-ph.GA", "authors": ["T. A. M. Berg", "S. L. Ellison", "R. Sanchez-Ramirez", "J. X. Prochaska", "S. Lopez", "V. D'Odorico", "G. Becker", "L. Christensen", "G. Cupani", "K. Denney", "G. Worseck"]}, "1529": {"id": "1410.8214v2", "title": "Detection of hot, metal-enriched outflowing gas around $z\\approx\\,$2.3 star-forming galaxies in the Keck Baryonic Structure Survey", "url": "http://arxiv.org/pdf/1410.8214v2", "date": "2015-04-25 13:16:12", "abs": "We use quasar absorption lines to study the physical conditions in the\ncircumgalactic medium of redshift $z\\approx 2.3$ star-forming galaxies taken\nfrom the Keck Baryonic Structure Survey (KBSS). In Turner et al. 2014 we used\nthe pixel optical depth technique to show that absorption by HI and the metal\nions OVI, NV, CIV, CIII and SiIV is strongly enhanced within $|\\Delta\nv|\\lesssim170$ km/s and projected distances $|d|\\lesssim180$ proper kpc from\nsightlines to the background quasars. Here we demonstrate that the OVI\nabsorption is also strongly enhanced at fixed HI, CIV, and SiIV optical depths,\nand that this enhancement extends out to $\\sim350$ km/s. At fixed HI the\nincrease in the median OVI optical depth near galaxies is 0.3-0.7 dex and is\ndetected at 2--3-$\\sigma$ confidence for all seven HI bins that have\n$\\log_{10}\\tau_{\\rm HI}\\ge-1.5$. We use ionization models to show that the\nobserved strength of OVI as a function of HI is consistent with enriched,\nphotoionized gas for pixels with $\\tau_{\\rm HI}\\gtrsim10$. However, for pixels\nwith $\\tau_{\\rm HI} \\lesssim 1$ this would lead to implausibly high\nmetallicities at low densities if the gas were photoionized by the background\nradiation. This indicates that the galaxies are surrounded by gas that is\nsufficiently hot to be collisionally ionized ($T > 10^5\\,$K) and that a\nsubstantial fraction of the hot gas has a metallicity $\\gtrsim 10^{-1}$ of\nsolar. Given the high metallicity and large velocity extent (out to\n$\\sim1.5\\times v_{\\rm circ}$) of this gas, we conclude that we have detected\nhot, metal enriched outflows arising from star-forming galaxies.", "cat": "astro-ph.GA", "authors": ["Monica L. Turner", "Joop Schaye", "Charles C. Steidel", "Gwen C. Rudie", "Allison L. Strom"]}, "1530": {"id": "2205.12498v1", "title": "A Survey of Graph-Theoretic Approaches for Analyzing the Resilience of Networked Control Systems", "url": "http://arxiv.org/pdf/2205.12498v1", "date": "2022-05-25 05:16:19", "abs": "As the scale of networked control systems increases and interactions between\ndifferent subsystems become more sophisticated, questions of the resilience of\nsuch networks increase in importance. The need to redefine classical system and\ncontrol-theoretic notions using the language of graphs has recently started to\ngain attention as a fertile and important area of research. This paper presents\nan overview of graph-theoretic methods for analyzing the resilience of\nnetworked control systems. We discuss various distributed algorithms operating\non networked systems and investigate their resilience against adversarial\nactions by looking at the structural properties of their underlying networks.\nWe present graph-theoretic methods to quantify the attack impact, and\nreinterpret some system-theoretic notions of robustness from a graph-theoretic\nstandpoint to mitigate the impact of the attacks. Moreover, we discuss\nmiscellaneous problems in the security of networked control systems which use\ngraph-theory as a tool in their analyses. We conclude by introducing some\navenues for further research in this field.", "cat": "eess.SY", "authors": ["Mohammad Pirani", "Aritra Mitra", "Shreyas Sundaram"]}, "1531": {"id": "2004.06457v2", "title": "A null test of the equivalence principle using relativistic effects in galaxy surveys", "url": "http://arxiv.org/pdf/2004.06457v2", "date": "2021-12-09 14:26:59", "abs": "The weak equivalence principle is one of the cornerstone of general\nrelativity. Its validity has been tested with impressive precision in the Solar\nSystem, with experiments involving baryonic matter and light. However, on\ncosmological scales and when dark matter is concerned, the validity of this\nprinciple is still unknown. In this paper we construct a null test that probes\nthe validity of the equivalence principle for dark matter. Our test has the\nstrong advantage that it can be applied on data without relying on any\nmodelling of the theory of gravity. It involves a combination of redshift-space\ndistortions and relativistic effects in the galaxy number-count fluctuation,\nthat vanishes if and only if the equivalence principle holds. We show that the\nnull test is very insensitive to typical uncertainties in other cosmological\nparameters, including the magnification bias parameter, and to non-linear\neffects, making this a robust null test for modified gravity.", "cat": "astro-ph.CO", "authors": ["Camille Bonvin", "Felipe Oliveira Franco", "Pierre Fleury"]}, "1532": {"id": "1608.01163v1", "title": "The survey operation software system development for Prime Focus Spectrograph (PFS) on Subaru Telescope", "url": "http://arxiv.org/pdf/1608.01163v1", "date": "2016-08-03 12:31:26", "abs": "The Prime Focus Spectrograph (PFS) is a wide-field, multi-object spectrograph\naccommodating 2394 fibers to observe the sky at the prime focus of the Subaru\ntelescope. The software system to operate a spectroscopic survey is structured\nby the four packages: Instrument control software, exposure targeting software,\ndata reduction pipeline, and survey planning and tracking software. In\naddition, we operate a database system where various information such as\nproperties of target objects, instrument configurations, and observation\nconditions is stored and is organized via a standardized data model for future\nreferences to update survey plans and to scientific researches. In this\narticle, we present an overview of the software system and describe the\nworkflows that need to be performed in the PFS operation, with some highlights\non the database that organizes various information from sub-processes in the\nsurvey operation, and on the process of fiber configuration from the software\nperspectives.", "cat": "astro-ph.IM", "authors": ["Atsushi Shimono", "Naoyuki Tamura", "Naruhisa Takato", "Naoki Yasuda", "Nao Suzuki", "Craig P. Loomis", "Robert H. Lupton", "Yuki Moritani", "Kiyoto Yabe"]}, "1533": {"id": "2004.10230v1", "title": "The Star Formation in Radio Survey: 3 - 33 GHz Imaging of Nearby Galaxy Nuclei and Extranuclear Star-forming Regions", "url": "http://arxiv.org/pdf/2004.10230v1", "date": "2020-04-21 18:29:13", "abs": "We present 3, 15, and 33 GHz imaging towards galaxy nuclei and extranuclear\nstar-forming regions using the Karl G. Jansky Very Large Array as part of the\nStar Formation in Radio Survey. With $3-33$ GHz radio spectra, we measured the\nspectral indices and corresponding thermal (free-free) emission fractions for a\nsample of 335 discrete regions having significant detections in at least two\nradio bands. After removing 14 likely background galaxies, we find that the\nmedian thermal fraction at 33 GHz is $92 \\pm 0.8\\%$ with a median absolute\ndeviation of $11\\%$, when a two-component power-law model is adopted to fit the\nradio spectrum. Limiting the sample to 238 sources that are confidently\nidentified as star-forming regions, and not affected by potential AGN\ncontamination (i.e., having galactocentric radii $r_{\\rm G} \\geq 250$ pc),\nresults in a median thermal fraction of $93 \\pm 0.8 \\%$ with a median absolute\ndeviation of $10\\%$. We further measure the thermal fraction at 33 GHz for 163\nregions identified at 7\" resolution to be $94 \\pm 0.8 \\%$ with a median\nabsolute deviation of $8\\%$. Together, these results confirm that free-free\nemission dominates the radio spectra of star-forming regions on scales up to\n$\\sim$500 pc in normal star-forming galaxies. We additionally find a factor of\n$\\sim$1.6 increase in the scatter of the measured spectral index and thermal\nfraction distributions as a function of decreasing galactocentric radius. This\ntrend is likely reflective of the continuous star-formation activity occurring\nin the galaxy centers, resulting a larger contribution of diffuse nonthermal\nemission relative to star-forming regions in the disk.", "cat": "astro-ph.GA", "authors": ["S. T. Linden", "E. J. Murphy", "D. Dong", "E. Momjian", "R. C. Kennicutt Jr.", "D. S. Meier", "E. Schinnerer", "J. L. Turner"]}, "1534": {"id": "2008.13413v2", "title": "A comprehensive survey on smart contract construction and execution: paradigms, tools, and systems", "url": "http://arxiv.org/pdf/2008.13413v2", "date": "2021-02-13 10:21:22", "abs": "Smart contracts are regarded as one of the most promising and appealing\nnotions in blockchain technology. Their self-enforcing and event-driven\nfeatures make some online activities possible without a trusted third party.\nNevertheless, problems such as miscellaneous attacks, privacy leakage, and low\nprocessing rates pre-vent them from being widely applied. Various schemes and\ntools have been proposed to facilitate the construction and execution of secure\nsmart contracts. However, a comprehensive survey for these proposals is absent,\nhindering new researchers and developers from a quick start. This paper surveys\nthe literature and online resources on smart contract construction and\nexecution over the period 2008-2020. We divide the studies into three\ncategories: (1) design paradigms that give examples and patterns on contract\nconstruction, (2) design tools that facilitate the development of secure smart\ncontracts, and (3) extensions and alternatives that improve the privacy or\nefficiency of the system. We start by grouping the relevant construction\nschemes into the first two categories. We then review the execution mechanisms\nin the last category and further divide the state-of-the-art solutions into\nthree classes: private contracts with extra tools, off-chain channels, and\nextensions on core functionalities. Finally, we summarize several challenges\nand identify future research directions toward developing secure,\nprivacy-preserving, and efficient smart contracts.", "cat": "cs.CR", "authors": ["Bin Hu", "Zongyang Zhang", "Jianwei Liu", "Yizhong Liu", "Jiayuan Yin", "Rongxing Lu", "Xiaodong Lin"]}, "1535": {"id": "2012.00750v1", "title": "Identification of AKARI infrared sources by Deep HSC Optical Survey: Construction of New Band-Merged Catalogue in the NEP-Wide field", "url": "http://arxiv.org/pdf/2012.00750v1", "date": "2020-12-01 10:35:57", "abs": "The north ecliptic pole (NEP) field is a natural deep field location for many\nsatellite observations. It has been targeted manytimes since it was surveyed by\nthe AKARI space telescope with its unique wavelength coverage from the near- to\nmid-infrared(mid-IR). Many follow-up observations have been carried out and\nmade this field one of the most frequently observed areas witha variety of\nfacilities, accumulating abundant panchromatic data from X-ray to radio\nwavelength range. Recently, a deep opticalsurvey with the Hyper Suprime-Cam\n(HSC) at the Subaru telescope covered the NEP-Wide (NEPW) field, which enabled\nus toidentify faint sources in the near- and mid-IR bands, and to improve the\nphotometric redshift (photo-z) estimation. In this work,we present newly\nidentified AKARI sources by the HSC survey, along with multi-band photometry\nfor 91,861 AKARI sourcesobserved over the NEPW field. We release a new\nband-merged catalogue combining various photometric data from GALEXUV to the\nsubmillimetre (sub-mm) bands (e.g., Herschel/SPIRE, JCMT/SCUBA-2). About 20,000\nAKARI sources are newlymatched to the HSC data, most of which seem to be faint\ngalaxies in the near- to mid-infrared AKARI bands. This cataloguemotivates a\nvariety of current research, and will be increasingly useful as recently\nlaunched (eROSITA/ART-XC) and futurespace missions (such as JWST, Euclid, and\nSPHEREx) plan to take deep observations in the NEP field.", "cat": "astro-ph.GA", "authors": ["Seong Jin Kim", "Nagisa Oi", "Tomotsugu Goto", "Hiroyuki Ikeda", "Simon C. -C. Ho", "Hyunjin Shim", "Yoshiki Toba", "Ho Seong Hwang", "Tetsuya Hashimoto", "Laia Barrufet", "Matthew Malkan", "Helen K. Kim", "Ting-Chi Huang", "Hideo Matsuhara", "Takamitsu Miyaji", "Chris Pearson", "Stephen Serjeant", "Daryl Joe Santos", "Eunbin Kim", "Agnieszka Pollo", "Woong-Seob Jeong", "Ting-Wen Wang", "Rieko Momose", "Toshinobu Takagi"]}, "1536": {"id": "1904.07695v1", "title": "Short Text Topic Modeling Techniques, Applications, and Performance: A Survey", "url": "http://arxiv.org/pdf/1904.07695v1", "date": "2019-04-13 09:08:46", "abs": "Analyzing short texts infers discriminative and coherent latent topics that\nis a critical and fundamental task since many real-world applications require\nsemantic understanding of short texts. Traditional long text topic modeling\nalgorithms (e.g., PLSA and LDA) based on word co-occurrences cannot solve this\nproblem very well since only very limited word co-occurrence information is\navailable in short texts. Therefore, short text topic modeling has already\nattracted much attention from the machine learning research community in recent\nyears, which aims at overcoming the problem of sparseness in short texts. In\nthis survey, we conduct a comprehensive review of various short text topic\nmodeling techniques proposed in the literature. We present three categories of\nmethods based on Dirichlet multinomial mixture, global word co-occurrences, and\nself-aggregation, with example of representative approaches in each category\nand analysis of their performance on various tasks. We develop the first\ncomprehensive open-source library, called STTM, for use in Java that integrates\nall surveyed algorithms within a unified interface, benchmark datasets, to\nfacilitate the expansion of new methods in this research field. Finally, we\nevaluate these state-of-the-art methods on many real-world datasets and compare\ntheir performance against one another and versus long text topic modeling\nalgorithm.", "cat": "cs.IR", "authors": ["Qiang Jipeng", "Qian Zhenyu", "Li Yun", "Yuan Yunhao", "Wu Xindong"]}, "1537": {"id": "2006.14961v3", "title": "A statistical standard siren measurement of the Hubble constant from the LIGO/Virgo gravitational wave compact object merger GW190814 and Dark Energy Survey galaxies", "url": "http://arxiv.org/pdf/2006.14961v3", "date": "2020-12-28 17:45:02", "abs": "We present a measurement of the Hubble constant $H_0$ using the gravitational\nwave (GW) event GW190814, which resulted from the coalescence of a 23 $M_\\odot$\nblack hole with a 2.6 $M_\\odot$ compact object, as a standard siren. No\ncompelling electromagnetic counterpart has been identified for this event, thus\nour analysis accounts for thousands of potential host galaxies within a\nstatistical framework. The redshift information is obtained from the\nphotometric redshift (photo-$z$) catalog from the Dark Energy Survey. The\nluminosity distance is provided by the LIGO/Virgo gravitational wave sky map.\nSince this GW event has the second-smallest localization volume after GW170817,\nGW190814 is likely to provide the best constraint on cosmology from a single\nstandard siren without identifying an electromagnetic counterpart. Our analysis\nuses photo-$z$ probability distribution functions and corrects for photo-$z$\nbiases. We also reanalyze the binary-black hole GW170814 within this updated\nframework. We explore how our findings impact the $H_0$ constraints from\nGW170817, the only GW merger associated with a unique host galaxy. From a\ncombination of GW190814, GW170814 and GW170817, our analysis yields $H_0 =\n72.0^{+ 12}_{- 8.2 }~{\\rm km~s^{-1}~Mpc^{-1}}$ (68\\% Highest Density Interval,\nHDI) for a prior in $H_0$ uniform between $[20,140]~{\\rm km~s^{-1}~Mpc^{-1}}$.\nThe addition of GW190814 and GW170814 to GW170817 improves the 68\\% HDI from\nGW170817 alone by $\\sim 18\\%$, showing how well-localized mergers without\ncounterparts can provide a significant contribution to standard siren\nmeasurements, provided that a complete galaxy catalog is available at the\nlocation of the event.", "cat": "astro-ph.CO", "authors": ["A. Palmese", "J. deVicente", "M. E. S. Pereira", "J. Annis", "W. Hartley", "K. Herner", "M. Soares-Santos", "M. Crocce", "D. Huterer", "I. Magana Hernandez", "T. M. Davis", "A. Garcia", "J. Garcia-Bellido", "J. Gschwend", "D. E. Holz", "R. Kessler", "O. Lahav", "R. Morgan", "C. Nicolaou", "C. Conselice", "R. J. Foley", "M. S. S. Gill", "T. M. C. Abbott", "M. Aguena", "S. Allam", "S. Avila", "K. Bechtol", "E. Bertin", "S. Bhargava", "D. Brooks", "E. Buckley-Geer", "D. L. Burke", "M. Carrasco Kind", "J. Carretero", "F. J. Castander", "C. Chang", "M. Costanzi", "L. N. da Costa", "S. Desai", "H. T. Diehl", "P. Doel", "J. Estrada", "S. Everett", "A. E. Evrard", "E. Fernandez", "D. A. Finley", "B. Flaugher", "P. Fosalba", "J. Frieman", "E. Gaztanaga", "D. W. Gerdes", "D. Gruen", "R. A. Gruendl", "G. Gutierrez", "S. R. Hinton", "D. L. Hollowood", "K. Honscheid", "D. J. James", "S. Kent", "E. Krause", "K. Kuehn", "H. Lin", "M. A. G. Maia", "M. March", "J. L. Marshall", "P. Melchior", "F. Menanteau", "R. Miquel", "R. L. C. Ogando", "F. Paz-Chinchon", "A. A. Plazas", "A. Roodman", "M. Sako", "E. Sanchez", "V. Scarpine", "M. Schubnell", "S. Serrano", "I. Sevilla-Noarbe", "J. Allyn Smith", "M. Smith", "E. Suchyta", "G. Tarle", "M. A. Troxel", "D. L. Tucker", "A. R. Walker", "W. Wester", "R. D. Wilkinson", "J. Zuntz"]}, "1538": {"id": "1709.03512v1", "title": "Extragalactic VLBI surveys in the MeerKAT era", "url": "http://arxiv.org/pdf/1709.03512v1", "date": "2017-09-11 18:00:04", "abs": "The past decade has seen significant advances in cm-wave VLBI extragalactic\nobservations due to a wide range of technical successes, including the increase\nin processed field-of-view and bandwidth. The future inclusion of MeerKAT into\nglobal VLBI networks would provide further enhancement, particularly the\ndramatic sensitivity boost to >7000 km baselines. This will not be without its\nlimitations, however, considering incomplete MeerKAT band overlap with current\nVLBI arrays and the small (real-time) field-of-view afforded by the phased up\nMeerKAT array. We provide a brief overview of the significant contributions\nMeerKAT-VLBI could make, with an emphasis on the scientific output of several\nMeerKAT extragalactic Large Survey Projects.", "cat": "astro-ph.IM", "authors": ["Roger P. Deane"]}, "1539": {"id": "2305.16616v2", "title": "Channel Measurement, Modeling, and Simulation for 6G: A Survey and Tutorial", "url": "http://arxiv.org/pdf/2305.16616v2", "date": "2024-03-28 08:06:24", "abs": "The sixth generation (6G) mobile communications have attracted substantial\nattention in the global research community of information and communication\ntechnologies (ICT). 6G systems are expected to support not only extended 5G\nusage scenarios, but also new usage scenarios, such as integrated sensing and\ncommunication (ISAC), integrated artificial intelligence (AI) and\ncommunication, and communication and ubiquitous connectivity. To realize this\ngoal, channel characteristics must be comprehensively studied and properly\nexploited, so as to promote the design, standardization, and optimization of 6G\nsystems. In this paper, we first summarize the requirements and challenges in\n6G channel research. Our focus is on channels for five promising technologies\nenabling 6G, including terahertz (THz), extreme MIMO (E-MIMO), ISAC,\nreconfigurable intelligent surface (RIS), and space-air-ground integrated\nnetwork (SAGIN). Then, a survey of the progress of the 6G channel research\nregarding the above five promising technologies is presented in terms of the\nlatest measurement campaigns, new characteristics, modeling methods, and\nresearch prospects. Moreover, a tutorial on the 6G channel simulations is\npresented. We introduce the BUPTCMG- 6G, a 6G link-level channel simulator,\ndeveloped based on the ITU/3GPP 3D geometry-based stochastic model (GBSM)\nmethodology. The simulator supports the channel simulation of the\naforementioned 6G potential technologies. To facilitate the use of the\nsimulator, the tutorial encompasses the design framework, user guidelines, and\napplication examples. This paper offers in-depth, hands-on insights into the\nbest practices of channel measurements, modeling, and simulations for the\nevaluation of 6G technologies, the development of 6G standards, and the\nimplementation and optimization of 6G systems.", "cat": "eess.SP", "authors": ["Jianhua Zhang", "Jiaxin Lin", "Pan Tang", "Yuxiang Zhang", "Huixin Xu", "Tianyang Gao", "Haiyang Miao", "Zeyong Chai", "Zhengfu Zhou", "Yi Li", "Huiwen Gong", "Yameng Liu", "Zhiqiang Yuan", "Lei Tian", "Shaoshi Yang", "Liang Xia", "Guangyi Liu", "Ping Zhang"]}, "1540": {"id": "2112.03426v1", "title": "A Survey of Verification, Validation and Testing Solutions for Smart Contracts", "url": "http://arxiv.org/pdf/2112.03426v1", "date": "2021-12-07 00:00:34", "abs": "Smart contracts are programs stored on a blockchain that run when\npredetermined conditions are met. However, designing and implementing a smart\ncontract is not trivial since upon deployment on a blockchain, it is no longer\npossible to modify it (neither for improving nor for bug fixing). It is only\npossible by deploying a new version of the smart contract which is costly\n(deployment cost for the new contract and destruction cost for the old\ncontract). To this end, there are many solutions for testing the smart\ncontracts before their deployment. Since realizing bug-free smart contracts\nincrease the reliability, as well as reduce the cost, testing is an essential\nactivity. In this paper, we group the existing solutions that attempt to tackle\nsmart contract testing into following categories: public test networks,\nsecurity analysis tools, blockchain emulators and blockchain simulators. Then,\nwe analyze these solutions, categorize them and show what their pros and cons\nare.", "cat": "cs.SE", "authors": ["Cha\u00efmaa Benabbou", "\u00d6nder G\u00fcrcan"]}, "1541": {"id": "1808.02320v1", "title": "A Survey of Refactoring Detection Techniques Based on Change History Analysis", "url": "http://arxiv.org/pdf/1808.02320v1", "date": "2018-08-07 12:24:21", "abs": "Refactoring is the process of changing a software system in such a way that\nit does not alter the external behavior of the code yet improves its internal\nstructure. Not only researchers, but also practitioners, need to know about\npast refactoring instances performed in a software development project. So far,\na number of techniques have been proposed for automatic detection of\nrefactoring instances. Those techniques have been presented in various\ninternational conferences and journals, however, it is difficult for\nresearchers and practitioners to grasp the current status of studies on\nrefactoring detection techniques. In this survey paper, we review various\nrefactoring detection techniques, especially techniques based on change history\nanalysis. First, we give the definition and categorization of refactoring\ndetection methods in this paper, and then introduce refactoring detection\ntechniques based on change history analysis. Finally, we discuss possible\nfuture research directions for refactoring detection.", "cat": "cs.SE", "authors": ["Eunjong Choi", "Kenji Fujiwara", "Norihiro Yoshida", "Shinpei Hayashi"]}, "1542": {"id": "2105.03212v1", "title": "A global view on star formation: The GLOSTAR Galactic plane survey IV. Radio continuum detections of young stellar objects in the Galactic Centre region", "url": "http://arxiv.org/pdf/2105.03212v1", "date": "2021-05-07 12:33:23", "abs": "The Central Molecular Zone (CMZ), a $\\sim$200 pc sized region around the\nGalactic Centre, is peculiar in that it shows a star formation rate (SFR) that\nis suppressed with respect to the available dense gas. To study the SFR in the\nCMZ, young stellar objects (YSOs) can be investigated. Here we present radio\nobservations of 334 2.2 $\\mu$m infrared sources that have been identified as\nYSO candidates. Our goal is to investigate the presence of centimetre\nwavelength radio continuum counterparts to this sample of YSO candidates which\nwe use to constrain the current SFR in the CMZ. As part of the GLOSTAR survey,\nD-configuration VLA data was obtained for the Galactic Centre, covering\n-2$^{\\circ} 120h^-1Mpc or k\n< 0.01hMpc^-1. We find that these errors can be ameliorated by weighting\ngalaxies based on their surface brightness and the local stellar density. We\nuse mock galaxy catalogs that simulate the CMASS selection function to\ndetermine that randomly selecting galaxy redshifts in order to simulate the\nradial selection function of a random sample imparts the least systematic error\non correlation function measurements and that this systematic error is\nnegligible for the spherically averaged correlation function. The methods we\nrecommend for the calculation of clustering measurements using the CMASS sample\nare adopted in companion papers that locate the position of the baryon acoustic\noscillation feature (Anderson et al. 2012), constrain cosmological models using\nthe full shape of the correlation function (Sanchez et al. 2012), and measure\nthe rate of structure growth (Reid et al. 2012). (abridged)", "cat": "astro-ph.CO", "authors": ["Ashley J. Ross", "Will J. Percival", "Ariel G. Sanchez", "Lado Samushia", "Shirley Ho", "Eyal Kazin", "Marc Manera", "Beth Reid", "Martin White", "Rita Tojeiro", "Cameron K. McBride", "Xiaoying Xu", "David A. Wake", "Michael A. Strauss", "Francesco Montesano", "Molly E. C. Swanson", "Stephen Bailey", "Adam S. Bolton", "Antonio Montero Dorta", "Daniel J. Eisenstein", "Hong Guo", "Jean-Christophe Hamilton", "Robert C. Nichol", "Nikhil Padmanabhan", "Francisco Prada", "David J. Schlegel", "Mariana Vargas Magana", "Idit Zehavi", "Michael Blanton", "Dmitry Bizyaev", "Howard Brewington", "Antonio J. Cuesta", "Elena Malanushenko", "Viktor Malanushenko", "Daniel Oravetz", "John Parejko", "Kaike Pan", "Donald P. Schneider Alaina Shelden", "Audrey Simmons", "Stephanie Snedden", "Gong-bo Zhao"]}, "1545": {"id": "1107.2759v1", "title": "The VLA Survey of the Chandra Deep Field South. V. Evolution and Luminosity Functions of sub-mJy radio sources and the issue of radio emission in radio-quiet AGN", "url": "http://arxiv.org/pdf/1107.2759v1", "date": "2011-07-14 09:09:09", "abs": "We present the evolutionary properties and luminosity functions of the radio\nsources belonging to the Chandra Deep Field South VLA survey, which reaches a\nflux density limit at 1.4 GHz of 43 microJy at the field center and redshift\n~5, and which includes the first radio-selected complete sample of radio-quiet\nactive galactic nuclei (AGN). We use a new, comprehensive classification scheme\nbased on radio, far- and near-IR, optical, and X-ray data to disentangle\nstar-forming galaxies from AGN and radio-quiet from radio-loud AGN. We confirm\nour previous result that star-forming galaxies become dominant only below 0.1\nmJy. The sub-mJy radio sky turns out to be a complex mix of star-forming\ngalaxies and radio-quiet AGN evolving at a similar, strong rate; non-evolving\nlow-luminosity radio galaxies; and declining radio powerful (P > 3 10^24 W/Hz)\nAGN. Our results suggest that radio emission from radio-quiet AGN is closely\nrelated to star formation. The detection of compact, high brightness\ntemperature cores in several nearby radio-quiet AGN can be explained by the\nco-existence of two components, one non-evolving and AGN-related and one\nevolving and star-formation-related. Radio-quiet AGN are an important class of\nsub-mJy sources, accounting for ~30% of the sample and ~60% of all AGN, and\noutnumbering radio-loud AGN at < 0.1 mJy. This implies that future, large area\nsub-mJy surveys, given the appropriate ancillary multi-wavelength data, have\nthe potential of being able to assemble vast samples of radio-quiet AGN\nby-passing the problems of obscuration, which plague the optical and soft X-ray\nbands.", "cat": "astro-ph.CO", "authors": ["P. Padovani", "N. Miller", "K. I. Kellermann", "V. Mainieri", "P. Rosati", "P. Tozzi"]}, "1546": {"id": "1211.5140v2", "title": "Extended Hot Halos Around Isolated Galaxies Observed in the ROSAT All-Sky Survey", "url": "http://arxiv.org/pdf/1211.5140v2", "date": "2012-12-07 21:28:22", "abs": "We place general constraints on the luminosity and mass of hot X-ray emitting\ngas residing in extended \"hot halos\" around nearby massive galaxies. We examine\nstacked images of 2165 galaxies from the 2MASS Very Isolated Galaxy Catalog\n(2MVIG), as well as subsets of this sample based on galaxy morphology and\nK-band luminosity. We detect X-ray emission at high confidence (ranging up to\nnearly 10\\sigma) for each subsample of galaxies. The average L_X within 50 kpc\nis 1.0\\pm0.1 (statistical) \\pm0.2 (systematic) x10^40 erg/s, although the\nearly-type galaxies are more than twice as luminous as the late-type galaxies.\nUsing a spatial analysis, we also find evidence for extended emission around\nfive out of seven subsamples (the full sample, the luminous galaxies,\nearly-type galaxies, luminous late-type galaxies, and luminous early-type\ngalaxies) at 92.7%, 99.3%, 89.3%, 98.7%, and 92.1% confidence, respectively.\nSeveral additional lines of evidence also support this conclusion and suggest\nthat about 1/2 of the total emission is extended, and about 1/3 of the extended\nemission comes from hot gas. For the sample of luminous galaxies, which has the\nstrongest evidence for extended emission, the average hot gas mass is 4x10^9\nMsun within 50 kpc and the implied accretion rate is 0.4 Msun/yr.", "cat": "astro-ph.CO", "authors": ["Michael E. Anderson", "Joel N. Bregman", "Xinyu Dai"]}, "1547": {"id": "2202.09363v1", "title": "Towards Digital Twin Oriented Modelling of Complex Networked Systems and Their Dynamics: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2202.09363v1", "date": "2022-02-15 15:44:00", "abs": "This paper aims to provide a comprehensive critical overview on how entities\nand their interactions in Complex Networked Systems (CNS) are modelled across\ndisciplines as they approach their ultimate goal of creating a Digital Twin\n(DT) that perfectly matches the reality. We propose a new framework to\nconceptually compare diverse existing modelling paradigms from different\nperspectives and create unified assessment criteria to assess their respective\ncapabilities of reaching such an ultimate goal. Using the proposed criteria, we\nalso appraise how far the reviewed current state-of-the-art approaches are from\nthe idealised DTs. We also identify and propose potential directions and ways\nof building a DT-orientated CNS based on the convergence and integration of CNS\nand DT utilising a variety of cross-disciplinary techniques.", "cat": "eess.SY", "authors": ["Jiaqi Wen", "Bogdan Gabrys", "Katarzyna Musial"]}, "1548": {"id": "1811.02374v4", "title": "First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey: Constraints on Cosmological Parameters", "url": "http://arxiv.org/pdf/1811.02374v4", "date": "2019-05-10 14:18:10", "abs": "We present the first cosmological parameter constraints using measurements of\ntype Ia supernovae (SNe Ia) from the Dark Energy Survey Supernova Program\n(DES-SN). The analysis uses a subsample of 207 spectroscopically confirmed SNe\nIa from the first three years of DES-SN, combined with a low-redshift sample of\n122 SNe from the literature. Our \"DES-SN3YR\" result from these 329 SNe Ia is\nbased on a series of companion analyses and improvements covering SN Ia\ndiscovery, spectroscopic selection, photometry, calibration, distance bias\ncorrections, and evaluation of systematic uncertainties. For a flat LCDM model\nwe find a matter density Omega_m = 0.331 +_ 0.038. For a flat wCDM model, and\ncombining our SN Ia constraints with those from the cosmic microwave background\n(CMB), we find a dark energy equation of state w = -0.978 +_ 0.059, and Omega_m\n= 0.321 +_ 0.018. For a flat w0waCDM model, and combining probes from SN Ia,\nCMB and baryon acoustic oscillations, we find w0 = -0.885 +_ 0.114 and wa =\n-0.387 +_ 0.430. These results are in agreement with a cosmological constant\nand with previous constraints using SNe Ia (Pantheon, JLA).", "cat": "astro-ph.CO", "authors": ["T. M. C. Abbott", "S. Allam", "P. Andersen", "C. Angus", "J. Asorey", "A. Avelino", "S. Avila", "B. A. Bassett", "K. Bechtol", "G. M. Bernstein", "E. Bertin", "D. Brooks", "D. Brout", "P. Brown", "D. L. Burke", "J. Calcino", "A. Carnero Rosell", "D. Carollo", "M. Carrasco Kind", "J. Carretero", "R. Casas", "F. J. Castander", "R. Cawthon", "P. Challis", "M. Childress", "A. Clocchiatti", "C. E. Cunha", "C. B. D'Andrea", "L. N. da Costa", "C. Davis", "T. M. Davis", "J. De Vicente", "D. L. DePoy", "S. Desai", "H. T. Diehl", "P. Doel", "A. Drlica-Wagner", "T. F. Eifler", "A. E. Evrard", "E. Fernandez", "A. V. Filippenko", "D. A. Finley", "B. Flaugher", "R. J. Foley", "P. Fosalba", "J. Frieman", "L. Galbany", "J. Garcia-Bellido", "E. Gaztanaga", "T. Giannantonio", "K. Glazebrook", "D. A. Goldstein", "S. Gonzalez-Gaitan", "D. Gruen", "R. A. Gruendl", "J. Gschwend", "R. R. Gupta", "G. Gutierrez", "W. G. Hartley", "S. R. Hinton", "D. L. Hollowood", "K. Honscheid", "J. K. Hoormann", "B. Hoyle", "D. J. James", "T. Jeltema", "M. W. G. Johnson", "M. D. Johnson", "E. Kasai", "S. Kent", "R. Kessler", "A. G. Kim", "R. P. Kirshner", "E. Kovacs", "E. Krause", "R. Kron", "K. Kuehn", "S. Kuhlmann", "N. Kuropatkin", "O. Lahav", "J. Lasker", "G. F. Lewis", "T. S. Li", "C. Lidman", "M. Lima", "H. Lin", "E. Macaulay", "M. A. G. Maia", "K. S. Mandel", "M. March", "J. Marriner", "J. L. Marshall", "P. Martini", "F. Menanteau", "C. J. Miller", "R. Miquel", "V. Miranda", "J. J. Mohr", "E. Morganson", "D. Muthukrishna", "A. M\u00f6ller", "E. Neilsen", "R. C. Nichol", "B. Nord", "P. Nugent", "R. L. C. Ogando", "A. Palmese", "Y. -C. Pan", "A. A. Plazas", "M. Pursiainen", "A. K. Romer", "A. Roodman", "E. Rozo", "E. S. Rykoff", "M. Sako", "E. Sanchez", "V. Scarpine", "R. Schindler", "M. Schubnell", "D. Scolnic", "S. Serrano", "I. Sevilla-Noarbe", "R. Sharp", "M. Smith", "M. Soares-Santos", "F. Sobreira", "N. E. Sommer", "H. Spinka", "E. Suchyta", "M. Sullivan", "E. Swann", "G. Tarle", "D. Thomas", "R. C. Thomas", "M. A. Troxel", "B. E. Tucker", "S. A. Uddin", "A. R. Walker", "W. Wester", "P. Wiseman", "R. C. Wolf", "B. Yanny", "B. Zhang", "Y. Zhang"]}, "1549": {"id": "1409.8355v1", "title": "The ensemble optical variability of type-1 AGN in the Sloan Digital Sky Survey Data Release 7", "url": "http://arxiv.org/pdf/1409.8355v1", "date": "2014-09-30 00:14:21", "abs": "We use a sample of over 5000 active galactic nuclei (AGN) with extended\nmorphologies at z<0.8 from the Sloan Digital Sky Survey (SDSS) to study the\nensemble optical variability as a function of rest-frame time lag and AGN\nluminosity with the aim of investigating these parameter relationships at lower\nluminosities than previously studied. We compare photometry from imaging data\nwith spectrophotometry obtained weeks to years later in the Sloan g, r, and i\nbands. We employ quasar and galaxy eigenspectra fitting to separate the AGN and\nhost galaxy components. A strong correlation between the variability amplitude\nand rest-frame time lag is observed, in agreement with quasar structure\nfunctions but extending to AGN several magnitudes fainter than previously\nstudied. The structure function slopes for our fainter AGN sample are slightly\nshallower than those found in quasars studies. An anticorrelation with\nluminosity is clearly detected, with lower luminosity AGN displaying greater\nvariability amplitudes. We demonstrate for the first time that this\nanticorrelation extends to AGN as faint as $M_{AGN_i}\\sim-18.5$, with a slight\ntrend towards shallower slopes at luminosities fainter than\n$M_{AGN_i}\\sim-20.2$.", "cat": "astro-ph.GA", "authors": ["Unai Gallastegui-Aizpun", "Vicki L. Sarajedini"]}, "1550": {"id": "2108.00443v1", "title": "A Survey on Audio Synthesis and Audio-Visual Multimodal Processing", "url": "http://arxiv.org/pdf/2108.00443v1", "date": "2021-08-01 12:35:16", "abs": "With the development of deep learning and artificial intelligence, audio\nsynthesis has a pivotal role in the area of machine learning and shows strong\napplicability in the industry. Meanwhile, significant efforts have been\ndedicated by researchers to handle multimodal tasks at present such as\naudio-visual multimodal processing. In this paper, we conduct a survey on audio\nsynthesis and audio-visual multimodal processing, which helps understand\ncurrent research and future trends. This review focuses on text to speech(TTS),\nmusic generation and some tasks that combine visual and acoustic information.\nThe corresponding technical methods are comprehensively classified and\nintroduced, and their future development trends are prospected. This survey can\nprovide some guidance for researchers who are interested in the areas like\naudio synthesis and audio-visual multimodal processing.", "cat": "eess.AS", "authors": ["Zhaofeng Shi"]}, "1551": {"id": "1103.5496v3", "title": "Survey of Morphologies Formed in the Wake of an Enslaved Phase-Separation Front in Two Dimensions", "url": "http://arxiv.org/pdf/1103.5496v3", "date": "2011-12-01 17:41:11", "abs": "A phase-separation front will leave in its wake a phase-separated morphology\nthat differs markedly from homogeneous phase-separation morphologies. For a\npurely diffusive system such a front, moving with constant velocity, will\ngenerate very regular, non-equilibrium structures. We present here a numerical\nstudy of these fronts using a lattice Boltzmann method. In two dimensions these\nstructures are regular stripes or droplet arrays. In general the kind and\norientation of the selected morphology and the size of the domains depends on\nthe speed of the front as well as the composition of the material overtaken by\nthe phase-separation front. We present a survey of morphologies as a function\nof these two parameters. We show that the resulting morphologies are initial\ncondition dependent. We then examine which of the potential morphologies is the\nmost stable. An analytical analysis for symmetrical compositions predicts the\ntransition point from orthogonal to parallel stripes.", "cat": "cond-mat.soft", "authors": ["E. M. Foard", "A. J. Wagner"]}, "1552": {"id": "1503.08675v1", "title": "Dynamical Schwinger process in a bifrequent electric field of finite duration: survey on amplification", "url": "http://arxiv.org/pdf/1503.08675v1", "date": "2015-03-30 14:01:40", "abs": "The electron-positron pair production due to the dynamical Schwinger process\nin a slowly oscillating strong electric field is enhanced by the superposition\nof a rapidly oscillating weaker electric field. A systematic account of the\nenhancement by the resulting bifrequent field is provided for the residual\nphase space distribution. The enhancement is explained by a severe reduction of\nthe suppression in both the tunneling and multiphoton regimes.", "cat": "hep-ph", "authors": ["Andreas Otto", "Daniel Seipt", "David Blaschke", "Stanislav Alexandrovich Smolyansky", "Burkhard K\u00e4mpfer"]}, "1553": {"id": "1707.00588v4", "title": "Constraints on the sum of neutrino masses using cosmological data including the latest extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample", "url": "http://arxiv.org/pdf/1707.00588v4", "date": "2018-04-05 02:36:15", "abs": "We investigate the constraints on the sum of neutrino masses ($\\Sigma m_\\nu$)\nusing the most recent cosmological data, which combines the distance\nmeasurement from baryonic acoustic oscillation in the extended Baryon\nOscillation Spectroscopic Survey DR14 quasar sample with the power spectra of\ntemperature and polarization anisotropies in the cosmic microwave background\nfrom the Planck 2015 data release. We also use other low-redshift observations\nincluding the baryonic acoustic oscillation at relatively low redshifts, the\nsupernovae of type Ia and the local measurement of Hubble constant. In the\nstandard cosmological constant $\\Lambda$ cold dark matter plus massive neutrino\nmodel, we obtain the $95\\%$ \\acl{CL} upper limit to be $\\Sigma\nm_\\nu<0.129~\\mathrm{eV}$ for the degenerate mass hierarchy, $\\Sigma\nm_{\\nu}<0.159~\\mathrm{eV}$ for the normal mass hierarchy, and $\\Sigma\nm_{\\nu}<0.189~\\mathrm{eV}$ for the inverted mass hierarchy. Based on Bayesian\nevidence, we find that the degenerate hierarchy is positively supported, and\nthe current data combination can not distinguish normal and inverted\nhierarchies. Assuming the degenerate mass hierarchy, we extend our study to\nnon-standard cosmological models including the generic dark energy, the spatial\ncurvature, and the extra relativistic degrees of freedom, respectively, but\nfind these models not favored by the data.", "cat": "astro-ph.CO", "authors": ["Sai Wang", "Yi-Fan Wang", "Dong-Mei Xia"]}, "1554": {"id": "2109.04786v5", "title": "Wi-Fi Meets ML: A Survey on Improving IEEE 802.11 Performance with Machine Learning", "url": "http://arxiv.org/pdf/2109.04786v5", "date": "2022-10-06 07:06:52", "abs": "Wireless local area networks (WLANs) empowered by IEEE 802.11 (Wi-Fi) hold a\ndominant position in providing Internet access thanks to their freedom of\ndeployment and configuration as well as the existence of affordable and highly\ninteroperable devices. The Wi-Fi community is currently deploying Wi-Fi 6 and\ndeveloping Wi-Fi 7, which will bring higher data rates, better multi-user and\nmulti-AP support, and, most importantly, improved configuration flexibility.\nThese technical innovations, including the plethora of configuration\nparameters, are making next-generation WLANs exceedingly complex as the\ndependencies between parameters and their joint optimization usually have a\nnon-linear impact on network performance. The complexity is further increased\nin the case of dense deployments and coexistence in shared bands. While\nclassical optimization approaches fail in such conditions, machine learning\n(ML) is able to handle complexity. Much research has been published on using ML\nto improve Wi-Fi performance and solutions are slowly being adopted in existing\ndeployments. In this survey, we adopt a structured approach to describe the\nvarious Wi-Fi areas where ML is applied. To this end, we analyze over 250\npapers in the field, providing readers with an overview of the main trends.\nBased on this review, we identify specific open challenges and provide general\nfuture research directions.", "cat": "cs.NI", "authors": ["Szymon Szott", "Katarzyna Kosek-Szott", "Piotr Gaw\u0142owicz", "Jorge Torres G\u00f3mez", "Boris Bellalta", "Anatolij Zubow", "Falko Dressler"]}, "1555": {"id": "2008.09243v2", "title": "The wide-field VLBA calibrator survey -- WFCS", "url": "http://arxiv.org/pdf/2008.09243v2", "date": "2020-11-03 03:54:41", "abs": "The paper presents the results of the largest to date VLBI absolute\nastrometry campaign of observations of 13,645 radio sources with the Very Long\nBaseline Array (VLBA). Of them, 7220 have been detected, including 6755 target\nsources that have never been observed with VLBI before. This makes the present\nVLBI catalogue the largest ever published. Positions of the target sources have\nbeen determined with the median uncertainty 1.7 mas, and 15,599 images of 7179\nsources have been generated. Unlike to previous absolute radio astrometry\ncampaigns, observations were made at 4.3 and 7.6 GHz simultaneously using a\nsingle wide-band receiver. Because of the fine spectral and time resolutions,\nthe field of view was 4 to 8 arcminutes -- much greater than 10 to 20\narcseconds in previous surveys. This made possible to use input catalogues with\nlow position accuracy and detect a compact component in extended sources.\nUnlike to previous absolute astrometry campaigns, both steep and flat spectrum\nsources were observed. The observations were scheduled in the so-called fill-in\nmode to fill the gaps between other high priority programs. That was achieved\nby development of the totally automatic scheduling procedure.", "cat": "astro-ph.IM", "authors": ["Leonid Petrov"]}, "1556": {"id": "2009.06843v2", "title": "Phase II of the LAMOST-Kepler/K2 survey. I. Time series of medium-resolution spectroscopic observations", "url": "http://arxiv.org/pdf/2009.06843v2", "date": "2020-09-23 10:44:25", "abs": "Phase \\RNum{2} of the LAMOST-{\\sl Kepler/K}2 survey (LK-MRS), initiated in\n2018, aims at collecting medium-resolution spectra ($R\\sim7,500$; hereafter\nMRS) for more than $50,000$ stars with multiple visits ($\\sim60$ epochs) over a\nperiod of 5 years (2018 September to 2023 June). We selected 20 footprints\ndistributed across the {\\sl Kepler} field and six {\\sl K}2 campaigns, with each\nplate containing a number of stars ranging from $\\sim2,000$ to $\\sim 3,000$.\nDuring the first year of observations, the LK-MRS has already collected\n$\\sim280,000$ and $\\sim369,000$ high-quality spectra in the blue and red\nwavelength range, respectively. The atmospheric parameters and radial\nvelocities for $\\sim259,000$ spectra of $21,053$ targets were successfully\ncalculated by the LASP pipeline. The internal uncertainties for the effective\ntemperature, surface gravity, metallicity, and radial velocity are found to be\n$100$\\,K, $0.15$\\,dex, $0.09$\\,dex, and $1.00$\\,km\\,s$^{-1}$, respectively. We\nfound $14,997$, $20,091$, and $1,514$ stars in common with the targets from the\nLAMOST low-resolution survey (LRS), GAIA and APOGEE, respectively,\ncorresponding to a fraction of $\\sim70\\%$, $\\sim95\\%$ and $\\sim7.2\\%$. In\ngeneral, the parameters derived from LK-MRS spectra are consistent with those\nobtained from the LRS and APOGEE spectra, but the scatter increases as the\nsurface gravity decreases when comparing with the measurements from APOGEE. A\nlarge discrepancy is found with the GAIA values of the effective temperature.\nThe comparisons of radial velocities of LK-MRS to GAIA and LK-MRS to APOGEE\nnearly follow an Gaussian distribution with a mean $\\mu\\sim1.10$ and\n$0.73$\\,km\\,s$^{-1}$, respectively.", "cat": "astro-ph.SR", "authors": ["Weikai Zong", "Jian-Ning Fu", "Peter De Cat", "Jiaxin Wang", "Jianrong Shi", "Ali Luo", "Haotong Zhang", "A. Frasca", "J. Molenda- \u017bakowicz", "R. O. Gray", "C. J. Corbally", "G. Catanzaro", "Tianqi Cang", "Jiangtao Wang", "Jianjun Chen", "Yonghui Hou", "Jiaming Liu", "Hubiao Niu", "Yang Pan", "Hao Tian", "Hongliang Yan", "Yong Zhang", "Heng Zuo"]}, "1557": {"id": "2302.03883v2", "title": "Multimodal Recommender Systems: A Survey", "url": "http://arxiv.org/pdf/2302.03883v2", "date": "2024-09-04 14:00:42", "abs": "The recommender system (RS) has been an integral toolkit of online services.\nThey are equipped with various deep learning techniques to model user\npreference based on identifier and attribute information. With the emergence of\nmultimedia services, such as short videos, news and etc., understanding these\ncontents while recommending becomes critical. Besides, multimodal features are\nalso helpful in alleviating the problem of data sparsity in RS. Thus,\nMultimodal Recommender System (MRS) has attracted much attention from both\nacademia and industry recently. In this paper, we will give a comprehensive\nsurvey of the MRS models, mainly from technical views. First, we conclude the\ngeneral procedures and major challenges for MRS. Then, we introduce the\nexisting MRS models according to four categories, i.e., Modality Encoder,\nFeature Interaction, Feature Enhancement and Model Optimization. Besides, to\nmake it convenient for those who want to research this field, we also summarize\nthe dataset and code resources. Finally, we discuss some promising future\ndirections of MRS and conclude this paper. To access more details of the\nsurveyed papers, such as implementation code, we open source a repository.", "cat": "cs.IR", "authors": ["Qidong Liu", "Jiaxi Hu", "Yutian Xiao", "Xiangyu Zhao", "Jingtong Gao", "Wanyu Wang", "Qing Li", "Jiliang Tang"]}, "1558": {"id": "2002.00444v2", "title": "Deep Reinforcement Learning for Autonomous Driving: A Survey", "url": "http://arxiv.org/pdf/2002.00444v2", "date": "2021-01-23 17:02:01", "abs": "With the development of deep representation learning, the domain of\nreinforcement learning (RL) has become a powerful learning framework now\ncapable of learning complex policies in high dimensional environments. This\nreview summarises deep reinforcement learning (DRL) algorithms and provides a\ntaxonomy of automated driving tasks where (D)RL methods have been employed,\nwhile addressing key computational challenges in real world deployment of\nautonomous driving agents. It also delineates adjacent domains such as behavior\ncloning, imitation learning, inverse reinforcement learning that are related\nbut are not classical RL algorithms. The role of simulators in training agents,\nmethods to validate, test and robustify existing solutions in RL are discussed.", "cat": "cs.LG", "authors": ["B Ravi Kiran", "Ibrahim Sobh", "Victor Talpaert", "Patrick Mannion", "Ahmad A. Al Sallab", "Senthil Yogamani", "Patrick P\u00e9rez"]}, "1559": {"id": "1703.07490v1", "title": "First Discoveries of z>6 Quasars with the DECam Legacy Survey and UKIRT Hemisphere Survey", "url": "http://arxiv.org/pdf/1703.07490v1", "date": "2017-03-22 02:10:30", "abs": "We present the first discoveries from a survey of $z\\gtrsim6$ quasars using\nimaging data from the DECam Legacy Survey (DECaLS) in the optical, the UKIRT\nDeep Infrared Sky Survey (UKIDSS) and a preliminary version of the UKIRT\nHemisphere Survey (UHS) in the near-IR, and ALLWISE in the mid-IR. DECaLS will\nimage 9000 deg$^2$ of sky down to $z_{\\rm AB}\\sim23.0$, and UKIDSS and UHS,\nwhich will map the northern sky at $06.5$ to $J_{\\rm VEGA}<19.5$.", "cat": "astro-ph.GA", "authors": ["Feige Wang", "Xiaohui Fan", "Jinyi Yang", "Xue-Bing Wu", "Qian Yang", "Fuyan Bian", "Ian D. McGreer", "Jiang-Tao Li", "Zefeng Li", "Jiani Ding", "Arjun Dey", "Simon Dye", "Joseph R. Findlay", "Richard Green", "David James", "Linhua Jiang", "Dustin Lang", "Andy Lawrence", "Adam D. Myers", "Nicholas P. Ross", "David J. Schlegel", "Tom Shanks"]}, "1560": {"id": "2311.00370v2", "title": "Discovery of four pulsars in a pilot survey at intermediate Galactic latitudes with FAST", "url": "http://arxiv.org/pdf/2311.00370v2", "date": "2023-12-28 12:58:17", "abs": "We present the discovery and timing results of four pulsars discovered in a\npilot survey at intermediate Galactic latitudes with the Five-hundred Aperture\nSpherical Telescope (FAST). Among these pulsars, two belong to the category of\nmillisecond pulsars (MSPs) with spin periods of less than 20 ms. The other two\nfall under the classification of \"mildly recycled\" pulsars, with massive white\ndwarfs as companions. Remarkably, this small survey, covering an area of 4.7\n$deg^2$ , led to the discovery of four recycled pulsars. Such success\nunderscores the immense potential of future surveys at intermediate Galactic\nlatitudes. In order to assess the potential yield of MSPs, we conducted\npopulation simulations and found that both FAST and Parkes new phased array\nfeed surveys, focusing on intermediate Galactic latitudes, have the capacity to\nuncover several hundred new MSPs.", "cat": "astro-ph.HE", "authors": ["Q. J. Zhi", "J. T. Bai", "S. Dai", "X. Xu", "S. J. Dang", "L. H. Shang", "R. S. Zhao", "D. Li", "W. W. Zhu", "N. Wang", "J. P. Yuan", "P. Wang", "L. Zhang", "Y. Feng", "J. B. Wang", "S. Q. Wang", "Q. D. Wu", "A. J. Dong", "H. Yang", "J. Tian", "W. Q. Zhong", "X. H. Luo", "Miroslav D. Filipovi", "G. J. Qiao"]}, "1561": {"id": "1902.10402v1", "title": "Social Credibility Incorporating Semantic Analysis and Machine Learning: A Survey of the State-of-the-Art and Future Research Directions", "url": "http://arxiv.org/pdf/1902.10402v1", "date": "2019-02-27 09:10:11", "abs": "The wealth of Social Big Data (SBD) represents a unique opportunity for\norganisations to obtain the excessive use of such data abundance to increase\ntheir revenues. Hence, there is an imperative need to capture, load, store,\nprocess, analyse, transform, interpret, and visualise such manifold social\ndatasets to develop meaningful insights that are specific to an application\ndomain. This paper lays the theoretical background by introducing the\nstate-of-the-art literature review of the research topic. This is associated\nwith a critical evaluation of the current approaches, and fortified with\ncertain recommendations indicated to bridge the research gap.", "cat": "cs.SI", "authors": ["Bilal Abu-Salih", "Bushra Bremie", "Pornpit Wongthongtham", "Kevin Duan", "Tomayess Issa", "Kit Yan Chan", "Mohammad Alhabashneh", "Teshreen Albtoush", "Sulaiman Alqahtani", "Abdullah Alqahtani", "Muteeb Alahmari", "Naser Alshareef", "Abdulaziz Albahlal"]}, "1562": {"id": "1809.08748v1", "title": "A Survey of Conventional and Artificial Intelligence / Learning based Resource Allocation and Interference Mitigation Schemes in D2D Enabled Networks", "url": "http://arxiv.org/pdf/1809.08748v1", "date": "2018-09-24 04:15:37", "abs": "5th generation networks are envisioned to provide seamless and ubiquitous\nconnection to 1000-fold more devices and is believed to provide ultra-low\nlatency and higher data rates up to tens of Gbps. Different technologies\nenabling these requirements are being developed including mmWave\ncommunications, Massive MIMO and beamforming, Device to Device (D2D)\ncommunications and Heterogeneous Networks. D2D communication is a promising\ntechnology to enable applications requiring high bandwidth such as online\nstreaming and online gaming etc. It can also provide ultra- low latencies\nrequired for applications like vehicle to vehicle communication for autonomous\ndriving. D2D communication can provide higher data rates with high energy\nefficiency and spectral efficiency compared to conventional communication. The\nperformance benefits of D2D communication can be best achieved when D2D users\nreuses the spectrum being utilized by the conventional cellular users. This\nspectrum sharing in a multi-tier heterogeneous network will introduce complex\ninterference among D2D users and cellular users which needs to be resolved.\nMotivated by limited number of surveys for interference mitigation and resource\nallocation in D2D enabled heterogeneous networks, we have surveyed different\nconventional and artificial intelligence based interference mitigation and\nresource allocation schemes developed in recent years. Our contribution lies in\nthe analysis of conventional interference mitigation techniques and their\nshortcomings. Finally, the strengths of AI based techniques are determined and\nopen research challenges deduced from the recent research are presented.", "cat": "cs.AI", "authors": ["Kamran Zia", "Nauman Javed", "Muhammad Nadeem Sial", "Sohail Ahmed", "Hifsa Iram", "Asad Amir Pirzada"]}, "1563": {"id": "1603.08353v1", "title": "Chandra ACIS Survey of X-ray Point Sources: The Source Catalog", "url": "http://arxiv.org/pdf/1603.08353v1", "date": "2016-03-28 10:38:44", "abs": "The $Chandra$ archival data is a valuable resource for various studies on\ndifferent topics of X-ray astronomy. In this paper, we utilize this wealth and\npresent a uniformly processed data set, which can be used to address a wide\nrange of scientific questions. The data analysis procedures are applied to\n10,029 ACIS observations, which produces 363,530 source detections, belonging\nto 217,828 distinct X-ray sources. This number is twice the size of the\n$Chandra$ Source Catalog (Version 1.1). The catalogs in this paper provide\nabundant estimates of the detected X-ray source properties, including source\npositions, counts, colors, fluxes, luminosities, variability statistics, etc.\nCross-correlation of these objects with galaxies shows 17,828 sources are\nlocated within the $D_{25}$ isophotes of 1110 galaxies, and 7504 sources are\nlocated between the $D_{25}$ and 2$D_{25}$ isophotes of 910 galaxies.\nContamination analysis with the log$N$--log$S$ relation indicates that 51.3\\%\nof objects within 2$D_{25}$ isophotes are truly relevant to galaxies, and the\n\"net\" source fraction increases to 58.9\\%, 67.3\\%, and 69.1\\% for sources with\nluminosities above $10^{37}$, $10^{38}$, and $10^{39}$ erg s$^{-1}$. Among the\npossible scientific uses of this catalog, we discuss the possibility to study\nintra-observation variability, inter-observation variability, and supersoft\nsources.", "cat": "astro-ph.SR", "authors": ["Song Wang", "Jifeng Liu", "Yanli Qiu", "Yu Bai", "Huiqin Yang", "Jincheng Guo", "Peng Zhang"]}, "1564": {"id": "2402.19088v3", "title": "Survey in Characterization of Semantic Change", "url": "http://arxiv.org/pdf/2402.19088v3", "date": "2024-07-18 12:28:27", "abs": "Live languages continuously evolve to integrate the cultural change of human\nsocieties. This evolution manifests through neologisms (new words) or\n\\textbf{semantic changes} of words (new meaning to existing words).\nUnderstanding the meaning of words is vital for interpreting texts coming from\ndifferent cultures (regionalism or slang), domains (e.g., technical terms), or\nperiods. In computer science, these words are relevant to computational\nlinguistics algorithms such as translation, information retrieval, question\nanswering, etc. Semantic changes can potentially impact the quality of the\noutcomes of these algorithms. Therefore, it is important to understand and\ncharacterize these changes formally. The study of this impact is a recent\nproblem that has attracted the attention of the computational linguistics\ncommunity. Several approaches propose methods to detect semantic changes with\ngood precision, but more effort is needed to characterize how the meaning of\nwords changes and to reason about how to reduce the impact of semantic change.\nThis survey provides an understandable overview of existing approaches to the\n\\textit{characterization of semantic changes} and also formally defines three\nclasses of characterizations: if the meaning of a word becomes more general or\nnarrow (change in dimension) if the word is used in a more pejorative or\npositive/ameliorated sense (change in orientation), and if there is a trend to\nuse the word in a, for instance, metaphoric or metonymic context (change in\nrelation). We summarized the main aspects of the selected publications in a\ntable and discussed the needs and trends in the research activities on semantic\nchange characterization.", "cat": "cs.CL", "authors": ["Jader Martins Camboim de S\u00e1", "Marcos Da Silveira", "C\u00e9dric Pruski"]}, "1565": {"id": "0705.1022v1", "title": "Identification of Very Red Counterparts of SiO Maser and OH/IR Objects in the GLIMPSE Survey", "url": "http://arxiv.org/pdf/0705.1022v1", "date": "2007-05-08 00:55:53", "abs": "Using the 3.6/4.5/5.8/8.0 micron images with 1.2 arcsec pixel resolution from\nthe Spitzer/GLIMPSE survey, we investigated 23 masing and 18 very red objects\nthat were not identified in the 2MASS survey. Counterparts for all selected\nobjects were found in the GLIMPSE images. Color indices in these IR bands\nsuggest the presence of a high-extinction layer of more than a few tenths of a\nsolar mass in front of the central star. Furthermore, radio observations in the\nSiO and H2O maser lines found characteristic maser-line spectra of the embedded\nobjects, e.g., the SiO J=1-0 line intensity in the v=2 state stronger than that\nof the v=1 state, or very widespread H2O maser emission spectra. This indicates\nthat these objects are actually enshrouded by very thick circumstellar matter,\nsome of which cannot be ascribed to the AGB wind of the central star.\nIndividually interesting objects are discussed, including two newly found water\nfountains and an SiO source with nebulosity.", "cat": "astro-ph", "authors": ["S. Deguchi", "J. Nakashima", "S. Kwok", "N. Koning"]}, "1566": {"id": "2109.13839v2", "title": "The NuSTAR Extragalactic Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field", "url": "http://arxiv.org/pdf/2109.13839v2", "date": "2021-12-29 14:47:02", "abs": "We present the $NuSTAR$ extragalactic survey of the $James$ $Webb$ $Space$\n$Telescope$ ($JWST$) North Ecliptic Pole (NEP) Time-Domain Field. The survey\ncovers a $\\sim$0.16 deg$^2$ area with a total exposure of 681 ks acquired in a\ntotal of nine observations from three epochs. The survey sensitivities at 20%\nof the area are 2.39, 1.14, 2.76, 1.52, and 5.20 $\\times$ 10$^{-14}$ erg\ncm$^{-2}$ s$^{-1}$ in the 3-24, 3-8, 8-24, 8-16, and 16-24 keV bands,\nrespectively. The NEP survey is one of the most sensitive extragalactic surveys\nwith $NuSTAR$ so far. A total of 33 sources were detected above 95% reliability\nin at least one of the five bands. We present the number counts, log$N$-log$S$,\nmeasured in the hard X-ray 8-24 and 8-16 keV bands, uniquely accessible by\n$NuSTAR$ down to such faint fluxes. We performed source detection on the\nXMM-$Newton$ and $Chandra$ observations of the same field to search for soft\nX-ray counterparts of each $NuSTAR$ detection. The soft band positions were\nused to identify optical and infrared associations. We present the X-ray\nproperties (hardness ratio and luminosity) and optical-to-X-ray properties of\nthe detected sources. The measured fraction of candidate Compton-thick (N$\\rm\n_H\\ge10^{24} cm^{-2}$) active galactic nuclei, derived from the hardness ratio,\nis between 3% to 27%. As this survey was designed to have variability as its\nprimary focus, we present preliminary results on multi-epoch flux variability\nin the 3-24 keV band.", "cat": "astro-ph.HE", "authors": ["X. Zhao", "F. Civano", "F. M. Fornasini", "D. M. Alexander", "N. Cappelluti", "C. T. Chen", "S. H. Cohen", "M. Elvis", "P. Gandhi", "N. A. Grogin", "R. C. Hickox", "R. A. Jansen", "A. Koekemoer", "G. Lanzuisi", "W. P. Maksym", "A. Masini", "D. J. Rosario", "M. J. Ward", "C. N. A. Willmer", "R. A. Windhorst"]}, "1567": {"id": "1606.05028v1", "title": "New variable stars discovered in the fields of three Galactic open clusters using the VVV Survey", "url": "http://arxiv.org/pdf/1606.05028v1", "date": "2016-06-16 02:05:09", "abs": "This project is a massive near-infrared (NIR) search for variable stars in\nhighly reddened and obscured open cluster (OC) fields projected on regions of\nthe Galactic bulge and disk. The search is performed using photometric NIR data\nin the $J$-, $H$- and $K_s$- bands obtained from the Vista Variables in the\nV\\'ia L\\'actea (VVV) Survey. We performed in each cluster field a variability\nsearch using Stetson's variability statistics to select the variable\ncandidates. Later, those candidates were subjected to a frequency analysis\nusing the Generalized Lomb-Scargle and the Phase Dispersion Minimization\nalgorithms. The number of independent observations range between 63 and 73. The\nnewly discovered variables in this study, 157 in total in three different known\nOCs, are classified based on their light curve shapes, periods, amplitudes and\ntheir location in the corresponding color-magnitude $(J-K_s,K_s)$ and\ncolor-color $(H-K_s,J-H)$ diagrams. We found 5 possible Cepheid stars which,\nbased on the period-luminosity relation, are very likely type II Cepheids\nlocated behind the bulge. Among the newly discovered variables, there are\neclipsing binaries, $\\delta$ Scuti, as well as background RR Lyrae stars. Using\nthe new version of the Wilson & Devinney code as well as the \"Physics Of\nEclipsing Binaries\" (PHOEBE) code, we analyzed some of the best eclipsing\nbinaries we discovered. Our results show that these studied systems turn out to\nbe ranging from detached to double-contact binaries, with low eccentricities\nand high inclinations of approximately $80^{\\circ}$. Their surface temperatures\nrange between $3500$K and $8000$K.", "cat": "astro-ph.SR", "authors": ["Tali Palma", "Dante Minniti", "Istvan D\u00e9k\u00e1ny", "Juan J. Clari\u00e1", "Javier Alonso-Garc\u00eda", "Luciana V. Gramajo", "Sebastian Ram\u00edrez Alegr\u00eda", "Charles Bonatto"]}, "1568": {"id": "2304.12197v2", "title": "The Gaia-ESO Survey: Empirical estimates of stellar ages from lithium equivalent widths (EAGLES)", "url": "http://arxiv.org/pdf/2304.12197v2", "date": "2023-04-25 17:18:33", "abs": "We present an empirical model of age-dependent photospheric lithium\ndepletion, calibrated using a large, homogeneously-analysed sample of 6200\nstars in 52 open clusters, with ages from 2--6000 Myr and $-0.3<{\\rm\n[Fe/H}]<0.2$, observed in the Gaia-ESO spectroscopic survey. The model is used\nto obtain age estimates and posterior age probability distributions from\nmeasurements of the Li I 6708A equivalent width for individual (pre) main\nsequence stars with $3000 < T_{\\rm eff}/{\\rm K} <6500$, a domain where age\ndetermination from the HR diagram is either insensitive or highly\nmodel-dependent. In the best cases, precisions of 0.1 dex in log age are\nachievable; even higher precision can be obtained for coeval groups and\nassociations where the individual age probabilities of their members can be\ncombined. The method is validated on a sample of exoplanet-hosting young stars,\nfinding agreement with claimed young ages for some, but not others. We obtain\nbetter than 10 per cent precision in age, and excellent agreement with\npublished ages, for seven well-studied young moving groups. The derived ages\nfor young clusters ($<1$ Gyr) in our sample are also in good agreement with\ntheir training ages, and consistent with several published, model-insensitive\nlithium depletion boundary ages. For older clusters there remain systematic age\nerrors that could be as large as a factor of two. There is no evidence to link\nthese errors to any strong systematic metallicity dependence of (pre) main\nsequence lithium depletion, at least in the range $-0.29 < {\\rm [Fe/H]} <\n0.18$. Our methods and model are provided as software -- \"Empirical AGes from\nLithium Equivalent widthS\" (EAGLES).", "cat": "astro-ph.SR", "authors": ["R. D. Jeffries", "R. J. Jackson", "Nicholas J. Wright", "G. Weaver", "G. Gilmore", "S. Randich", "A. Bragaglia", "A. J. Korn", "R. Smiljanic", "K. Biazzo", "A. R. Casey", "A. Frasca", "A. Gonneau", "G. Guiglion", "L. Morbidelli", "L. Prisinzano", "G. G. Sacco", "G. Tautvai\u0161ien\u0117", "C. C. Worley", "S. Zaggia"]}, "1569": {"id": "2011.14554v1", "title": "A Selective Survey on Versatile Knowledge Distillation Paradigm for Neural Network Models", "url": "http://arxiv.org/pdf/2011.14554v1", "date": "2020-11-30 05:22:02", "abs": "This paper aims to provide a selective survey about knowledge\ndistillation(KD) framework for researchers and practitioners to take advantage\nof it for developing new optimized models in the deep neural network field. To\nthis end, we give a brief overview of knowledge distillation and some related\nworks including learning using privileged information(LUPI) and generalized\ndistillation(GD). Even though knowledge distillation based on the\nteacher-student architecture was initially devised as a model compression\ntechnique, it has found versatile applications over various frameworks.\n In this paper, we review the characteristics of knowledge distillation from\nthe hypothesis that the three important ingredients of knowledge distillation\nare distilled knowledge and loss,teacher-student paradigm, and the distillation\nprocess. In addition, we survey the versatility of the knowledge distillation\nby studying its direct applications and its usage in combination with other\ndeep learning paradigms. Finally we present some future works in knowledge\ndistillation including explainable knowledge distillation where the analytical\nanalysis of the performance gain is studied and the self-supervised learning\nwhich is a hot research topic in deep learning community.", "cat": "cs.LG", "authors": ["Jeong-Hoe Ku", "JiHun Oh", "YoungYoon Lee", "Gaurav Pooniwala", "SangJeong Lee"]}, "1570": {"id": "2110.00273v5", "title": "From SLAM to Situational Awareness: Challenges and Survey", "url": "http://arxiv.org/pdf/2110.00273v5", "date": "2023-04-27 16:14:24", "abs": "The capability of a mobile robot to efficiently and safely perform complex\nmissions is limited by its knowledge of the environment, namely the situation.\nAdvanced reasoning, decision-making, and execution skills enable an intelligent\nagent to act autonomously in unknown environments. Situational Awareness (SA)\nis a fundamental capability of humans that has been deeply studied in various\nfields, such as psychology, military, aerospace, and education. Nevertheless,\nit has yet to be considered in robotics, which has focused on single\ncompartmentalized concepts such as sensing, spatial perception, sensor fusion,\nstate estimation, and Simultaneous Localization and Mapping (SLAM). Hence, the\npresent research aims to connect the broad multidisciplinary existing knowledge\nto pave the way for a complete SA system for mobile robotics that we deem\nparamount for autonomy. To this aim, we define the principal components to\nstructure a robotic SA and their area of competence. Accordingly, this paper\ninvestigates each aspect of SA, surveying the state-of-the-art robotics\nalgorithms that cover them, and discusses their current limitations.\nRemarkably, essential aspects of SA are still immature since the current\nalgorithmic development restricts their performance to only specific\nenvironments. Nevertheless, Artificial Intelligence (AI), particularly Deep\nLearning (DL), has brought new methods to bridge the gap that maintains these\nfields apart from the deployment to real-world scenarios. Furthermore, an\nopportunity has been discovered to interconnect the vastly fragmented space of\nrobotic comprehension algorithms through the mechanism of Situational Graph\n(S-Graph), a generalization of the well-known scene graph. Therefore, we\nfinally shape our vision for the future of robotic Situational Awareness by\ndiscussing interesting recent research directions.", "cat": "cs.RO", "authors": ["Hriday Bavle", "Jose Luis Sanchez-Lopez", "Claudio Cimarelli", "Ali Tourani", "Holger Voos"]}, "1571": {"id": "1803.01746v1", "title": "Low Redshift Baryon Acoustic Oscillation Measurement from the Reconstructed 6-degree Field Galaxy Survey", "url": "http://arxiv.org/pdf/1803.01746v1", "date": "2018-03-05 15:56:03", "abs": "Low redshift measurements of Baryon Acoustic Oscillations (BAO) test the late\ntime evolution of the Universe and are a vital probe of Dark Energy. Over the\npast decade both the 6-degree Field Galaxy Survey (6dFGS) and Sloan Digital Sky\nSurvey (SDSS) have provided important distance constraints at $z < 0.3$. In\nthis paper we re-evaluate the cosmological information from the BAO detection\nin 6dFGS making use of HOD populated COLA mocks for a robust covariance matrix\nand taking advantage of the now commonly implemented technique of density field\nreconstruction. For the 6dFGS data, we find consistency with the previous\nanalysis, and obtain an isotropic volume averaged distance measurement of\n$D_{V}(z_{\\mathrm{eff}}=0.097) =\n372\\pm17(r_{s}/r_{s}^{\\mathrm{fid}})\\,\\mathrm{Mpc}$, which has a non-Gaussian\nlikelihood outside the $1\\sigma$ region. We combine our measurement from both\nthe post-reconstruction clustering of 6dFGS and SDSS MGS offering the most\nrobust constraint to date in this redshift regime,\n$D_{V}(z_{\\mathrm{eff}}=0.122)=539\\pm17(r_{s}/r^{\\mathrm{fid}}_{s})\\,\\mathrm{Mpc}$.\nThese measurements are consistent with standard $\\Lambda\\mathrm{CDM}$ and after\nfixing the standard ruler using a Planck prior on $\\Omega_{m}h^{2}$, the joint\nanalysis gives $H_{0}=64.0\\pm3.5\\,\\mathrm{kms}^{-1}\\mathrm{Mpc}^{-1}$. In the\nnear future both the Taipan Galaxy Survey and the Dark Energy Spectroscopic\nInstrument (DESI) will improve this measurement to $1\\%$ at low redshift.", "cat": "astro-ph.CO", "authors": ["Paul Carter", "Florian Beutler", "Will J. Percival", "Chris Blake", "Jun Koda", "Ashley J. Ross"]}, "1572": {"id": "1504.06106v1", "title": "A Short Survey on Arithmetic Transforms and the Arithmetic Hartley Transform", "url": "http://arxiv.org/pdf/1504.06106v1", "date": "2015-04-23 09:37:28", "abs": "Arithmetic complexity has a main role in the performance of algorithms for\nspectrum evaluation. Arithmetic transform theory offers a method for computing\ntrigonometrical transforms with minimal number of multiplications. In this\npaper, the proposed algorithms for the arithmetic Fourier transform are\nsurveyed. A new arithmetic transform for computing the discrete Hartley\ntransform is introduced: the Arithmetic Hartley transform. The interpolation\nprocess is shown to be the key element of the arithmetic transform theory.", "cat": "math.CA", "authors": ["R. J. Cintra", "H. M. de Oliveira"]}, "1573": {"id": "2309.15948v2", "title": "The ALMA Reionization Era Bright Emission Line Survey (REBELS): The molecular gas content of galaxies at z~7", "url": "http://arxiv.org/pdf/2309.15948v2", "date": "2023-09-29 13:18:04", "abs": "A key to understanding the formation of the first galaxies is to quantify the\ncontent of the molecular gas as the fuel for star formation activity through\nthe epoch of reionization. In this paper, we use the 158$\\mu$m [CII]\nfine-structure emission line as a tracer of the molecular gas in the\ninterstellar medium (ISM) in a sample of $z=6.5-7.5$ galaxies recently unveiled\nby the Reionization Era Bright Line Emission Survey, REBELS, with the Atacama\nLarge Millimeter/submillimeter Array. We find substantial amounts of molecular\ngas ($\\sim10^{10.5}\\ M_\\odot$) comparable to those found in lower redshift\ngalaxies for similar stellar masses ($\\sim10^{10}\\ M_\\odot$). The REBELS\ngalaxies appear to follow the standard scaling relations of molecular gas to\nstellar mass ratio ($\\mu_{\\rm mol}$) and gas depletion timescale ($t_{\\rm\ndep}$) with distance to the star-forming main-sequence expected from\nextrapolations of $z\\sim1-4$ observations. We find median values at $z\\sim7$ of\n$\\mu_{\\rm mol}=2.6_{-1.4}^{4.1}$ and $t_{\\rm dep}=0.5_{-0.14}^{+0.26}$ Gyr,\nindicating that the baryonic content of these galaxies is gas-phase dominated\nand little evolution from $z\\sim7$ to 4. Our measurements of the cosmic density\nof molecular gas, log$(\\rho_{\\rm mol}/(M_\\odot {\\rm\nMpc}^{-3}))=6.34^{+0.34}_{-0.31}$, indicate a steady increase by an order of\nmagnitude from $z\\sim7$ to 4.", "cat": "astro-ph.GA", "authors": ["M. Aravena", "K. E. Heintz", "M. Dessauges-Zavadsky", "P. A. Oesch", "H. S. B. Algera", "R. J. Bouwens", "E. Da Cunha", "P. Dayal", "I. De Looze", "A. Ferrara", "Y. Fudamoto", "V. Gonzalez", "L. Graziani", "H. Inami", "A. Pallottini", "R. Schneider", "S. Schouws", "L. Sommovigo", "M. Topping", "P. van der Werf", "M. Palla"]}, "1574": {"id": "2105.12584v2", "title": "A Comprehensive Survey on Community Detection with Deep Learning", "url": "http://arxiv.org/pdf/2105.12584v2", "date": "2021-10-11 11:52:48", "abs": "A community reveals the features and connections of its members that are\ndifferent from those in other communities in a network. Detecting communities\nis of great significance in network analysis. Despite the classical spectral\nclustering and statistical inference methods, we notice a significant\ndevelopment of deep learning techniques for community detection in recent years\nwith their advantages in handling high dimensional network data. Hence, a\ncomprehensive overview of community detection's latest progress through deep\nlearning is timely to academics and practitioners. This survey devises and\nproposes a new taxonomy covering different state-of-the-art methods, including\ndeep learning-based models upon deep neural networks, deep nonnegative matrix\nfactorization and deep sparse filtering. The main category, i.e., deep neural\nnetworks, is further divided into convolutional networks, graph attention\nnetworks, generative adversarial networks and autoencoders. The survey also\nsummarizes the popular benchmark data sets, evaluation metrics, and open-source\nimplementations to address experimentation settings. We then discuss the\npractical applications of community detection in various domains and point to\nimplementation scenarios. Finally, we outline future directions by suggesting\nchallenging topics in this fast-growing deep learning field.", "cat": "cs.SI", "authors": ["Xing Su", "Shan Xue", "Fanzhen Liu", "Jia Wu", "Jian Yang", "Chuan Zhou", "Wenbin Hu", "Cecile Paris", "Surya Nepal", "Di Jin", "Quan Z. Sheng", "Philip S. Yu"]}, "1575": {"id": "0912.0293v1", "title": "The Keck+Magellan Survey for Lyman Limit Absorption II: A Case Study on Metallicity Variations", "url": "http://arxiv.org/pdf/0912.0293v1", "date": "2009-12-01 22:48:37", "abs": "We present an absorption line analysis of the Lyman limit system (LLS) at\nz=3.55 in our Magellan/MIKE spectrum of PKS2000-330. Our analysis of the Lyman\nlimit and full HI Lyman series constrains the total HI column density of the\nLLS (N_HI = 10^[18.0 +/- 0.25] cm^{-2} for b_HI >= 20 km/s) and also the N_HI\nvalues of the velocity subsystems comprising the absorber. We measure ionic\ncolumn densities for metal-line transitions associated with the subsystems and\nuse these values to constrain the ionization state (>90% ionized) and relative\nabundances of the gas. We find an order of magnitude dispersion in the\nmetallicities of the subsystems, marking the first detailed analysis of\nmetallicity variations in an optically thick absorber. The results indicate\nthat metals are not well mixed within the gas surrounding high $z$ galaxies.\nAssuming a single-phase photoionization model, we also derive an N_H-weighted\nmetallicity, <[Si/H]> = -1.66 +/- 0.25, which matches the mean metallicity in\nthe neutral ISM in high z damped Lya systems (DLAs). Because the line density\nof LLSs is ~10 times higher than the DLAs, we propose that the former dominate\nthe metal mass-density at z~3 and that these metals reside in the galaxy/IGM\ninterface. Considerations of a multi-phase model do not qualitatively change\nthese conclusions. Finally, we comment on an anomalously large O^0/Si^+ ratio\nin the LLS that suggests an ionizing radiation field dominated by soft UV\nsources (e.g. a starburst galaxy). Additional abundance analysis is performed\non the super-LLS systems at z=3.19.", "cat": "astro-ph.CO", "authors": ["Gabriel E. Prochter", "J. Xavier Prochaska", "John M. O'Meara", "Scott Burles", "Rebecca A. Bernstein"]}, "1576": {"id": "1408.4288v1", "title": "Selecting asteroids for a targeted spectroscopic survey", "url": "http://arxiv.org/pdf/1408.4288v1", "date": "2014-08-19 10:41:45", "abs": "Asteroid spectroscopy reflects surface mineralogy. There are few thousand\nasteroids whose surfaces have been observed spectrally. Determining the surface\nproperties of those objects is important for many practical and scientific\napplications, such as for example developing impact deflection strategies or\nstudying history and evolution of the Solar System and planet formation.\n The aim of this study is to develop a pre-selection method that can be\nutilized in searching for asteroids of any taxonomic complex. The method could\nthen be utilized im multiple applications such as searching for the missing\nV-types or looking for primitive asteroids.\n We used the Bayes Naive Classifier combined with observations obtained in the\ncourse of the Sloan Digital Sky Survey and the Wide-field Infrared Survey\nExplorer surveys as well as a database of asteroid phase curves for asteroids\nwith known taxonomic type. Using the new classification method we have selected\na number of possible V-type candidates. Some of the candidates were than\nspectrally observed at the Nordic Optical Telescope and South African Large\nTelescope.\n We have developed and tested the new pre-selection method. We found three\nasteroids in the mid/outer Main Belt that are likely of differentiated type.\nNear-Infrared are still required to confirm this discovery. Similarly to other\nstudies we found that V-type candidates cluster around the Vesta family and are\nrare in the mid/oter Main Belt.\n The new method shows that even largely explored large databases combined\ntogether could still be further exploited in for example solving the missing\ndunite problem.", "cat": "astro-ph.EP", "authors": ["D. A. Oszkiewicz", "T. Kwiatkowski", "T. Tomov", "M. Birlan", "S. Geier", "A. Penttil\u00e4", "M. Poli\u0144ska"]}, "1577": {"id": "2111.05339v2", "title": "GASKAP-HI Pilot Survey Science I: ASKAP Zoom Observations of HI Emission in the Small Magellanic Cloud", "url": "http://arxiv.org/pdf/2111.05339v2", "date": "2021-12-11 02:47:28", "abs": "We present the most sensitive and detailed view of the neutral hydrogen (HI)\nemission associated with the Small Magellanic Cloud (SMC), through the\ncombination of data from the Australian Square Kilometre Array Pathfinder\n(ASKAP) and Parkes (Murriyang), as part of the Galactic Australian Square\nKilometre Array Pathfinder (GASKAP) pilot survey. These GASKAP-HI pilot\nobservations, for the first time, reveal HI in the SMC on similar physical\nscales as other important tracers of the interstellar medium, such as molecular\ngas and dust. The resultant image cube possesses an rms noise level of 1.1 K\n(1.6 mJy/beam) per 0.98 km s$^{-1}$ spectral channel with an angular resolution\nof 30$''$ ($\\sim$10 pc). We discuss the calibration scheme and the custom\nimaging pipeline that utilizes a joint deconvolution approach, efficiently\ndistributed across a computing cluster, to accurately recover the emission\nextending across the entire $\\sim$25 deg$^2$ field-of-view. We provide an\noverview of the data products and characterize several aspects including the\nnoise properties as a function of angular resolution and the represented\nspatial scales by deriving the global transfer function over the full spectral\nrange. A preliminary spatial power spectrum analysis on individual spectral\nchannels reveals that the power-law nature of the density distribution extends\ndown to scales of 10 pc. We highlight the scientific potential of these data by\ncomparing the properties of an outflowing high velocity cloud with previous\nASKAP+Parkes HI test observations.", "cat": "astro-ph.GA", "authors": ["N. M. Pingel", "J. Dempsey", "N. M. McClure-Griffiths", "J. M. Dickey", "K. E. Jameson", "H. Arce", "G. Anglada", "J. Bland-Hawthorn", "S. L. Breen", "F. Buckland-Willis", "S. E. Clark", "J. R. Dawson", "H. D\u00e9nes", "E. M. Di Teodoro", "B. -Q. For", "Tyler J. Foster", "J. F. G\u00f3mez", "H. Imai", "G. Joncas", "C. -G. Kim", "M. -Y. Lee", "C. Lynn", "D. Leahy", "Y. K. Ma", "A. Marchal", "D. McConnell", "M. -A. Miville-Desch\u00eanes", "V. A. Moss", "C. E. Murray", "D. Nidever", "J. Peek", "S. Stanimirovi\u0107", "L. Staveley-Smith", "T. Tepper-Garcia", "C. D. Tremblay", "L. Uscanga", "J. Th. van Loon", "E. V\u00e1zquez-Semadeni", "J. R. Allison", "C. S. Anderson", "Lewis Ball", "M. Bell", "D. C. -J. Bock", "J. Bunton", "F. R. Cooray", "T. Cornwell", "B. S. Koribalski", "N. Gupta", "D. B. Hayman", "L. Harvey-Smith", "K. Lee-Waddell", "A. Ng", "C. J. Phillips", "M. Voronkov", "T. Westmeier", "M. T. Whiting"]}, "1578": {"id": "1711.03846v4", "title": "\"Dave...I can assure you...that it's going to be all right...\" -- A definition, case for, and survey of algorithmic assurances in human-autonomy trust relationships", "url": "http://arxiv.org/pdf/1711.03846v4", "date": "2018-08-28 17:07:30", "abs": "People who design, use, and are affected by autonomous artificially\nintelligent agents want to be able to \\emph{trust} such agents -- that is, to\nknow that these agents will perform correctly, to understand the reasoning\nbehind their actions, and to know how to use them appropriately. Many\ntechniques have been devised to assess and influence human trust in\nartificially intelligent agents. However, these approaches are typically ad\nhoc, and have not been formally related to each other or to formal trust\nmodels. This paper presents a survey of \\emph{algorithmic assurances}, i.e.\nprogrammed components of agent operation that are expressly designed to\ncalibrate user trust in artificially intelligent agents. Algorithmic assurances\nare first formally defined and classified from the perspective of formally\nmodeled human-artificially intelligent agent trust relationships. Building on\nthese definitions, a synthesis of research across communities such as machine\nlearning, human-computer interaction, robotics, e-commerce, and others reveals\nthat assurance algorithms naturally fall along a spectrum in terms of their\nimpact on an agent's core functionality, with seven notable classes ranging\nfrom integral assurances (which impact an agent's core functionality) to\nsupplemental assurances (which have no direct effect on agent performance).\nCommon approaches within each of these classes are identified and discussed;\nbenefits and drawbacks of different approaches are also investigated.", "cat": "cs.CY", "authors": ["Brett W Israelsen", "Nisar R Ahmed"]}, "1579": {"id": "2307.15747v1", "title": "z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [II] Dust properties", "url": "http://arxiv.org/pdf/2307.15747v1", "date": "2023-07-28 18:04:03", "abs": "(Abridged) We present the dust properties of 125 bright Herschel galaxies\nselected from the z-GAL survey. The large instantaneous bandwidth of NOEMA\nprovides an exquisite sampling of the underlying dust continuum emission at 2\nand 3 mm in the observed frame, with flux densities in at least four side bands\nfor each source. Together with the available Herschel 250, 350, and 500 micron\nand SCUBA-2 850 micron flux densities, the spectral energy distribution of each\nsource can be analyzed from the far-infrared to the millimeter, with a fine\nsampling of the Rayleigh-Jeans tail. This wealth of data provides a solid basis\nto derive robust dust properties, in particular the dust emissivity index,\nbeta, and the dust temperature, T(dust). In order to demonstrate our ability to\nconstrain the dust properties, we used a flux-generated mock catalog and\nanalyzed the results under the assumption of an optically thin and optically\nthick modified black body emission. For the z-GAL sources, we report a range of\ndust emissivities with beta ~ 1.5 - 3 estimated up to high precision with\nrelative uncertainties that vary in the range 7% - 15%, and an average of 2.2\n+/- 0.3. We find dust temperatures varying from 20 to 50 K with an average of\nT(dust) ~ 30 K for the optically thin case and ~38 K in the optically thick\ncase. For all the sources, we estimate the dust masses and apparent infrared\nluminosities (based on the optically thin approach). An inverse correlation is\nfound between T(dust) and beta, which is similar to what is seen in the local\nUniverse. Finally, we report an increasing trend in the dust temperature as a\nfunction of redshift at a rate of 6.5 +/- 0.5 K/z for this 500 micron-selected\nsample. Based on this study, future prospects are outlined to further explore\nthe evolution of dust temperature across cosmic time.", "cat": "astro-ph.GA", "authors": ["D. Ismail", "A. Beelen", "V. Buat", "S. Berta", "P. Cox", "F. Stanley", "A. Young", "S. Jin", "R. Neri", "T. Bakx", "H. Dannerbauer", "K. Butler", "A. Cooray", "A. Nanni", "A. Omont", "S. Serjeant", "P. van der Werf", "C. Vlahakis", "A. Weiss", "C. Yang", "A. J. Baker", "G. Bendo", "E. Borsato", "N. Chartab", "S. Dye", "S. Eales", "R. Gavazzi", "D. Hughes", "R. Ivison", "B. M. Jones M. Krips", "M. Lehnert", "L. Marchetti", "H. Messias", "M. Negrello", "I. Perez-Fournon", "D. A. Riechers", "S. Urquhart"]}, "1580": {"id": "2204.07356v5", "title": "Vision-and-Language Pretrained Models: A Survey", "url": "http://arxiv.org/pdf/2204.07356v5", "date": "2022-05-03 21:31:58", "abs": "Pretrained models have produced great success in both Computer Vision (CV)\nand Natural Language Processing (NLP). This progress leads to learning joint\nrepresentations of vision and language pretraining by feeding visual and\nlinguistic contents into a multi-layer transformer, Visual-Language Pretrained\nModels (VLPMs). In this paper, we present an overview of the major advances\nachieved in VLPMs for producing joint representations of vision and language.\nAs the preliminaries, we briefly describe the general task definition and\ngenetic architecture of VLPMs. We first discuss the language and vision data\nencoding methods and then present the mainstream VLPM structure as the core\ncontent. We further summarise several essential pretraining and fine-tuning\nstrategies. Finally, we highlight three future directions for both CV and NLP\nresearchers to provide insightful guidance.", "cat": "cs.CV", "authors": ["Siqu Long", "Feiqi Cao", "Soyeon Caren Han", "Haiqin Yang"]}, "1581": {"id": "2111.10219v1", "title": "A Survey on Rural Internet Connectivity in India", "url": "http://arxiv.org/pdf/2111.10219v1", "date": "2021-08-26 15:07:59", "abs": "Rural connectivity is widely research topic for several years. In India,\naround 70% of the population have poor or no connectivity to access digital\nservices. Different solutions are being tested and trialled around the world,\nespecially in India. They key driving factor for reducing digital divide is\nexploring different solutions both technologically and economically to lower\nthe cost for the network deployments and improving service adoption rate. In\nthis survey, we aim to study the rural connectivity use-cases, state of art\nprojects and initiatives, challenges, and technologies to improve digital\nconnectivity in rural parts of India. The strengths and weakness of different\ntechnologies which are being tested for rural connectivity is analyzed. We also\nexplore the rural use-case of 6G communication system which would be suitable\nfor rural Indian scenario.", "cat": "cs.NI", "authors": ["Shruthi K A", "Ihita G V", "Sachin Chaudhari"]}, "1582": {"id": "2207.12599v2", "title": "A Survey of Explainable Graph Neural Networks: Taxonomy and Evaluation Metrics", "url": "http://arxiv.org/pdf/2207.12599v2", "date": "2023-05-23 03:32:23", "abs": "Graph neural networks (GNNs) have demonstrated a significant boost in\nprediction performance on graph data. At the same time, the predictions made by\nthese models are often hard to interpret. In that regard, many efforts have\nbeen made to explain the prediction mechanisms of these models from\nperspectives such as GNNExplainer, XGNN and PGExplainer. Although such works\npresent systematic frameworks to interpret GNNs, a holistic review for\nexplainable GNNs is unavailable. In this survey, we present a comprehensive\nreview of explainability techniques developed for GNNs. We focus on explainable\ngraph neural networks and categorize them based on the use of explainable\nmethods. We further provide the common performance metrics for GNNs\nexplanations and point out several future research directions.", "cat": "cs.LG", "authors": ["Yiqiao Li", "Jianlong Zhou", "Sunny Verma", "Fang Chen"]}, "1583": {"id": "1808.10700v2", "title": "Kiloparsec Scale Properties of Star-Formation Driven Outflows at z~2.3 in the SINS/zC-SINF AO Survey", "url": "http://arxiv.org/pdf/1808.10700v2", "date": "2019-02-14 10:50:54", "abs": "We investigate the relationship between star formation activity and outflow\nproperties on kiloparsec scales in a sample of 28 star forming galaxies at\n$z\\sim$ 2-2.6, using adaptive optics assisted integral field observations from\nSINFONI on the VLT. The narrow and broad components of the H$\\alpha$ emission\nare used to simultaneously determine the local star formation rate surface\ndensity ($\\Sigma_{\\rm SFR}$), and the outflow velocity $v_{\\rm out}$ and mass\noutflow rate $\\dot{M}_{\\rm out}$, respectively. We find clear evidence for\nfaster outflows with larger mass loading factors at higher $\\Sigma_{\\rm SFR}$.\nThe outflow velocities scale as $v_{\\rm out}$ $\\propto$ $\\Sigma_{\\rm SFR}^{0.34\n\\pm 0.10}$, which suggests that the outflows may be driven by a combination of\nmechanical energy released by supernova explosions and stellar winds, as well\nas radiation pressure acting on dust grains. The majority of the outflowing\nmaterial does not have sufficient velocity to escape from the galaxy halos, but\nwill likely be re-accreted and contribute to the chemical enrichment of the\ngalaxies. In the highest $\\Sigma_{\\rm SFR}$ regions the outflow component\ncontains an average of $\\sim$45% of the H$\\alpha$ flux, while in the lower\n$\\Sigma_{\\rm SFR}$ regions only $\\sim$10% of the H$\\alpha$ flux is associated\nwith outflows. The mass loading factor, $\\eta$ = $\\dot{M}_{\\rm out}$/SFR, is\npositively correlated with $\\Sigma_{\\rm SFR}$ but is relatively low even at the\nhighest $\\Sigma_{\\rm SFR}$: $\\eta \\lesssim$ 0.5 $\\times$ (380 cm$^{-3}$/n$_e$).\nThis may be in tension with the $\\eta$ $\\gtrsim$ 1 required by cosmological\nsimulations, unless a significant fraction of the outflowing mass is in other\ngas phases and has sufficient velocity to escape the galaxy halos.", "cat": "astro-ph.GA", "authors": ["Rebecca L. Davies", "Natascha M. F\u00f6rster Schreiber", "Hannah \u00dcbler", "Reinhard Genzel", "Dieter Lutz", "Alvio Renzini", "Sandro Tacchella", "Linda J. Tacconi", "Sirio Belli", "Andreas Burkert", "C. Marcella Carollo", "Richard I. Davies", "Rodrigo Herrera-Camus", "Simon J. Lilly", "Chiara Mancini", "Thorsten Naab", "Erica J. Nelson", "Sedona H. Price", "Thomas Taro Shimizu", "Amiel Sternberg", "Emily Wisnioski", "Stijn Wuyts"]}, "1584": {"id": "2208.07399v3", "title": "A Survey of Recommender System Techniques and the Ecommerce Domain", "url": "http://arxiv.org/pdf/2208.07399v3", "date": "2023-02-21 14:57:33", "abs": "In this big data era, it is hard for the current generation to find the right\ndata from the huge amount of data contained within online platforms. In such a\nsituation, there is a need for an information filtering system that might help\nthem find the information they are looking for. In recent years, a research\nfield has emerged known as recommender systems. Recommenders have become\nimportant as they have many real-life applications. This paper reviews the\ndifferent techniques and developments of recommender systems in e-commerce,\ne-tourism, e-resources, e-government, e-learning, and e-library. By analyzing\nrecent work on this topic, we will be able to provide a detailed overview of\ncurrent developments and identify existing difficulties in recommendation\nsystems. The final results give practitioners and researchers the necessary\nguidance and insights into the recommendation system and its application.", "cat": "cs.IR", "authors": ["Imran Hossain", "Md Aminul Haque Palash", "Anika Tabassum Sejuty", "Noor A Tanjim", "MD Abdullah AL Nasim", "Sarwar Saif", "Abu Bokor Suraj", "Md Mahim Anjum Haque", "Nazmul Karim"]}, "1585": {"id": "1507.07564v2", "title": "Sagittarius II, Draco II and Laevens 3: three new Milky Way satellites discovered in the Pan-STARRS 1 3pi Survey", "url": "http://arxiv.org/pdf/1507.07564v2", "date": "2015-10-31 09:47:15", "abs": "We present the discovery of three new Milky Way satellites from our search\nfor compact stellar overdensities in the photometric catalog of the Panoramic\nSurvey Telescope and Rapid Response System 1 (Pan-STARRS 1, or PS1) 3pi survey.\nThe first satellite, Laevens 3, is located at a heliocentric distance of\nd=67+/-3 kpc. With a total magnitude of Mv=-4.4+/-0.3 and a half-light radius\nrh=7+/-2 pc, its properties resemble those of outer halo globular clusters. The\nsecond system, Draco II/Laevens 4 (Dra II), is a closer and fainter satellite\n(d~20 kpc, Mv =-2.9+/-0.8), whose uncertain size (rh = 19 +8/-6 pc) renders its\nclassification difficult without kinematic information; it could either be a\nfaint and extended globular cluster or a faint and compact dwarf galaxy. The\nthird satellite, Sagittarius II/Laevens 5 (Sgr II), has an ambiguous nature as\nit is either the most compact dwarf galaxy or the most extended globular\ncluster in its luminosity range (rh = 37 +9/-8 pc and Mv=-5.2+/-0.4). At a\nheliocentric distance of 67+/-5 kpc, this satellite lies intriguingly close to\nthe expected location of the trailing arm of the Sagittarius stellar stream\nbehind the Sagittarius dwarf spheroidal galaxy (Sgr dSph). If confirmed through\nspectroscopic follow up, this connection would locate this part of the trailing\narm of the Sagittarius stellar stream that has so far gone undetected. It would\nfurther suggest that Sgr II was brought into the Milky Way halo as a satellite\nof the Sgr dSph.", "cat": "astro-ph.GA", "authors": ["Benjamin P. M. Laevens", "Nicolas F. Martin", "Edouard J. Bernard", "Edward F. Schlafly", "Branimir Sesar", "Hans-Walter Rix", "Eric F. Bell", "Annette M. N. Ferguson", "Colin T. Slater", "William E. Sweeney", "Rosemary F. G. Wyse", "Avon P. Huxor", "William S. Burgett", "Kenneth C. Chambers", "Peter W. Draper", "Eugene A. Magnier", "Nigel Metcalfe", "John L. Tonry", "Richard J. Wainscoat", "Christopher Waters"]}, "1586": {"id": "2003.12471v1", "title": "Towards Autonomous Industrial-Scale Bathymetric Surveying", "url": "http://arxiv.org/pdf/2003.12471v1", "date": "2020-03-27 15:31:00", "abs": "Both higher efficiency and cost reduction can be gained from automating\nbathymetric surveying for offshore applications such as pipeline,\ntelecommunication or power cables installation and inspection on the seabed. We\npresent a SLAM system that optimizes the geo-referencing of bathymetry surveys\nby fusing the dead-reckoning sensor data from the surveying vehicle with\nconstraints from the maximization of the geometric consistency of overlapping\nregions of the survey. The framework has been extensively tested on bathymetric\nmaps from both simulation and several actual industrial surveys and has proved\nrobustness over different types of terrain. We demonstrate that our system is\nable to maximize the consistency of the final map even when there are large\nsections of the survey with reduced topographic variation. The framework has\nbeen made publicly available together with the simulation environment used to\ntest it and some of the datasets.", "cat": "cs.RO", "authors": ["Ignacio Torrobam Nils Bore", "John Folkesson"]}, "1587": {"id": "1712.04454v2", "title": "Robo-AO Kepler Survey IV: the effect of nearby stars on 3857 planetary candidate systems", "url": "http://arxiv.org/pdf/1712.04454v2", "date": "2018-03-08 16:35:44", "abs": "We present the overall statistical results from the Robo-AO Kepler planetary\ncandidate survey, comprising of 3857 high-angular resolution observations of\nplanetary candidate systems with Robo-AO, an automated laser adaptive optics\nsystem. These observations reveal previously unknown nearby stars blended with\nthe planetary candidate host star which alter the derived planetary radii or\nmay be the source of an astrophysical false positive transit signal. In the\nfirst three papers in the survey, we detected 440 nearby stars around 3313\nplanetary candidate host stars. In this paper, we present observations of 532\nplanetary candidate host stars, detecting 94 companions around 88 stars; 84 of\nthese companions have not previously been observed in high-resolution. We also\nreport 50 more-widely-separated companions near 715 targets previously observed\nby Robo-AO. We derive corrected planetary radius estimates for the 814\nplanetary candidates in systems with a detected nearby star. If planetary\ncandidates are equally likely to orbit the primary or secondary star, the\nradius estimates for planetary candidates in systems with likely bound nearby\nstars increase by a factor of 1.54, on average. We find that 35\npreviously-believed rocky planet candidates are likely not rocky due to the\npresence of nearby stars. From the combined data sets from the complete Robo-AO\nKOI survey, we find that 14.5\\pm0.5% of planetary candidate hosts have a nearby\nstar with 4\", while 1.2% have two nearby stars and 0.08% have three. We find\nthat 16% of Earth-sized, 13% of Neptune-sized, 14% of Saturn-sized, and 19% of\nJupiter-sized planet candidates have detected nearby stars.", "cat": "astro-ph.EP", "authors": ["Carl Ziegler", "Nicholas M. Law", "Christoph Baranec", "Reed Riddle", "Dmitry A. Duev", "Ward Howard", "Rebecca Jensen-Clem", "S. R. Kulkarni", "Tim Morton", "Ma\u00efssa Salama"]}, "1588": {"id": "2211.01821v1", "title": "A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).XIV. The main sequence relation in a rich environment down to M_star ~ 10^6 Mo", "url": "http://arxiv.org/pdf/2211.01821v1", "date": "2022-11-03 14:00:32", "abs": "Using a compilation of Halpha fluxes for 384 star forming galaxies detected\nduring the VESTIGE survey, we study several important scaling relations for a\ncomplete sample of galaxies in a rich environment. The extraordinary\nsensitivity of the data allows us to sample the whole dynamic range of the\nHalpha luminosity function, from massive (M*~10^11 Mo) to dwarf systems\n(M*~10^6 Mo). This extends previous works to a dynamic range in stellar mass\nand star formation rate (10^-4 1),\nwith the sample average V$_{C}$/{\\sigma}$_{int}$ value much smaller than at\nlower redshift. After carefully selecting comparable star-forming samples at\nmultiple epochs, we find that the rotation-dominated fraction evolves with\nredshift with a z$^{-0.2}$ dependence. The rotation-dominated KDS galaxies show\nno clear offset from the local rotation velocity-stellar mass (i.e.\nV$_{C}$-M$_{\\star}$) relation, although a smaller fraction of the galaxies are\non the relation due to the increase in the dispersion-dominated fraction. These\nobservations are consistent with a simple equilibrium model picture, in which\nrandom motions are boosted in high redshift galaxies by a combination of the\nincreasing gas fractions, accretion efficiency, specific star-formation rate\nand stellar feedback and which may provide significant pressure support against\ngravity on the galactic disk scale.", "cat": "astro-ph.GA", "authors": ["O. J. Turner", "M. Cirasuolo", "C. M. Harrison", "R. J. McLure", "J. S. Dunlop", "A. M. Swinbank", "H. L. Johnson", "D. Sobral", "J. Matthee", "R. M. Sharples"]}, "1590": {"id": "2106.13733v3", "title": "Graph and hypergraph colouring via nibble methods: A survey", "url": "http://arxiv.org/pdf/2106.13733v3", "date": "2021-11-16 08:54:16", "abs": "This paper provides a survey of methods, results, and open problems on graph\nand hypergraph colourings, with a particular emphasis on semi-random `nibble'\nmethods. We also give a detailed sketch of some aspects of the recent proof of\nthe Erd\\H{o}s-Faber-Lov\\'{a}sz conjecture.", "cat": "math.CO", "authors": ["Dong Yeap Kang", "Tom Kelly", "Daniela K\u00fchn", "Abhishek Methuku", "Deryk Osthus"]}, "1591": {"id": "1507.05977v1", "title": "Cross-correlation cosmic shear with the SDSS and VLA FIRST surveys", "url": "http://arxiv.org/pdf/1507.05977v1", "date": "2015-07-21 20:08:55", "abs": "We measure the cosmic shear power spectrum on large angular scales by\ncross-correlating the shapes of ~9 million galaxies measured in the optical\nSDSS survey with the shapes of ~2.7x10^5 radio galaxies measured by the\noverlapping VLA-FIRST survey. Our measurements span the multipole range 10 < l\n< 130, corresponding to angular scales 2deg < {\\theta} < 20deg. On these\nscales, the shear maps from both surveys suffer from significant systematic\neffects that prohibit a measurement of the shear power spectrum from either\nsurvey alone. Conversely we demonstrate that a power spectrum measured by\ncross-correlating the two surveys is unbiased.\n We measure an E-mode power spectrum from the data that is inconsistent with\nzero signal at the 99\\% confidence (~2.7{\\sigma}) level. The odd-parity B-mode\nsignal and the EB cross- correlation are both found to be consistent with zero\n(within 1{\\sigma}). These constraints are obtained after a careful error\nanalysis that accounts for uncertainties due to cosmic variance, random galaxy\nshape noise and shape measurement errors, as well as additional errors\nassociated with the observed large-scale systematic effects in the two surveys.\nOur constraints are consistent with the expected signal in the concordance\ncosmological model assuming recent estimates of the cosmological parameters\nfrom the Planck satellite, and literature values for the median redshifts of\nthe SDSS and FIRST galaxy populations.\n The cross-power spectrum approach described in this paper represents a\npowerful technique for mitigating shear systematics and will be ideal for\nextracting robust results, with the exquisite control of systematics required,\nfrom future cosmic shear surveys with the SKA, LSST, Euclid and WFIRST-AFTA.", "cat": "astro-ph.CO", "authors": ["Constantinos Demetroullas", "Michael L. Brown"]}, "1592": {"id": "2406.20023v1", "title": "The Mean Longitudinal Magnetic Field and its Uses in Radial-Velocity Surveys", "url": "http://arxiv.org/pdf/2406.20023v1", "date": "2024-06-28 16:13:50", "abs": "This work focuses on the analysis of the mean longitudinal magnetic field as\na stellar activity tracer in the context of small exoplanet detection and\ncharacterisation in radial-velocity (RV) surveys. We use SDO/HMI filtergrams to\nderive Sun-as-a-star magnetic field measurements, and show that the mean\nlongitudinal magnetic field is an excellent rotational period detector and a\nuseful tracer of the solar magnetic cycle. To put these results into context,\nwe compare the mean longitudinal magnetic field to three common activity\nproxies derived from HARPS-N Sun-as-a-star data: the full-width at\nhalf-maximum, the bisector span and the S-index. The mean longitudinal magnetic\nfield does not correlate with the RVs and therefore cannot be used as a\none-to-one proxy. However, with high cadence and a long baseline, the mean\nlongitudinal magnetic field outperforms all other considered proxies as a solar\nrotational period detector, and can be used to inform our understanding of the\nphysical processes happening on the surface of the Sun. We also test the mean\nlongitudinal magnetic field as a \"stellar proxy\" on a reduced solar dataset to\nsimulate stellar-like observational sampling. With a Gaussian Process\nregression analysis, we confirm that the solar mean longitudinal magnetic field\nis the most effective of the considered indicators, and is the most efficient\nrotational period indicator over different levels of stellar activity. This\nwork highlights the need for polarimetric time series observations of stars.", "cat": "astro-ph.SR", "authors": ["F. Rescigno", "A. Mortier", "X. Dumusque", "B. S. Lakeland", "R. Haywood", "N. Piskunov", "B. A. Nicholson", "M. L\u00f3pez-Morales", "S. Dalal", "M. Cretignier", "B. Klein", "A. Collier Cameron", "A. Ghedina", "M. Gonzalez", "R. Cosentino", "A. Sozzetti", "S. H. Saar"]}, "1593": {"id": "0903.4136v1", "title": "Downsizing of supermassive black holes from the SDSS quasar survey", "url": "http://arxiv.org/pdf/0903.4136v1", "date": "2009-03-24 17:06:33", "abs": "Starting from the ~50000 quasars of the Sloan Digital Sky Survey for which\nMgII line width and 3000 A monochromatic flux are available, we aim to study\nthe dependence of the mass of active black holes on redshift. We focus on the\nobserved distribution in the FWHM - nuclear luminosity plane, which can be\nreproduced at all redshifts assuming a limiting BH mass, a maximum Eddington\nratio and a minimum luminosity (due to the survey flux limit). We study the\nz-dependence of the best fit parameters of assumed distributions at increasing\nredshift and find that the maximum mass of the quasar population evolves as\nlog[M_BH(max)/M_Sun]~0.3z+9, while the maximum Eddington ratio (~0.45) is\npractically independent of cosmic time. These results are unaffected by the\nMalmquist bias.", "cat": "astro-ph.CO", "authors": ["Marzia Labita", "Roberto Decarli", "Aldo Treves", "Renato Falomo"]}, "1594": {"id": "1410.3838v1", "title": "The Hector Survey: integral field spectroscopy of 100,000 galaxies", "url": "http://arxiv.org/pdf/1410.3838v1", "date": "2014-10-14 20:01:59", "abs": "In March 2013, the Sydney--AAO Multi-object Integral field spectrograph\n(SAMI) began a major survey of 3400 galaxies at the AAT, the largest of its\nkind to date. At the time of writing, over a third of the targets have been\nobserved and the scientific impact has been immediate. The Manga galaxy survey\nhas now started at the SDSS telescope and will target an even larger sample of\nnearby galaxies. In Australia, the community is now gearing up to deliver a\nmajor new facility called Hector that will allow integral field spectroscopy of\n100 galaxies observed simultaneously. By the close of the decade, it will be\npossible to obtain integral field spectroscopy of 100,000 galaxies over 3000\nsquare degrees of sky down to r=17 (median). Many of these objects will have HI\nimaging from the new ASKAP radio surveys. We discuss the motivation for such a\nsurvey and the use of new cosmological simulations that are properly matched to\nthe integral field observations. The Hector survey will open up a new and\nunique parameter space for galaxy evolution studies.", "cat": "astro-ph.GA", "authors": ["Joss Bland-Hawthorn"]}, "1595": {"id": "1902.07913v1", "title": "A Comprehensive Survey of Interface Protocols for Software Defined Networks", "url": "http://arxiv.org/pdf/1902.07913v1", "date": "2019-02-21 08:45:19", "abs": "Software Defined Networks has seen tremendous growth and deployment in\ndifferent types of networks. Compared to traditional networks it decouples the\ncontrol logic from network layer devices, and centralizes it for efficient\ntraffic forwarding and flow management across the domain. This multi-layered\narchitecture has data forwarding devices at the bottom in data plane, which are\nprogrammed by controllers in the control plane. The high level application or\nmanagement plane interacts with control layer to program the whole network and\nenforce different policies. The interaction among these layers is done through\ninterfaces which work as communication/programming protocols. In this survey,\nwe present a comprehensive study of such interfaces available for southbound,\nnorthbound, and east/westbound communication. We have classified each type into\ndifferent categories based on their properties and capabilities. Virtualization\nof networks devices is a common practice in Software Defined Networks. This\npaper also analyzes interface solution which work with different virtualization\nschemes. In addition, the paper highlights a number of short term and long term\nresearch challenges and open issues related to SDN interfaces.", "cat": "cs.NI", "authors": ["Zohaib Latif", "Kashif Sharif", "Fan Li", "Md Monjurul Karim", "Yu Wang"]}, "1596": {"id": "1705.03049v1", "title": "Dust Abundance Variations in the Magellanic Clouds: Probing the Lifecycle of Metals with All-Sky Surveys", "url": "http://arxiv.org/pdf/1705.03049v1", "date": "2017-05-08 18:55:39", "abs": "Observations and modeling suggest that the dust abundance (gas-to-dust ratio,\nG/D) depends on (surface) density. The variations of the G/D provide\nconstraints on the timescales for the different processes involved in the\nlifecycle of metals in galaxies. Recent G/D measurements based on Herschel data\nsuggest a factor 5---10 decrease in the dust abundance between the dense and\ndiffuse interstellar medium (ISM) in the Magellanic Clouds. However, the\nrelative nature of the Herschel measurements precludes definitive conclusions\non the magnitude of those variations. We investigate the variations of the dust\nabundance in the LMC and SMC using all-sky far-infrared surveys, which do not\nsuffer from the limitations of Herschel on their zero-point calibration. We\nstack the dust spectral energy distribution (SED) at 100, 350, 550, and 850\nmicrons from IRAS and Planck in intervals of gas surface density, model the\nstacked SEDs to derive the dust surface density, and constrain the relation\nbetween G/D and gas surface density in the range 10---100 \\Msu pc$^{-2}$ on\n$\\sim$ 80 pc scales. We find that G/D decreases by factors of 3 (from 1500 to\n500) in the LMC and 7 (from 1.5$\\times 10^4$ to 2000) in the SMC between the\ndiffuse and dense ISM. The surface density dependence of G/D is consistent with\nelemental depletions and with simple modeling of the accretion of gas-phase\nmetals onto dust grains. This result has important implications for the\nsub-grid modeling of galaxy evolution, and for the calibration of dust-based\ngas mass estimates, both locally and at high-redshift.", "cat": "astro-ph.GA", "authors": ["Julia Roman-Duval", "Caroline Bot", "Jeremy Chastenet", "Karl Gordon"]}, "1597": {"id": "2011.05847v1", "title": "A Survey and Implementation of Performance Metrics for Self-Organized Maps", "url": "http://arxiv.org/pdf/2011.05847v1", "date": "2020-11-11 15:28:33", "abs": "Self-Organizing Map algorithms have been used for almost 40 years across\nvarious application domains such as biology, geology, healthcare, industry and\nhumanities as an interpretable tool to explore, cluster and visualize\nhigh-dimensional data sets. In every application, practitioners need to know\nwhether they can \\textit{trust} the resulting mapping, and perform model\nselection to tune algorithm parameters (e.g. the map size). Quantitative\nevaluation of self-organizing maps (SOM) is a subset of clustering validation,\nwhich is a challenging problem as such. Clustering model selection is typically\nachieved by using clustering validity indices. While they also apply to\nself-organized clustering models, they ignore the topology of the map, only\nanswering the question: do the SOM code vectors approximate well the data\ndistribution? Evaluating SOM models brings in the additional challenge of\nassessing their topology: does the mapping preserve neighborhood relationships\nbetween the map and the original data? The problem of assessing the performance\nof SOM models has already been tackled quite thoroughly in literature, giving\nbirth to a family of quality indices incorporating neighborhood constraints,\ncalled \\textit{topographic} indices. Commonly used examples of such metrics are\nthe topographic error, neighborhood preservation or the topographic product.\nHowever, open-source implementations are almost impossible to find. This is the\nissue we try to solve in this work: after a survey of existing SOM performance\nmetrics, we implemented them in Python and widely used numerical libraries, and\nprovide them as an open-source library, SOMperf. This paper introduces each\nmetric available in our module along with usage examples.", "cat": "cs.NE", "authors": ["Florent Forest", "Mustapha Lebbah", "Hanane Azzag", "J\u00e9r\u00f4me Lacaille"]}, "1598": {"id": "1407.3502v1", "title": "Automated Real-Time Classification and Decision Making in Massive Data Streams from Synoptic Sky Surveys", "url": "http://arxiv.org/pdf/1407.3502v1", "date": "2014-07-13 19:09:30", "abs": "The nature of scientific and technological data collection is evolving\nrapidly: data volumes and rates grow exponentially, with increasing complexity\nand information content, and there has been a transition from static data sets\nto data streams that must be analyzed in real time. Interesting or anomalous\nphenomena must be quickly characterized and followed up with additional\nmeasurements via optimal deployment of limited assets. Modern astronomy\npresents a variety of such phenomena in the form of transient events in digital\nsynoptic sky surveys, including cosmic explosions (supernovae, gamma ray\nbursts), relativistic phenomena (black hole formation, jets), potentially\nhazardous asteroids, etc. We have been developing a set of machine learning\ntools to detect, classify and plan a response to transient events for astronomy\napplications, using the Catalina Real-time Transient Survey (CRTS) as a\nscientific and methodological testbed. The ability to respond rapidly to the\npotentially most interesting events is a key bottleneck that limits the\nscientific returns from the current and anticipated synoptic sky surveys.\nSimilar challenge arise in other contexts, from environmental monitoring using\nsensor networks to autonomous spacecraft systems. Given the exponential growth\nof data rates, and the time-critical response, we need a fully automated and\nrobust approach. We describe the results obtained to date, and the possible\nfuture developments.", "cat": "astro-ph.IM", "authors": ["S. G. Djorgovski", "A. A. Mahabal", "C. Donalek", "M. J. Graham", "A. J. Drake", "M. Turmon", "T. Fuchs"]}, "1599": {"id": "1305.3917v1", "title": "A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys", "url": "http://arxiv.org/pdf/1305.3917v1", "date": "2013-05-16 20:00:03", "abs": "We present an investigation into how well the properties of the accretion\nflow onto a supermassive black hole may be coupled to those of the overlying\nhot corona. To do so, we specifically measure the characteristic spectral\nindex, Gamma, of a power-law energy distribution, over an energy range of 2 to\n10 keV, for X-ray selected, broad-lined radio-quiet AGN up to z~2 in COSMOS and\nE-CDF-S. We test the previously reported dependence between Gamma and black\nhole mass, FWHM and Eddington ratio using a sample of AGN covering a broad\nrange in these parameters based on both the Mg ii and H-alpha emission lines\nwith the later afforded by recent near infrared spectroscopic observations\nusing Subaru/FMOS. We calculate the Eddington ratios, lambda_Edd, for sources\nwhere a bolometric luminosity (L_Bol) has been presented in the literature,\nbased on SED fitting, or, for sources where these data do not exist, we\ncalculate L_Bol using a bolometric correction to the LX, derived from a\nrelationship between the bolometric correction, and LX/L3000. From a sample of\n69 X-ray bright sources (>250 counts), where Gamma can be measured with\ngreatest precision, with an estimate of L_Bol, we find a statistically\nsignificant correlation between Gamma and lambda_Edd, which is highly\nsignificant with a chance probability of 6.59x10^-8. A statistically\nsignificant correlation between Gamma and the FWHM of the optical lines is\nconfirmed, but at lower significance than with lambda_Edd indicating that\nlambda_Edd is the key parameter driving conditions in the corona. Linear\nregression analysis reveals that Gamma=(0.32+/-0.05)log10\nlambda_Edd+(2.27+/-0.06) and\nGamma=(-0.69+/-0.11)log10(FWHM/km/s)+(4.44+/-0.42). Our results on\nGamma-lambda_Edd are in very good agreement with previous results. (ABRIDGED)", "cat": "astro-ph.HE", "authors": ["M. Brightman", "J. D. Silverman", "V. Mainieri", "Y. Ueda", "M. Schramm", "K. Matsuoka", "T. Nagao", "C. Steinhardt", "J. Kartaltepe", "D. B. Sanders", "E. Treister", "O. Shemmer", "W. N. Brandt", "M. Brusa", "A. Comastri", "L. C. Ho", "G. Lanzuisi", "E. Lusso", "K. Nandra", "M. Salvato", "G. Zamorani", "M. Akiyama", "D. M. Alexander", "A. Bongiorno", "P. Capak", "F. Civano", "A. Del Moro", "A. Doi", "M. Elvis", "G. Hasinger", "E. S. Laird", "D. Masters", "M. Mignoli", "K. Ohta", "K. Schawinski", "Y. Taniguchi"]}, "1600": {"id": "1907.09408v2", "title": "A Survey of Deep Learning-based Object Detection", "url": "http://arxiv.org/pdf/1907.09408v2", "date": "2019-10-10 17:09:59", "abs": "Object detection is one of the most important and challenging branches of\ncomputer vision, which has been widely applied in peoples life, such as\nmonitoring security, autonomous driving and so on, with the purpose of locating\ninstances of semantic objects of a certain class. With the rapid development of\ndeep learning networks for detection tasks, the performance of object detectors\nhas been greatly improved. In order to understand the main development status\nof object detection pipeline, thoroughly and deeply, in this survey, we first\nanalyze the methods of existing typical detection models and describe the\nbenchmark datasets. Afterwards and primarily, we provide a comprehensive\noverview of a variety of object detection methods in a systematic manner,\ncovering the one-stage and two-stage detectors. Moreover, we list the\ntraditional and new applications. Some representative branches of object\ndetection are analyzed as well. Finally, we discuss the architecture of\nexploiting these object detection methods to build an effective and efficient\nsystem and point out a set of development trends to better follow the\nstate-of-the-art algorithms and further research.", "cat": "cs.CV", "authors": ["Licheng Jiao", "Fan Zhang", "Fang Liu", "Shuyuan Yang", "Lingling Li", "Zhixi Feng", "Rong Qu"]}, "1601": {"id": "2211.04324v1", "title": "Machine Learning-Aided Operations and Communications of Unmanned Aerial Vehicles: A Contemporary Survey", "url": "http://arxiv.org/pdf/2211.04324v1", "date": "2022-11-07 15:34:36", "abs": "The ongoing amalgamation of UAV and ML techniques is creating a significant\nsynergy and empowering UAVs with unprecedented intelligence and autonomy. This\nsurvey aims to provide a timely and comprehensive overview of ML techniques\nused in UAV operations and communications and identify the potential growth\nareas and research gaps. We emphasise the four key components of UAV operations\nand communications to which ML can significantly contribute, namely, perception\nand feature extraction, feature interpretation and regeneration, trajectory and\nmission planning, and aerodynamic control and operation. We classify the latest\npopular ML tools based on their applications to the four components and conduct\ngap analyses. This survey also takes a step forward by pointing out significant\nchallenges in the upcoming realm of ML-aided automated UAV operations and\ncommunications. It is revealed that different ML techniques dominate the\napplications to the four key modules of UAV operations and communications.\nWhile there is an increasing trend of cross-module designs, little effort has\nbeen devoted to an end-to-end ML framework, from perception and feature\nextraction to aerodynamic control and operation. It is also unveiled that the\nreliability and trust of ML in UAV operations and applications require\nsignificant attention before full automation of UAVs and potential cooperation\nbetween UAVs and humans come to fruition.", "cat": "cs.RO", "authors": ["Harrison Kurunathan", "Hailong Huang", "Kai Li", "Wei Ni", "Ekram Hossain"]}, "1602": {"id": "1509.06371v2", "title": "The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations in the correlation function of LOWZ and CMASS galaxies in Data Release 12", "url": "http://arxiv.org/pdf/1509.06371v2", "date": "2016-01-11 15:08:52", "abs": "We present distance scale measurements from the baryon acoustic oscillation\nsignal in the CMASS and LOWZ samples from the Data Release 12 of the Baryon\nOscillation Spectroscopic Survey (BOSS). The total volume probed is 14.5\nGpc$^3$, a 10 per cent increment from Data Release 11. From an analysis of the\nspherically averaged correlation function, we infer a distance to $z=0.57$ of\n$D_V(z)r^{\\rm fid}_{\\rm d}/r_ {\\rm d}=2028\\pm21$ Mpc and a distance to $z=0.32$\nof $D_V(z)r^{\\rm fid}_{\\rm d}/r_{\\rm d}=1264\\pm22$ Mpc assuming a cosmology in\nwhich $r^{\\rm fid}_{\\rm d}=147.10$ Mpc. From the anisotropic analysis, we find\nan angular diameter distance to $z=0.57$ of $D_{\\rm A}(z)r^{\\rm fid}_{\\rm\nd}/r_{\\rm d}=1401\\pm21$ Mpc and a distance to $z=0.32$ of $981\\pm20$ Mpc, a 1.5\nper cent and 2.0 per cent measurement respectively. The Hubble parameter at\n$z=0.57$ is $H(z)r_{\\rm d}/r^{\\rm fid}_{\\rm d}=100.3\\pm3.7$ km s$^{-1}$\nMpc$^{-1}$ and its value at $z=0.32$ is $79.2\\pm5.6$ km s$^{-1}$ Mpc$^{-1}$, a\n3.7 per cent and 7.1 per cent measurement respectively. These cosmic distance\nscale constraints are in excellent agreement with a $\\Lambda$CDM model with\ncosmological parameters released by the recent Planck 2015 results.", "cat": "astro-ph.CO", "authors": ["Antonio J. Cuesta", "Mariana Vargas-Maga\u00f1a", "Florian Beutler", "Adam S. Bolton", "Joel R. Brownstein", "Daniel J. Eisenstein", "H\u00e9ctor Gil-Mar\u00edn", "Shirley Ho", "Cameron K. McBride", "Claudia Maraston", "Nikhil Padmanabhan", "Will J. Percival", "Beth A. Reid", "Ashley J. Ross", "Nicholas P. Ross", "Ariel G. S\u00e1nchez", "David J. Schlegel", "Donald P. Schneider", "Daniel Thomas", "Jeremy Tinker", "Rita Tojeiro", "Licia Verde", "Martin White"]}, "1603": {"id": "2004.00216v3", "title": "Heterogeneous Network Representation Learning: A Unified Framework with Survey and Benchmark", "url": "http://arxiv.org/pdf/2004.00216v3", "date": "2020-12-17 01:44:03", "abs": "Since real-world objects and their interactions are often multi-modal and\nmulti-typed, heterogeneous networks have been widely used as a more powerful,\nrealistic, and generic superclass of traditional homogeneous networks (graphs).\nMeanwhile, representation learning (\\aka~embedding) has recently been\nintensively studied and shown effective for various network mining and\nanalytical tasks. In this work, we aim to provide a unified framework to deeply\nsummarize and evaluate existing research on heterogeneous network embedding\n(HNE), which includes but goes beyond a normal survey. Since there has already\nbeen a broad body of HNE algorithms, as the first contribution of this work, we\nprovide a generic paradigm for the systematic categorization and analysis over\nthe merits of various existing HNE algorithms. Moreover, existing HNE\nalgorithms, though mostly claimed generic, are often evaluated on different\ndatasets. Understandable due to the application favor of HNE, such indirect\ncomparisons largely hinder the proper attribution of improved task performance\ntowards effective data preprocessing and novel technical design, especially\nconsidering the various ways possible to construct a heterogeneous network from\nreal-world application data. Therefore, as the second contribution, we create\nfour benchmark datasets with various properties regarding scale, structure,\nattribute/label availability, and \\etc.~from different sources, towards handy\nand fair evaluations of HNE algorithms. As the third contribution, we carefully\nrefactor and amend the implementations and create friendly interfaces for 13\npopular HNE algorithms, and provide all-around comparisons among them over\nmultiple tasks and experimental settings.", "cat": "cs.SI", "authors": ["Carl Yang", "Yuxin Xiao", "Yu Zhang", "Yizhou Sun", "Jiawei Han"]}, "1604": {"id": "1806.10143v1", "title": "The Stripe 82 1-2 GHz Very Large Array Snapshot Survey: host galaxy properties and accretion rates of radio galaxies", "url": "http://arxiv.org/pdf/1806.10143v1", "date": "2018-06-26 18:00:02", "abs": "A sample of 1161 radio galaxies with $0.01 < z < 0.7$ and $10^{21} <\nL_{1.4~\\rm GHz} / \\textrm{W Hz}^{-1} < 10^{27}$ is selected from the Stripe 82\n1-2 GHz Karl G. Jansky Very Large Array Snapshot Survey, which covers 100\nsquare degrees and has a 1$\\sigma$ noise level of 88 $\\mu$Jy beam$^{-1}$.\nOptical spectra are used to classify these sources as high excitation and low\nexcitation radio galaxies (HERGs and LERGs), resulting in 60 HERGs, 149 LERGs\nand 600 `probable LERGs'. The host galaxies of the LERGs have older stellar\npopulations than those of the HERGs, in agreement with previous results in the\nliterature. We find that the HERGs tend to have higher Eddington-scaled\naccretion rates than the LERGs but that there is some overlap between the two\ndistributions. We show that the properties of the host galaxies vary\ncontinuously with accretion rate, with the most slowly accreting sources having\nthe oldest stellar populations, consistent with the idea that these sources\nlack a supply of cold gas. We find that 84 per cent of our sample release more\nthan 10 per cent of their accretion power in their jets, showing that\nmechanical AGN feedback is significantly underestimated in many hydrodynamical\nsimulations. There is a scatter of $\\sim 2$ dex in the fraction of the accreted\nAGN power deposited back into the ISM in mechanical form, showing that the\nassumption in many simulations that there is a direct scaling between accretion\nrate and radio-mode feedback does not necessarily hold. We also find that\nmechanical feedback is significant for many of the HERGs in our sample as well\nas the LERGs.", "cat": "astro-ph.GA", "authors": ["Imogen H. Whittam", "Matthew Prescott", "Kim McAlpine", "Matt J. Jarvis", "Ian Heywood"]}, "1605": {"id": "2010.06064v1", "title": "The End of Galaxy Surveys", "url": "http://arxiv.org/pdf/2010.06064v1", "date": "2020-10-12 22:57:11", "abs": "For nearly a century, imaging and spectroscopic surveys of galaxies have\ngiven us information about the contents of the universe. We attempt to define\nthe logical endpoint of such surveys by defining not the next galaxy survey,\nbut the final galaxy survey at NIR wavelengths; this would be the galaxy survey\nthat exhausts the information content useful for addressing extant questions.\nSuch a survey would require incredible advances in a number of technologies and\nthe survey details will depend on the as yet poorly constrained properties of\nthe earliest galaxies. Using an exposure time calculator, we define nominal\nsurveys for extracting the useful information for three science cases: dark\nenergy cosmology, galaxy evolution, and supernovae. We define scaling relations\nthat trade off sky background, telescope aperture, and focal plane size to\nallow for a survey of a given depth over a given area. For optimistic\nassumptions, a 280m telescope with a marginally resolved focal plane of 20\ndeg$^2$ operating at L2 could potentially exhaust the cosmological information\ncontent of galaxies in a 10 year survey. For galaxy evolution (making use of\ngravitational lensing to magnify the earliest galaxies) and SN, the same\ntelescope would suffice. We discuss the technological advances needed to\ncomplete the last galaxy survey. While the final galaxy survey remains well\noutside of our technical reach today, we present scaling relations that show\nhow we can progress toward the goal of exhausting the information content\nencoded in the shapes, positions, and colors of galaxies.", "cat": "astro-ph.GA", "authors": ["Jason Rhodes", "Eric Huff", "Daniel Masters", "Anna Nierenberg"]}, "1606": {"id": "1908.06825v1", "title": "Hunt's Hypothesis (H) for Markov Processes: Survey and Beyond", "url": "http://arxiv.org/pdf/1908.06825v1", "date": "2019-08-19 14:20:57", "abs": "The goal of this paper is threefold. First, we survey the existing results on\nHunt's hypothesis (H) for Markov processes and Getoor's conjecture for L\\'{e}vy\nprocesses. Second, we investigate (H) for multidimensional L\\'{e}vy processes\nfrom the viewpoints of projections and energy, respectively. Third, we present\na few open questions for further study.", "cat": "math.PR", "authors": ["Ze-Chun Hu", "Wei Sun"]}, "1607": {"id": "1211.4027v1", "title": "The Allen Telescope Array Pi GHz Sky Survey - III: The ELAIS-N1, Coma, and Lockman Hole Fields", "url": "http://arxiv.org/pdf/1211.4027v1", "date": "2012-11-16 21:00:00", "abs": "We present results from a total of 459 repeated 3.1 GHz radio continuum\nobservations (of which 379 were used in a search for transient sources) of the\nELAIS-N1, Coma, Lockman Hole, and NOAO Deep Wide Field Survey fields as part of\nthe Pi GHz Sky Survey (PiGSS). The observations were taken approximately once\nper day between 2009 May and 2011 April. Each image covers 11.8 square degrees\nand has 100 arcsecond FWHM resolution. Deep images for each of the four fields\nhave rms noise between 180 and 310 uJy and the corresponding catalogs contain\n~200 sources in each field. Typically 40 - 50 of these sources are detected in\neach single-epoch image. This represents one of the shortest cadence, largest\narea, multi-epoch surveys undertaken at these frequencies.\n We compare the catalogs generated from the combined images to those from\nindividual epochs, and from monthly averages, as well as to legacy surveys. We\nundertake a search for transients, with particular emphasis on excluding false\npositive sources. We find no confirmed transients, defined here as sources that\ncan be shown to have varied by at least a factor 10. However, we find one\nsource which brightened in a single-epoch image to at least six times the upper\nlimit from the corresponding deep image. We also find a source associated with\na z = 0.6 quasar which appears to have brightened by a factor of about three in\none of our deep images, when compared to catalogs from legacy surveys.\n We place new upper limits on the number of transients brighter than 10 mJy:\nfewer than 0.08 transients / sq. deg. with characteristic timescales of months\nto years; fewer than 0.02 / sq. deg. with timescales of months; and fewer than\n0.009 / sq. deg with timescales of days. We also plot upper limits as a\nfunction of flux density for transients on the same timescales.", "cat": "astro-ph.CO", "authors": ["Steve Croft", "Geoffrey C. Bower", "David Whysong"]}, "1608": {"id": "1412.3360v1", "title": "Range, Doppler and astrometric observables computed from Time Transfer Functions: a survey", "url": "http://arxiv.org/pdf/1412.3360v1", "date": "2014-12-10 16:35:42", "abs": "Determining range, Doppler and astrometric observables is of crucial interest\nfor modelling and analyzing space observations. We recall how these observables\ncan be computed when the travel time of a light ray is known as a function of\nthe positions of the emitter and the receiver for a given instant of reception\n(or emission). For a long time, such a function--called a reception (or\nemission) time transfer function--has been almost exclusively calculated by\nintegrating the null geodesic equations describing the light rays. However,\nother methods avoiding such an integration have been considerably developped in\nthe last twelve years. We give a survey of the analytical results obtained with\nthese new methods up to the third order in the gravitational constant $G$ for a\nmass monopole. We briefly discuss the case of quasi-conjunctions, where\nhigher-order enhanced terms must be taken into account for correctly\ncalculating the effects. We summarize the results obtained at the first order\nin $G$ when the multipole structure and the motion of an axisymmetric body is\ntaken into account. We present some applications to on-going or future missions\nlike Gaia and Juno. We give a short review of the recent works devoted to the\nnumerical estimates of the time transfer functions and their derivatives.", "cat": "gr-qc", "authors": ["A. Hees", "S. Bertone", "C. Le Poncin-Lafitte", "P. Teyssandier"]}, "1609": {"id": "1104.0884v1", "title": "The Non-Uniform Distribution of Galaxies from Data of the SDSS DR7 Survey", "url": "http://arxiv.org/pdf/1104.0884v1", "date": "2011-04-05 16:25:43", "abs": "We have analyzed the spatial distribution of galaxies from the release of the\nSloan Digital Sky Survey of galactic redshifts (SDSS DR7), applying the\ncomplete correlation function (conditional density), two-point conditional\ndensity (cylinder), and radial density methods. Our analysis demonstrates that\nthe conditional density has a power-law form for scales lengths 0.5-30 Mpc/h,\nwith the power-law corresponding to the fractal dimension D = 2.2+-0.2; for\nscale lengths in excess of 30 Mpc/h, it enters an essentially flat regime, as\nis expected for a uniform distribution of galaxies. However, in the analysis\napplying the cylinder method, the power-law character with D = 2.0+-0.3\npersists to scale lengths of 70 Mpc/h. The radial density method reveals\ninhomogeneities in the spatial distribution of galaxies on scales of 200 Mpc/h\nwith a density contrast of two, confirming that translation invariance is\nviolated in the distribution of galaxies to 300 Mpc/h, with the sampling depth\nof the SDSS galaxies being 600 Mpc/h.", "cat": "astro-ph.CO", "authors": ["A. O. Verevkin", "Yu. L. Bukhmastova", "Yu. V. Baryshev"]}, "1610": {"id": "1712.03844v2", "title": "The Galaxy-Halo Connection for $1.5\\lesssim z\\lesssim5$ as revealed by the \\emph{Spitzer} Matching survey of the UltraVISTA ultra-deep Stripes", "url": "http://arxiv.org/pdf/1712.03844v2", "date": "2018-01-11 15:10:23", "abs": "The \\emph{Spitzer} Matching Survey of the UltraVISTA ultra-deep Stripes\n(SMUVS) provides unparalleled depth at $3.6$ and $4.5$~$\\mu$m over\n$\\sim0.66$~deg$^2$ of the COSMOS field, allowing precise photometric\ndeterminations of redshift and stellar mass. From this unique dataset we can\nconnect galaxy samples, selected by stellar mass, to their host dark matter\nhalos for $1.5 10\ndegrees, respectively. The Second Palermo Swift-BAT hard X-ray catalogue\nincludes 1079 (86%) hard X-ray sources with an associated counterpart (26 with\na double association and 2 with a triple association) and 177 BAT excesses\n(14%) that still lack a counterpart. The distribution of the BAT sources among\nthe different object classes consists of 19% Galactic sources, 57%\nextragalactic sources, and 10% sources with a counterpart at softer energies\nwhose nature has not yet been determined. About half of the BAT associated\nsources lack a counterpart in the ROSAT catalogues. This suggests that either\nmoderate or strong absorption may be preventing their detection in the ROSAT\nenergy band. The comparison of our BAT catalogue with the Fermi Large Area\nTelescope First Source Catalogue identifies 59 BAT/Fermi correspondences: 48\nblazars, 3 Seyfert galaxies, 1 interacting galaxy, 3 high mass X-ray binaries,\nand 4 pulsars/supernova remnants. This small number of correspondences\nindicates that different populations make the sky shine in these two different\nenergy bands.", "cat": "astro-ph.HE", "authors": ["G. Cusumano", "V. La Parola", "A. Segreto", "C. Ferrigno", "A. Maselli", "B. Sbarufatti", "P. Romano", "G. Chincarini", "P. Giommi", "N. Masetti", "A. Moretti", "P. Parisi", "G. Tagliaferri"]}, "1616": {"id": "2209.11685v1", "title": "Opportunities for Technosignature Science in the Planetary Science and Astrobiology Decadal Survey", "url": "http://arxiv.org/pdf/2209.11685v1", "date": "2022-09-21 21:24:06", "abs": "Solar system exploration provides numerous possibilities for advancing\ntechnosignature science. The search for life in the solar system includes\nmissions designed to search for evidence of biosignatures on other planetary\nbodies, but many missions could also attempt to search for and constrain the\npresence of technology within the solar system. Technosignatures and\nbiosignatures represent complementary approaches toward searching for evidence\nof life in our solar neighborhood, and beyond. This report summarizes the\npotential technosignature opportunities within ongoing solar system exploration\nand the recommendations of the \"Origins, Worlds, and Life\" Planetary Science\nand Astrobiology Decadal Survey. We discuss opportunities for constraining the\nprevalence of technosignatures within the solar system using current or future\nmissions at negligible additional cost, and we present a preliminary assessment\nof gaps that may exist in the search for technosignatures within the solar\nsystem.", "cat": "astro-ph.IM", "authors": ["Jacob Haqq-Misra", "Reza Ashtari", "James Benford", "Jonathan Carroll-Nellenback", "Niklas A. D\u00f6bler", "Wael Farah", "Thomas J. Fauchez", "Vishal Gajjar", "David Grinspoon", "Advait Huggahalli", "Ravi K. Kopparapu", "Joseph Lazio", "George Profitiliotis", "Evan L. Sneed", "Savin Shynu Varghese", "Cl\u00e9ment Vidal"]}, "1617": {"id": "2209.04229v2", "title": "A survey on rational curves on complex surfaces", "url": "http://arxiv.org/pdf/2209.04229v2", "date": "2023-04-05 10:58:00", "abs": "In this survey we discuss the problem of the existence of rational curves on\ncomplex surfaces, both in the K\\\"ahler and non-K\\\"ahler setup. We\nsystematically go through the Enriques--Kodaira classification of complex\nsurfaces to highlight the different approaches applied to the study of rational\ncurves in each class. We also provide several examples and point out some open\nproblems.", "cat": "math.AG", "authors": ["Giuseppe Barbaro", "Filippo Fagioli", "\u00c1ngel David R\u00edos Ortiz"]}, "1618": {"id": "2007.10565v1", "title": "The Next Generation Virgo Cluster Survey (NGVS). XXX. Ultra-Diffuse Galaxies and their Globular Cluster Systems", "url": "http://arxiv.org/pdf/2007.10565v1", "date": "2020-07-21 02:17:27", "abs": "We present a study of ultra-diffuse galaxies (UDGs) in the Virgo Cluster\nbased on deep imaging from the Next Generation Virgo Cluster Survey (NGVS).\nApplying a new definition for the UDG class based on galaxy scaling relations,\nwe define samples of 44 and 26 UDGs using expansive and restrictive selection\ncriteria, respectively. Our UDG sample includes objects that are significantly\nfainter than previously known UDGs: i.e., more than half are fainter than\n$\\langle\\mu\\rangle_e \\sim27.5$ mag arcsec$^{-2}$. The UDGs in Virgo's core\nregion show some evidence for being structurally distinct from \"normal\" dwarf\ngalaxies, but this separation disappears when considering the full sample of\ngalaxies throughout the cluster. UDGs are more centrally concentrated in their\nspatial distribution than other Virgo galaxies of similar luminosity, while\ntheir morphologies demonstrate that at least some UDGs owe their diffuse nature\nto physical processes---such as tidal interactions or low-mass mergers---that\nare at play within the cluster environment. The globular cluster (GC) systems\nof Virgo UDGs have a wide range in specific frequency ($S_N$), with a higher\nmean $S_N$ than \"normal\" Virgo dwarfs, but a lower mean $S_N$ than Coma UDGs at\nfixed luminosity. Their GCs are predominantly blue, with a small contribution\nfrom red clusters in the more massive UDGs. The combined GC luminosity function\nis consistent with those observed in dwarf galaxies, showing no evidence of\nbeing anomalously luminous. The diversity in their morphologies and their GC\nproperties suggests no single process has given rise to all objects within the\nUDG class. Based on the available evidence, we conclude that UDGs are simply\nthose systems that occupy the extended tails of the galaxy size and surface\nbrightness distributions.", "cat": "astro-ph.GA", "authors": ["Sungsoon Lim", "Patrick C\u00f4t\u00e9", "Eric W. Peng", "Laura Ferrarese", "Joel C. Roediger", "Patrick R. Durrell", "J. Christopher Mihos", "Kaixiang Wang", "S. D. J. Gwyn", "Jean-Charles Cuillandre", "Chengze Liu", "Rub\u00e9n S\u00e1nchez-Janssen", "Elisa Toloba", "Laura V. Sales", "Puragra Guhathakurta", "Ariane Lan\u00e7on", "Thomas H. Puzia"]}, "1619": {"id": "2306.06313v4", "title": "The DESI One-Percent Survey: Exploring A Generalized SHAM for Multiple Tracers with the UNIT Simulation", "url": "http://arxiv.org/pdf/2306.06313v4", "date": "2023-11-14 14:07:10", "abs": "We perform SubHalo Abundance Matching (SHAM) studies on UNIT simulations with\n\\{$\\sigma, V_{\\rm ceil}, v_{\\rm smear}$\\}-SHAM and \\{$\\sigma, V_{\\rm\nceil},f_{\\rm sat}$\\}-SHAM. They are designed to reproduce the clustering on\n5--30$\\,\\hmpc$ of Luminous Red Galaxies (LRGs), Emission Line Galaxies (ELGs)\nand Quasi-Stellar Objects (QSOs) at $0.4100 clusters, or ~20% of\nthe full SPT-SZ sample.", "cat": "astro-ph.CO", "authors": ["M. B. Bayliss", "J. Ruel", "C. W. Stubbs", "S. W. Allen", "D. E. Applegate", "M. L. N. Ashby", "M. Bautz", "B. A. Benson", "L. E. Bleem", "S. Bocquet", "M. Brodwin", "R. Capasso", "J. E. Carlstrom", "C. L. Chang", "I. Chiu", "H-M. Cho", "A. Clocchiatti", "T. M. Crawford", "A. T. Crites", "T. de Haan", "S. Desai", "J. P. Dietrich", "M. A. Dobbs", "A. N. Doucouliagos", "R. J. Foley", "W. R. Forman", "G. P. Garmire", "E. M. George", "M. D. Gladders", "A. H. Gonzalez", "N. Gupta", "N. W. Halverson", "J. Hlavacek-Larrondo", "H. Hoekstra", "G. P. Holder", "W. L. Holzapfel", "Z. Hou", "J. D. Hrubes", "N. Huang", "C. Jones", "R. Keisler", "L. Knox", "A. T. Lee", "E. M. Leitch", "A. von der Linden", "D. Luong-Van", "A. Mantz", "D. P. Marrone", "M. McDonald", "J. J. McMahon", "S. S. Meyer", "L. M. Mocanu", "J. J. Mohr", "S. S. Murray", "S. Padin", "C. Pryke", "D. Rapetti", "C. L. Reichardt", "A. Rest", "J. E. Ruhl", "B. R. Saliwanchik", "A. Saro", "J. T. Sayre", "K. K. Schaffer", "T. Schrabback", "E. Shirokoff", "J. Song", "H. G. Spieler", "B. Stalder", "S. A. Stanford", "Z. Staniszewski", "A. A. Stark", "K. T. Story", "K. Vanderlinde", "J. D. Vieira", "A. Vikhlinin", "R. Williamson", "A. Zenteno"]}, "1621": {"id": "1901.01158v1", "title": "Continued Fractions and Generalizations with Many Limits: A Survey", "url": "http://arxiv.org/pdf/1901.01158v1", "date": "2019-01-03 03:34:14", "abs": "There are infinite processes (matrix products, continued fractions,\n$(r,s)$-matrix continued fractions, recurrence sequences) which, under certain\ncircumstances, do not converge but instead diverge in a very predictable way.\nWe give a survey of results in this area, focusing on recent results of the\nauthors.", "cat": "math.NT", "authors": ["Douglas Bowman", "James Mc Laughlin"]}, "1622": {"id": "1603.06885v1", "title": "SHELS: Complete Redshift Surveys of Two Widely Separated Fields", "url": "http://arxiv.org/pdf/1603.06885v1", "date": "2016-03-22 17:40:17", "abs": "The SHELS (Smithsonian Hectospec Lensing Survey) is a complete redshift\nsurvey covering two well-separated fields (F1 and F2) of the Deep Lens Survey.\nBoth fields are more than 94% complete to a Galactic extinction corrected R0 =\n20.2. Here we describe the redshift survey of the F1 field centered at R.A. =\n00h53m25.3s and Decl = 12d33m55s; like F2, the F1 field covers 4 sq deg. The\nredshift survey of the F1 field includes 9426 new galaxy redshifts measured\nwith Hectospec on the MMT (published here). As a guide to future uses of the\ncombined survey we compare the mass metallicity relation and the distributions\nof D4000 as a function of stellar mass and redshift for the two fields. The\nmass-metallicity relations differ by an insignificant 1.6 sigma. For galaxies\nin the stellar mass range 1.e10 to 1.e11 MSun, the increase in the star-forming\nfraction with redshift is remarkably similar in the two fields. The seemingly\nsurprising 31-38% difference in the overall galaxy counts in F1 and F2 is\nprobably consistent with the expected cosmic variance given the subtleties of\nthe relative systematics in the two surveys. We also review the Deep Lens\nSurvey cluster detections in the two fields: poorer photometric data for F1\nprecluded secure detection of the single massive cluster at z = 0.35 that we\nfind in SHELS. Taken together the two fields include 16,055 redshifts for\ngalaxies with R0 <= 20.2 and 20,754 redshifts for galaxies with R <= 20.6.\nThese dense surveys in two well-separated fields provide a basis for future\ninvestigations of galaxy properties and large-scale structure.", "cat": "astro-ph.GA", "authors": ["Margaret J. Geller", "Ho Seong Hwang", "Ian P. Dell'Antonio", "Harus Jabran Zahid", "Michael J. Kurtz", "Daniel G. Fabricant"]}, "1623": {"id": "1711.08973v1", "title": "A Survey and Taxonomy of Resource Optimisation for Executing Bag-of-Task Applications on Public Clouds", "url": "http://arxiv.org/pdf/1711.08973v1", "date": "2017-11-24 14:20:05", "abs": "Cloud computing has been widely adopted due to the flexibility in resource\nprovisioning and on-demand pricing models. Entire clusters of Virtual Machines\n(VMs) can be dynamically provisioned to meet the computational demands of\nusers. However, from a user's perspective, it is still challenging to utilise\ncloud resources efficiently. This is because an overwhelmingly wide variety of\nresource types with different prices and significant performance variations are\navailable.\n This paper presents a survey and taxonomy of existing research in optimising\nthe execution of Bag-of-Task applications on cloud resources. A BoT application\nconsists of multiple independent tasks, each of which can be executed by a VM\nin any order; these applications are widely used by both the scientific\ncommunities and commercial organisations. The objectives of this survey are as\nfollows: (i) to provide the reader with a concise understanding of existing\nresearch on optimising the execution of BoT applications on the cloud, (ii) to\ndefine a taxonomy that categorises current frameworks to compare and contrast\nthem, and (iii) to present current trends and future research directions in the\narea.", "cat": "cs.DC", "authors": ["Long Thai", "Blesson Varghese", "Adam Barker"]}, "1624": {"id": "1308.3349v1", "title": "High Ecliptic Latitude Survey for Small Main-Belt Asteroids", "url": "http://arxiv.org/pdf/1308.3349v1", "date": "2013-08-15 10:00:00", "abs": "Main-belt asteroids have been continuously colliding with one another since\nthey were formed. Its size distribution is primarily determined by the size\ndependence of asteroid strength against catastrophic impacts. The strength\nscaling law as a function of body size could depend on collision velocity, but\nthe relationship remains unknown especially under hypervelocity collisions\ncomparable to 10 km/sec. We present a wide-field imaging survey at ecliptic\nlatitude of around 25 deg for investigating the size distribution of small\nmain-belt asteroids which have highly inclined orbits. The analysis technique\nallowing for efficient asteroid detections and high-accuracy photometric\nmeasurements provide sufficient sample data to estimate the size distribution\nof sub-km asteroids with inclinations larger than 14 deg. The best-fit\npower-law slopes of the cumulative size distribution is 1.25 +/- 0.03 in the\ndiameter range of 0.6-1.0 km and 1.84 +/- 0.27 in 1.0-3.0 km. We provide a\nsimple size distribution model that takes into consideration the oscillations\nof the power-law slope due to the transition from the gravity-scaled regime to\nthe strength-scaled regime. We find that the high-inclination population has a\nshallow slope of the primary components of the size distribution compared to\nthe low-inclination populations. The asteroid population exposed to\nhypervelocity impacts undergoes collisional processes that large bodies have a\nhigher disruptive strength and longer life-span relative to tiny bodies than\nthe ecliptic asteroids.", "cat": "astro-ph.EP", "authors": ["Tsuyoshi Terai", "Jun Takahashi", "Yoichi Itoh"]}, "1625": {"id": "1010.1962v1", "title": "A Submillimeter Array Survey of Protoplanetary Disks in the Orion Nebula Cluster", "url": "http://arxiv.org/pdf/1010.1962v1", "date": "2010-10-10 20:03:30", "abs": "We present the full results of our 3-year long Submillimeter Array survey of\nprotoplanetary disks in the Orion Nebula Cluster. We imaged 23 fields at 880\nmicrons and 2 fields at 1330 microns, covering an area of ~6.5 arcmin^2 and\ncontaining 67 disks. We detected 42 disks with fluxes between 6-135 mJy and at\nrms noise levels between 0.6 to 5.3 mJy/beam. Thermal dust emission above any\nfree-free component was measured in 40 of the 42 detections, and the inferred\ndisk masses range from 0.003-0.07 Msolar. We find that disks located within 0.3\npc of theta^1 Ori C have a truncated mass distribution, while disks located\nbeyond 0.3 pc have masses more comparable to those found in low-mass star\nforming regions. The disk mass distribution in Orion has a distance dependence,\nwith a derived relationship max(M_(disk)) = 0.046Msolar(d/0.3pc)^0.33 for the\nmaximum disk masses. We found evidence of grain growth in disk 197-427, the\nonly disk detected at both 880 microns and 1330 microns with the SMA. Despite\nthe rapid erosion of the outer parts of the Orion disks by photoevaporation,\nthe potential for planet formation remains high in this massive star forming\nregion, with approximately 18% of the surveyed disks having masses greater than\nor equal to 0.01 Msolar within 60 AU.", "cat": "astro-ph.SR", "authors": ["Rita K. Mann", "Jonathan P. Williams"]}, "1626": {"id": "1912.01621v2", "title": "The ALPINE-ALMA [CII] Survey: Multi-Wavelength Ancillary Data and Basic Physical Measurements", "url": "http://arxiv.org/pdf/1912.01621v2", "date": "2020-03-13 02:24:23", "abs": "We present the ancillary data and basic physical measurements for the\ngalaxies in the ALMA Large Program to Investigate C+ at Early Times (ALPINE)\nsurvey - the first large multi-wavelength survey which aims at characterizing\nthe gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 < z\n< 5.9 via the measurement of [CII]-emission at 158 micro-meter (64% at\n>3.5$\\sigma$) and the surrounding far-infrared (FIR) continuum in conjunction\nwith a wealth of optical and near-infrared data. We outline in detail the\nspectroscopic data and selection of the galaxies as well as the ground- and\nspace-based imaging products. In addition, we provide several basic\nmeasurements including stellar masses, star formation rates (SFR), rest-frame\nultra-violet (UV) luminosities, UV continuum slopes ($\\beta$), and absorption\nline redshifts, as well as H-alpha emission derived from Spitzer colors. We\nfind that the ALPINE sample is representative of the 4 < z < 6 galaxy\npopulation selected by photometric methods and only slightly biased towards\nbluer colors ($\\Delta\\beta$ ~ 0.2). Using [CII] as tracer of the systemic\nredshift (confirmed for one galaxy at z=4.5 out of 118 for which we obtained\noptical [OII]$\\lambda$3727A emission), we confirm red shifted Ly-alpha emission\nand blue shifted absorption lines similar to findings at lower redshifts. By\nstacking the rest-frame UV spectra in the [CII] rest-frame we find that the\nabsorption lines in galaxies with high specific SFR are more blue shifted,\nwhich could be indicative of stronger winds and outflows.", "cat": "astro-ph.GA", "authors": ["A. L. Faisst", "D. Schaerer", "B. C. Lemaux", "P. A. Oesch", "Y. Fudamoto", "P. Cassata", "M. Bethermin", "P. L. Capak", "O. Le Fevre", "J. D. Silverman", "L. Yan", "M. Ginolfi", "A. M. Koekemoer", "L. Morselli", "R. Amorin", "S. Bardelli", "M. Boquien", "G. Brammer", "A. Cimatti", "M. Dessauges-Zavadsky", "S. Fujimoto", "C. Gruppioni", "N. P. Hathi", "S. Hemmati", "E. Ibar", "G. C. Jones", "Y. Khusanova", "F. Loiacono", "F. Pozzi", "M. Talia", "L. A. M. Tasca", "D. A. Riechers", "G. Rodighiero", "M. Romano", "N. Scoville", "S. Toft", "L. Vallini", "D. Vergani", "G. Zamorani", "E. Zucca"]}, "1627": {"id": "2004.05618v1", "title": "Noise from Undetected Sources in Dark Energy Survey Images", "url": "http://arxiv.org/pdf/2004.05618v1", "date": "2020-04-12 14:17:08", "abs": "For ground-based optical imaging with current CCD technology, the Poisson\nfluctuations in source and sky background photon arrivals dominate the noise\nbudget and are readily estimated. Another component of noise, however, is the\nsignal from the undetected population of stars and galaxies. Using injection of\nartificial galaxies into images, we demonstrate that the measured variance of\ngalaxy moments (used for weak gravitational lensing measurements) in Dark\nEnergy Survey (DES) images is significantly in excess of the Poisson\npredictions, by up to 30\\%, and that the background sky levels are\noverestimated by current software. By cross-correlating distinct images of\n\"empty\" sky regions, we establish that there is a significant image noise\ncontribution from undetected static sources (US), which on average are mildly\nresolved at DES resolution. Treating these US as a stationary noise source, we\ncompute a correction to the moment covariance matrix expected from Poisson\nnoise. The corrected covariance matrix matches the moment variances measured on\nthe injected DES images to within 5\\%. Thus we have an empirical method to\nstatistically account for US in weak lensing measurements, rather than\nrequiring extremely deep sky simulations. We also find that local sky\ndeterminations can remove the bias in flux measurements, at a small penalty in\nadditional, but quantifiable, noise.", "cat": "astro-ph.IM", "authors": ["K. Eckert", "G. M. Bernstein", "A. Amara", "A. Amon", "A. Choi", "S. Everett", "D. Gruen", "R. A. Gruendl", "E. M. Huff", "N. Kuropatkin", "A. Roodman", "E. Sheldon", "B. Yanny", "Y. Zhang", "T. M. C. Abbott", "M. Aguena", "S. Avila", "K. Bechtol", "D. Brooks", "D. L. Burke", "A. Carnero Rosell", "M. Carrasco Kind", "J. Carretero", "M. Costanzi", "L. N. da Costa", "J. De Vicente", "S. Desai", "H. T. Diehl", "J. P. Dietrich", "T. F. Eifler", "A. E. Evrard", "B. Flaugher", "J. Frieman", "J. Garc\u00eda-Bellido", "E. Gaztanaga", "J. Gschwend", "G. Gutierrez", "W. G. Hartley", "D. L. Hollowood", "K. Honscheid", "D. J. James", "R. Kron", "K. Kuehn", "M. A. G. Maia", "J. L. Marshall", "P. Melchior", "F. Menanteau", "R. Miquel", "R. L. C. Ogando", "A. Palmese", "F. Paz-Chinch\u00f3n", "A. A. Plazas", "A. K. Romer", "E. Sanchez", "V. Scarpine", "S. Serrano", "I. Sevilla-Noarbe", "M. Smith", "M. Soares-Santos", "E. Suchyta", "M. E. C. Swanson", "G. Tarle", "D. Thomas", "T. N. Varga", "A. R. Walker", "W. Wester", "R. D. Wilkinson", "J. Zuntz", "the DES Collaboration"]}, "1628": {"id": "1707.00238v1", "title": "A Survey of Bandwidth and Latency Enhancement Approaches for Mobile Cloud Game Multicasting", "url": "http://arxiv.org/pdf/1707.00238v1", "date": "2017-07-02 05:09:17", "abs": "Among mobile cloud applications, mobile cloud gaming has gained a significant\npopularity in the recent years. In mobile cloud games, textures, game objects,\nand game events are typically streamed from a server to the mobile client.\n One of the challenges in cloud mobile gaming is how to efficiently multicast\ngaming contents and updates in Massively Multi-player Online Games (MMOGs).\nThis report surveys the state of art techniques introduced for game\nsynchronization and multicasting mechanisms to decrease latency and bandwidth\nconsumption, and discuss several schemes that have been proposed in this area\nthat can be applied to any networked gaming context. From our point of view,\ngaming applications demand high interactivity. Therefore, concentrating on\ngaming applications will eventually cover a wide range of applications without\nviolating the limited scope of this survey.", "cat": "cs.NI", "authors": ["Mohammad Hosseini"]}, "1629": {"id": "2211.16517v2", "title": "MUSE-ALMA Haloes VII: Survey Science Goals & Design, Data Processing and Final Catalogues", "url": "http://arxiv.org/pdf/2211.16517v2", "date": "2022-12-01 13:35:00", "abs": "The gas cycling in the circumgalactic regions of galaxies is known to be\nmulti-phase. The MUSE-ALMA Haloes survey gathers a large multi-wavelength\nobservational sample of absorption and emission data with the goal to\nsignificantly advance our understanding of the physical properties of such CGM\ngas. A key component of the MUSE-ALMA Haloes survey is the multi-facility\nobservational campaign conducted with VLT/MUSE, ALMA and HST. MUSE-ALMA Haloes\ntargets comprise 19 VLT/MUSE IFS quasar fields, including 32 $z_{\\rm abs}<$0.85\nstrong absorbers with measured N$_{HI}$ $\\geq 10^{18}$ cm$^{\\rm -2}$ from\nUV-spectroscopy. We additionally use a new complementary HST medium program to\ncharacterise the stellar content of the galaxies through a 40-orbit three-band\nUVIS and IR WFC3 imaging. Beyond the absorber-selected targets, we detect 3658\nsources all fields combined, including 703 objects with spectroscopic\nredshifts. This galaxy-selected sample constitutes the main focus of the\ncurrent paper. We have secured millimeter ALMA observations of some of the\nfields to probe the molecular gas properties of these objects. Here, we present\nthe overall survey science goals, target selection, observational strategy,\ndata processing and source identification of the full sample. Furthermore, we\nprovide catalogues of magnitude measurements for all objects detected in\nVLT/MUSE, ALMA and HST broad-band images and associated spectroscopic redshifts\nderived from VLT/MUSE observations. Together, this data set provides robust\ncharacterisation of the neutral atomic gas, molecular gas and stars in the same\nobjects resulting in the baryon census of condensed matter in complex galaxy\nstructures.", "cat": "astro-ph.GA", "authors": ["C\u00e9line P\u00e9roux", "Simon Weng", "Arjun Karki", "Ramona Augustin", "Varsha P. Kulkarni", "Roland Szakacs", "Anne Klitsch", "Aleksandra Hamanowicz", "Alejandra Y. Fresco", "Martin A. Zwaan", "Andrew Biggs", "Andrew J. Fox", "Mattjew Hayes", "J. Christopher Howk", "Glenn G. Kacprzak", "Susan Kassin", "Harald Kuntschner", "Dylan Nelson", "Max Pettini"]}, "1630": {"id": "1405.4994v1", "title": "A Search for Strongly Mg-enhanced Stars from the Sloan Digital Sky Survey", "url": "http://arxiv.org/pdf/1405.4994v1", "date": "2014-05-20 08:40:49", "abs": "Strongly Mg-enhanced stars with [Mg/Fe] $>$ 1.0 show peculiar abundance\npatterns and hence are of great interest for our understanding of stellar\nformation and chemical evolution of the Galaxy. A systematical search for\nstrongly Mg-enhanced stars based on the low-resolution $(R\\simeq2000)$ spectra\nof the Sloan Digital Sky Survey (SDSS) is carried out by finding the best\nmatched synthetic spectrum to the observed one in the region of Mg I b lines\naround $\\lambda$5170\\AA$~$via a profile matching method. The advantage of our\nmethod is that fitting parameters are refined by reproducing the [Mg/Fe] ratios\nof 47 stars from very precise high-resolution spectroscopic (HRS) analysis by\nNissen and Schuster (2010); and these parameters are crucial to the precision\nand validity of the derived Mg abundances. As a further check of our method, Mg\nabundances are estimated with our method for member stars in four Galactic\nglobular clusters (M92, M13, M3, M71) which cover the same metallicity range as\nour sample, and the results are in good agreement with those of HRS analysis in\nthe literature. The validation of our method is also proved by the agreement of\n[Mg/Fe] between our values and those of HRS analysis by Aoki et al.(2013).\nFinally, 33 candidates of strongly Mg-enhanced stars with [Mg/Fe]$>$1.0 are\nselected from 14850 F and G stars. Follow-up observations will be carried out\non these candidates with high-resolution spectroscopy by large telescopes in\nthe near future, so as to check our selection procedure and to perform a\nprecise and detailed abundance analysis and to explore the origins of these\nstars.", "cat": "astro-ph.SR", "authors": ["Xiang Li", "Gang Zhao", "Yu-Qin Chen", "Hai-Ning Li"]}, "1631": {"id": "1410.0790v1", "title": "The Murchison Widefield Array Commissioning Survey: A Low-Frequency Catalogue of 14,110 Compact Radio Sources over 6,100 Square Degrees", "url": "http://arxiv.org/pdf/1410.0790v1", "date": "2014-10-03 09:21:54", "abs": "We present the results of an approximately 6,100 square degree 104--196MHz\nradio sky survey performed with the Murchison Widefield Array during instrument\ncommissioning between 2012 September and 2012 December: the Murchison Widefield\nArray Commissioning Survey (MWACS). The data were taken as meridian drift scans\nwith two different 32-antenna sub-arrays that were available during the\ncommissioning period. The survey covers approximately 20.5 h < Right Ascension\n(RA) < 8.5 h, -58 deg < Declination (Dec) < -14 deg over three frequency bands\ncentred on 119, 150 and 180 MHz, with image resolutions of 6--3 arcmin. The\ncatalogue has 3-arcmin angular resolution and a typical noise level of 40\nmJy/beam, with reduced sensitivity near the field boundaries and bright\nsources. We describe the data reduction strategy, based upon mosaiced\nsnapshots, flux density calibration and source-finding method. We present a\ncatalogue of flux density and spectral index measurements for 14,110 sources,\nextracted from the mosaic, 1,247 of which are sub-components of complexes of\nsources.", "cat": "astro-ph.IM", "authors": ["Natasha Hurley-Walker", "John Morgan", "Randall B. Wayth", "Paul J. Hancock", "Martin E. Bell", "Gianni Bernardi", "Ramesh Bhat", "Frank Briggs", "Avinash A. Deshpande", "Aaron Ewall-Wice", "Lu Feng", "Bryna J. Hazelton", "Luke Hindson", "Daniel C. Jacobs", "David L. Kaplan Nadia Kudryavtseva", "Emil Lenc", "Benjamin McKinley", "Daniel Mitchell", "Bart Pindor", "Pietro Procopio", "Divya Oberoi", "Andr\u00e9 Offringa", "Stephen Ord", "Jennifer Riding", "Judd D. Bowman", "Roger Cappallo", "Brian Corey", "David Emrich", "B. M. Gaensler", "Robert Goeke", "Lincoln Greenhill", "Jacqueline Hewitt", "Melanie Johnston-Hollitt", "Justin Kasper", "Eric Kratzenberg", "Colin Lonsdale", "Mervyn Lynch", "Russell McWhirter", "Miguel F. Morales", "Edward Morgan", "Thiagaraj Prabu", "Alan Rogers", "Anish Roshi", "Udaya Shankar", "K. Srivani", "Ravi Subrahmanyan", "Steven Tingay", "Mark Waterson", "Rachel Webster", "Alan Whitney", "Andrew Williams", "Chris Williams"]}, "1632": {"id": "1102.1996v1", "title": "Preliminary Results from NEOWISE: An Enhancement to the Wide-field Infrared Survey Explorer for Solar System Science", "url": "http://arxiv.org/pdf/1102.1996v1", "date": "2011-02-09 22:14:19", "abs": "The \\emph{Wide-field Infrared Survey Explorer} has surveyed the entire sky at\nfour infrared wavelengths with greatly improved sensitivity and spatial\nresolution compared to its predecessors, the \\emph{Infrared Astronomical\nSatellite} and the \\emph{Cosmic Background Explorer}. NASA's Planetary Science\nDivision has funded an enhancement to the \\WISE\\ data processing system called\n\"NEOWISE\" that allows detection and archiving of moving objects found in the\n\\WISE\\ data. NEOWISE has mined the \\WISE\\ images for a wide array of small\nbodies in our Solar System, including Near-Earth Objects (NEOs), Main Belt\nasteroids, comets, Trojans, and Centaurs. By the end of survey operations in\nFebruary 2011, NEOWISE identified over 157,000 asteroids, including more than\n500 NEOs and $\\sim$120 comets. The NEOWISE dataset will enable a panoply of new\nscientific investigations.", "cat": "astro-ph.EP", "authors": ["A. Mainzer", "J. Bauer", "T. Grav", "J. Masiero", "R. M. Cutri", "J. Dailey", "P. Eisenhardt", "R. S. McMillan", "E. Wright", "R. Walker", "R. Jedicke", "T. Spahr", "D. Tholen", "R. Alles", "R. Beck", "H. Brandenburg", "T. Conrow", "T. Evans", "J. Fowler", "T. Jarrett", "K. Marsh", "F. Masci", "H. McCallon", "S. Wheelock", "M. Wittman", "P. Wyatt", "E. DeBaun", "G. Elliott", "D. Elsbury", "T. Gautier IV", "S. Gomillion", "D. Leisawitz", "C. Maleszewski", "M. Micheli", "A. Wilkins"]}, "1633": {"id": "1005.2413v2", "title": "Galaxy Clustering in the Completed SDSS Redshift Survey: The Dependence on Color and Luminosity", "url": "http://arxiv.org/pdf/1005.2413v2", "date": "2011-04-18 17:16:12", "abs": "We measure the luminosity and color dependence of galaxy clustering in the\nSDSS DR7 main galaxy sample, focusing on the projected correlation function\nw_p(r_p) of volume-limited samples. We interpret our measurements using halo\noccupation distribution (HOD) modeling assuming a Lambda-CDM cosmology. The\namplitude of w_p(r_p) grows slowly with luminosity for L < L_* and increases\nsharply at higher luminosities, with bias factor b(>L)=1.06+0.23(L/L_*)^{1.12}.\nAt fixed luminosity, redder galaxies have a stronger and steeper w_p(r_p), a\ntrend that runs steadily from the bluest galaxies to the reddest galaxies. The\nindividual luminosity trends for the red and blue galaxy populations are\nstrikingly different. Blue galaxies show a slow but steady increase of w_p(r_p)\nwith luminosity, at all scales. The large-scale clustering of red galaxies\nshows little luminosity dependence until a sharp increase at L > 4L_*, but the\nlowest luminosity red galaxies (0.04-0.25 L_*) show very strong clustering on\nscales r_p < 2 Mpc/h. Most of the observed trends can be naturally understood\nwithin the LCDM+HOD framework. The growth of w_p(r_p) with luminosity reflects\nan overall shift in the halo mass scale, in particular an increase in the\nminimum host halo mass Mmin. The mass at which a halo has, on average, one\nsatellite galaxy brighter than L is M_1 ~ 17 Mmin(L) over most of the\nluminosity range. The growth and steepening of w_p(r_p) for redder galaxies\nreflects the increasing fraction of galaxies that are satellite systems in high\nmass halos instead of central systems in low mass halos, a trend that is\nespecially marked at low luminosities. Our extensive measurements, provided in\ntabular form, will allow detailed tests of theoretical models of galaxy\nformation, a firm grounding of semi-empirical models of the galaxy population,\nand new cosmological tests.", "cat": "astro-ph.CO", "authors": ["Idit Zehavi", "Zheng Zheng", "David H. Weinberg", "Michael R. Blanton", "Neta A. Bahcall", "Andreas A. Berlind", "Jon Brinkmann", "Joshua A. Frieman", "James E. Gunn", "Robert H. Lupton", "Robert C. Nichol", "Will J. Percival", "Donald P. Schneider", "Ramin A. Skibba", "Michael A. Strauss", "Max Tegmark", "Donald G. York"]}, "1634": {"id": "2212.05985v1", "title": "Interstellar Polarization Survey II: General Interstellar Medium", "url": "http://arxiv.org/pdf/2212.05985v1", "date": "2022-12-12 15:42:15", "abs": "Magnetic fields permeate the entire Galaxy and are essential to, for example,\nthe regulation of several stages of the star formation process and cosmic ray\ntransportation. Unraveling its properties, such as intensity and topology, is\nan observational challenge that requires combining different and complementary\ntechniques. The polarization of starlight due to the absorption by\nfield-aligned non-spherical dust grains provides a unique source of information\nabout the interstellar magnetic field in the optical band. This work introduces\na first analysis of a new catalog of optical observations of linearly polarized\nstarlight in the diffuse interstellar medium (ISM), the Interstellar\nPolarization Survey, General ISM (IPS-GI). We used data from the IPS-GI,\nfocusing on 38 fields sampling lines of sight in the diffuse medium. The fields\nare about 0.3$^{\\circ}$ by 0.3$^{\\circ}$ in size and each of them contains\n$\\sim1000$ stars on average. The IPS-GI catalog has polarimetric measurements\nof over 40000 stars, over 18000 of which have ${P}/\\sigma_{P} > 5$. We added\ndistances and other parameters from auxiliary catalogs to over 36000 of these\nstars. We analyzed parameter distributions and correlations between parameters\nof a high-quality subsample of 10516 stars (i.e. $\\sim275$ stars per field). As\nexpected, the degree of polarization tends to increase with the extinction,\nproducing higher values of polarization at greater distances or at lower\nabsolute Galactic latitudes. Furthermore, we find evidence for a large-scale\nordered Galactic magnetic field.", "cat": "astro-ph.GA", "authors": ["M. J. F. Versteeg", "A. M. Magalh\u00e3es", "M. Haverkorn", "Y. Angarita", "C. V. Rodrigues", "R. Santos-Lima", "Koji S. Kawabata"]}, "1635": {"id": "2202.07145v6", "title": "GAN-generated Faces Detection: A Survey and New Perspectives", "url": "http://arxiv.org/pdf/2202.07145v6", "date": "2023-11-09 16:03:48", "abs": "Generative Adversarial Networks (GAN) have led to the generation of very\nrealistic face images, which have been used in fake social media accounts and\nother disinformation matters that can generate profound impacts. Therefore, the\ncorresponding GAN-face detection techniques are under active development that\ncan examine and expose such fake faces. In this work, we aim to provide a\ncomprehensive review of recent progress in GAN-face detection. We focus on\nmethods that can detect face images that are generated or synthesized from GAN\nmodels. We classify the existing detection works into four categories: (1) deep\nlearning-based, (2) physical-based, (3) physiological-based methods, and (4)\nevaluation and comparison against human visual performance. For each category,\nwe summarize the key ideas and connect them with method implementations. We\nalso discuss open problems and suggest future research directions.", "cat": "cs.CV", "authors": ["Xin Wang", "Hui Guo", "Shu Hu", "Ming-Ching Chang", "Siwei Lyu"]}, "1636": {"id": "1904.01626v2", "title": "White dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 14", "url": "http://arxiv.org/pdf/1904.01626v2", "date": "2019-04-13 23:16:56", "abs": "White dwarfs carry information on the structure and evolution of the Galaxy,\nespecially through their luminosity function and initial-to-final mass\nrelation. Very cool white dwarfs provide insight into the early ages of each\npopulation. Examining the spectra of all stars with $3\\sigma$ proper motion in\nthe Sloan Digital Sky Survey Data Release 14, we report the classification for\n20 088 spectroscopically confirmed white dwarfs, plus 415 hot subdwarfs, and\n311 cataclysmic variables. We obtain Teff, log g and mass for hydrogen\natmosphere white dwarf stars (DAs), warm helium atmosphere white dwarfs (DBs),\nhot subdwarfs (sdBs and sdOs), and estimate photometric Teff for white dwarf\nstars with continuum spectra (DCs). We find 15793 sdAs and 447 dCs between the\nwhite dwarf cooling sequence and the main sequence, especially below Teff=\n10000 K; most are likely low-mass metal-poor main sequence stars, but some\ncould be the result of interacting binary evolution.", "cat": "astro-ph.SR", "authors": ["S. O. Kepler", "Ingrid Pelisoli", "Detlev Koester", "Nicole Reindl", "Stephan Geier", "Alejandra D. Romero", "Gustavo Ourique", "Cristiane de Paula Oliveira", "Larissa A. Amaral"]}, "1637": {"id": "2303.14567v1", "title": "Photometric classification of QSOs from ALHAMBRA survey using random forest", "url": "http://arxiv.org/pdf/2303.14567v1", "date": "2023-03-25 21:30:27", "abs": "Context: Given the current big data era in Astronomy, machine learning based\nmethods have being applied over the last years to identify or classify objects\nlike quasars, galaxies and stars from full sky photometric surveys. Aims: Here\nwe systematically evaluate the performance of Random Forests (RF) in\nclassifying quasars using either magnitudes or colours, both from broad and\nnarrow-band filters, as features. Methods: The working data consists of\nphotometry from the ALHAMBRA Gold Catalogue that we cross-matched with the\nSloan Digital Sky Survey (SDSS) and with the Million Quasars Catalogue\n(Milliquas) for objects labelled as quasars, galaxies or stars. A RF classifier\nis trained and tested to evaluate the effect on final accuracy and precision of\nvarying the free parameters and the effect of using narrow or broad-band\nmagnitudes or colours. Results: Best performances of the classifier yielded\nglobal accuracy and quasar precision around 0.9. Varying model free parameters\n(within reasonable ranges of values) has no significant effects on the final\nclassification. Using colours instead of magnitudes as features results in\nbetter performances of the classifier, especially using colours from the\nALHAMBRA Survey. Colours that contribute the most to the classification are\nthose containing the near-infrared $JHK$ bands.", "cat": "astro-ph.GA", "authors": ["Benjamin Arroquia-Cuadros", "Nestor Sanchez", "Vicent Gomez", "Pere Blay", "Vicent Martinez-Badenes", "Lorena Nieves-Seoane"]}, "1638": {"id": "1806.05193v1", "title": "An ALMA survey of CO in submillimetre galaxies: companions, triggering, and the environment in blended sources", "url": "http://arxiv.org/pdf/1806.05193v1", "date": "2018-06-13 18:00:06", "abs": "We present ALMA observations of the mid-J 12CO emission from six single-dish\nselected 870-micron sources in the Extended Chandra Deep Field-South (ECDFS)\nand UKIDSS Ultra-Deep Survey (UDS) fields. These six single-dish submillimetre\nsources were selected based on previous ALMA continuum observations, which\nshowed that each comprised a blend of emission from two or more individual\nsubmillimetre galaxies (SMGs), separated on 5--10 arcsec scales. The six\nsingle-dish submillimetre sources targeted correspond to a total of 14\nindividual SMGs, of which seven have previously-measured robust\noptical/near-infrared spectroscopic redshifts, which were used to tune our ALMA\nobservations. We detect CO(3-2) or CO(4-3) at z=2.3--3.7 in seven of the 14\nSMGs, and in addition serendipitously detect line emission from three gas-rich\ncompanion galaxies, as well as identify four new 3.3-mm selected continuum\nsources in the six fields. Joint analysis of our CO spectroscopy and existing\ndata suggests that 64 \\pm 18% of the SMGs in blended submillimetre sources are\nunlikely to be physically associated. However, three of the SMG fields (50%)\ncontain new, serendipitously-detected CO-emitting (but submillimetre-faint)\nsources at similar redshifts to the 870-micron selected SMGs we targeted. These\ndata suggest that the SMGs inhabit overdense regions, but that these are not\nsufficiently overdense on ~100 kpc scales to influence the source blending\ngiven the short lifetimes of SMGs. We find that 21 \\pm 12% of SMGs have\nspatially-distinct and kinematically-close companion galaxies (~8--150 kpc and\n<~300 km/s), which may have enhanced their star-formation via gravitational\ninteractions.", "cat": "astro-ph.GA", "authors": ["J. L. Wardlow", "J. M. Simpson", "Ian Smail", "A. M. Swinbank", "A. W. Blain", "W. N. Brandt", "S. C. Chapman", "Chian-Chou Chen", "E. A. Cooke", "H. Dannerbauer", "B. Gullberg", "J. A. Hodge", "R. J. Ivison", "K. K. Knudsen", "Douglas Scott", "A. P. Thomson", "A. Weiss", "P. P. van der Werf"]}, "1639": {"id": "1404.4871v1", "title": "The K giant stars from the LAMOST survey data I: identification, metallicity, and distance", "url": "http://arxiv.org/pdf/1404.4871v1", "date": "2014-04-18 20:00:03", "abs": "We present a support vector machine classifier to identify the K giant stars\nfrom the LAMOST survey directly using their spectral line features. The\ncompleteness of the identification is about 75% for tests based on LAMOST\nstellar parameters. The contamination in the identified K giant sample is lower\nthan 2.5%. Applying the classification method to about 2 million LAMOST spectra\nobserved during the pilot survey and the first year survey, we select 298,036 K\ngiant candidates. The metallicities of the sample are also estimated with\nuncertainty of $0.13\\sim0.29$\\,dex based on the equivalent widths of Mg$_{\\rm\nb}$ and iron lines. A Bayesian method is then developed to estimate the\nposterior probability of the distance for the K giant stars, based on the\nestimated metallicity and 2MASS photometry. The synthetic isochrone-based\ndistance estimates have been calibrated using 7 globular clusters with a wide\nrange of metallicities. The uncertainty of the estimated distance modulus at\n$K=11$\\,mag, which is the median brightness of the K giant sample, is about\n0.6\\,mag, corresponding to $\\sim30$% in distance. As a scientific verification\ncase, the trailing arm of the Sagittarius stream is clearly identified with the\nselected K giant sample. Moreover, at about 80\\,kpc from the Sun, we use our K\ngiant stars to confirm a detection of stream members near the apo-center of the\ntrailing tail. These rediscoveries of the features of the Sagittarius stream\nillustrate the potential of the LAMOST survey for detecting substructures in\nthe halo of the Milky Way.", "cat": "astro-ph.GA", "authors": ["Chao Liu", "Li-Cai Deng", "Jeffrey L. Carlin", "Martin C. Smith", "Jing Li", "Heidi Jo Newberg", "Shuang Gao", "Fan Yang", "Xiang-Xiang Xue", "Yan Xu", "Yue-Yang Zhang", "Yu Xin", "Ge Jin"]}, "1640": {"id": "0708.0845v1", "title": "The SCUBA HAlf Degree Extragalactic Survey (SHADES) -- V. Submillimetre properties of near-infrared--selected galaxies in the Subaru/XMM--Newton deep field", "url": "http://arxiv.org/pdf/0708.0845v1", "date": "2007-08-06 21:20:33", "abs": "We have studied the submillimetre (submm) properties of the following classes\nof near-infrared (NIR)-selected massive galaxies at high redshifts:\nBzK-selected star-forming galaxies (BzKs); distant red galaxies (DRGs); and\nextremely red objects (EROs). We used the SCUBA HAlf Degree Extragalactic\nSurvey (SHADES), the largest uniform submm survey to date. Partial overlap of\nSIRIUS/NIR images and SHADES in SXDF has allowed us to identify 4 submm-bright\nNIR-selected galaxies, which are detected in the mid-infrared, 24 micron, and\nthe radio, 1.4 GHz. We find that all of our submm-bright NIR-selected galaxies\nsatisfy the BzK selection criteria, except for one galaxy whose B-z and z-K\ncolours are however close to the BzK colour boundary. Two of the submm-bright\nNIR-selected galaxies satisfy all of the selection criteria we considered, i.e.\nthey belong to the BzK-DRG-ERO overlapping population, or `extremely red' BzKs.\nAlthough these extremely red BzKs are rare (0.25 arcmin^{-2}), up to 20 % of\nthis population could be submm galaxies. This fraction is significantly higher\nthan that found for other galaxy populations studied here. Via a stacking\nanalysis, we have detected the 850 micron flux of submm-faint BzKs and EROs in\nour SCUBA maps. While the contribution of z~2 BzKs to the submm background is\nabout 10--15 % and similar to that from EROs typically at z~1, BzKs have a\nhigher fraction (~30 %) of submm flux in resolved sources compared with EROs\nand submm sources as a whole. From the SED fitting analysis for both\nsubmm-bright and submm-faint BzKs, we found no clear signature that\nsubmm-bright BzKs are experiencing a specifically luminous evolutionary phase,\ncompared with submm-faint BzKs. An alternative explanation might be that\nsubmm-bright BzKs are more massive than submm-faint ones.", "cat": "astro-ph", "authors": ["T. Takagi", "A. M. J. Mortier", "K. Shimasaku", "K. Coppin", "A. Pope", "R. J. Ivison", "H. Hanami", "S. Serjeant", "D. L. Clements", "R. S. Priddey", "J. S. Dunlop", "T. Takata", "I. Aretxaga", "S. C. Chapman", "S. A. Eales", "D. Farrah", "G. L. Granato", "M. Halpern", "D. H. Hughes", "E. van Kampen", "D. Scott", "K. Sekiguchi", "I. Smail", "M. Vaccari"]}, "1641": {"id": "2303.05012v2", "title": "Spatio-Temporal Trajectory Similarity Measures: A Comprehensive Survey and Quantitative Study", "url": "http://arxiv.org/pdf/2303.05012v2", "date": "2023-03-17 06:12:17", "abs": "Spatio-temporal trajectory analytics is at the core of smart mobility\nsolutions, which offers unprecedented information for diversified applications\nsuch as urban planning, infrastructure development, and vehicular networks.\nTrajectory similarity measure, which aims to evaluate the distance between two\ntrajectories, is a fundamental functionality of trajectory analytics. In this\npaper, we propose a comprehensive survey that investigates all the most common\nand representative spatio-temporal trajectory measures. First, we provide an\noverview of spatio-temporal trajectory measures in terms of three hierarchical\nperspectives: Non-learning vs. Learning, Free Space vs. Road Network, and\nStandalone vs. Distributed. Next, we present an evaluation benchmark by\ndesigning five real-world transformation scenarios. Based on this benchmark,\nextensive experiments are conducted to study the effectiveness,\nrobustness,nefficiency, and scalability of each measure, which offers\nguidelines for trajectory measure selection among multiple techniques and\napplications such as trajectory data mining, deep learning, and distributed\nprocessing.", "cat": "cs.DS", "authors": ["Danlei Hu", "Lu Chen", "Hanxi Fang", "Ziquan Fang", "Tianyi Li", "Yunjun Gao"]}, "1642": {"id": "1012.3864v1", "title": "Generalized Young and Cauchy--Bunyakowsky Inequalities with Applications: a survey", "url": "http://arxiv.org/pdf/1012.3864v1", "date": "2010-12-17 12:30:08", "abs": "In this survey we consider generalizations for Young and Cauchy--Bunyakowsky\ninequalities with applications.", "cat": "math.CA", "authors": ["Sergei M. Sitnik"]}, "1643": {"id": "2002.07828v1", "title": "The Environment of Lyman Break Analogues (ELBA) survey: Star-forming galaxies in small groups", "url": "http://arxiv.org/pdf/2002.07828v1", "date": "2020-02-18 19:02:07", "abs": "The Environment of Lyman Break Analogues (ELBA) survey is an imaging survey\nof 33 $deg^{2}$ of the southern sky. The survey was observed in {\\it u}, {\\it\ng}, {\\it r}, and {\\it i} bands with the Dark Energy Camera (DECam) on the\nBlanco telescope. The main goal of this project is to investigate the\nenvironment of Lyman break analogues (LBAs), low-redshift (z $\\sim $0.2)\ngalaxies that are remarkably similar to typical star-forming galaxies at z\n$\\sim$ 3. We explore whether the environment has any influence on the observed\nproperties of these galaxies, providing valuable insight on the formation and\nevolution of galaxies over cosmic time. Using the Nearest Neighbour method, we\nmeasure the local density of each object ranging from small to large scales\n(clusters of galaxies). Comparing the environment around LBAs with that of the\ngeneral galaxy population in the field, we conclude that LBAs, on average,\npopulate denser regions at small scales ($\\sim$ $1.5Mpc$), but are located in\nsimilar environment to other star-forming galaxies at larger scales ($\\sim$\n$3.0 Mpc$). This offers evidence that nearby encounters such as mergers may\ninfluence the star formation activity in LBAs, before infall onto larger galaxy\nclusters. We interpret this an indication of galaxy preprocessing, in agreement\nwith theoretical expectations for galaxies at z $\\sim$ 2 -3 where the\ngravitational interactions are more intense in early formation processes of\nthis objects", "cat": "astro-ph.GA", "authors": ["L. Santana-Silva", "T. S. Gon\u00e7alves", "A. Basu-Zych", "M. Soares-Santos", "K. Men\u00e9ndez-Delmestre", "A. Drlica-Wagner", "L. Riguccini", "N. P. Kuropatkin", "B. Yanny", "R. T. Eufrasio"]}, "1644": {"id": "2109.10734v3", "title": "Autocorrelation Functions, Cosmology and Investigating The CMB Cold Spot With EMU-ASKAP Radio Continuum Survey", "url": "http://arxiv.org/pdf/2109.10734v3", "date": "2022-02-08 20:08:35", "abs": "Galaxy angular-power spectrum and autocorrelation functions (ACFs) provide\ninformation about the distribution of matter by using galaxy counts as a proxy.\nIn this study, we are going to estimate autocorrelation angular power spectrum\nand angular autocorrelation function for EMU-ASKAP 5 sigma sources and then\ncompare them with results from NVSS. We will also use SUMSS data to compare ACF\nresults using Landy-Szalay estimator. EMU-ASKAP will provide excellent\nopportunity to observe universe with high sensitivity and is likely going to\nobserve millions of high redshift sources which will help in studying the\nclustering of the large scale structures, constraining cosmological parameters\nand exploring mysteries like the existence of a cosmic cold spot or the CMB\ncold spot as observed by both Planck and WMAP probes. We will discuss some\npossible ways, the CMB cold spot puzzle can be explored further by using the\ngalaxy clustering, integral source count and galaxy bias analysis with a highly\nsensitive survey like EMU-ASKAP.", "cat": "astro-ph.CO", "authors": ["Syed Faisalur Rahman"]}, "1645": {"id": "1104.2537v1", "title": "FIRE Spectroscopy of Five Late-type T Dwarfs Discovered with the Wide-field Infrared Survey Explorer", "url": "http://arxiv.org/pdf/1104.2537v1", "date": "2011-04-13 16:08:06", "abs": "We present the discovery of five late-type T dwarfs identified with the\nWide-field Infrared Survey Explorer (WISE). Low-resolution near-infrared\nspectroscopy obtained with the Magellan Folded-port InfraRed Echellette (FIRE)\nreveal strong water and methane absorption in all five sources, and spectral\nindices and comparison to spectral templates indicate classifications ranging\nfrom T5.5 to T8.5:. The spectrum of the latest-type source, WISE J1812+2721, is\nan excellent match to that of the T8.5 companion brown dwarf Wolf 940B.\nWISE-based spectrophotometric distance estimates place these T dwarfs at 12-13\npc from the Sun, assuming they are single. Preliminary fits of the spectral\ndata to the atmosphere models of Saumon & Marley indicate effective\ntemperatures ranging from 600 K to 930 K, both cloudy and cloud-free\natmospheres, and a broad range of ages and masses. In particular, two sources\nshow evidence of both low surface gravity and cloudy atmospheres, tentatively\nsupporting a trend noted in other young brown dwarfs and exoplanets. In\ncontrast, the high proper motion T dwarf WISE J2018-7423 exhibits a suppressed\nK-band peak and blue spectrophotometric J-K colors indicative of an old,\nmassive brown dwarf; however, it lacks the broadened Y-band peak seen in\nmetal-poor counterparts. These results illustrate the broad diversity of\nlow-temperature brown dwarfs that will be uncovered with WISE.", "cat": "astro-ph.SR", "authors": ["Adam J. Burgasser", "Michael C. Cushing", "J. Davy Kirkpatrick", "Christopher R. Gelino", "Roger L. Griffith", "Dagny L. Looper", "Christopher Tinney", "Robert A. Simcoe", "John J. Bochanski", "Michael F. Skrutskie", "A. Mainzer", "Maggie A. Thompson", "Kenneth A. Marsh", "James M. Bauer", "Edward L. Wright"]}, "1646": {"id": "0911.3348v1", "title": "Spitzer-IRS high resolution spectroscopic survey of the 12 micron Seyfert galaxies: II. Results for the Complete Dataset", "url": "http://arxiv.org/pdf/0911.3348v1", "date": "2009-11-17 17:01:02", "abs": "We present the Spitzer 10-37um IRS high resolution (R~600) spectroscopic\nsurvey of the Seyfert galaxies of the 12 micron Galaxy Sample. The new spectra\nof 61 galaxies, with those already published, gives us a total of 91 12micron\nSeyfert galaxies observed, out of 112. We use an improved AGN classification\nfor Seyfert galaxies: instead of the type 1 and 2 classes, we use the\nspectropolarimetric data to divide them into \"AGN 1\" and \"AGN 2\", where AGN 1's\ninclude all broad-line objects, including the Seyfert 2's showing hidden broad\nlines in polarized light, while AGN 2's contains only Seyferts with no\ndetectable broad lines at all. We present various mid-IR observables and we\nfind that these properties characterize the AGN 1's objects as a single family,\nwith strongly AGN-dominated spectra. In contrast, the AGN 2's can be divided in\ntwo groups, the first one with properties similar to the AGN 1's and the second\nsimilar to the non-Seyfert galaxies, such as LINERs or starburst galaxies. We\ncomputed a semianalytical model to estimate the AGN and the starburst\ncontributions to the mid-IR galaxy emission at 19um. We find that AGN 1 have an\nAGN contribution >73% and AGN 2 >45% of their total emission at 19um. The\ndetection of [NeV] lines is an almost perfect signature of energy production by\nan AGN. We present mean spectra of the various AGN categories. We derive the\nfirst local luminosity functions for the mid-infrared lines and the PAH\nfeature. No statistical difference is found in the space densities for Seyfert\n1's and 2's, nor for the new classes of AGN 1's and 2's. The global output of\naccretion-powered galactic nuclei in the local universe is derived from the\ncorrelation between [NeV] line and the nonstellar IR continuum luminosity.", "cat": "astro-ph.CO", "authors": ["Silvia Tommasin", "Luigi Spinoglio", "Matthew A. Malkan", "Giovanni Fazio"]}, "1647": {"id": "1312.1916v1", "title": "All Weather Calibration of Wide Field Optical and NIR Surveys", "url": "http://arxiv.org/pdf/1312.1916v1", "date": "2013-12-06 16:42:42", "abs": "The science goals for ground-based large-area surveys, such as the Dark\nEnergy Survey, Pan-STARRS, and the Large Synoptic Survey Telescope, require\ncalibration of broadband photometry that is stable in time and uniform over the\nsky to precisions of a per cent or better. This performance will need to be\nachieved with data taken over the course of many years, and often in less than\nideal conditions. This paper describes a strategy to achieve precise internal\ncalibration of imaging survey data taken in less than photometric conditions,\nand reports results of an observational study of the techniques needed to\nimplement this strategy. We find that images of celestial fields used in this\ncase study with stellar densities of order one per arcmin-squared and taken\nthrough cloudless skies can be calibrated with relative precision of 0.5 per\ncent (reproducibility). We report measurements of spatial structure functions\nof cloud absorption observed over a range of atmospheric conditions, and find\nit possible to achieve photometric measurements that are reproducible to 1 per\ncent in images that were taken through cloud layers that transmit as little as\n25 per cent of the incident optical flux (1.5 magnitudes of extinction). We\nfind, however, that photometric precision below 1 per cent is impeded by the\nthinnest detectable cloud layers. We comment on implications of these results\nfor the observing strategies of future surveys.", "cat": "astro-ph.IM", "authors": ["David L. Burke", "Abhijit Saha", "Jenna Claver", "T. Axelrod", "Chuck Claver", "Darren DePoy", "Zeljko Ivezic", "Lynne Jones", "R. Chris Smith", "Christopher W. Stubbs"]}, "1648": {"id": "2306.08451v3", "title": "A Survey on Blood Pressure Measurement Technologies: Addressing Potential Sources of Bias", "url": "http://arxiv.org/pdf/2306.08451v3", "date": "2023-12-15 19:57:34", "abs": "Regular blood pressure (BP) monitoring in clinical and ambulatory settings\nplays a crucial role in the prevention, diagnosis, treatment, and management of\ncardiovascular diseases. Recently, the widespread adoption of ambulatory BP\nmeasurement devices has been driven predominantly by the increased prevalence\nof hypertension and its associated risks and clinical conditions. Recent\nguidelines advocate for regular BP monitoring as part of regular clinical\nvisits or even at home. This increased utilization of BP measurement\ntechnologies has brought up significant concerns, regarding the accuracy of\nreported BP values across settings. In this survey, focusing mainly on\ncuff-based BP monitoring technologies, we highlight how BP measurements can\ndemonstrate substantial biases and variances due to factors such as measurement\nand device errors, demographics, and body habitus. With these inherent biases,\nthe development of a new generation of cuff-based BP devices which use\nartificial-intelligence (AI) has significant potential. We present future\navenues where AI-assisted technologies can leverage the extensive clinical\nliterature on BP-related studies together with the large collections of BP\nrecords available in electronic health records. These resources can be combined\nwith machine learning approaches, including deep learning and Bayesian\ninference, to remove BP measurement biases and to provide individualized\nBP-related cardiovascular risk indexes.", "cat": "physics.med-ph", "authors": ["Seyedeh Somayyeh Mousavi", "Matthew A. Reyna", "Gari D. Clifford", "Reza Sameni"]}, "1649": {"id": "2207.07971v1", "title": "A Survey of Decision Making in Adversarial Games", "url": "http://arxiv.org/pdf/2207.07971v1", "date": "2022-07-16 16:04:01", "abs": "Game theory has by now found numerous applications in various fields,\nincluding economics, industry, jurisprudence, and artificial intelligence,\nwhere each player only cares about its own interest in a noncooperative or\ncooperative manner, but without obvious malice to other players. However, in\nmany practical applications, such as poker, chess, evader pursuing, drug\ninterdiction, coast guard, cyber-security, and national defense, players often\nhave apparently adversarial stances, that is, selfish actions of each player\ninevitably or intentionally inflict loss or wreak havoc on other players. Along\nthis line, this paper provides a systematic survey on three main game models\nwidely employed in adversarial games, i.e., zero-sum normal-form and\nextensive-form games, Stackelberg (security) games, zero-sum differential\ngames, from an array of perspectives, including basic knowledge of game models,\n(approximate) equilibrium concepts, problem classifications, research\nfrontiers, (approximate) optimal strategy seeking techniques, prevailing\nalgorithms, and practical applications. Finally, promising future research\ndirections are also discussed for relevant adversarial games.", "cat": "cs.GT", "authors": ["Xiuxian Li", "Min Meng", "Yiguang Hong", "Jie Chen"]}, "1650": {"id": "0704.2051v1", "title": "A 610 MHz Survey of the 1H XMM-Newton/Chandra Survey Field", "url": "http://arxiv.org/pdf/0704.2051v1", "date": "2007-04-16 17:10:54", "abs": "We present the results of a deep 610 MHz survey of the 1^H XMM/Chandra survey\narea with the GMRT. The resulting maps have a resolution of ~7 arcsec and an\nrms noise limit of 60 microJy. To a 5 sigma detection limit of 300 microJy we\ndetect 223 sources within a survey area of diameter 64 arcmin. We compute the\n610 MHz source counts and compare them to those measured at other radio\nwavelengths. The well know flattening of the Euclidean-normalised 1.4 GHz\nsource counts below ~2 mJy, usually explained by a population of starburst\ngalaxies undergoing luminosity evolution, is seen at 610 MHz. The 610 MHz\nsource counts can be modelled by the same populations that explain the 1.4 GHz\nsource counts, assuming a spectral index of -0.7 for the starburst galaxies and\nthe steep spectrum AGN population. We find a similar dependence of luminosity\nevolution on redshift for the starburst galaxies at 610 MHz as is found at 1.4\nGHz (i.e. 'Q'= 2.45 (+0.3,-0.4)).", "cat": "astro-ph", "authors": ["D. Moss", "N. Seymour", "I. M. McHardy", "T. Dwelly", "M. J. Page", "N. S. Loaring"]}, "1651": {"id": "1303.1552v1", "title": "The VIRUS-P Exploration of Nearby Galaxies (VENGA): Survey Design, Data Processing, and Spectral Analysis Methods", "url": "http://arxiv.org/pdf/1303.1552v1", "date": "2013-03-06 21:28:35", "abs": "We present the survey design, data reduction, and spectral fitting pipeline\nfor the VIRUS-P Exploration of Nearby Galaxies (VENGA). VENGA is an integral\nfield spectroscopic survey, which maps the disks of 30 nearby spiral galaxies.\nTargets span a wide range in Hubble type, star formation activity, morphology,\nand inclination. The VENGA data-cubes have 5.6'' FWHM spatial resolution, ~5A\nFWHM spectral resolution, sample the 3600A-6800A range, and cover large areas\ntypically sampling galaxies out to ~0.7 R_25. These data-cubes can be used to\nproduce 2D maps of the star formation rate, dust extinction, electron density,\nstellar population parameters, the kinematics and chemical abundances of both\nstars and ionized gas, and other physical quantities derived from the fitting\nof the stellar spectrum and the measurement of nebular emission lines. To\nexemplify our methods and the quality of the data, we present the VENGA\ndata-cube on the face-on Sc galaxy NGC 628 (a.k.a. M 74). The VENGA\nobservations of NGC 628 are described, as well as the construction of the\ndata-cube, our spectral fitting method, and the fitting of the stellar and\nionized gas velocity fields. We also propose a new method to measure the\ninclination of nearly face-on systems based on the matching of the stellar and\ngas rotation curves using asymmetric drift corrections. VENGA will measure\nrelevant physical parameters across different environments within these\ngalaxies, allowing a series of studies on star formation, structure assembly,\nstellar populations, chemical evolution, galactic feedback, nuclear activity,\nand the properties of the interstellar medium in massive disk galaxies.", "cat": "astro-ph.CO", "authors": ["Guillermo A. Blanc", "Tim Weinzirl", "Mimi Song", "Amanda Heiderman", "Karl Gebhardt", "Shardha Jogee", "Neal J. Evans II", "Remco C. E. van den Bosch", "Rongxin Luo", "Niv Drory", "Maximilian Fabricius", "David Fisher", "Lei Hao", "Kyle Kaplan", "Irina Marinova", "Nalin Vutisalchavakul", "Peter Yoachim"]}, "1652": {"id": "2103.15698v2", "title": "A Systematic Survey on Multi-relational Community Detection", "url": "http://arxiv.org/pdf/2103.15698v2", "date": "2021-04-01 08:38:19", "abs": "Complex networks contain various interactions among similar or different\nentities. These kinds of networks are called multi-relational networks, in\nwhich each layer corresponds to a special type of interaction. Multi-relational\nnetworks are a particular type of multilayer networks in which nodes are\nsimilar entities; however, edges or communications demonstrate different types\nof interactions among similar entities. In this survey, we study community\ndetection methods for multi-relational networks. The considered models are\ndivided into two main groups, namely, direct methods and indirect methods. We\nput indirect methods in two classes: flattening and ensembling, and the direct\nmethods are further divided into four groups which are: probabilistic methods,\nalgebraic methods, modular-based methods, and graph feature-based methods. For\neach approach and each method, we explain their pros and cons. Additionally,\nall the used datasets in the multilayer community detection studies are\ncategorized into synthetic and real data. We elaborate on the most important\ndatasets. Afterward, the utilized evaluation metrics by the papers are\ndescribed. Finally, the current models' challenges and shortcomings are\ndiscussed. Finally, some suggestions for future research are developed. Putting\nall this together, this study, to the best of our knowledge, is the most\ncomprehensive survey dedicated to multi-relational networks community\ndetection.", "cat": "cs.SI", "authors": ["Zahra Roozbahani", "Hanif Emamgholizadeh", "Jalal Rezaeenour", "Mahshid Hajialikhani"]}, "1653": {"id": "2407.05200v1", "title": "First Results from the Dragonfly Ultrawide Survey: the Largest Eleven Quenched Diffuse Dwarf Galaxies in 3100 deg$^2$ with Spectroscopic Confirmation", "url": "http://arxiv.org/pdf/2407.05200v1", "date": "2024-07-06 22:29:34", "abs": "The Dragonfly Telephoto Array employs a unique design to detect very large\nand diffuse galaxies, which might be missed with conventional telescopes. The\nDragonfly Ultrawide Survey (DFUWS) is a new wide-field survey which will cover\n10,000 deg$^2$ of the northern sky, and it provides an ideal dataset to find\nthese large diffuse galaxies. From 3100 deg$^2$ of DFUWS data, we identified\neleven large, low surface brightness galaxies as a pilot sample for\nspectroscopic follow-up. These are the largest galaxies in the examined area\nthat appear smooth and isolated, with effective radii of 12\"-27\". Eight are\nbelow 24 $\\mathrm{mag\\,arcsec^{-2}}$ in central $g$-band surface brightness.\nKeck Cosmic Web Imager (KCWI) spectra of the diffuse light show that all eleven\ngalaxies in this sample are quiescent, and seven qualify as ultra-diffuse\ngalaxies (UDGs). Eight galaxies have distances between 15 and 30 Mpc, while the\nother three are in the Pegasus cluster at 50 Mpc. Their spectra show evidence\nof a $\\sim 1$Gyr old stellar population in addition to an even older stellar\npopulation. The intermediate-age component is present in group and satellite\ngalaxies but not in the Pegasus cluster UDGs. All galaxies in this sample are\ndetected in both Dragonfly and Legacy imaging, and the sample partially\noverlaps with existing UDG catalogs. This pilot sample provides an excellent\ntraining set for our analysis of the upcoming full 10,000 deg$^2$ DFUWS data,\nfrom which we may expect to discover even larger, previously-unknown galaxies.", "cat": "astro-ph.GA", "authors": ["Zili Shen", "William P. Bowman", "Pieter van Dokkum", "Roberto G. Abraham", "Imad Pasha", "Michael A. Keim", "Qing Liu", "Deborah M. Lokhorst", "Steven R. Janssens", "Seery Chen"]}, "1654": {"id": "1511.00343v1", "title": "Sejong open cluster survey (SOS) - V. The active star forming region Sh 2-255 -- 257", "url": "http://arxiv.org/pdf/1511.00343v1", "date": "2015-11-02 00:24:32", "abs": "There is much observational evidence that active star formation is taking\nplace in the HII regions Sh 2-255 -- 257. We present a photometric study of\nthis star forming region (SFR) using imaging data obtained in passbands from\nthe optical to the mid-infrared in order to study the star formation process. A\ntotal of 218 members were identified using various selection criteria based on\ntheir observational properties. The SFR is reddened by at least E(B-V) = 0.8\nmag, and the reddening law toward the region is normal (R_V = 3.1). From the\nzero-age main sequence fitting method it is confirmed that the SFR is 2.1 +/-\n0.3 kpc from the Sun. The median age of the identified members is estimated to\nbe about 1.3 Myr from comparison of the Hertzsprung-Russell diagram (HRD) with\nstellar evolutionary models. The initial mass function (IMF) is derived from\nthe HRD and the near-infrared (J, J-H) color-magnitude diagram. The slope of\nthe IMF is about Gamma = -1.6 +/- 0.1, which is slightly steeper than that of\nthe Salpeter/Kroupa IMF. It implies that low-mass star formation is dominant in\nthe SFR. The sum of the masses of all the identified members provides the lower\nlimit of the cluster mass (169M_sun). We also analyzed the spectral energy\ndistribution (SED) of pre-main sequence stars using the SED fitting tool of\nRobitaille et al. and confirm that there is a significant discrepancy between\nstellar mass and age obtained from two different methods based on the SED\nfitting tool and the HRD.", "cat": "astro-ph.SR", "authors": ["Beomdu Lim", "Hwankyung Sung", "Hyeonoh Hur", "Byeong-Cheol Lee", "Michael S. Bessell", "Jinyoung S. Kim", "Kang Hwan Lee", "Byeong-Gon Park", "Gwanghui Jeong"]}, "1655": {"id": "2204.05907v1", "title": "Galapagos-2/Galfitm/GAMA -- multi-wavelength measurement of galaxy structure: separating the properties of spheroid and disk components in modern surveys", "url": "http://arxiv.org/pdf/2204.05907v1", "date": "2022-04-12 16:07:29", "abs": "We present the capabilities of Galapagos--2 and Galfitm in the context of\nfitting 2-component profiles to galaxies, on the way to providing complete\nmulti-band, multi-component fitting of large samples of galaxies in future\nsurveys. We release both the code and the fit results to 234,239 objects from\nthe DR3 of the Gama survey, a sample significantly deeper than previous works.\nWe use stringent tests on both simulated and real data, as well as comparison\nto public catalogues to evaluate the advantages of using multi-band over\nsingle-band data. We show that multi-band fitting using Galfitm provides\nsignificant advantages when trying to decompose galaxies into their individual\nconstituents, as more data are being used, by effectively being able to use the\ncolour information buried in the individual exposures to its advantage. Using\nsimulated data, we find that multi-band fitting significantly reduces the\ndeviations from real parameter values, allows component sizes and S\\'ersic\nindices to be recovered more accurately, and, by design, constrains the\nband-to-band variations of these parameters to more physical values. On both\nsimulated and real data, we confirm that the SEDs of the 2 main components can\nbe recovered to fainter magnitudes compared to using single-band fitting, which\ntends to recover disks and bulges to - on average - have identical SEDs when\nthe galaxies become too faint, instead of the different SEDs they truly have.\nBy comparing our results to those provided by other fitting codes, we confirm\nthat they agree in general, but measurement errors can be significantly reduced\nby using the multi-band tools developed by the MegaMorph project. We conclude\nthat the multi-band fitting employed by Galapagos-2 and Galfitm significantly\nimproves the accuracy of structural galaxy parameters and enables much larger\nsamples to be be used in a scientific analysis.", "cat": "astro-ph.GA", "authors": ["Boris H\u00e4u\u00dfler", "Marina Vika", "Steven P. Bamford", "Evelyn J. Johnston", "Sarah Brough", "Sarah Casura", "Benne W. Holwerda", "Lee S. Kelvin", "Cristina Popescu"]}, "1656": {"id": "2010.12309v3", "title": "A Survey on Recent Approaches for Natural Language Processing in Low-Resource Scenarios", "url": "http://arxiv.org/pdf/2010.12309v3", "date": "2021-04-09 13:48:02", "abs": "Deep neural networks and huge language models are becoming omnipresent in\nnatural language applications. As they are known for requiring large amounts of\ntraining data, there is a growing body of work to improve the performance in\nlow-resource settings. Motivated by the recent fundamental changes towards\nneural models and the popular pre-train and fine-tune paradigm, we survey\npromising approaches for low-resource natural language processing. After a\ndiscussion about the different dimensions of data availability, we give a\nstructured overview of methods that enable learning when training data is\nsparse. This includes mechanisms to create additional labeled data like data\naugmentation and distant supervision as well as transfer learning settings that\nreduce the need for target supervision. A goal of our survey is to explain how\nthese methods differ in their requirements as understanding them is essential\nfor choosing a technique suited for a specific low-resource setting. Further\nkey aspects of this work are to highlight open issues and to outline promising\ndirections for future research.", "cat": "cs.CL", "authors": ["Michael A. Hedderich", "Lukas Lange", "Heike Adel", "Jannik Str\u00f6tgen", "Dietrich Klakow"]}, "1657": {"id": "2312.14479v1", "title": "Navigating the Concurrency Landscape: A Survey of Race Condition Vulnerability Detectors", "url": "http://arxiv.org/pdf/2312.14479v1", "date": "2023-12-22 07:05:39", "abs": "As technology continues to advance and we usher in the era of Industry 5.0,\nthere has been a profound paradigm shift in operating systems, file systems,\nweb, and network applications. The conventional utilization of multiprocessing\nand multicore systems has made concurrent programming increasingly pervasive.\nHowever, this transformation has brought about a new set of issues known as\nconcurrency bugs, which, due to their wide prevalence in concurrent programs,\nhave led to severe failures and potential security exploits. Over the past two\ndecades, numerous researchers have dedicated their efforts to unveiling,\ndetecting, mitigating, and preventing these bugs, with the last decade\nwitnessing a surge in research within this domain. Among the spectrum of\nconcurrency bugs, data races or race condition vulnerabilities stand out as the\nmost prevalent, accounting for a staggering 80\\% of all concurrency bugs. This\nsurvey paper is focused on the realm of race condition bug detectors. We\nsystematically categorize these detectors based on the diverse methodologies\nthey employ. Additionally, we delve into the techniques and algorithms\nassociated with race detection, tracing the evolution of this field over time.\nFurthermore, we shed light on the application of fuzzing techniques in the\ndetection of race condition vulnerabilities. By reviewing these detectors and\ntheir static analyses, we draw conclusions and outline potential future\nresearch directions, including enhancing accuracy, performance, applicability,\nand comprehensiveness in race condition vulnerability detection.", "cat": "cs.CR", "authors": ["Aishwarya Upadhyay", "Vijay Laxmi", "Smita Naval"]}, "1658": {"id": "1205.1048v2", "title": "Impact of Redshift Information on Cosmological Applications with Next-Generation Radio Surveys", "url": "http://arxiv.org/pdf/1205.1048v2", "date": "2012-09-12 10:21:53", "abs": "In this paper, we explore how the forthcoming generation of large-scale radio\ncontinuum surveys, with the inclusion of some degree of redshift information,\ncan constrain cosmological parameters. By cross-matching these radio surveys\nwith shallow optical to near-infrared surveys, we can essentially separate the\nsource distribution into a low- and a high-redshift sample, thus providing a\nconstraint on the evolution of cosmological parameters such as those related to\ndark energy. We examine two radio surveys, the Evolutionary Map of the Universe\n(EMU) and the Westerbork Observations of the Deep APERTIF Northern sky (WODAN).\nA crucial advantage is their combined potential to provide a deep, full-sky\nsurvey. The surveys used for the cross-identifications are SkyMapper and SDSS,\nfor the southern and northern skies, respectively. We concentrate on the galaxy\nclustering angular power spectrum as our benchmark observable, and find that\nthe possibility of including such low redshift information yields major\nimprovements in the determination of cosmological parameters. With this\napproach, and provided a good knowledge of the galaxy bias evolution, we are\nable to put strict constraints on the dark energy parameters, i.e.\nw_0=-0.9+/-0.041 and w_a=-0.24+/-0.13, with type Ia supernovae and CMB priors\n(with a one-parameter bias in this case); this corresponds to a Figure of Merit\n(FoM) > 600, which is twice better than what is obtained by using only the\ncross-identified sources and greater than four time better than the case\nwithout any redshift information at all.", "cat": "astro-ph.CO", "authors": ["Stefano Camera", "M\u00e1rio G. Santos", "David J. Bacon", "Matt J. Jarvis", "Kim McAlpine", "Ray P. Norris", "Alvise Raccanelli", "Huub R\u00f6ttgering"]}, "1659": {"id": "1201.5617v2", "title": "New measurements of the cosmic infrared background fluctuations in deep Spitzer/IRAC survey data and their cosmological implications", "url": "http://arxiv.org/pdf/1201.5617v2", "date": "2012-04-19 15:06:23", "abs": "We extend previous measurements of cosmic infrared background (CIB)\nfluctuations to ~ 1 deg using new data from the Spitzer Extended Deep Survey.\nTwo fields, with depths of ~12 hr/pixel over 3 epochs, are analyzed at 3.6 and\n4.5 mic. Maps of the fields were assembled using a self-calibration method\nuniquely suitable for probing faint diffuse backgrounds. Resolved sources were\nremoved from the maps to a magnitude limit of AB mag ~ 25, as indicated by the\nlevel of the remaining shot noise. The maps were then Fourier-transformed and\ntheir power spectra were evaluated. Instrumental noise was estimated from the\ntime-differenced data, and subtracting this isolates the spatial fluctuations\nof the actual sky. The power spectra of the source-subtracted fields remain\nidentical (within the observational uncertainties) for the three epochs\nindicating that zodiacal light contributes negligibly to the fluctuations.\nComparing to 8 mic power spectra shows that Galactic cirrus cannot account for\nthe fluctuations. The signal appears isotropically distributed on the sky as\nrequired for an extragalactic origin. The CIB fluctuations continue to diverge\nto > 10 times those of known galaxy populations on angular scales out to < 1\ndeg. The low shot noise levels remaining in the diffuse maps indicate that the\nlarge scale fluctuations arise from the spatial clustering of faint sources\nwell below the confusion noise. The spatial spectrum of these fluctuations is\nin reasonable agreement with an origin in populations clustered according to\nthe standard cosmological model (LCDM) at epochs coinciding with the first\nstars era.", "cat": "astro-ph.CO", "authors": ["A. Kashlinsky", "R. G. Arendt", "M. L. N. Ashby", "G. G. Fazio", "J. Mather", "S. H. Moseley"]}, "1660": {"id": "2008.13538v1", "title": "Scientific Paper Recommendation: A Survey", "url": "http://arxiv.org/pdf/2008.13538v1", "date": "2020-08-10 03:17:06", "abs": "Globally, recommendation services have become important due to the fact that\nthey support e-commerce applications and different research communities.\nRecommender systems have a large number of applications in many fields\nincluding economic, education, and scientific research. Different empirical\nstudies have shown that recommender systems are more effective and reliable\nthan keyword-based search engines for extracting useful knowledge from massive\namounts of data. The problem of recommending similar scientific articles in\nscientific community is called scientific paper recommendation. Scientific\npaper recommendation aims to recommend new articles or classical articles that\nmatch researchers' interests. It has become an attractive area of study since\nthe number of scholarly papers increases exponentially. In this survey, we\nfirst introduce the importance and advantages of paper recommender systems.\nSecond, we review the recommendation algorithms and methods, such as\nContent-Based methods, Collaborative Filtering methods, Graph-Based methods and\nHybrid methods. Then, we introduce the evaluation methods of different\nrecommender systems. Finally, we summarize open issues in the paper recommender\nsystems, including cold start, sparsity, scalability, privacy, serendipity and\nunified scholarly data standards. The purpose of this survey is to provide\ncomprehensive reviews on scholarly paper recommendation.", "cat": "cs.IR", "authors": ["Xiaomei Bai", "Mengyang Wang", "Ivan Lee", "Zhuo Yang", "Xiangjie Kong", "Feng Xia"]}, "1661": {"id": "2102.01330v2", "title": "AI4VIS: Survey on Artificial Intelligence Approaches for Data Visualization", "url": "http://arxiv.org/pdf/2102.01330v2", "date": "2021-07-19 16:56:18", "abs": "Visualizations themselves have become a data format. Akin to other data\nformats such as text and images, visualizations are increasingly created,\nstored, shared, and (re-)used with artificial intelligence (AI) techniques. In\nthis survey, we probe the underlying vision of formalizing visualizations as an\nemerging data format and review the recent advance in applying AI techniques to\nvisualization data (AI4VIS). We define visualization data as the digital\nrepresentations of visualizations in computers and focus on data visualization\n(e.g., charts and infographics). We build our survey upon a corpus spanning ten\ndifferent fields in computer science with an eye toward identifying important\ncommon interests. Our resulting taxonomy is organized around WHAT is\nvisualization data and its representation, WHY and HOW to apply AI to\nvisualization data. We highlight a set of common tasks that researchers apply\nto the visualization data and present a detailed discussion of AI approaches\ndeveloped to accomplish those tasks. Drawing upon our literature review, we\ndiscuss several important research questions surrounding the management and\nexploitation of visualization data, as well as the role of AI in support of\nthose processes. We make the list of surveyed papers and related material\navailable online at ai4vis.github.io.", "cat": "cs.HC", "authors": ["Aoyu Wu", "Yun Wang", "Xinhuan Shu", "Dominik Moritz", "Weiwei Cui", "Haidong Zhang", "Dongmei Zhang", "Huamin Qu"]}, "1662": {"id": "1504.08145v1", "title": "Online survey for collective clustering of computer generated architectural floor plans", "url": "http://arxiv.org/pdf/1504.08145v1", "date": "2015-04-30 09:44:38", "abs": "The aim of this study is to understand what are the collective actions of\narchitecture practitioners when grouping floor plan designs. The understanding\nof how professionals and students solve this complex problem may help to\ndevelop specific programmes for the teaching of architecture. In addition, the\nfindings of this study can help in the development of query mechanisms for\ndatabase retrieval of floor plans and the implementation of clustering\nmechanisms to aggregate floor plans resulting from generative design methods.\nThe study aims to capture how practitioners define similarity between floor\nplans from a pool of available designs. A hybrid evolutionary strategy is used,\nwhich takes into account the building's functional program to generate\nalternative floor plan designs. The first step of this methodology consisted in\nan online survey to gather information on how the respondents would perform a\nclustering task. Online surveys have been used in several applications and are\na method of data collection that conveys several advantages. When properly\ndeveloped and implemented, a survey portrays the characteristics of large\ngroups of respondents on a specific topic and allows assessing its\nrepresentation. Several types of surveys are available; e.g. questionnaire and\ninterview formats, phone survey, and online surveys, which can be coupled with\ninference engines that act and direct the survey according to respondents'\nanswers. In the present study, the survey was posed as an online exercise in\nwhich respondents had to perform a pre-defined task, which makes it similar to\nrunning an experiment in an online environment. The experiment aimed to\nunderstand the perception and criteria of the target population to perform the\nclustering task by comparing the results with the respondents' answers to a\nquestionnaire presented at the end of the exercise.", "cat": "cs.HC", "authors": ["David Sousa-Rodrigues", "Mafalda Teixeira de Sampayo", "Eug\u00e9nio Rodrigues", "Ad\u00e9lio Rodrigues Gaspar", "\u00c1lvaro Gomes", "Carlos Henggeler Antunes"]}, "1663": {"id": "1909.07985v1", "title": "The ALMA Survey of 70 $\u03bc$m dark High-mass clumps in Early Stages (ASHES). I. Pilot Survey: Clump Fragmentation", "url": "http://arxiv.org/pdf/1909.07985v1", "date": "2019-09-17 18:00:02", "abs": "(Abridged) ASHES has been designed to systematically characterize the\nearliest stages and to constrain theories of high-mass star formation. A total\nof 12 massive (>500 $M_{\\odot}$), cold (<15 K), 3.6-70 $\\mu$m dark prestellar\nclump candidates, embedded in IRDCs, were carefully selected in the pilot\nsurvey to be observed with ALMA. We mosaiced each clump (~1 arcmin^2) in dust\nand line emission with the 12m/7m/TP arrays at 224 GHz, resulting in ~1.2\"\nresolution (~4800 AU). As the first paper of the series, we concentrate on the\ndust emission to reveal the clump fragmentation. We detect 294 cores, from\nwhich 84 (29%) are categorized as protostellar based on outflow activity or\n'warm core' line emission. The remaining 210 (71%) are considered prestellar\ncore candidates. The number of detected cores is independent of the mass\nsensitivity range of the observations. On average, more massive clumps tend to\nform more cores. We find a large population of low-mass (<1 M) cores and no\nhigh-mass (>30 $M_{\\odot}$) prestellar cores. The most massive prestellar core\nhas a mass of 11 $M_{\\odot}$. From the prestellar CMF, we derive a power law\nindex of 1.17+-0.1, slightly shallower than Salpeter (1.35). We use the MST\ntechnique to characterize the separation between cores and their spatial\ndistribution, and derive mass segregation ratios. While there is a range of\ncore masses and separations detected in the sample, the mean separation and\nmass of cores are well explained by thermal fragmentation and are inconsistent\nwith turbulent Jeans fragmentation. The core spatial distribution is well\ndescribed by hierarchical subclustering rather than centrally peaked\nclustering. There is no conclusive evidence of mass segregation. We test\nseveral theoretical conditions, and conclude that overall, competitive\naccretion and global hierarchical collapse scenarios are favored over the\nturbulent core accretion scenario.", "cat": "astro-ph.GA", "authors": ["Patricio Sanhueza", "Yanett Contreras", "Benjamin Wu", "James M. Jackson", "Andr\u00e9s E. Guzm\u00e1n", "Qizhou Zhang", "Shanghuo Li", "Xing Lu", "Andrea Silva", "Natsuko Izumi", "Tie Liu", "Rie E. Miura", "Ken'ichi Tatematsu", "Takeshi Sakai", "Henrik Beuther", "Guido Garay", "Satoshi Ohashi", "Masao Saito", "Fumitaka Nakamura", "Kazuya Saigo", "V. S. Veena", "Quang Nguyen-Luong", "Daniel Tafoya"]}, "1664": {"id": "2003.07741v1", "title": "Methodology and Performance of the Two-Year Galactic Plane Scanning Survey of Insight-HXMT", "url": "http://arxiv.org/pdf/2003.07741v1", "date": "2020-03-17 14:19:56", "abs": "The Galactic plane scanning survey is one of the main scientific objectives\nof the Hard X-ray Modulation Telescope (known as Insight-HXMT). During the\ntwo-year operation of Insight-HXMT, more than 1000 scanning observations have\nbeen performed and the whole Galactic plane ($\\rm 0^{\\circ} $10^{43}$ erg s$^{-1}$ the kinetic\nluminosity of the radio jets is not longer correlated with the X-ray luminosity\nand discuss various reasons. We find an anti-correlation between the central\ncooling time t_cool and the radio luminosity L_R indicating a need for more\npowerful AGN in clusters with short central cooling times.", "cat": "astro-ph.CO", "authors": ["K. B\u00f6ckmann", "M. Br\u00fcggen", "B. Koribalski", "A. Veronica", "T. H. Reiprich", "E. Bulbul", "Y. E. Bahar", "F. Balzer", "J. Comparat", "C. Garrel", "V. Ghirardini", "G. G\u00fcrkan", "M. Kluge", "D. Leahy", "A. Merloni", "A. Liu", "M. E. Ramos-Ceja", "M. Salvato", "J. Sanders", "S. Shabala", "X. Zhang"]}, "1669": {"id": "1507.01214v1", "title": "Early type galaxies and structural parameters from ESO public survey KiDS", "url": "http://arxiv.org/pdf/1507.01214v1", "date": "2015-07-05 12:38:34", "abs": "The Kilo Degree survey (KiDS) is a large-scale optical imaging survey carried\nout with the VLT Survey Telescope (VST), which is the ideal tool for galaxy\nevolution studies. We expect to observe millions of galaxies for which we\nextract the structural parameters in four wavebands (u, g, r and i). This\nsample will represent the largest dataset with measured structural parameters\nup to a redshift $z=0.5$. In this paper we will introduce the sample, and\ndescribe the 2D fitting procedure using the 2DPHOT environment and the\nvalidation of the parameters with an external catalog.", "cat": "astro-ph.GA", "authors": ["N. Roy", "N. R. Napolitano", "F. La Barbera", "C. Tortora", "F. Getman", "M. Radovich", "M. Capaccioli", "the KiDS collaboration"]}, "1670": {"id": "1711.03740v1", "title": "Estimation of Cusp Location of Stochastic Processes: a Survey", "url": "http://arxiv.org/pdf/1711.03740v1", "date": "2017-11-10 09:31:56", "abs": "We present a review of some recent results on estimation of location\nparameter for several models of observations with cusp-type singularity at the\nchange point. We suppose that the cusp-type models fit better to the real\nphenomena described usually by change point models. The list of models includes\nGaussian, inhomogeneous Poisson, ergodic diffusion processes, time series and\nthe classical case of i.i.d. observations. We describe the properties of the\nmaximum likelihood and Bayes estimators under some asymptotic assumptions. The\nasymptotic efficiency of estimators are discussed as well and the results of\nsome numerical simulations are presented. We provide some heuristic arguments\nwhich demonstrate the convergence of log-likelihood ratios in the models under\nconsideration to the fractional Brownian motion.", "cat": "math.ST", "authors": ["S. Dachian", "N. Kordzakhia", "Yu. A. Kutoyants", "A. Novikov"]}, "1671": {"id": "1810.09461v2", "title": "A-type stars in the Canada-France Imaging Survey II. Tracing the height of the disc at large distances with Blue Stragglers", "url": "http://arxiv.org/pdf/1810.09461v2", "date": "2018-12-04 18:10:02", "abs": "We present the kinematics of Blue Straggler (BS) stars identified in the\nCanada-France-Imaging-Survey (CFIS), covering 4000 deg$^2$ on the sky in the\n$u$-band. The BS sample, characterised through CFIS and Pan-STARRS photometry,\nhas been kinematically decomposed into putative halo and disc populations after\ncross-matching with Gaia astrometry and SDSS/SEGUE/LAMOST spectroscopy. This\ndecomposition clearly reveals the strong flaring of the outer Milky Way disc.\nIn particular, we show that we can detect this flaring up to a vertical height\nof $|Z| \\simeq 8$ kpc at a Galactocentric distance of $R\\sim $27 kpc. While\nsome small level of flaring is expected for extended discs built up by radial\nmigration, we demonstrate that this observed very strong flaring of the Milky\nWay disc is more likely consistent with it being dynamically heated by the\nrepeated passage of the Sagittarius dwarf spheroidal galaxy through the\nmidplane.", "cat": "astro-ph.GA", "authors": ["Guillaume F. Thomas", "Chervin F. P. Laporte", "Alan W. McConnachie", "Benoit Famaey", "Rodrigo Ibata", "Nicolas F. Martin", "Else Starkenburg", "Raymond Carlberg", "Khyati Malhan", "Kim Venn"]}, "1672": {"id": "2112.06745v1", "title": "A Survey of Unsupervised Domain Adaptation for Visual Recognition", "url": "http://arxiv.org/pdf/2112.06745v1", "date": "2021-12-13 15:55:23", "abs": "While huge volumes of unlabeled data are generated and made available in many\ndomains, the demand for automated understanding of visual data is higher than\never before. Most existing machine learning models typically rely on massive\namounts of labeled training data to achieve high performance. Unfortunately,\nsuch a requirement cannot be met in real-world applications. The number of\nlabels is limited and manually annotating data is expensive and time-consuming.\nIt is often necessary to transfer knowledge from an existing labeled domain to\na new domain. However, model performance degrades because of the differences\nbetween domains (domain shift or dataset bias). To overcome the burden of\nannotation, Domain Adaptation (DA) aims to mitigate the domain shift problem\nwhen transferring knowledge from one domain into another similar but different\ndomain. Unsupervised DA (UDA) deals with a labeled source domain and an\nunlabeled target domain. The principal objective of UDA is to reduce the domain\ndiscrepancy between the labeled source data and unlabeled target data and to\nlearn domain-invariant representations across the two domains during training.\nIn this paper, we first define UDA problem. Secondly, we overview the\nstate-of-the-art methods for different categories of UDA from both traditional\nmethods and deep learning based methods. Finally, we collect frequently used\nbenchmark datasets and report results of the state-of-the-art methods of UDA on\nvisual recognition problem.", "cat": "cs.CV", "authors": ["Youshan Zhang"]}, "1673": {"id": "2308.07426v3", "title": "A Survey on Point-of-Interest Recommendations Leveraging Heterogeneous Data", "url": "http://arxiv.org/pdf/2308.07426v3", "date": "2024-02-25 13:40:56", "abs": "Tourism is an important application domain for recommender systems. In this\ndomain, recommender systems are for example tasked with providing personalized\nrecommendations for transportation, accommodation, points-of-interest (POIs),\netc. Among these tasks, in particular the problem of recommending POIs that are\nof likely interest to individual tourists has gained growing attention in\nrecent years. Providing POI recommendations to tourists can however be\nespecially challenging due to the variability of the user's context. With the\nrapid development of the Web and today's multitude of online services, vast\namounts of data from various sources have become available, and these\nheterogeneous data represent a huge potential to better address the challenges\nof POI recommendation problems. In this work, we provide a survey of published\nresearch on the problem of POI recommendation between 2021 and 2023. The\nliterature was surveyed to identify the information types, techniques and\nevaluation methods employed. Based on the analysis, it was observed that the\ncurrent research tends to focus on a relatively narrow range of information\ntypes and there is a significant potential in improving POI recommendation by\nleveraging heterogeneous data. As the first information-centric survey on POI\nrecommendation research, this study serves as a reference for researchers\naiming to develop increasingly accurate, personalized and context-aware POI\nrecommender systems.", "cat": "cs.IR", "authors": ["Zehui Wang", "Wolfram H\u00f6pken", "Dietmar Jannach"]}, "1674": {"id": "2310.12919v1", "title": "Validation of the Survey Simulator tool for the NEO Surveyor mission using NEOWISE data", "url": "http://arxiv.org/pdf/2310.12919v1", "date": "2023-10-19 17:11:06", "abs": "The Near Earth Object Surveyor mission has a requirement to find two-thirds\nof the potentially hazardous asteroids larger than 140 meters in size. In order\nto determine the mission's expected progress toward this goal during design and\ntesting, as well as the actual progress during the survey, a simulation tool\nhas been developed to act as a consistent and quantifiable yardstick. We test\nthat the survey simulation software is correctly predicting on-sky positions\nand thermal infrared fluxes by using it to reproduce the published measurements\nof asteroids from the NEOWISE mission. We then extended this work to find\npreviously unreported detections of known near Earth asteroids in the NEOWISE\ndata archive, a search that resulted in 21,661 recovery detections, including\n1,166 objects that had no previously reported NEOWISE observations. These\nefforts demonstrate the reliability of the NEOS Survey Simulator tool, and the\nperennial value of searchable image and source catalog archives for extending\nour knowledge of the small bodies of the Solar System.", "cat": "astro-ph.EP", "authors": ["Joseph R. Masiero", "Dar W. Dahlen", "Amy K. Mainzer", "William F. Bottke", "Jennifer C. Bragg", "James. M. Bauer", "Tommy Grav"]}, "1675": {"id": "0905.3743v1", "title": "Galactic Globular and Open Clusters in the Sloan Digital Sky Survey. II. Test of Theoretical Stellar Isochrones", "url": "http://arxiv.org/pdf/0905.3743v1", "date": "2009-05-22 20:00:09", "abs": "We perform an extensive test of theoretical stellar models for main-sequence\nstars in ugriz, using cluster fiducial sequences obtained in the previous paper\nof this series. We generate a set of isochrones using the Yale Rotating\nEvolutionary Code (YREC) with updated input physics, and derive magnitudes and\ncolors in ugriz from MARCS model atmospheres. These models match cluster main\nsequences over a wide range of metallicity within the errors of the adopted\ncluster parameters. However, we find a large discrepancy of model colors at the\nlower main sequence (Teff < ~4500 K) for clusters at and above solar\nmetallicity. We also reach similar conclusions using the theoretical isochrones\nof Girardi et al. and Dotter et al., but our new models are generally in better\nagreement with the data. Using our theoretical isochrones, we also derive\nmain-sequence fitting distances and turn-off ages for five key globular\nclusters, and demonstrate the ability to derive these quantities from\nphotometric data in the Sloan Digital Sky Survey. In particular, we exploit\nmultiple color indices (g - r, g - i, and g - z) in the parameter estimation,\nwhich allows us to evaluate internal systematic errors. Our distance estimates,\nwith an error of sigma(m - M) = 0.03-0.11 mag for individual clusters, are\nconsistent with Hipparcos-based subdwarf fitting distances derived in the\nJohnson-Cousins or Stromgren photometric systems.", "cat": "astro-ph.SR", "authors": ["Deokkeun An", "Marc H. Pinsonneault", "Thomas Masseron", "Franck Delahaye", "Jennifer A. Johnson", "Donald M. Terndrup", "Timothy C. Beers", "Inese I. Ivans", "Zeljko Ivezic"]}, "1676": {"id": "1708.00314v1", "title": "An Optically Faint Quasar Survey at z~5 in the CFHTLS Wide Field: Estimates of the Black Hole Masses and Eddington Ratios", "url": "http://arxiv.org/pdf/1708.00314v1", "date": "2017-08-01 13:44:40", "abs": "We present the result of our spectroscopic follow-up observation for faint\nquasar candidates at z~5 in a part of the Canada-France-Hawaii Telescope Legacy\nSurvey wide field. We select nine photometric candidates and identify three z~5\nfaint quasars, one z~4 faint quasar, and a late-type star. Since two faint\nquasar spectra show Civ emission line without suffering from a heavy\natmospheric absorption, we estimate the black hole mass (M$_{BH}$) and\nEddington ratio (L/L$_{Edd}$) of them. The inferred log M$_{BH}$ are\n9.04+/-0.14 and 8.53+/-0.20, respectively. In addition, the inferred log\n(L/L$_{Edd}$) are -1.00+/-0.15 and -0.42+/-0.22, respectively. If we adopt that\nL/L$_{Edd}$= constant or $\\propto$ (1+z)^2, the seed black hole masses\n(M$_{seed}$) of our z~5 faint quasars are expected to be >10^5 M$_\\odot$ in\nmost cases. We also compare the observational results with a mass accretion\nmodel where angular momentum is lost due to supernova explosions (Kawakatu &\nWada 2008). Accordingly, M$_{BH}$ of the z~5 faint quasars in our sample can be\nexplained even if M$_{seed}$ is ~10^3M$_\\odot$. Since z~6 luminous qusars and\nour z~5 faint quasars are not on the same evolutionary track, z~6 luminous\nquasars and our z~5 quasars are not the same populations but different\npopulations, due to the difference of a period of the mass supply from host\ngalaxies. Furthermore, we confirm that one can explain M$_{BH}$ of z~6 luminous\nquasars and our z~5 faint quasars even if their seed black holes of them are\nformed at z~7.", "cat": "astro-ph.GA", "authors": ["H. Ikeda", "T. Nagao", "K. Matsuoka", "N. Kawakatu", "M. Kajisawa", "M. Akiyama", "T. Miyaji", "T. Morokuma"]}, "1677": {"id": "2401.04955v1", "title": "Classification and characterization using HCT/HFOSC spectra of carbon stars selected from the HES survey", "url": "http://arxiv.org/pdf/2401.04955v1", "date": "2024-01-10 06:45:26", "abs": "We present results from the analysis of 88 carbon stars selected from\nHamburg/ESO (HES) survey using low-resolution spectra (R$\\sim$1330 \\& 2190).\nThe spectra were obtained with the Himalayan Faint Object Spectrograph Camera\n(HFOSC) attached to the 2-m Himalayan Chandra Telescope (HCT). Using a\nwell-defined spectral criteria based on the strength of carbon molecular bands,\nthe stars are classified into different groups. In our sample, we have\nidentified 53 CH stars, four C-R stars, and two C-N type stars. Twenty-nine\nstars could not be classified due to the absence of prominent C$_{2}$ molecular\nbands in their spectra. We could derive the atmospheric parameters for 36\nstars. The surface temperature is determined using photometric calibrations and\nsynthesis of the H-alpha line profile. The surface gravity log g estimates are\nobtained using parallax estimates from the Gaia DR3 database whenever possible.\nMicroturbulent velocity ($\\zeta$) is derived using calibration equation of log\ng \\& ${\\zeta}$. We could determine metallicity for 48 objects from\nnear-infrared Ca II triplet features using calibration equations. The derived\nmetallicity ranges from $-$0.43$\\leq$[Fe/H]$\\leq$$-$3.49. Nineteen objects are\nfound to be metal-poor ([Fe/H] $\\leq$$-$1), 14 very metal-poor\n([Fe/H]$\\leq$$-$2), and five extremely metal-poor ([Fe/H]$\\leq$$-$3.0) stars.\nEleven objects are found to have a metallicity in the range $-$0.43\n$\\leq$[Fe/H]$\\leq$$-$0.97. We could derive the carbon abundance for 25 objects\nusing the spectrum synthesis calculation of the C$_{2}$ band around 5165\\AA.\nThe most metal-poor objects found will make important targets for follow-up\ndetailed chemical composition studies based on high-resolution spectroscopy,\nthat are likely to provide insight into the Galactic chemical evolution.", "cat": "astro-ph.SR", "authors": ["Meenakshi Purandardas", "Aruna Goswami"]}, "1678": {"id": "1011.0710v1", "title": "A High-Resolution Survey of HI Absorption toward the Central 200 pc of the Galactic Center", "url": "http://arxiv.org/pdf/1011.0710v1", "date": "2010-11-02 19:34:37", "abs": "We present an HI absorption survey of the central 250 pc of the Galaxy. Very\nLarge Array (VLA) observations were made at 21 cm in the DnC and CnB\nconfigurations and have a resolution of ~15\"(0.6 pc at the Galactic Center (GC)\ndistance) and a velocity resolution of ~2.5 km/s. This study provides HI data\nwith high spatial resolution, comparable with the many high resolution\nobservations which have been made of GC sources over the past ten years. Here\nwe present an overview of the HI absorption toward ~40 well-known continuum\nsources and a detailed comparison of the ionized, atomic and molecular\ncomponents of the interstellar medium for the Sgr B, Radio Arc and Sgr C\nregions. In these well-known regions, the atomic gas appears to be closely\ncorrelated in both velocity and distribution to the ionized and molecular gas,\nindicating that it resides in photo-dissociation regions related to the HII\nregions in the GC. Toward the majority of the radio continuum sources, HI\nabsorption by the 3-kpc arm is detected, constraining these sources to lie\nbeyond a 5 kpc distance in the Galaxy.", "cat": "astro-ph.GA", "authors": ["Cornelia C. Lang", "W. Miller Goss", "Claudia Cyganowski", "Kelsey I. Clubb"]}, "1679": {"id": "2402.06076v1", "title": "The Gaia-ESO Survey: The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars", "url": "http://arxiv.org/pdf/2402.06076v1", "date": "2024-02-08 21:57:11", "abs": "The Gaia-ESO Survey is an European Southern Observatory (ESO) public\nspectroscopic survey that targeted $10^5$ stars in the Milky Way covering the\nmajor populations of the disk, bulge and halo. The observations were made using\nFLAMES on the VLT obtaining both UVES high ($R\\sim47,000$) and GIRAFFE medium\n($R\\sim20,000$) resolution spectra.\n The analysis of the Gaia-ESO spectra was the work of multiple analysis teams\n(nodes) within five working groups (WG). The homogenisation of the stellar\nparameters within WG11 (high resolution observations of FGK stars) and the\nhomogenisation of the stellar parameters within WG10 (medium resolution\nobservations of FGK stars) is described here. In both cases, the homogenisation\nwas carried out using a bayesian Inference method developed specifically for\nthe Gaia-ESO Survey by WG11.\n The WG10 homogenisation primarily used the cross-match of stars with WG11 as\nthe reference set in both the stellar parameter and chemical abundance\nhomogenisation. In this way the WG10 homogenised results have been placed\ndirectly onto the WG11 stellar parameter and chemical abundance scales. The\nreference set for the metal-poor end was sparse which limited the effectiveness\nof the homogenisation in that regime.\n For WG11, the total number of stars for which stellar parameters were derived\nwas 6,231 with typical uncertainties for Teff, log g and [Fe/H] of 32~K, 0.05\nand 0.05 respectively. One or more chemical abundances out of a possible 39\nelements were derived for 6,188 of the stars.\n For WG10, the total number of stars for which stellar parameters were derived\nwas 76,675 with typical uncertainties for Teff, log g and [Fe/H] of 64~K, 0.15\nand 0.07 respectively. One or more chemical abundances out of a possible 30\nelements were derived for 64,177 of the stars.", "cat": "astro-ph.SR", "authors": ["C. C. Worley", "R. Smiljanic", "L. Magrini", "A. Frasca", "E. Franciosini", "D. Montes", "D. K. Feuillet", "H. M. Tabernero", "J. I. Gonz\u00e1lez Hern\u00e1ndez", "S. Villanova", "\u0160. Mikolaitis", "K. Lind", "G. Tautvai\u0161ien\u0117", "A. R. Casey", "A. J. Korn", "P. Bonifacio", "C. Soubiran", "E. Caffau", "G. Guiglion", "T. Merle", "A. Hourihane", "A. Gonneau", "P. Fran\u00e7ois", "S. Randich", "G. Gilmore", "J. R. Lewis", "D. N. A. Murphy", "R. D. Jeffries", "S. E. Koposov", "R. Blomme", "A. C. Lanzafame", "T. Bensby", "A. Bragaglia", "E. J. Alfaro", "N. A. Walton", "A. Vallenari", "T. Prusti", "K. Biazzo", "P. Jofr\u00e9", "S. Zaggia", "U. Heiter", "E. Marfil", "F. Jim\u00e9nez-Esteban", "M. L. Guti\u00e9rrez Albarr\u00e1n", "L. Morbidelli"]}, "1680": {"id": "2311.10232v1", "title": "Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey: III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-Transit Jupiter Orbiting TOI-2010", "url": "http://arxiv.org/pdf/2311.10232v1", "date": "2023-11-16 23:06:50", "abs": "Large-scale exoplanet surveys like the TESS mission are powerful tools for\ndiscovering large numbers of exoplanet candidates. Single-transit events are\ncommonplace within the resulting candidate list due to the unavoidable\nlimitation of observing baseline. These single-transit planets often remain\nunverified due to their unknown orbital period and consequent difficulty in\nscheduling follow up observations. In some cases, radial velocity (RV) follow\nup can constrain the period enough to enable a future targeted transit\ndetection. We present the confirmation of one such planet: TOI-2010 b. Nearly\nthree years of RV coverage determined the period to a level where a broad\nwindow search could be undertaken with the Near-Earth Object Surveillance\nSatellite (NEOSSat), detecting an additional transit. An additional detection\nin a much later TESS sector solidified our final parameter estimation. We find\nTOI-2010 b to be a Jovian planet ($M_P = 1.29 \\ M_{\\rm Jup}$, $R_P = 1.05 \\\nR_{\\rm Jup}$) on a mildly eccentric orbit ($e = 0.21$) with a period of $P =\n141.83403$ days. Assuming a simple model with no albedo and perfect heat\nredistribution, the equilibrium temperature ranges from about 360 K to 450 K\nfrom apoastron to periastron. Its wide orbit and bright host star ($V=9.85$)\nmake TOI-2010 b a valuable test-bed for future low-insolation atmospheric\nanalysis.", "cat": "astro-ph.EP", "authors": ["Christopher R. Mann", "Paul A. Dalba", "David Lafreni\u00e8re", "Benjamin J. Fulton", "Guillaume H\u00e9brard", "Isabelle Boisse", "Shweta Dalal", "Magali Deleuil", "Xavier Delfosse", "Olivier Demangeon", "Thierry Forveille", "Neda Heidari", "Flavien Kiefer", "Eder Martioli", "Claire Moutou", "Michael Endl", "William D. Cochran", "Phillip MacQueen", "Franck Marchis", "Diana Dragomir", "Arvind F. Gupta", "Dax L. Feliz", "Belinda A. Nicholson", "Carl Ziegler", "Steven Villanueva Jr.", "Jason Rowe", "Geert Jan Talens", "Daniel Thorngren", "Daryll LaCourse", "Tom Jacobs", "Andrew W. Howard", "Allyson Bieryla", "David W. Latham", "Markus Rabus", "Tara Fetherolf", "Coel Hellier", "Steve B. Howell", "Peter Plavchan", "Michael Reefe", "Deven Combs", "Michael Bowen", "Justin Wittrock", "George R. Ricker", "S. Seager", "Joshua N. Winn", "Jon M. Jenkins", "Thomas Barclay", "David Watanabe", "Karen A. Collins", "Jason D. Eastman", "Eric B. Ting"]}, "1681": {"id": "2112.06366v1", "title": "Deep Extragalactic VIsible Legacy Survey (DEVILS): Identification of AGN through SED Fitting and the Evolution of the Bolometric AGN Luminosity Function", "url": "http://arxiv.org/pdf/2112.06366v1", "date": "2021-12-13 01:01:32", "abs": "Active galactic nuclei (AGN) are typically identified through radio,\nmid-infrared, or X-ray emission or through the presence of broad and/or narrow\nemission lines. AGN can also leave an imprint on a galaxy's spectral energy\ndistribution (SED) through the re-processing of photons by the dusty torus.\nUsing the SED fitting code ProSpect with an incorporated AGN component, we fit\nthe far ultraviolet to far-infrared SEDs of $\\sim$494,00 galaxies in the\nD10-COSMOS field and $\\sim$230,000 galaxies from the GAMA survey. By combining\nan AGN component with a flexible star formation and metallicity implementation,\nwe obtain estimates for the AGN luminosities, stellar masses, star formation\nhistories, and metallicity histories for each of our galaxies. We find that\nProSpect can identify AGN components in 91 per cent of galaxies pre-selected as\ncontaining AGN through narrow-emission line ratios and the presence of broad\nlines. Our ProSpect-derived AGN luminosities show close agreement with\nluminosities derived for X-ray selected AGN using both the X-ray flux and\nprevious SED fitting results. We show that incorporating the flexibility of an\nAGN component when fitting the SEDs of galaxies with no AGN has no significant\nimpact on the derived galaxy properties. However, in order to obtain accurate\nestimates of the stellar properties of AGN host galaxies, it is crucial to\ninclude an AGN component in the SED fitting process. We use our derived AGN\nluminosities to map the evolution of the AGN luminosity function for $010 deg with test statistic greater than 100 (corresponding to about 10\nsigma). Two methods, based on the CGRaBS, CRATES and BZCat catalogs, indicate\nhigh-confidence associations of 106 of these sources with known AGNs. This\nsample is referred to as the LAT Bright AGN Sample (LBAS). It contains two\nradio galaxies, namely Centaurus A and NGC 1275, and 104 blazars consisting of\n57 flat spectrum radio quasars (FSRQs), 42 BL Lac objects, and 5 blazars with\nuncertain classification. Four new blazars were discovered on the basis of the\nLAT detections. Remarkably, the LBAS includes 10 high-energy peaked BL Lacs\n(HBLs), sources which were so far hard to detect in the GeV range. Another 10\nlower-confidence associations are found. Only thirty three of the sources, plus\ntwo at |b|>10 deg, were previously detected with EGRET, probably due to the\nvariable nature of these sources. The analysis of the gamma-ray properties of\nthe LBAS sources reveals that the average GeV spectra of BL Lac objects are\nsignificantly harder than the spectra of FSRQs. No significant correlation\nbetween radio and peak gamma-ray fluxes is observed. Blazar log N - log S and\nluminosity functions are constructed to investigate the evolution of the\ndifferent blazar classes, with positive evolution indicated for FSRQs but none\nfor BLLacs. The contribution of LAT-blazars to the total extragalactic\ngamma-ray intensity is estimated.", "cat": "astro-ph.HE", "authors": ["A. A. Abdo"]}, "1695": {"id": "2106.07499v1", "title": "An Empirical Survey of Data Augmentation for Limited Data Learning in NLP", "url": "http://arxiv.org/pdf/2106.07499v1", "date": "2021-06-14 15:27:22", "abs": "NLP has achieved great progress in the past decade through the use of neural\nmodels and large labeled datasets. The dependence on abundant data prevents NLP\nmodels from being applied to low-resource settings or novel tasks where\nsignificant time, money, or expertise is required to label massive amounts of\ntextual data. Recently, data augmentation methods have been explored as a means\nof improving data efficiency in NLP. To date, there has been no systematic\nempirical overview of data augmentation for NLP in the limited labeled data\nsetting, making it difficult to understand which methods work in which\nsettings. In this paper, we provide an empirical survey of recent progress on\ndata augmentation for NLP in the limited labeled data setting, summarizing the\nlandscape of methods (including token-level augmentations, sentence-level\naugmentations, adversarial augmentations, and hidden-space augmentations) and\ncarrying out experiments on 11 datasets covering topics/news classification,\ninference tasks, paraphrasing tasks, and single-sentence tasks. Based on the\nresults, we draw several conclusions to help practitioners choose appropriate\naugmentations in different settings and discuss the current challenges and\nfuture directions for limited data learning in NLP.", "cat": "cs.CL", "authors": ["Jiaao Chen", "Derek Tam", "Colin Raffel", "Mohit Bansal", "Diyi Yang"]}, "1696": {"id": "2206.02690v3", "title": "A Survey on Sentence Embedding Models Performance for Patent Analysis", "url": "http://arxiv.org/pdf/2206.02690v3", "date": "2022-08-05 14:38:44", "abs": "Patent data is an important source of knowledge for innovation research,\nwhile the technological similarity between pairs of patents is a key enabling\nindicator for patent analysis. Recently researchers have been using patent\nvector space models based on different NLP embeddings models to calculate the\ntechnological similarity between pairs of patents to help better understand\ninnovations, patent landscaping, technology mapping, and patent quality\nevaluation. More often than not, Text Embedding is a vital precursor to patent\nanalysis tasks. A pertinent question then arises: How should we measure and\nevaluate the accuracy of these embeddings? To the best of our knowledge, there\nis no comprehensive survey that builds a clear delineation of embedding models'\nperformance for calculating patent similarity indicators. Therefore, in this\nstudy, we provide an overview of the accuracy of these algorithms based on\npatent classification performance and propose a standard library and dataset\nfor assessing the accuracy of embeddings models based on PatentSBERTa approach.\nIn a detailed discussion, we report the performance of the top 3 algorithms at\nsection, class, and subclass levels. The results based on the first claim of\npatents show that PatentSBERTa, Bert-for-patents, and TF-IDF Weighted Word\nEmbeddings have the best accuracy for computing sentence embeddings at the\nsubclass level. According to the first results, the performance of the models\nin different classes varies, which shows researchers in patent analysis can\nutilize the results of this study to choose the best proper model based on the\nspecific section of patent data they used.", "cat": "cs.CL", "authors": ["Hamid Bekamiri", "Daniel S. Hain", "Roman Jurowetzki"]}, "1697": {"id": "1902.10313v1", "title": "Efficient and Secure ECDSA Algorithm and its Applications: A Survey", "url": "http://arxiv.org/pdf/1902.10313v1", "date": "2019-02-27 02:48:46", "abs": "Public-key cryptography algorithms, especially elliptic curve cryptography\n(ECC) and elliptic curve digital signature algorithm (ECDSA) have been\nattracting attention from many researchers in different institutions because\nthese algorithms provide security and high performance when being used in many\nareas such as electronic-healthcare, electronic-banking, electronic-commerce,\nelectronic-vehicular, and electronic-governance. These algorithms heighten\nsecurity against various attacks and at the same time improve performance to\nobtain efficiencies (time, memory, reduced computation complexity, and energy\nsaving) in an environment of the constrained source and large systems. This\npaper presents detailed and a comprehensive survey of an update of the ECDSA\nalgorithm in terms of performance, security, and applications.", "cat": "cs.CR", "authors": ["Mishall Al-Zubaidie", "Zhongwei Zhang", "Ji Zhang"]}, "1698": {"id": "1611.05043v1", "title": "Emission-line stars in M31 from the SPLASH and PHAT surveys", "url": "http://arxiv.org/pdf/1611.05043v1", "date": "2016-11-15 21:00:02", "abs": "We present a sample of 224 stars that emit H$\\alpha$ (H$\\alpha$ stars) in the\nAndromeda galaxy (M31). The stars were selected from $\\sim$ 5000 spectra,\ncollected as part of the Spectroscopic and Photometric Landscape of Andromeda's\nStellar Halo survey using Keck II/DEIMOS. We used six-filter Hubble Space\nTelescope photometry from the Panchromatic Hubble Andromeda Treasury survey to\nclassify and investigate the properties of the H$\\alpha$ stars. We identified\nfive distinct categories of H$\\alpha$ star: B-type main sequence (MS) stars,\n`transitioning'-MS (T-MS) stars, red core He burning (RHeB) stars, non-C-rich\nasymptotic giant branch (AGB) stars, and C-rich AGB stars. We found $\\sim$ 12\nper cent of B-type stars exhibit H$\\alpha$ emission (Be stars). The frequency\nof Be to all B stars is known to vary with the metallicity of their\nenvironment. Comparing this proportion of Be stars with other environments\naround the Local Group, the result could indicate that M31 is more metal rich\nthan the Milky Way. We predict that the 17 T-MS H$\\alpha$ stars are Be stars\nevolving off the MS with fading H$\\alpha$ emission. We separated RHeB from AGB\nH$\\alpha$ stars. We conclude that the 61 RHeB and AGB stars are likely to be\nLong Period Variables. We found that $\\sim$ 14 per cent of C-rich AGB stars (C\nstars) emit H$\\alpha$, which is an upper limit for the ratio of C-rich Miras to\nC stars. This catalogue of H$\\alpha$ stars will be useful to constrain stellar\nevolutionary models, calibrate distance indicators for intermediate age\npopulations, and investigate the properties of M31.", "cat": "astro-ph.SR", "authors": ["Laura J. Prichard", "Puragra Guhathakurta", "Katherine M. Hamren", "Julianne J. Dalcanton", "Claire E. Dorman", "Anil C. Seth", "Benjamin F. Williams", "Gabriel A. Damon", "Anita Ilango", "Megha Ilango"]}, "1699": {"id": "1602.07314v2", "title": "The Herschel Orion Protostar Survey: Spectral Energy Distributions and Fits Using a Grid of Protostellar Models", "url": "http://arxiv.org/pdf/1602.07314v2", "date": "2016-03-30 16:32:07", "abs": "We present key results from the Herschel Orion Protostar Survey (HOPS):\nspectral energy distributions (SEDs) and model fits of 330 young stellar\nobjects, predominantly protostars, in the Orion molecular clouds. This is the\nlargest sample of protostars studied in a single, nearby star-formation\ncomplex. With near-infrared photometry from 2MASS, mid- and far-infrared data\nfrom Spitzer and Herschel, and sub-millimeter photometry from APEX, our SEDs\ncover 1.2-870 $\\mu$m and sample the peak of the protostellar envelope emission\nat ~100 $\\mu$m. Using mid-IR spectral indices and bolometric temperatures, we\nclassify our sample into 92 Class 0 protostars, 125 Class I protostars, 102\nflat-spectrum sources, and 11 Class II pre-main-sequence stars. We implement a\nsimple protostellar model (including a disk in an infalling envelope with\noutflow cavities) to generate a grid of 30400 model SEDs and use it to\ndetermine the best-fit model parameters for each protostar. We argue that\nfar-IR data are essential for accurate constraints on protostellar envelope\nproperties. We find that most protostars, and in particular the flat-spectrum\nsources, are well-fit. The median envelope density and median inclination angle\ndecrease from Class 0 to Class I to flat-spectrum protostars, despite the broad\nrange in best-fit parameters in each of the three categories. We also discuss\ndegeneracies in our model parameters. Our results confirm that the different\nprotostellar classes generally correspond to an evolutionary sequence with a\ndecreasing envelope infall rate, but the inclination angle also plays a role in\nthe appearance, and thus interpretation, of the SEDs.", "cat": "astro-ph.SR", "authors": ["E. Furlan", "W. J. Fischer", "B. Ali", "A. M. Stutz", "T. Stanke", "J. J. Tobin", "S. T. Megeath", "M. Osorio", "L. Hartmann", "N. Calvet", "C. A. Poteet", "J. Booker", "P. Manoj", "D. M. Watson", "L. Allen"]}, "1700": {"id": "2007.12314v1", "title": "The VANDELS survey: Discovery of massive overdensities of galaxies at z>2", "url": "http://arxiv.org/pdf/2007.12314v1", "date": "2020-07-24 01:22:12", "abs": "We want to investigate whether we can use Lyalpha emission to obtain\ninformation on the environment properties and whether Lyalpha emitters show\ndifferent characteristics as a function of their environment. We estimated\nlocal densities in the VANDELS Chandra Deep Field-South (CDFS) and UKIDSS Ultra\nDeep Survey (UDS) fields, by using a three-dimensional algorithm which works in\nthe RA-dec-redshift space. We selected a sample of 131 Lyalpha-emitting\ngalaxies (EW(Lyalpha)>0 A), unbiased with respect to environmental density, to\nstudy their location with respect to the over- or under-dense environment. We\nidentify 13 (proto)cluster candidates in the CDFS and nine in the UDS at 250$ per cent, although a uniformly high spot coverage does not match the CMD\nwell across the full luminosity range considered.", "cat": "astro-ph.SR", "authors": ["A. S. Binks", "R. D. Jeffries", "R. J. Jackson", "E. Franciosini", "G. G. Sacco", "A. Bayo", "L. Magrini", "S. Randich", "J. Arancibia", "M. Bergemann", "A. Bragaglia", "G. Gilmore", "A. Gonneau", "A. Hourihane", "P. Jofr\u00e9", "A. J. Korn", "L. Morbidelli", "L. Prisinzano", "C. C. Worley", "S. Zaggia"]}, "1719": {"id": "1204.6055v2", "title": "The Chandra X-ray Survey of Planetary Nebulae (ChanPlaNS): Probing Binarity, Magnetic Fields, and Wind Collisions", "url": "http://arxiv.org/pdf/1204.6055v2", "date": "2012-06-01 00:39:17", "abs": "We present an overview of the initial results from the Chandra Planetary\nNebula Survey (ChanPlaNS), the first systematic (volume-limited) Chandra X-ray\nObservatory survey of planetary nebulae (PNe) in the solar neighborhood. The\nfirst phase of ChanPlaNS targeted 21 mostly high-excitation PNe within ~1.5 kpc\nof Earth, yielding 4 detections of diffuse X-ray emission and 9 detections of\nX-ray-luminous point sources at the central stars (CSPNe) of these objects.\nCombining these results with those obtained from Chandra archival data for all\n(14) other PNe within ~1.5 kpc that have been observed to date, we find an\noverall X-ray detection rate of ~70%. Roughly 50% of the PNe observed by\nChandra harbor X-ray-luminous CSPNe, while soft, diffuse X-ray emission tracing\nshocks formed by energetic wind collisions is detected in ~30%; five objects\ndisplay both diffuse and point-like emission components. The presence of X-ray\nsources appears correlated with PN density structure, in that molecule-poor,\nelliptical nebulae are more likely to display X-ray emission (either point-like\nor diffuse) than molecule-rich, bipolar or Ring-like nebulae. All but one of\nthe X-ray point sources detected at CSPNe display X-ray spectra that are harder\nthan expected from hot (~100 kK) central star photospheres, possibly indicating\na high frequency of binary companions to CSPNe. Other potential explanations\ninclude self-shocking winds or PN mass fallback. Most PNe detected as diffuse\nX-ray sources are elliptical nebulae that display a nested shell/halo structure\nand bright ansae; the diffuse X-ray emission regions are confined within inner,\nsharp-rimmed shells. All sample PNe that display diffuse X-ray emission have\ninner shell dynamical ages <~5x10^3 yr, placing firm constraints on the\ntimescale for strong shocks due to wind interactions in PNe.", "cat": "astro-ph.SR", "authors": ["J. H. Kastner", "R. Montez Jr", "B. Balick", "D. J. Frew", "B. Miszalski", "R. Sahai", "E. Blackman", "Y. -H. Chu", "O. De Marco", "A. Frank", "M. A. Guerrero", "J. A. Lopez", "V. Rapson", "A. Zijlstra", "E. Behar", "V. Bujarrabal", "R. L. M. Corradi", "J. Nordhaus", "Q. Parker", "C. Sandin", "D. Sch\u00f6nberner", "N. Soker", "J. L. Sokoloski", "M. Steffen", "T. Ueta", "E. Villaver"]}, "1720": {"id": "1902.07285v6", "title": "Towards a Robust Deep Neural Network in Texts: A Survey", "url": "http://arxiv.org/pdf/1902.07285v6", "date": "2021-04-21 10:14:36", "abs": "Deep neural networks (DNNs) have achieved remarkable success in various tasks\n(e.g., image classification, speech recognition, and natural language\nprocessing (NLP)). However, researchers have demonstrated that DNN-based models\nare vulnerable to adversarial examples, which cause erroneous predictions by\nadding imperceptible perturbations into legitimate inputs. Recently, studies\nhave revealed adversarial examples in the text domain, which could effectively\nevade various DNN-based text analyzers and further bring the threats of the\nproliferation of disinformation. In this paper, we give a comprehensive survey\non the existing studies of adversarial techniques for generating adversarial\ntexts written by both English and Chinese characters and the corresponding\ndefense methods. More importantly, we hope that our work could inspire future\nstudies to develop more robust DNN-based text analyzers against known and\nunknown adversarial techniques.\n We classify the existing adversarial techniques for crafting adversarial\ntexts based on the perturbation units, helping to better understand the\ngeneration of adversarial texts and build robust models for defense. In\npresenting the taxonomy of adversarial attacks and defenses in the text domain,\nwe introduce the adversarial techniques from the perspective of different NLP\ntasks. Finally, we discuss the existing challenges of adversarial attacks and\ndefenses in texts and present the future research directions in this emerging\nand challenging field.", "cat": "cs.CL", "authors": ["Wenqi Wang", "Run Wang", "Lina Wang", "Zhibo Wang", "Aoshuang Ye"]}, "1721": {"id": "2210.04675v2", "title": "A Survey of Methods for Addressing Class Imbalance in Deep-Learning Based Natural Language Processing", "url": "http://arxiv.org/pdf/2210.04675v2", "date": "2023-02-22 10:39:43", "abs": "Many natural language processing (NLP) tasks are naturally imbalanced, as\nsome target categories occur much more frequently than others in the real\nworld. In such scenarios, current NLP models still tend to perform poorly on\nless frequent classes. Addressing class imbalance in NLP is an active research\ntopic, yet, finding a good approach for a particular task and imbalance\nscenario is difficult.\n With this survey, the first overview on class imbalance in deep-learning\nbased NLP, we provide guidance for NLP researchers and practitioners dealing\nwith imbalanced data. We first discuss various types of controlled and\nreal-world class imbalance. Our survey then covers approaches that have been\nexplicitly proposed for class-imbalanced NLP tasks or, originating in the\ncomputer vision community, have been evaluated on them. We organize the methods\nby whether they are based on sampling, data augmentation, choice of loss\nfunction, staged learning, or model design. Finally, we discuss open problems\nsuch as dealing with multi-label scenarios, and propose systematic benchmarking\nand reporting in order to move forward on this problem as a community.", "cat": "cs.CL", "authors": ["Sophie Henning", "William Beluch", "Alexander Fraser", "Annemarie Friedrich"]}, "1722": {"id": "1310.0083v1", "title": "HST hot Jupiter Transmission Spectral Survey: A detection of Na and strong optical absorption in HAT-P-1b", "url": "http://arxiv.org/pdf/1310.0083v1", "date": "2013-09-30 22:34:07", "abs": "We present an optical to near-infrared transmission spectrum of the hot\nJupiter HAT-P-1b, based on HST observations, covering the spectral regime from\n0.29 to 1.027{\\mu}m with STIS, which is coupled with a recent WFC3 transit\n(1.087 to 1.687{\\mu}m). We derive refined physical parameters of the HAT-P-1\nsystem, including an improved orbital ephemeris. The transmission spectrum\nshows a strong absorption signature shortward of 0.55{\\mu}m, with a strong\nblueward slope into the near-ultraviolet. We detect atmospheric sodium\nabsorption at a 3.3{\\sigma} significance level, but find no evidence for the\npotassium feature. The red data implies a marginally flat spectrum with a\ntentative absorption enhancement at wavelength longer than ~0.85{\\mu}m. The\nSTIS and WFC3 spectra differ significantly in absolute radius level (4.3 +/-\n1.6 pressure scale heights), implying strong optical absorption in the\natmosphere of HAT-P-1b. The optical to near-infrared difference cannot be\nexplained by stellar activity, as simulta- neous stellar activity monitoring of\nthe G0V HAT-P-1b host star and its identical companion show no significant\nactivity that could explain the result. We compare the complete STIS and WFC3\ntransmission spectrum with theoretical atmospheric mod- els which include haze,\nsodium and an extra optical absorber. We find that both an optical absorber and\na super-solar sodium to water abundance ratio might be a sce- nario explaining\nthe HAT-P-1b observations. Our results suggest that strong optical absorbers\nmay be a dominant atmospheric feature in some hot Jupiter exoplanets.", "cat": "astro-ph.SR", "authors": ["N. Nikolov", "D. K. Sing", "F. Pont", "A. S. Burrows", "J. J. Fortney", "G. E. Ballester", "T. M. Evans", "C. M. Huitson", "H. R. Wakeford", "P. A. Wilson", "S. Aigrain", "D. Deming", "N. P. Gibson", "G. W. Henry", "H. Knutson", "A. Lecavelier des Etangs", "A. P. Showman", "A. Vidal-Madjar", "K. Zahnle"]}, "1723": {"id": "2406.01197v2", "title": "A Survey of Generative Information Retrieval", "url": "http://arxiv.org/pdf/2406.01197v2", "date": "2024-06-04 04:12:39", "abs": "Generative Retrieval (GR) is an emerging paradigm in information retrieval\nthat leverages generative models to directly map queries to relevant document\nidentifiers (DocIDs) without the need for traditional query processing or\ndocument reranking. This survey provides a comprehensive overview of GR,\nhighlighting key developments, indexing and retrieval strategies, and\nchallenges. We discuss various document identifier strategies, including\nnumerical and string-based identifiers, and explore different document\nrepresentation methods. Our primary contribution lies in outlining future\nresearch directions that could profoundly impact the field: improving the\nquality of query generation, exploring learnable document identifiers,\nenhancing scalability, and integrating GR with multi-task learning frameworks.\nBy examining state-of-the-art GR techniques and their applications, this survey\naims to provide a foundational understanding of GR and inspire further\ninnovations in this transformative approach to information retrieval. We also\nmake the complementary materials such as paper collection publicly available at\nhttps://github.com/MiuLab/GenIR-Survey/", "cat": "cs.IR", "authors": ["Tzu-Lin Kuo", "Tzu-Wei Chiu", "Tzung-Sheng Lin", "Sheng-Yang Wu", "Chao-Wei Huang", "Yun-Nung Chen"]}, "1724": {"id": "2407.17505v2", "title": "Survey on biomarkers in human vocalizations", "url": "http://arxiv.org/pdf/2407.17505v2", "date": "2024-08-08 20:22:10", "abs": "Recent years has witnessed an increase in technologies that use speech for\nthe sensing of the health of the talker. This survey paper proposes a general\ntaxonomy of the technologies and a broad overview of current progress and\nchallenges. Vocal biomarkers are often secondary measures that are\napproximating a signal of another sensor or identifying an underlying mental,\ncognitive, or physiological state. Their measurement involve disturbances and\nuncertainties that may be considered as noise sources and the biomarkers are\ncoarsely qualified in terms of the various sources of noise involved in their\ndetermination. While in some proposed biomarkers the error levels seem high,\nthere are vocal biomarkers where the errors are expected to be low and thus are\nmore likely to qualify as candidates for adoption in healthcare applications.", "cat": "q-bio.NC", "authors": ["Aki H\u00e4rm\u00e4", "Bert den Brinker", "Ulf Grossekathofer", "Okke Ouweltjes", "Srikanth Nallanthighal", "Sidharth Abrol", "Vibhu Sharma"]}, "1725": {"id": "2208.04960v1", "title": "Hundreds of Low-Mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey", "url": "http://arxiv.org/pdf/2208.04960v1", "date": "2022-08-09 18:00:01", "abs": "We present an entirely new sample of 388 low-mass galaxies ($M_\\star \\leq\n10^{10} M_\\odot$) that have spectroscopic signatures indicating the presence of\nmassive black holes (BHs) in the form of active galactic nuclei (AGNs) or tidal\ndisruption events (TDEs). Of these, 70 have stellar masses in the dwarf galaxy\nregime with $10^8 \\lesssim M_\\star/M_\\odot \\lesssim 10^{9.5}$. We identify the\nactive galaxies by analyzing optical spectra of a parent sample of $\\sim$23,000\nlow-mass emission-line galaxies in the Galaxy and Mass Assembly (GAMA) Survey\nData Release 4, and employing four different diagnostics based on narrow\nemission line ratios and the detection of high-ionization coronal lines. We\nfind that 47 of the 388 low-mass active galaxies exhibit broad H$\\alpha$ in\ntheir spectra, corresponding to virial BH masses in the range $M_{\\rm BH} \\sim\n10^{5.0-7.7} M_\\odot$ with a median BH mass of $\\langle M_{\\rm BH}\\rangle \\sim\n10^{6.2} M_\\odot$. Our sample extends to higher redshifts ($z \\le 0.3; \\langle\nz \\rangle=0.13$) than previous samples of AGNs in low-mass/dwarf galaxies based\non Sloan Digital Sky Survey spectroscopy, which can be attributed to the\nspectroscopic limit of GAMA being $\\sim 2$ magnitudes deeper. Moreover, our\nmulti-diagnostic approach has revealed low-mass active galaxies spanning a wide\nrange of properties, from blue star-forming dwarfs to luminous \"miniquasars\"\npowered by low-mass BHs. As such, this work has implications for BH seeding and\nAGN feedback at low masses.", "cat": "astro-ph.GA", "authors": ["S. Salehirad", "A. E. Reines", "M. Molina"]}, "1726": {"id": "2304.00485v2", "title": "Graph Mining for Cybersecurity: A Survey", "url": "http://arxiv.org/pdf/2304.00485v2", "date": "2023-10-16 09:42:16", "abs": "The explosive growth of cyber attacks nowadays, such as malware, spam, and\nintrusions, caused severe consequences on society. Securing cyberspace has\nbecome an utmost concern for organizations and governments. Traditional Machine\nLearning (ML) based methods are extensively used in detecting cyber threats,\nbut they hardly model the correlations between real-world cyber entities. In\nrecent years, with the proliferation of graph mining techniques, many\nresearchers investigated these techniques for capturing correlations between\ncyber entities and achieving high performance. It is imperative to summarize\nexisting graph-based cybersecurity solutions to provide a guide for future\nstudies. Therefore, as a key contribution of this paper, we provide a\ncomprehensive review of graph mining for cybersecurity, including an overview\nof cybersecurity tasks, the typical graph mining techniques, and the general\nprocess of applying them to cybersecurity, as well as various solutions for\ndifferent cybersecurity tasks. For each task, we probe into relevant methods\nand highlight the graph types, graph approaches, and task levels in their\nmodeling. Furthermore, we collect open datasets and toolkits for graph-based\ncybersecurity. Finally, we outlook the potential directions of this field for\nfuture research.", "cat": "cs.CR", "authors": ["Bo Yan", "Cheng Yang", "Chuan Shi", "Yong Fang", "Qi Li", "Yanfang Ye", "Junping Du"]}, "1727": {"id": "2008.12199v3", "title": "Privacy Intelligence: A Survey on Image Privacy in Online Social Networks", "url": "http://arxiv.org/pdf/2008.12199v3", "date": "2023-02-07 06:34:49", "abs": "Image sharing on online social networks (OSNs) has become an indispensable\npart of daily social activities, but it has also led to an increased risk of\nprivacy invasion. The recent image leaks from popular OSN services and the\nabuse of personal photos using advanced algorithms (e.g. DeepFake) have\nprompted the public to rethink individual privacy needs in OSN image sharing.\nHowever, OSN image privacy itself is quite complicated, and solutions currently\nin place for privacy management in reality are insufficient to provide\npersonalized, accurate and flexible privacy protection. A more intelligent\nenvironment for privacy-friendly OSN image sharing is in demand. To fill the\ngap, we contribute a survey of \"privacy intelligence\" that targets modern\nprivacy issues in dynamic OSN image sharing from a user-centric perspective.\nSpecifically, we present a definition and a taxonomy of OSN image privacy, and\na high-level privacy analysis framework based on the lifecycle of OSN image\nsharing. The framework consists of three stages with different principles of\nprivacy by design. At each stage, we identify typical user behaviors in OSN\nimage sharing and the privacy issues associated with these behaviors. Then a\nsystematic review on the representative intelligent solutions targeting those\nprivacy issues is conducted, also in a stage-based manner. The resulting\nanalysis describes an intelligent privacy firewall for closed-loop privacy\nmanagement. We also discuss the challenges and future directions in this area.", "cat": "cs.CR", "authors": ["Chi Liu", "Tianqing Zhu", "Jun Zhang", "Wanlei Zhou"]}, "1728": {"id": "2003.11423v1", "title": "Design-unbiased statistical learning in survey sampling", "url": "http://arxiv.org/pdf/2003.11423v1", "date": "2020-03-25 14:27:39", "abs": "Design-consistent model-assisted estimation has become the standard practice\nin survey sampling. However, a general theory is lacking so far, which allows\none to incorporate modern machine-learning techniques that can lead to\npotentially much more powerful assisting models. We propose a subsampling\nRao-Blackwell method, and develop a statistical learning theory for exactly\ndesign-unbiased estimation with the help of linear or non-linear prediction\nmodels. Our approach makes use of classic ideas from Statistical Science as\nwell as the rapidly growing field of Machine Learning. Provided rich auxiliary\ninformation, it can yield considerable efficiency gains over standard linear\nmodel-assisted methods, while ensuring valid estimation for the given target\npopulation, which is robust against potential mis-specifications of the\nassisting model at the individual level.", "cat": "stat.ML", "authors": ["Luis Sanguiao Sande", "Li-Chun Zhang"]}, "1729": {"id": "1807.00048v3", "title": "Formal Specification and Verification of Autonomous Robotic Systems: A Survey", "url": "http://arxiv.org/pdf/1807.00048v3", "date": "2019-05-01 12:45:09", "abs": "Autonomous robotic systems are complex, hybrid, and often safety-critical;\nthis makes their formal specification and verification uniquely challenging.\nThough commonly used, testing and simulation alone are insufficient to ensure\nthe correctness of, or provide sufficient evidence for the certification of,\nautonomous robotics. Formal methods for autonomous robotics has received some\nattention in the literature, but no resource provides a current overview. This\npaper systematically surveys the state-of-the-art in formal specification and\nverification for autonomous robotics. Specially, it identifies and categorises\nthe challenges posed by, the formalisms aimed at, and the formal approaches for\nthe specification and verification of autonomous robotics.", "cat": "cs.FL", "authors": ["Matt Luckcuck", "Marie Farrell", "Louise Dennis", "Clare Dixon", "Michael Fisher"]}, "1730": {"id": "1506.01641v1", "title": "Numerical survey of the tunable condensate shape and scaling laws in pair-factorized steady states", "url": "http://arxiv.org/pdf/1506.01641v1", "date": "2015-06-04 16:30:41", "abs": "We numerically survey predictions on the shapes and scaling laws of particle\ncondensates that emerge as a result of spontaneous symmetry breaking in pair-\nfactorized steady states of a stochastic transport process. The specific model\nconsists of indistinguishable particles that stochastically hop between sites\ncontrolled by a tunable potential. We identify the different condensate shapes\nwithin their respective parameter regimes as well as determine precisely the\ncondensate width scaling.", "cat": "cond-mat.stat-mech", "authors": ["Eugen Ehrenpreis", "Hannes Nagel", "Wolfhard Janke"]}, "1731": {"id": "2010.00481v1", "title": "The Faint End of the Quasar Luminosity Function at $z \\sim 5$ from the Subaru Hyper Suprime-Cam Survey", "url": "http://arxiv.org/pdf/2010.00481v1", "date": "2020-10-01 15:18:56", "abs": "We present the quasar luminosity function at $z \\sim 5$ derived from the\noptical wide-field survey data obtained as a part of the Subaru strategic\nprogram (SSP) with Hyper Suprime-Cam (HSC). From $\\sim$81.8 deg$^2$ area in the\nWide layer of the HSC-SSP survey, we selected 224 candidates of low-luminosity\nquasars at $z \\sim 5$ by adopting the Lyman-break method down to $i = 24.1$\nmag. Based on our candidates and spectroscopically-confirmed quasars from the\nSloan Digital Sky Survey (SDSS), we derived the quasar luminosity function at\n$z \\sim 5$ covering a wide luminosity range of $-28.76 < M_{\\rm 1450} < -22.32$\nmag. We found that the quasar luminosity function is fitted by a double\npower-law model with a break magnitude of $M^{*}_{1450} =\n-25.05^{+0.10}_{-0.24}$ mag. The inferred number density of low-luminosity\nquasars is lower, and the derived faint-end slope, $-1.22^{+0.03}_{-0.10}$, is\nflatter than those of previous studies at $z \\sim 5$. A compilation of the\nquasar luminosity function at $4 \\leq z \\leq 6$ from the HSC-SSP suggests that\nthere is little redshift evolution in the break magnitude and in the faint-end\nslope within this redshift range, although previous studies suggest that the\nfaint-end slope becomes steeper at higher redshifts. The number density of\nlow-luminosity quasars decreases more rapidly from $z \\sim 5$ to $z \\sim 6$\nthan from $z \\sim 4$ to $z \\sim 5$.", "cat": "astro-ph.GA", "authors": ["Mana Niida", "Tohru Nagao", "Hiroyuki Ikeda", "Masayuki Akiyama", "Yoshiki Matsuoka", "Wanqiu He", "Kenta Matsuoka", "Yoshiki Toba", "Masafusa Onoue", "Masakazu A. R. Kobayashi", "Yoshiaki Taniguchi", "Hisanori Furusawa", "Yuichi Harikane", "Masatoshi Imanishi", "Nobunari Kashikawa", "Toshihiro Kawaguchi", "Yutaka Komiyama", "Hikari Shirakata", "Yuichi Terashima", "Yoshihiro Ueda"]}, "1732": {"id": "1204.2830v3", "title": "Tomographic Magnification of Lyman Break Galaxies in The Deep Lens Survey", "url": "http://arxiv.org/pdf/1204.2830v3", "date": "2012-09-13 21:26:36", "abs": "Using about 450,000 galaxies in the Deep Lens Survey, we present a detection\nof the gravitational magnification of z > 4 Lyman Break Galaxies by massive\nforeground galaxies with 0.4 < z < 1.0, grouped by redshift. The magnification\nsignal is detected at S/N greater than 20, and rigorous checks confirm that it\nis not contaminated by any galaxy sample overlap in redshift. The inferred\ngalaxy mass profiles are consistent with earlier lensing analyses at lower\nredshift. We then explore the tomographic lens magnification signal by\nsplitting our foreground galaxy sample into 7 redshift bins. Combining\ngalaxy-magnification cross-correlations and galaxy angular auto-correlations,\nwe develop a bias-independent estimator of the tomographic signal. As a\ndiagnostic of magnification tomography, the measurement of this estimator\nrejects a flat dark matter dominated Universe at > 7.5{\\sigma} with a fixed\n\\sigma_8 and is found to be consistent with the expected redshift-dependence of\nthe WMAP7 {\\Lambda}CDM cosmology.", "cat": "astro-ph.CO", "authors": ["Christopher B. Morrison", "Ryan Scranton", "Brice M\u00e9nard", "Samuel J. Schmidt", "J. Anthony Tyson", "Russell Ryan", "Ami Choi", "David Wittman"]}, "1733": {"id": "1206.5708v1", "title": "Molecular Outflows Identified in the FCRAO CO Survey of the Taurus Molecular Cloud", "url": "http://arxiv.org/pdf/1206.5708v1", "date": "2012-06-25 15:26:47", "abs": "The 100 square degree FCRAO CO survey of the Taurus molecular cloud provides\nan excellent opportunity to undertake an unbiased survey of a large, nearby,\nmolecular cloud complex for molecular outflow activity. Our study provides\ninformation on the extent, energetics and frequency of outflows in this region,\nwhich are then used to assess the impact of outflows on the parent molecular\ncloud. The search identified 20 outflows in the Taurus region, 8 of which were\npreviously unknown. Both $^{12}$CO and $^{13}$CO data cubes from the Taurus\nmolecular map were used, and dynamical properties of the outflows are derived.\nEven for previously known outflows, our large-scale maps indicate that many of\nthe outflows are much larger than previously suspected, with eight of the flows\n(40%) being more than a parsec long. The mass, momentum and kinetic energy from\nthe 20 outflows are compared to the repository of turbulent energy in Taurus.\nComparing the energy deposition rate from outflows to the dissipation rate of\nturbulence, we conclude that outflows by themselves cannot sustain the observed\nturbulence seen in the entire cloud. However, when the impact of outflows is\nstudied in selected regions of Taurus, it is seen that locally, outflows can\nprovide a significant source of turbulence and feedback. Five of the eight\nnewly discovered outflows have no known associated stellar source, indicating\nthat they may be embedded Class 0 sources. In Taurus, 30% of Class I sources\nand 12% of Flat spectrum sources from the Spitzer YSO catalogue have outflows,\nwhile 75% of known Class 0 objects have outflows. Overall, the paucity of\noutflows in Taurus compared to the embedded population of Class I and Flat\nSpectrum YSOs indicate that molecular outflows are a short-lived stage marking\nthe youngest phase of protostellar life.", "cat": "astro-ph.SR", "authors": ["Gopal Narayanan", "Ronald Snell", "Ashley Bemis"]}, "1734": {"id": "2312.13355v1", "title": "The universal variability of the stellar initial mass function probed by the TIMER survey", "url": "http://arxiv.org/pdf/2312.13355v1", "date": "2023-12-20 19:00:02", "abs": "The debate about the universality of the stellar initial mass function (IMF)\nrevolves around two competing lines of evidence. While measurements in the\nMilky Way, an archetypal spiral galaxy, seem to support an invariant IMF, the\nobserved properties of massive early-type galaxies (ETGs) favor an IMF somehow\nsensitive to the local star formation conditions. The fundamental\nmethodological and physical differences between both approaches have hampered,\nhowever, a comprehensive understanding of IMF variations. We describe here an\nimproved modelling scheme that allows for the first time consistent IMF\nmeasurements across stellar populations with different ages and complex star\nformation histories. Making use of the exquisite MUSE optical data from the\nTIMER survey and powered by the MILES stellar population models, we show the\nage, metallicity, [Mg/Fe], and IMF slope maps of the inner regions of NGC 3351,\na spiral galaxy with a mass similar to that of the Milky Way. The measured IMF\nvalues in NGC3351 follow the expectations from a Milky Way-like IMF, although\nthey simultaneously show systematic and spatially coherent variations,\nparticularly for low-mass stars. In addition, our stellar population analysis\nreveals the presence of metal-poor and Mg-enhanced star-forming regions that\nappear to be predominantly enriched by the stellar ejecta of core-collapse\nsupernovae. Our findings showcase therefore the potential of detailed studies\nof young stellar populations to better understand the early stages of galaxy\nevolution and, in particular, the origin of the observed IMF variations beyond\nand within the Milky Way.", "cat": "astro-ph.GA", "authors": ["Ignacio Mart\u00edn-Navarro", "Adriana de Lorenzo-C\u00e1ceres", "Dimitri A. Gadotti", "Jairo M\u00e9ndez-Abreu", "Jes\u00fas Falc\u00f3n-Barroso", "Patricia S\u00e1nchez-Bl\u00e1zquez", "Paula Coelho", "Justus Neumann", "Glenn van de Ven", "Isabel P\u00e9rez"]}, "1735": {"id": "2211.10412v3", "title": "Video Unsupervised Domain Adaptation with Deep Learning: A Comprehensive Survey", "url": "http://arxiv.org/pdf/2211.10412v3", "date": "2024-07-27 14:54:24", "abs": "Video analysis tasks such as action recognition have received increasing\nresearch interest with growing applications in fields such as smart healthcare,\nthanks to the introduction of large-scale datasets and deep learning-based\nrepresentations. However, video models trained on existing datasets suffer from\nsignificant performance degradation when deployed directly to real-world\napplications due to domain shifts between the training public video datasets\n(source video domains) and real-world videos (target video domains). Further,\nwith the high cost of video annotation, it is more practical to use unlabeled\nvideos for training. To tackle performance degradation and address concerns in\nhigh video annotation cost uniformly, the video unsupervised domain adaptation\n(VUDA) is introduced to adapt video models from the labeled source domain to\nthe unlabeled target domain by alleviating video domain shift, improving the\ngeneralizability and portability of video models. This paper surveys recent\nprogress in VUDA with deep learning. We begin with the motivation of VUDA,\nfollowed by its definition, and recent progress of methods for both closed-set\nVUDA and VUDA under different scenarios, and current benchmark datasets for\nVUDA research. Eventually, future directions are provided to promote further\nVUDA research. The repository of this survey is provided at\nhttps://github.com/xuyu0010/awesome-video-domain-adaptation.", "cat": "cs.CV", "authors": ["Yuecong Xu", "Haozhi Cao", "Zhenghua Chen", "Xiaoli Li", "Lihua Xie", "Jianfei Yang"]}, "1736": {"id": "2405.09431v1", "title": "A Survey On Text-to-3D Contents Generation In The Wild", "url": "http://arxiv.org/pdf/2405.09431v1", "date": "2024-05-15 15:23:22", "abs": "3D content creation plays a vital role in various applications, such as\ngaming, robotics simulation, and virtual reality. However, the process is\nlabor-intensive and time-consuming, requiring skilled designers to invest\nconsiderable effort in creating a single 3D asset. To address this challenge,\ntext-to-3D generation technologies have emerged as a promising solution for\nautomating 3D creation. Leveraging the success of large vision language models,\nthese techniques aim to generate 3D content based on textual descriptions.\nDespite recent advancements in this area, existing solutions still face\nsignificant limitations in terms of generation quality and efficiency. In this\nsurvey, we conduct an in-depth investigation of the latest text-to-3D creation\nmethods. We provide a comprehensive background on text-to-3D creation,\nincluding discussions on datasets employed in training and evaluation metrics\nused to assess the quality of generated 3D models. Then, we delve into the\nvarious 3D representations that serve as the foundation for the 3D generation\nprocess. Furthermore, we present a thorough comparison of the rapidly growing\nliterature on generative pipelines, categorizing them into feedforward\ngenerators, optimization-based generation, and view reconstruction approaches.\nBy examining the strengths and weaknesses of these methods, we aim to shed\nlight on their respective capabilities and limitations. Lastly, we point out\nseveral promising avenues for future research. With this survey, we hope to\ninspire researchers further to explore the potential of open-vocabulary\ntext-conditioned 3D content creation.", "cat": "cs.CV", "authors": ["Chenhan Jiang"]}, "1737": {"id": "1904.00651v2", "title": "Transit least-squares survey - I. Discovery and validation of an Earth-sized planet in the four-planet system K2-32 near the 1:2:5:7 resonance", "url": "http://arxiv.org/pdf/1904.00651v2", "date": "2019-05-22 13:11:21", "abs": "We apply, for the first time, the Transit Least Squares (TLS) algorithm to\nsearch for new transiting exoplanets. TLS is a successor to the Box Least\nSquares (BLS) algorithm, which has served as a standard tool for the detection\nof periodic transits. In this proof-of-concept paper, we demonstrate how TLS\nfinds small planets that have previously been missed. We showcase TLS'\ncapabilities using the K2 EVEREST-detrended light curve of the star K2-32\n(EPIC205071984) that was known to have three transiting planets. TLS detects\nthese known Neptune-sized planets K2-32b, d, and c in an iterative search and\nfinds an additional transit signal with a high signal detection efficiency\n(SDE_TLS) of 26.1 at a period of 4.34882 (-0.00075, +0.00069) d. We show that\nthis signal remains detectable (SDE_TLS = 13.2) with TLS in the K2SFF light\ncurve of K2-32, which includes a less optimal detrending of the systematic\ntrends. The signal is below common detection thresholds, however, if searched\nwith BLS in the K2SFF light curve (SDE_BLS = 8.9) as in previous searches.\nMarkov Chain Monte Carlo sampling shows that the radius of this candidate is\n1.01 (-0.09, +0.10) Earth radii. We analyze its phase-folded transit light\ncurve using the vespa software and calculate a false positive probability FPP =\n3.1e-3, formally validating K2-32e as a planet. Taking into account the\nmultiplicity boost of the system, FPP < 3.1e-4. K2-32 now hosts at least four\nplanets that are very close to a 1:2:5:7 mean motion resonance chain. The\noffset of the orbital periods of K2-32e and b from a 1:2 mean motion resonance\nis in very good agreement with the sample of transiting multi-planet systems\nfrom Kepler, lending further credence to the planetary nature of K2-32e. We\nexpect that TLS can find many more transits of Earth-sized and smaller planets\nin the Kepler data that have hitherto remained undetected with BLS and similar\nalgorithms.", "cat": "astro-ph.EP", "authors": ["Ren\u00e9 Heller", "Kai Rodenbeck", "Michael Hippke"]}, "1738": {"id": "1401.3052v3", "title": "Equivariant bordism of 2-torus manifolds and unitary toric manifolds--a survey", "url": "http://arxiv.org/pdf/1401.3052v3", "date": "2019-09-08 01:34:15", "abs": "In this paper we survey results and recent progresses on the equivariant\nbordism classification of 2-torus manifolds and unitary toric manifolds.", "cat": "math.AT", "authors": ["Zhi L\u00fc"]}, "1739": {"id": "2301.09780v1", "title": "JEMS: A deep medium-band imaging survey in the Hubble Ultra-Deep Field with JWST NIRCam & NIRISS", "url": "http://arxiv.org/pdf/2301.09780v1", "date": "2023-01-24 01:55:46", "abs": "We present JEMS (JWST Extragalactic Medium-band Survey), the first public\nmedium-band imaging survey carried out using JWST/NIRCam and NIRISS. These\nobservations use $\\sim2\\mu$m and $\\sim4\\mu$m medium-band filters (NIRCam F182M,\nF210M, F430M, F460M, F480M; and NIRISS F430M & F480M in parallel) over 15.6\nsquare arcminutes in the Hubble Ultra Deep Field (UDF), thereby building on the\ndeepest multi-wavelength public datasets available anywhere on the sky. We\ndescribe our science goals, survey design, NIRCam and NIRISS image reduction\nmethods, and describe our first data release of the science-ready mosaics. Our\nchosen filters create a JWST imaging survey in the UDF that enables novel\nanalysis of a range of spectral features potentially across the redshift range\nof $0.31$ magnitude)\nacross redshifts $1.5= 7 (corresponding to a\nconfidence level of 99.91%). The catalog consists of 1245 sources in total\nincluding 32 extended-source candidates. The averaged log N-log S relations are\nin good agreement with previous results, bridging the flux range between\nChandra deep surveys and brighter surveys. The log N-log S relations show\nsignificant spatial variation among pointings on a scale of 0.2 deg^2.\nAnalyzing the auto correlation function, we detect significant clustering\nsignals from the 0.5-2 keV band sample, which can be fit with a power law form\n(\\theta/\\theta_c)^{-0.8} with a correlation length of\n\\theta_c=5.9^{+1.0}_{-0.9} arcsec when the integral constraint term is\nincluded. In the 2-10 keV band, however, the clustering is not significant with\na 90% upper limit of \\theta_c < 1.5 arcsec.", "cat": "astro-ph", "authors": ["Yoshihiro Ueda", "Michael G. Watson", "Ian M. Stewart", "Masayuki Akiyama", "Axel D. Schwope", "Georg Lamer", "Jacobo Ebrero", "Francisco J. Carrera", "Kazuhiro Sekiguchi", "Tohru Yamada", "Chris Simpson", "Guenther Hasinger", "Silvia Mateos"]}, "1746": {"id": "1609.02481v2", "title": "MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters -- II. Cataclysmic variables -- progenitors and population at birth", "url": "http://arxiv.org/pdf/1609.02481v2", "date": "2016-12-02 19:54:46", "abs": "This is the second in a series of papers associated with cataclysmic\nvariables (CVs) and related objects, formed in a suite of simulations for\nglobular cluster evolution performed with the MOCCA Monte Carlo code. We study\nthe properties of our simulated CV populations throughout the entire cluster\nevolution. We find that dynamics extends the range of binary CV progenitor\nproperties, causing CV formation from binary progenitors that would otherwise\nnot become CVs. The CV formation rate in our simulations can be separated into\ntwo regimes: an initial burst ($\\lesssim$ 1 Gyr) connected with the formation\nof the most massive white dwarfs, followed by a nearly constant formation rate.\nThis result holds for all models regardless of the adopted initial conditions,\neven when most CVs form dynamically. Given the cluster age-dependence of CV\nproperties, we argue that direct comparisons to observed Galactic field CVs\ncould be misleading, since cluster CVs can be up to 4 times older than their\nfield counterparts. Our results also illustrate that, due mainly to unstable\nmass transfer, some CVs that form in our simulations are destroyed before the\npresent-day. Finally, some field CVs might have originated from globular\nclusters, as found in our simulations, although the fraction of such escapers\nshould be small relative to the entire Galactic field CV population.", "cat": "astro-ph.GA", "authors": ["Diogo Belloni", "Mirek Giersz", "Helio J. Rocha-Pinto", "Nathan Leigh", "Abbas Askar"]}, "1747": {"id": "1810.10052v1", "title": "A survey of models for $(\\infty, n)$-categories", "url": "http://arxiv.org/pdf/1810.10052v1", "date": "2018-10-23 19:02:51", "abs": "We give describe several models for $(\\infty,n)$-categories, with an emphasis\non models given by diagrams of sets and simplicial sets. We look most closely\nat the cases when $n \\leq 2$, then summarize methods of generalizing for all\n$n$.", "cat": "math.AT", "authors": ["Julia E. Bergner"]}, "1748": {"id": "0911.1365v2", "title": "A Keck/DEIMOS spectroscopic survey of the faint M31 satellites And IX, And XI, And XII, and And XIII", "url": "http://arxiv.org/pdf/0911.1365v2", "date": "2010-03-16 11:08:37", "abs": "We present the first spectroscopic analysis of the faint M31 satellite\ngalaxies, AndXI and AndXIII, and a reanalysis of existing spectroscopic data\nfor two further faint companions, And IX and AndXII. By combining data obtained\nusing the DEIMOS spectrograph mounted on the Keck II telescope with deep\nphotometry from the Suprime-Cam instrument on Subaru, we have calculated global\nproperties for the dwarfs, such as systemic velocities, metallicites and\nhalf-light radii.We find each dwarf to be very metal poor ([Fe/H] -2 both\nphotometrically and spectroscopically, from their stacked spectrum), and as\nsuch, they continue to follow the luminosity-metallicity relationship\nestablished with brighter dwarfs. We are unable to resolve a dispersion for And\nXI due to small sample size and low S/N, but we set a one sigma upper limit of\nsigma-v <5 km/s. For And IX, And XII and And XIII we resolve velocity\ndispersions of v=4.5 (+3.4,-3.2), 2.6(+5.1,-2.6) and 9.7(+8.9,-4.5) km/s, and\nderive masses within the half light radii of 6.2(+5.3,-5.1)x10^6 Msun, 2.4\n(+6.5,-2.4)x10^6 Msun and 1.1(+1.4,-0.7)x10^7 Msun respectively. We discuss\neach satellite in the context of the Mateo relations for dwarf spheroidal\ngalaxies, and the Universal halo profiles established for Milky Way dwarfs\n(Walker et al. 2009). For both galaxies, this sees them fall below the\nUniversal halo profiles of Walker et al. (2009). When combined with the\nfindings of McConnachie & Irwin (2006a), which reveal that the M31 satellites\nare twice as extended (in terms of both half-light and tidal radii) as their\nMilky Way counterparts, these results suggest that the satellite population of\nthe Andromeda system could inhabit halos that are significantly different from\nthose of the Milky Way in terms of their central densities (abridged).", "cat": "astro-ph.CO", "authors": ["M. L. M. Collins", "S. C. Chapman", "M. J. Irwin", "N. F. Martin", "R. A. Ibata", "D. B. Zucker", "A. Blain", "A. M. N. Ferguson", "G. F. Lewis", "A. W. McConnachie", "J. Penarrubia"]}, "1749": {"id": "1501.03989v1", "title": "Cosmology with a SKA HI intensity mapping survey", "url": "http://arxiv.org/pdf/1501.03989v1", "date": "2015-01-16 14:33:23", "abs": "HI intensity mapping (IM) is a novel technique capable of mapping the\nlarge-scale structure of the Universe in three dimensions and delivering\nexquisite constraints on cosmology, by using HI as a biased tracer of the dark\nmatter density field. This is achieved by measuring the intensity of the\nredshifted 21cm line over the sky in a range of redshifts without the\nrequirement to resolve individual galaxies. In this chapter, we investigate the\npotential of SKA1 to deliver HI intensity maps over a broad range of\nfrequencies and a substantial fraction of the sky. By pinning down the baryon\nacoustic oscillation and redshift space distortion features in the matter power\nspectrum -- thus determining the expansion and growth history of the Universe\n-- these surveys can provide powerful tests of dark energy models and\nmodifications to General Relativity. They can also be used to probe physics on\nextremely large scales, where precise measurements of spatial curvature and\nprimordial non-Gaussianity can be used to test inflation; on small scales, by\nmeasuring the sum of neutrino masses; and at high redshifts where non-standard\nevolution models can be probed. We discuss the impact of foregrounds as well as\nvarious instrumental and survey design parameters on the achievable\nconstraints. In particular we analyse the feasibility of using the SKA1\nautocorrelations to probe the large-scale signal.", "cat": "astro-ph.CO", "authors": ["Mario G. Santos", "Philip Bull", "David Alonso", "Stefano Camera", "Pedro G. Ferreira", "Gianni Bernardi", "Roy Maartens", "Matteo Viel", "Francisco Villaescusa-Navarro", "Filipe B. Abdalla", "Matt Jarvis", "R. Benton Metcalf", "A. Pourtsidou", "Laura Wolz"]}, "1750": {"id": "2002.07191v1", "title": "MNELLS: The MUSE Nearby Early-Type Galaxy Lens Locator Survey", "url": "http://arxiv.org/pdf/2002.07191v1", "date": "2020-02-17 19:00:02", "abs": "Low-redshift strong-lensing galaxies can provide robust measurements of the\nstellar mass-to-light ratios in early-type galaxies (ETG), and hence constrain\nvariations in the stellar initial mass function (IMF). At present, only a few\nsuch systems are known. Here, we report the first results from a blind search\nfor gravitationally-lensed emission line sources behind 52 massive $z$ $<$ 0.07\nETGs with MUSE integral field spectroscopy. For 16 galaxies, new observations\nwere acquired, whilst the other 36 were analysed from archival data. This\nproject has previously yielded one confirmed galaxy-scale strong lens\n(J0403-0239) which we report in an earlier paper. J0403-0239 has since received\nfollow-up observations, presented here, which indicate support for our earlier\nIMF results. Three cluster-scale, and hence dark-matter-dominated, lensing\nsystems were also discovered (central galaxies of A4059, A2052 and AS555). For\nnine further galaxies, we detect a singly-imaged but closely-projected source\nwithin 6 arcsec (including one candidate with sources at three different\nredshifts); such cases can be exploited to derive upper limits on the IMF\nmass-excess factor, $\\alpha$. Combining the new lens and new upper limits, with\nthe previously-discovered systems, we infer an average $\\langle \\alpha \\rangle$\n= 1.06 $\\pm$ 0.08 (marginalised over the intrinsic scatter), which is\ninconsistent with a Salpeter-like IMF ($\\alpha$ = 1.55) at the 6$\\sigma$ level.\nWe test the detection threshold in these short-exposure MUSE observations with\nthe injection and recovery of simulated sources, and predict that one in\ntwenty-five observations is expected to yield a new strong-lens system. Our\nobservational results are consistent with this expected yield.", "cat": "astro-ph.GA", "authors": ["William P. Collier", "Russell J. Smith", "John R. Lucey"]}, "1751": {"id": "1806.00750v1", "title": "Location Privacy in Cognitive Radio Networks: A Survey", "url": "http://arxiv.org/pdf/1806.00750v1", "date": "2018-06-03 08:19:38", "abs": "Cognitive radio networks (CRNs) have emerged as an essential technology to\nenable dynamic and opportunistic spectrum access which aims to exploit\nunderutilized licensed channels to solve the spectrum scarcity problem. Despite\nthe great benefits that CRNs offer in terms of their ability to improve\nspectrum utilization efficiency, they suffer from user location privacy issues.\nKnowing that their whereabouts may be exposed can discourage users from joining\nand participating in the CRNs, thereby potentially hindering the adoption and\ndeployment of this technology in future generation networks. The location\ninformation leakage issue in the CRN context has recently started to gain\nattention from the research community due to its importance, and several\nresearch efforts have been made to tackle it. However, to the best of our\nknowledge, none of these works have tried to identify the vulnerabilities that\nare behind this issue or discuss the approaches that could be deployed to\nprevent it. In this paper, we try to fill this gap by providing a comprehensive\nsurvey that investigates the various location privacy risks and threats that\nmay arise from the different components of this CRN technology, and explores\nthe different privacy attacks and countermeasure solutions that have been\nproposed in the literature to cope with this location privacy issue. We also\ndiscuss some open research problems, related to this issue, that need to be\novercome by the research community to take advantage of the benefits of this\nkey CRN technology without having to sacrifice the users' privacy.", "cat": "cs.NI", "authors": ["Mohamed Grissa", "Bechir Hamdaoui", "Attila A. Yavuz"]}, "1752": {"id": "2101.06426v2", "title": "A Survey on Extraction of Causal Relations from Natural Language Text", "url": "http://arxiv.org/pdf/2101.06426v2", "date": "2021-11-01 02:07:11", "abs": "As an essential component of human cognition, cause-effect relations appear\nfrequently in text, and curating cause-effect relations from text helps in\nbuilding causal networks for predictive tasks. Existing causality extraction\ntechniques include knowledge-based, statistical machine learning(ML)-based, and\ndeep learning-based approaches. Each method has its advantages and weaknesses.\nFor example, knowledge-based methods are understandable but require extensive\nmanual domain knowledge and have poor cross-domain applicability. Statistical\nmachine learning methods are more automated because of natural language\nprocessing (NLP) toolkits. However, feature engineering is labor-intensive, and\ntoolkits may lead to error propagation. In the past few years, deep learning\ntechniques attract substantial attention from NLP researchers because of its'\npowerful representation learning ability and the rapid increase in\ncomputational resources. Their limitations include high computational costs and\na lack of adequate annotated training data. In this paper, we conduct a\ncomprehensive survey of causality extraction. We initially introduce primary\nforms existing in the causality extraction: explicit intra-sentential\ncausality, implicit causality, and inter-sentential causality. Next, we list\nbenchmark datasets and modeling assessment methods for causal relation\nextraction. Then, we present a structured overview of the three techniques with\ntheir representative systems. Lastly, we highlight existing open challenges\nwith their potential directions.", "cat": "cs.IR", "authors": ["Jie Yang", "Soyeon Caren Han", "Josiah Poon"]}, "1753": {"id": "2308.03045v3", "title": "Machine learning methods for the search for L&T brown dwarfs in the data of modern sky surveys", "url": "http://arxiv.org/pdf/2308.03045v3", "date": "2023-08-18 07:10:29", "abs": "According to various estimates, brown dwarfs (BD) should account for up to 25\npercent of all objects in the Galaxy. However, few of them are discovered and\nwell-studied, both individually and as a population. Homogeneous and complete\nsamples of brown dwarfs are needed for these kinds of studies. Due to their\nweakness, spectral studies of brown dwarfs are rather laborious. For this\nreason, creating a significant reliable sample of brown dwarfs, confirmed by\nspectroscopic observations, seems unattainable at the moment. Numerous attempts\nhave been made to search for and create a set of brown dwarfs using their\ncolours as a decision rule applied to a vast amount of survey data. In this\nwork, we use machine learning methods such as Random Forest Classifier,\nXGBoost, SVM Classifier and TabNet on PanStarrs DR1, 2MASS and WISE data to\ndistinguish L and T brown dwarfs from objects of other spectral and luminosity\nclasses. The explanation of the models is discussed. We also compare our models\nwith classical decision rules, proving their efficiency and relevance.", "cat": "astro-ph.SR", "authors": ["Aleksandra Avdeeva"]}, "1754": {"id": "1911.02195v2", "title": "FPFS Shear Estimator: Systematic Tests on the Hyper Suprime-Cam Survey First Year Data", "url": "http://arxiv.org/pdf/1911.02195v2", "date": "2021-02-18 07:26:50", "abs": "We apply the Fourier Power Function Shapelets (FPFS) shear estimator to the\nfirst year data of the Hyper Suprime-Cam survey to construct a shape catalog.\nThe FPFS shear estimator has been demonstrated to have multiplicative bias less\nthan $1\\%$ in the absence of blending, regardless of complexities of galaxy\nshapes, smears of point spread functions (PSFs) and contamination from noise.\nThe blending bias is calibrated with realistic image simulations, which include\nthe impact of neighboring objects, using the COSMOS Hubble Space Telescope\nimages. Here we carefully test the influence of PSF model residual on the FPFS\nshear estimation and the uncertainties in the shear calibration. Internal null\ntests are conducted to characterize potential systematics in the FPFS shape\ncatalog and the results are compared with those measured using a catalog where\nthe shapes were estimated using the re-Gaussianization algorithms. Furthermore,\nwe compare various weak lensing measurements between the FPFS shape catalog and\nthe re-Gaussianization shape catalog and conclude that the weak lensing\nmeasurements between these two shape catalogs are consistent with each other\nwithin the statistical uncertainty.", "cat": "astro-ph.CO", "authors": ["Xiangchong Li", "Masamune Oguri", "Nobuhiko Katayama", "Wentao Luo", "Wenting Wang", "Jiaxin Han", "Hironao Miyatake", "Keigo Nakamura", "Surhud More"]}, "1755": {"id": "2105.15106v4", "title": "A Survey of Knowledge Tracing: Models, Variants, and Applications", "url": "http://arxiv.org/pdf/2105.15106v4", "date": "2024-04-11 02:57:17", "abs": "Modern online education has the capacity to provide intelligent educational\nservices by automatically analyzing substantial amounts of student behavioral\ndata. Knowledge Tracing (KT) is one of the fundamental tasks for student\nbehavioral data analysis, aiming to monitor students' evolving knowledge state\nduring their problem-solving process. In recent years, a substantial number of\nstudies have concentrated on this rapidly growing field, significantly\ncontributing to its advancements. In this survey, we will conduct a thorough\ninvestigation of these progressions. Firstly, we present three types of\nfundamental KT models with distinct technical routes. Subsequently, we review\nextensive variants of the fundamental KT models that consider more stringent\nlearning assumptions. Moreover, the development of KT cannot be separated from\nits applications, thereby we present typical KT applications in various\nscenarios. To facilitate the work of researchers and practitioners in this\nfield, we have developed two open-source algorithm libraries: EduData that\nenables the download and preprocessing of KT-related datasets, and EduKTM that\nprovides an extensible and unified implementation of existing mainstream KT\nmodels. Finally, we discuss potential directions for future research in this\nrapidly growing field. We hope that the current survey will assist both\nresearchers and practitioners in fostering the development of KT, thereby\nbenefiting a broader range of students.", "cat": "cs.CY", "authors": ["Shuanghong Shen", "Qi Liu", "Zhenya Huang", "Yonghe Zheng", "Minghao Yin", "Minjuan Wang", "Enhong Chen"]}, "1756": {"id": "2004.06380v1", "title": "A Survey of Energy Efficient Schemes in Ad-hoc Networks", "url": "http://arxiv.org/pdf/2004.06380v1", "date": "2020-04-14 09:32:36", "abs": "Ad hoc network is a collection of different types of nodes, which are\nconnected in heterogeneous or homogeneous manner. It is also known as\nself-organizing-wireless network. The dynamic nature of ad hoc networks make\nthem more attractive, which is used in many different applications. Every coin\nhas two sides: one is the advantage part and other is disadvantages, in the\nsame manner nature of ad hoc network make it more attractive from one side in\nother hand there are some issues too. Energy efficiency is a core factor which\neffects on ad hoc network in terms of battery life, throughput, overhead of\nmessages, transmission error. For solving issues of energy constraints,\ndifferent mechanisms are proposed by various researchers. In this paper, we\nsurvey various existing schemes which attempt to improve energy efficiency of\ndifferent types of ad hoc routing protocol to increase network lifetime.\nFurthermore we outline future scope of these existing schemes which may help\nresearches to carry out further research in this direction.", "cat": "cs.NI", "authors": ["Priya P. Patel", "Rutvij H. Jhaveri"]}, "1757": {"id": "0910.1310v1", "title": "Peaks in the cosmological density field: parameter constraints from 2dF Galaxy Redshift Survey data", "url": "http://arxiv.org/pdf/0910.1310v1", "date": "2009-10-07 16:36:19", "abs": "We use the number density of peaks in the smoothed cosmological density field\ntaken from the 2dF Galaxy Redshift Survey to constrain parameters related to\nthe power spectrum of mass fluctuations, n (the spectral index), dn/d(lnk)\n(rolling in the spectral index), and the neutrino mass, m_nu. In a companion\npaper we use N-body simulations to study how the peak density responds to\nchanges in the power spectrum, the presence of redshift distortions and the\nrelationship between galaxies and dark matter halos. In the present paper we\nmake measurements of the peak density from 2dF Galaxy Redshift Survey data, for\na range of smoothing filter scales from 4-33 h^-1 Mpc. We use these\nmeasurements to constrain the cosmological parameters, finding n=1.36\n(+0.75)(-0.64), m_nu < 1.76 eV, dn/d(lnk)=-0.012 (+0.192)(-0.208), at the 68 %\nconfidence level, where m_nu is the total mass of three massive neutrinos. At\n95% confidence we find m_nu< 2.48 eV. These measurements represent an\nalternative way to constrain cosmological parameters to the usual direct fits\nto the galaxy power spectrum, and are expected to be relatively insensitive to\nnon-linear clustering evolution and galaxy biasing.", "cat": "astro-ph.CO", "authors": ["S. De", "R. A. C. Croft"]}, "1758": {"id": "2110.01389v1", "title": "A Survey of Selected Algorithms Used in Military Applications from the Viewpoints of Dataflow and GaAs", "url": "http://arxiv.org/pdf/2110.01389v1", "date": "2021-09-30 21:57:41", "abs": "This is a short survey of ten algorithms that are often used for military\npurposes, followed by analysis of their potential suitability for dataflow and\nGaAs, which are a specific architecture and technology for supercomputers on a\nchip, respectively.\n Whenever an algorithm or a device is used in military settings, it is natural\nto assume strict requirements related to speed, reliability, scale, energy,\nsize, and accuracy. The two aforementioned paradigms seem to be promising in\nfulfilling most of these requirements.", "cat": "cs.DC", "authors": ["Ilir Capuni", "Veljko Milutinovic"]}, "1759": {"id": "0909.2258v1", "title": "The roadmap for unification in galaxy group selection:. I. A search for extended X-ray emission in the CNOC2 survey", "url": "http://arxiv.org/pdf/0909.2258v1", "date": "2009-09-11 20:02:54", "abs": "X-ray properties of galaxy groups can unlock some of the most challenging\nresearch topics in modern extragalactic astronomy: the growth of structure and\nits influence on galaxy formation. Only with the advent of the Chandra and XMM\nfacilities have X-ray observations reached the depths required to address these\nquestions in a satisfactory manner. Here we present an X-ray imaging study of\ntwo patches from the CNOC2 spectroscopic galaxy survey using combined Chandra\nand XMM data. A state of the art extended source finding algorithm has been\napplied, and the resultant source catalog, including redshifts from a\nspectroscopic follow-up program, is presented. The total number of\nspectroscopically identified groups is 25 spanning a redshift range 0.04-0.79.\nApproximately 50% of CNOC2 spectroscopically selected groups in the deeper\nX-ray (RA14h) field are likely X-ray detections, compared to 20% in the\nshallower (RA21h) field. Statistical modeling shows that this is consistent\nwith expectations, assuming an expected evolution of the Lx-M relation. A\nsignificant detection of a stacked shear signal for both spectroscopic and\nX-ray groups indicates that both samples contain real groups of about the\nexpected mass. We conclude that the current area and depth of X-ray and\nspectroscopic facilities provide a unique window of opportunity at z~0.4 to\ntest the X-ray appearance of galaxy groups selected in various ways. There is\nat present no evidence that the correlation between X-ray luminosity and\nvelocity dispersion evolves significantly with redshift, which implies that\ncatalogs based on either method can be fairly compared and modeled.", "cat": "astro-ph.CO", "authors": ["A. Finoguenov", "J. L. Connelly", "L. C. Parker", "D. J. Wilman", "J. S. Mulchaey", "R. P. Saglia", "M. L. Balogh", "R. G. Bower", "S. L. McGee"]}, "1760": {"id": "2303.04810v1", "title": "A Survey of Data Pricing for Data Marketplaces", "url": "http://arxiv.org/pdf/2303.04810v1", "date": "2023-03-07 04:35:56", "abs": "A data marketplace is an online venue that brings data owners, data brokers,\nand data consumers together and facilitates commoditisation of data amongst\nthem. Data pricing, as a key function of a data marketplace, demands\nquantifying the monetary value of data. A considerable number of studies on\ndata pricing can be found in literature. This paper attempts to comprehensively\nreview the state-of-the-art on existing data pricing studies to provide a\ngeneral understanding of this emerging research area. Our key contribution lies\nin a new taxonomy of data pricing studies that unifies different attributes\ndetermining data prices. The basis of our framework categorises these studies\nby the kind of market structure, be it sell-side, buy-side, or two-sided. Then\nin a sell-side market, the studies are further divided by query type, which\ndefines the way a data consumer accesses data, while in a buy-side market, the\nstudies are divided according to privacy notion, which defines the way to\nquantify privacy of data owners. In a two-sided market, both privacy notion and\nquery type are used as criteria. We systematically examine the studies falling\ninto each category in our taxonomy. Lastly, we discuss gaps within the existing\nresearch and define future research directions.", "cat": "cs.GT", "authors": ["Mengxiao Zhang", "Fernando Beltran", "Jiamou Liu"]}, "1761": {"id": "1602.07526v1", "title": "Detecting the cosmic web with radio surveys", "url": "http://arxiv.org/pdf/1602.07526v1", "date": "2016-02-24 14:35:22", "abs": "We study the challenges to detect the cosmic web at radio wavelengths with\nstate-of-the-art cosmological simulations of extragalactic magnetic fields. The\nincoming generation of radio surveys operating at low frequency, like LOFAR,\nSKA-LOW and MWA will have the best chance to detect the large-scale, low\nsurface brightness emission from the shocked cosmic web. The detected radio\nemission will enable to constrain the average magnetisation level of the gas in\nfilaments and the acceleration efficiency of electrons by strong shocks. In\ncase of detections, through statistical modelling (e.g. correlation functions)\nit will be possible to discriminate among competing scenarios for the\nmagnetisation of large-scale structures (i.e. astrophysical versus primordial\nscenarios), making radio surveys an important probe of cosmic magnetogenesis.", "cat": "astro-ph.CO", "authors": ["F. Vazza", "M. Brueggen", "C. Gheller", "C. Ferrari", "A. Bonafede"]}, "1762": {"id": "2209.05872v1", "title": "Smart Contract Vulnerability Detection Technique: A Survey", "url": "http://arxiv.org/pdf/2209.05872v1", "date": "2022-09-13 10:35:42", "abs": "Smart contract, one of the most successful applications of blockchain, is\ntaking the world by storm, playing an essential role in the blockchain\necosystem. However, frequent smart contract security incidents not only result\nin tremendous economic losses but also destroy the blockchain-based credit\nsystem. The security and reliability of smart contracts thus gain extensive\nattention from researchers worldwide. In this survey, we first summarize the\ncommon types and typical cases of smart contract vulnerabilities from three\nlevels, i.e., Solidity code layer, EVM execution layer, and Block dependency\nlayer. Further, we review the research progress of smart contract vulnerability\ndetection and classify existing counterparts into five categories, i.e., formal\nverification, symbolic execution, fuzzing detection, intermediate\nrepresentation, and deep learning. Empirically, we take 300 real-world smart\ncontracts deployed on Ethereum as the test samples and compare the\nrepresentative methods in terms of accuracy, F1-Score, and average detection\ntime. Finally, we discuss the challenges in the field of smart contract\nvulnerability detection and combine with the deep learning technology to look\nforward to future research directions.", "cat": "cs.CR", "authors": ["Peng Qian", "Zhenguang Liu", "Qinming He", "Butian Huang", "Duanzheng Tian", "Xun Wang"]}, "1763": {"id": "1902.09159v2", "title": "A Survey of Crowdsourcing in Medical Image Analysis", "url": "http://arxiv.org/pdf/1902.09159v2", "date": "2019-09-04 12:47:16", "abs": "Rapid advances in image processing capabilities have been seen across many\ndomains, fostered by the application of machine learning algorithms to\n\"big-data\". However, within the realm of medical image analysis, advances have\nbeen curtailed, in part, due to the limited availability of large-scale,\nwell-annotated datasets. One of the main reasons for this is the high cost\noften associated with producing large amounts of high-quality meta-data.\nRecently, there has been growing interest in the application of crowdsourcing\nfor this purpose; a technique that has proven effective for creating\nlarge-scale datasets across a range of disciplines, from computer vision to\nastrophysics. Despite the growing popularity of this approach, there has not\nyet been a comprehensive literature review to provide guidance to researchers\nconsidering using crowdsourcing methodologies in their own medical imaging\nanalysis. In this survey, we review studies applying crowdsourcing to the\nanalysis of medical images, published prior to July 2018. We identify common\napproaches, challenges and considerations, providing guidance of utility to\nresearchers adopting this approach. Finally, we discuss future opportunities\nfor development within this emerging domain.", "cat": "cs.CV", "authors": ["Silas \u00d8rting", "Andrew Doyle", "Arno van Hilten", "Matthias Hirth", "Oana Inel", "Christopher R. Madan", "Panagiotis Mavridis", "Helen Spiers", "Veronika Cheplygina"]}, "1764": {"id": "0707.4260v1", "title": "Orbit Determination with Topocentric Correction: Algorithms for the Next Generation Surveys", "url": "http://arxiv.org/pdf/0707.4260v1", "date": "2007-07-28 20:39:14", "abs": "Given a set of astrometric observations of the same object, the problem of\norbit determination is to compute the orbit and to assess its uncertainty and\nreliability. For the next generation surveys, with much larger number density\nof observed objects, new algorithms or substantial revisions of the classical\nones are needed. The problem has three main steps, preliminary orbit, least\nsquares orbit, and quality control. The classical theory of preliminary orbits\nwas incomplete: the consequences of the topocentric correction had not been\nfully studied. We show that it is possible to account for this correction,\npossibly with an increase in the number of preliminary solutions, without\nimpairing the overall orbit determination performance. We have developed\nmodified least squares orbit determination algorithms that can be used to\nimprove the reliability of the procedure. We have tested the complete procedure\non two simulations with number densities comparable to that expected from the\nnext generation surveys such as Pan-STARRS and LSST. To control the problem of\nfalse identifications we have introduced a quality control on the fit residuals\nbased on an array of metrics and a procedure to remove duplications and\ncontradictions in the output. The results confirm that large sets of\ndiscoveries can be obtained with good quality orbits and very high success rate\nlosing only 0.6 to 1.3% of objects and a false identification rate in the range\n0.02 to 0.06%.", "cat": "astro-ph", "authors": ["Andrea Milani", "Giovanni F. Gronchi", "Davide Farnocchia", "Zoran Knezevic", "Robert Jedicke", "Larry Denneau", "Francesco Pierfederici"]}, "1765": {"id": "2212.08540v1", "title": "A Comprehensive Survey of Benchmarks for Automated Improvement of Software's Non-Functional Properties", "url": "http://arxiv.org/pdf/2212.08540v1", "date": "2022-12-16 15:43:08", "abs": "Performance is a key quality of modern software. Although recent years have\nseen a spike in research on automated improvement of software's execution time,\nenergy, memory consumption, etc., there is a noticeable lack of standard\nbenchmarks for such work. It is also unclear how such benchmarks are\nrepresentative of current software. Furthermore, frequently non-functional\nproperties of software are targeted for improvement one-at-a-time, neglecting\npotential negative impact on other properties.\n In order to facilitate more research on automated improvement of\nnon-functional properties of software, we conducted a survey gathering\nbenchmarks used in previous work. We considered 5 major online repositories of\nsoftware engineering work: ACM Digital Library, IEEE Xplore, Scopus, Google\nScholar, and ArXiV. We gathered 5000 publications (3749 unique), which were\nsystematically reviewed to identify work that empirically improves\nnon-functional properties of software. We identified 386 relevant papers.\n We find that execution time is the most frequently targeted property for\nimprovement (in 62% of relevant papers), while multi-objective improvement is\nrarely considered (5%). Static approaches are prevalent (in 53% of papers),\nwith exploratory approaches (evolutionary in 18% and non-evolutionary in 14% of\npapers) increasingly popular in the last 10 years. Only 40% of 386 papers\ndescribe work that uses benchmark suites, rather than single software, of those\nSPEC is most popular (covered in 33 papers). We also provide recommendations\nfor choice of benchmarks in future work, noting, e.g., lack of work that covers\nPython or JavaScript. We provide all programs found in the 386 papers on our\ndedicated webpage at https://bloa.github.io/nfunc_survey/\n We hope that this effort will facilitate more research on the topic of\nautomated improvement of software's non-functional properties.", "cat": "cs.SE", "authors": ["Aymeric Blot", "Justyna Petke"]}, "1766": {"id": "1706.04459v2", "title": "The SUrvey for Pulsars and Extragalactic Radio Bursts I: Survey Description and Overview", "url": "http://arxiv.org/pdf/1706.04459v2", "date": "2017-08-14 11:17:28", "abs": "We describe the Survey for Pulsars and Extragalactic Radio Bursts (SUPERB),\nan ongoing pulsar and fast transient survey using the Parkes radio telescope.\nSUPERB involves real-time acceleration searches for pulsars and single-pulse\nsearches for pulsars and fast radio bursts. We report on the observational\nsetup, data analysis, multi-wavelength/messenger connections, survey\nsensitivities to pulsars and fast radio bursts and the impact of radio\nfrequency interference. We further report on the first 10 pulsars discovered in\nthe project. Among these is PSR~J1306$-$40, a millisecond pulsar in a binary\nsystem where it appears to be eclipsed for a large fraction of the orbit.\nPSR~J1421$-$4407 is another binary millisecond pulsar; its orbital period is\n$30.7$ days. This orbital period is in a range where only highly eccentric\nbinaries are known, and expected by theory; despite this its orbit has an\neccentricity of $10^{-5}$.", "cat": "astro-ph.IM", "authors": ["E. F. Keane", "E. D. Barr", "A. Jameson", "V. Morello", "M. Caleb", "S. Bhandari", "E. Petroff", "A. Possenti", "M. Burgay", "C. Tiburzi", "M. Bailes", "N. D. R. Bhat", "S. Burke-Spolaor", "R. P. Eatough", "C. Flynn", "F. Jankowski", "S. Johnston", "M. Kramer", "L. Levin", "C. Ng", "W. van Straten", "V. Venkatraman Krishnan"]}, "1767": {"id": "1711.00750v1", "title": "VEGAS-SSS II: Comparing the globular cluster systems in NGC3115 and NGC1399 using VEGAS and FDS survey data", "url": "http://arxiv.org/pdf/1711.00750v1", "date": "2017-11-02 14:09:37", "abs": "We analyze the globular cluster (GC) systems in two very different galaxies,\nN3115 and N1399. With the papers of this series, we aim at highlighting common\nand different properties in the GC systems in galaxies covering a wide range of\nparameter space. We compare the GCs in N3115 and N1399 as derived from the\nanalysis of u, g, and i band images taken with the VST telescope as part of the\nVEGAS and FDS surveys. We selected GC candidates using as reference the\nmorpho-photometric and color properties of confirmed GCs. The surface density\nof GCs in N3115 reveal a morphology similar to the profile of field stars; the\nsame is true when blue and red GCs are taken separately. The GC maps for N1399\nare richer in structure and confirm the existence of an intracluster GC\ncomponent. We confirm the presence of a spatial offset in the N1399 GC centroid\nand find that the centroid of the GCs for N3115 coincides well with the galaxy\ncenter. Both GC systems show unambiguous color bimodality in g-i and u-i. The\nazimuthal average of the radial density profiles in both galaxies reveals a\nlarger spatial extent for the total GCs population with respect to the galaxy\nsurface brightness profile. As for the specific frequency of GCs, Sn, we find\nit is a factor of two higher in N1399 than for N3115. By inspecting the radial\nbehavior of the specific frequency, Sn(3.0 Mpc) counterpart\nto HVC274.68+74.70-123 has been identified on our images. The point source\nphotometry in the central 17.3' X 7.7' chips reaches r<= 26.5, and is expected\nto contain most of the stellar counterparts to the UCHVCs. However, no obvious\nstellar over-density is detected in any of our fields, in marked contrast to\nour comparison LeoP field in which the dwarf galaxy is detected at a >30 sigma\nsignificance level. Only HVC352.45+59.06+263 may be associated with a weak\nover-density, whose nature cannot be ascertained with our data. Sensitivity\ntests shows that our survey would have detected any dwarf galaxy dominated by\nan old stellar population, with an integrated absolute magnitude M_V<= -8.0, a\nhalf-light radius r_h<= 300 pc, and lying within 1.5 Mpc from us, thereby\nconfirming that it is unlikely that the observed UCHVCs are associated with\nstellar counterparts typical of known Local Group dwarf galaxies.", "cat": "astro-ph.GA", "authors": ["M. Bellazzini", "G. Beccari", "G. Battaglia", "N. Martin", "V. Testa", "R. Ibata", "M. Correnti", "F. Cusano", "E. Sani"]}, "1771": {"id": "2303.01202v1", "title": "A Survey of Fusion Frames in Hilbert Spaces", "url": "http://arxiv.org/pdf/2303.01202v1", "date": "2023-03-02 12:36:09", "abs": "Fusion frames are a very active area of research today because of their\nmyriad of applications in pure mathematics, applied mathematics, engineering,\nmedicine, signal and image processing and much more. They provide a great\nflexibility for designing sets of vectors for applications and are therefore\nprominent in all these areas, including e.g. mitigating the effects of noise in\na signal or giving robustness to erasures. In this chapter, we present the\nfundamentals of fusion frame theory with an emphasis on their delicate relation\nto frame theory. The goal here is to provide researchers and students with an\neasy entry into this topic. Proofs for fusion frames will be self-contained and\ndifferences between frames and fusion frames are analyzed. In particular, we\nfocus on the subtleties of fusion frame duality. We also provide a reproducible\nresearch implementation.", "cat": "math.FA", "authors": ["Lukas K\u00f6hldorfer", "Peter Balazs", "Pete Casazza", "Sigrid Heineken", "Clara Hollomey", "Patricia Morillas", "Mitra Shamsabadi"]}, "1772": {"id": "2203.00557v2", "title": "MeerTRAP: Twelve Galactic fast transients detected in a real-time, commensal MeerKAT survey", "url": "http://arxiv.org/pdf/2203.00557v2", "date": "2022-03-04 10:12:44", "abs": "MeerTRAP is a real-time untargeted search project using the MeerKAT telescope\nto find single pulses from fast radio transients and pulsars. It is performed\ncommensally with the MeerKAT large survey projects (LSPs), using data from up\nto 64 of MeerKAT's 13.96~m dishes to form hundreds of coherent beams on sky,\neach of which is processed in real time to search for millisecond-duration\npulses. We present the first twelve Galactic sources discovered by MeerTRAP,\nwith DMs in the range of 33--381~pc~cm$^{-3}$. One source may be Galactic or\nextragalactic depending on the Galactic electron density model assumed.\nFollow-up observations performed with the MeerKAT, Lovell, and Parkes radio\ntelescopes have detected repeat pulses from seven of the twelve sources. Pulse\nperiods have been determined for four sources. Another four sources could be\nlocalised to the arcsecond-level using a novel implementation of the tied-array\nbeam localisation method.", "cat": "astro-ph.HE", "authors": ["M. C. Bezuidenhout", "E. Barr", "M. Caleb", "L. N. Driessen", "F. Jankowski", "M. Kramer", "M. Malenta", "V. Morello", "K. Rajwade", "S. Sanidas", "B. W. Stappers", "M. Surnis"]}, "1773": {"id": "2308.09766v3", "title": "Time Series Predictions in Unmonitored Sites: A Survey of Machine Learning Techniques in Water Resources", "url": "http://arxiv.org/pdf/2308.09766v3", "date": "2024-08-14 17:20:19", "abs": "Prediction of dynamic environmental variables in unmonitored sites remains a\nlong-standing challenge for water resources science. The majority of the\nworld's freshwater resources have inadequate monitoring of critical\nenvironmental variables needed for management. Yet, the need to have widespread\npredictions of hydrological variables such as river flow and water quality has\nbecome increasingly urgent due to climate and land use change over the past\ndecades, and their associated impacts on water resources. Modern machine\nlearning methods increasingly outperform their process-based and empirical\nmodel counterparts for hydrologic time series prediction with their ability to\nextract information from large, diverse data sets. We review relevant\nstate-of-the art applications of machine learning for streamflow, water\nquality, and other water resources prediction and discuss opportunities to\nimprove the use of machine learning with emerging methods for incorporating\nwatershed characteristics into deep learning models, transfer learning, and\nincorporating process knowledge into machine learning models. The analysis here\nsuggests most prior efforts have been focused on deep learning learning\nframeworks built on many sites for predictions at daily time scales in the\nUnited States, but that comparisons between different classes of machine\nlearning methods are few and inadequate. We identify several open questions for\ntime series predictions in unmonitored sites that include incorporating dynamic\ninputs and site characteristics, mechanistic understanding and spatial context,\nand explainable AI techniques in modern machine learning frameworks.", "cat": "cs.LG", "authors": ["Jared D. Willard", "Charuleka Varadharajan", "Xiaowei Jia", "Vipin Kumar"]}, "1774": {"id": "2305.13689v1", "title": "Know Your Self-supervised Learning: A Survey on Image-based Generative and Discriminative Training", "url": "http://arxiv.org/pdf/2305.13689v1", "date": "2023-05-23 04:54:09", "abs": "Although supervised learning has been highly successful in improving the\nstate-of-the-art in the domain of image-based computer vision in the past, the\nmargin of improvement has diminished significantly in recent years, indicating\nthat a plateau is in sight. Meanwhile, the use of self-supervised learning\n(SSL) for the purpose of natural language processing (NLP) has seen tremendous\nsuccesses during the past couple of years, with this new learning paradigm\nyielding powerful language models. Inspired by the excellent results obtained\nin the field of NLP, self-supervised methods that rely on clustering,\ncontrastive learning, distillation, and information-maximization, which all\nfall under the banner of discriminative SSL, have experienced a swift uptake in\nthe area of computer vision. Shortly afterwards, generative SSL frameworks that\nare mostly based on masked image modeling, complemented and surpassed the\nresults obtained with discriminative SSL. Consequently, within a span of three\nyears, over $100$ unique general-purpose frameworks for generative and\ndiscriminative SSL, with a focus on imaging, were proposed. In this survey, we\nreview a plethora of research efforts conducted on image-oriented SSL,\nproviding a historic view and paying attention to best practices as well as\nuseful software packages. While doing so, we discuss pretext tasks for\nimage-based SSL, as well as techniques that are commonly used in image-based\nSSL. Lastly, to aid researchers who aim at contributing to image-focused SSL,\nwe outline a number of promising research directions.", "cat": "cs.CV", "authors": ["Utku Ozbulak", "Hyun Jung Lee", "Beril Boga", "Esla Timothy Anzaku", "Homin Park", "Arnout Van Messem", "Wesley De Neve", "Joris Vankerschaver"]}, "1775": {"id": "2301.06767v1", "title": "The Recent Advances in Automatic Term Extraction: A survey", "url": "http://arxiv.org/pdf/2301.06767v1", "date": "2023-01-17 09:02:15", "abs": "Automatic term extraction (ATE) is a Natural Language Processing (NLP) task\nthat eases the effort of manually identifying terms from domain-specific\ncorpora by providing a list of candidate terms. As units of knowledge in a\nspecific field of expertise, extracted terms are not only beneficial for\nseveral terminographical tasks, but also support and improve several complex\ndownstream tasks, e.g., information retrieval, machine translation, topic\ndetection, and sentiment analysis. ATE systems, along with annotated datasets,\nhave been studied and developed widely for decades, but recently we observed a\nsurge in novel neural systems for the task at hand. Despite a large amount of\nnew research on ATE, systematic survey studies covering novel neural approaches\nare lacking. We present a comprehensive survey of deep learning-based\napproaches to ATE, with a focus on Transformer-based neural models. The study\nalso offers a comparison between these systems and previous ATE approaches,\nwhich were based on feature engineering and non-neural supervised learning\nalgorithms.", "cat": "cs.CL", "authors": ["Hanh Thi Hong Tran", "Matej Martinc", "Jaya Caporusso", "Antoine Doucet", "Senja Pollak"]}, "1776": {"id": "2202.09506v1", "title": "From Quantum Graph Computing to Quantum Graph Learning: A Survey", "url": "http://arxiv.org/pdf/2202.09506v1", "date": "2022-02-19 02:56:47", "abs": "Quantum computing (QC) is a new computational paradigm whose foundations\nrelate to quantum physics. Notable progress has been made, driving the birth of\na series of quantum-based algorithms that take advantage of quantum\ncomputational power. In this paper, we provide a targeted survey of the\ndevelopment of QC for graph-related tasks. We first elaborate the correlations\nbetween quantum mechanics and graph theory to show that quantum computers are\nable to generate useful solutions that can not be produced by classical systems\nefficiently for some problems related to graphs. For its practicability and\nwide-applicability, we give a brief review of typical graph learning techniques\ndesigned for various tasks. Inspired by these powerful methods, we note that\nadvanced quantum algorithms have been proposed for characterizing the graph\nstructures. We give a snapshot of quantum graph learning where expectations\nserve as a catalyst for subsequent research. We further discuss the challenges\nof using quantum algorithms in graph learning, and future directions towards\nmore flexible and versatile quantum graph learning solvers.", "cat": "quant-ph", "authors": ["Yehui Tang", "Junchi Yan", "Hancock Edwin"]}, "1777": {"id": "1710.00834v2", "title": "Empirical Modeling of the Redshift Evolution of the [NII]/H$\u03b1$-ratio for Galaxy Redshift Surveys", "url": "http://arxiv.org/pdf/1710.00834v2", "date": "2018-03-17 19:12:23", "abs": "We present an empirical parameterization of the [NII]/H$\\alpha$ flux ratio as\na function of stellar mass and redshift valid at 0 < z < 2.7 and 8.5 < log(M) <\n11.0. This description can easily be applied to (i) simulations for modeling\n[NII]$\\lambda6584$ line emission, (ii) deblend [NII] and H$\\alpha$ in current\nlow-resolution grism and narrow-band observations to derive intrinsic H$\\alpha$\nfluxes, and (iii) to reliably forecast the number counts of H$\\alpha$\nemission-line galaxies for future surveys, such as those planned for Euclid and\nthe Wide Field Infrared Survey Telescope (WFIRST). Our model combines the\nevolution of the locus on the Baldwin, Phillips & Terlevich (BPT) diagram\nmeasured in spectroscopic data out to z = 2.5 with the strong dependence of\n[NII]/H$\\alpha$ on stellar mass and [OIII]/H$\\beta$ observed in local galaxy\nsamples. We find large variations in the [NII]/H$\\alpha$ flux ratio at a fixed\nredshift due to its dependency on stellar mass; hence, the assumption of a\nconstant [NII] flux contamination fraction can lead to a significant under- or\noverestimate of H$\\alpha$ luminosities. Specifically, measurements of the\nintrinsic H$\\alpha$ luminosity function derived from current low-resolution\ngrism spectroscopy assuming a constant 29% contamination of [NII] can be\noverestimated by factors of ~8 at log(L) > 43.0 for galaxies at redshifts z =\n1.5. This has implications for the prediction of H$\\alpha$ emitters for Euclid\nand WFIRST. We also study the impact of blended H$\\alpha$ and [NII] on the\naccuracy of measured spectroscopic redshifts.", "cat": "astro-ph.GA", "authors": ["Andreas L. Faisst", "Daniel Masters", "Yun Wang", "Alexander Merson", "Peter Capak", "Sangeeta Malhotra", "James E. Rhoads"]}, "1778": {"id": "2402.11143v1", "title": "Foundation Models for Recommender Systems: A Survey and New Perspectives", "url": "http://arxiv.org/pdf/2402.11143v1", "date": "2024-02-17 00:22:03", "abs": "Recently, Foundation Models (FMs), with their extensive knowledge bases and\ncomplex architectures, have offered unique opportunities within the realm of\nrecommender systems (RSs). In this paper, we attempt to thoroughly examine\nFM-based recommendation systems (FM4RecSys). We start by reviewing the research\nbackground of FM4RecSys. Then, we provide a systematic taxonomy of existing\nFM4RecSys research works, which can be divided into four different parts\nincluding data characteristics, representation learning, model type, and\ndownstream tasks. Within each part, we review the key recent research\ndevelopments, outlining the representative models and discussing their\ncharacteristics. Moreover, we elaborate on the open problems and opportunities\nof FM4RecSys aiming to shed light on future research directions in this area.\nIn conclusion, we recap our findings and discuss the emerging trends in this\nfield.", "cat": "cs.IR", "authors": ["Chengkai Huang", "Tong Yu", "Kaige Xie", "Shuai Zhang", "Lina Yao", "Julian McAuley"]}, "1779": {"id": "1508.03175v2", "title": "Metrics for Optimization of Large Synoptic Survey Telescope Observations of Stellar Variables and Transients", "url": "http://arxiv.org/pdf/1508.03175v2", "date": "2015-08-17 04:10:33", "abs": "The Large Synoptic Survey Telescope (LSST) will be the largest time-domain\nphotometric survey ever. In order to maximize the LSST science yield for a\nbroad array of transient stellar phenomena, it is necessary to optimize the\nsurvey cadence, coverage, and depth via quantitative metrics that are\nspecifically designed to characterize the time-domain behavior of various types\nof stellar transients. In this paper we present three such metrics built on the\nLSST Metric Analysis Framework (MAF) model (Jones et al. 2014). Two of the\nmetrics quantify the ability of LSST to detect non-periodic and/or\nnon-recurring transient events, and the ability of LSST to reliably measure\nperiodic signals of various timescales. The third metric provides a way to\nquantify the range of stellar parameters in the stellar populations that LSST\nwill probe. We provide example uses of these metrics and discuss some\nimplications based on these metrics for optimization of the LSST survey for\nobservations of stellar variables and transients.", "cat": "astro-ph.IM", "authors": ["Michael B. Lund", "Robert J. Siverd", "Joshua A. Pepper", "Keivan G. Stassun"]}, "1780": {"id": "1109.0639v1", "title": "Very Strong Emission-Line Galaxies in the WISP Survey and Implications for High-Redshift Galaxies", "url": "http://arxiv.org/pdf/1109.0639v1", "date": "2011-09-03 17:30:03", "abs": "The WFC3 Infrared Spectroscopic Parallel Survey (WISP) uses the Hubble Space\nTelescope (HST) infrared grism capabilities to obtain slitless spectra of\nthousands of galaxies over a wide redshift range including the peak of star\nformation history of the Universe. We select a population of very strong\nemission-line galaxies with rest-frame equivalent widths higher than 200 A. A\ntotal of 176 objects are found over the redshift range 0.35 < z < 2.3 in the\n180 arcmin^2 area we analyzed so far. After estimating the AGN fraction in the\nsample, we show that this population consists of young and low-mass starbursts\nwith higher specific star formation rates than normal star-forming galaxies at\nany redshift. After spectroscopic follow-up of one of these galaxies with\nKeck/LRIS, we report the detection at z = 0.7 of an extremely metal-poor galaxy\nwith 12+Log(O/H)= 7.47 +- 0.11. The nebular emission-lines can substantially\naffect the broadband flux density with a median brightening of 0.3 mag, with\nexamples producing brightening of up to 1 mag. The presence of strong emission\nlines in low-z galaxies can mimic the color-selection criteria used in the z ~\n8 dropout surveys. In order to effectively remove low redshift interlopers,\ndeep optical imaging is needed, at least 1 mag deeper than the bands in which\nthe objects are detected. Finally, we empirically demonstrate that strong\nnebular lines can lead to an overestimation of the mass and the age of galaxies\nderived from fitting of their SED. Without removing emission lines, the age and\nthe stellar mass estimates are overestimated by a factor of 2 on average and up\nto a factor of 10 for the high-EW galaxies. Therefore the contribution of\nemission lines should be systematically taken into account in SED fitting of\nstar-forming galaxies at all redshifts.", "cat": "astro-ph.CO", "authors": ["H. Atek", "B. Siana", "C. Scarlata", "M. Malkan", "P. McCarthy", "H. Teplitz", "A. Henry", "J. Colbert", "C. Bridge", "A. J. Bunker", "A. Dressler", "R. Fosbury", "N. P. Hathi", "C. Martin", "N. R. Ross", "H. Shim"]}, "1781": {"id": "2005.05272v1", "title": "Harmonised LUCAS in-situ data and photos on land cover and use from 5 tri-annual surveys in the European Union", "url": "http://arxiv.org/pdf/2005.05272v1", "date": "2020-05-11 17:16:25", "abs": "Accurately characterizing land surface changes with Earth Observation\nrequires geo-localized ground truth. In the European Union (EU), a tri-annual\nsurveyed sample of land cover and land use has been collected since 2006 under\nthe Land Use/Cover Area frame Survey (LUCAS). A total of 1,351,293 observations\nat 651,780 unique locations for 117 variables along with 5.4 million photos\nwere collected during five LUCAS surveys. Until now, these data have never been\nharmonised into one database, limiting full exploitation of the information.\nThis paper describes the LUCAS point sampling/surveying methodology, including\ncollection of standard variables such as land cover, environmental parameters,\nand full resolution landscape and point photos, and then describes the\nharmonisation process. The resulting harmonised database is the most\ncomprehensive in-situ dataset on land cover and use in the EU. The database is\nvaluable for geo-spatial and statistical analysis of land use and land cover\nchange. Furthermore, its potential to provide multi-temporal in-situ data will\nbe enhanced by recent computational advances such as deep learning.", "cat": "stat.AP", "authors": ["Rapha\u00ebl d'Andrimont", "Momchil Yordanov", "Laura Martinez-Sanchez", "Beatrice Eiselt", "Alessandra Palmieri", "Paolo Dominici", "Javier Gallego", "Hannes Isaak Reuter", "Christian Joebges", "Guido Lemoine", "Marijn van der Velde"]}, "1782": {"id": "2106.13025v1", "title": "From downtown to the outskirts: a radio survey of the Orion Nebula Cluster", "url": "http://arxiv.org/pdf/2106.13025v1", "date": "2021-06-24 13:56:46", "abs": "We present a newly enlarged census of the compact radio population towards\nthe Orion Nebula Cluster (ONC) using high-sensitivity continuum maps (3-10\n$\\mu$Jy bm$^{-1}$) from a total of $\\sim30$ h centimeter-wavelength\nobservations over an area of $\\sim$20$'\\times20'$ obtained in the C-band (4$-$8\nGHz) with the Karl G. Jansky Very Large Array (VLA) in its high-resolution\nA-configuration. We thus complement our previous deep survey of the innermost\nareas of the ONC, now covering the field of view of the Chandra Orion\nUltra-deep Project (COUP). Our catalog contains 521 compact radio sources of\nwhich 198 are new detections. Overall, we find that 17% of the (mostly stellar)\nCOUP sources have radio counterparts, while 53% of the radio sources have COUP\ncounterparts. Most notably, the radio detection fraction of X-ray sources is\nhigher in the inner cluster and almost constant for $r>3'$ (0.36 pc) from\n$\\theta^1$ Ori C suggesting a correlation between the radio emission mechanism\nof these sources and their distance from the most massive stars at the center\nof the cluster, for example due to increased photoionisation of circumstellar\ndisks. The combination with our previous observations four years prior lead to\nthe discovery of fast proper motions of up to $\\sim$373 km s$^{-1}$ from faint\nradio sources associated with ejecta of the OMC1 explosion. Finally, we search\nfor strong radio variability. We found changes in flux density by a factor of\n$\\lesssim$5 within our observations and a few sources with changes by a factor\n$>$10 on long timescales of a few years.", "cat": "astro-ph.GA", "authors": ["Jaime Vargas-Gonz\u00e1lez", "Jan Forbrich", "Sergio A. Dzib", "John Bally"]}, "1783": {"id": "2211.16509v2", "title": "Multimodal Learning for Multi-Omics: A Survey", "url": "http://arxiv.org/pdf/2211.16509v2", "date": "2022-12-19 14:26:02", "abs": "With advanced imaging, sequencing, and profiling technologies, multiple omics\ndata become increasingly available and hold promises for many healthcare\napplications such as cancer diagnosis and treatment. Multimodal learning for\nintegrative multi-omics analysis can help researchers and practitioners gain\ndeep insights into human diseases and improve clinical decisions. However,\nseveral challenges are hindering the development in this area, including the\navailability of easily accessible open-source tools. This survey aims to\nprovide an up-to-date overview of the data challenges, fusion approaches,\ndatasets, and software tools from several new perspectives. We identify and\ninvestigate various omics data challenges that can help us understand the field\nbetter. We categorize fusion approaches comprehensively to cover existing\nmethods in this area. We collect existing open-source tools to facilitate their\nbroader utilization and development. We explore a broad range of omics data\nmodalities and a list of accessible datasets. Finally, we summarize future\ndirections that can potentially address existing gaps and answer the pressing\nneed to advance multimodal learning for multi-omics data analysis.", "cat": "q-bio.GN", "authors": ["Sina Tabakhi", "Mohammod Naimul Islam Suvon", "Pegah Ahadian", "Haiping Lu"]}, "1784": {"id": "0704.1744v1", "title": "Blazar surveys with WMAP and Swift", "url": "http://arxiv.org/pdf/0704.1744v1", "date": "2007-04-13 11:57:14", "abs": "We present the preliminary results from two new surveys of blazars that have\ndirect implications on the GLAST detection of extragalactic sources from two\ndifferent perspectives: microwave selection and a combined deep X-ray/radio\nselection. The first one is a 41 GHz flux-limited sample extracted from the\nWMAP 3-yr catalog of microwave point sources. This is a statistically well\ndefined sample of about 200 blazars and radio galaxies, most of which are\nexpected to be detected by GLAST. The second one is a new deep survey of\nBlazars selected among the radio sources that are spatially coincident with\nserendipitous sources detected in deep X-ray images (0.3-10 keV) centered on\nthe Gamma Ray Bursts (GRB) discovered by the Swift satellite. This sample is\nparticularly interesting from a statistical viewpoint since a) it is unbiased\nas GRBs explode at random positions in the sky, b) it is very deep in the X-ray\nband (\\fx \\simgt $10^{-15}$ \\ergs) with a position accuracy of a few\narc-seconds, c) it will cover a fairly large (20-30 square deg.) area of sky,\nd) it includes all blazars with radio flux (1.4 GHz) larger than 10 mJy, making\nit approximately two orders of magnitude deeper than the WMAP sample and about\none order of magnitude deeper than the deepest existing complete samples of\nradio selected blazars, and e) it can be used to estimate the amount of\nunresolved GLAST high latitude gamma-ray background and its anisotropy\nspectrum.", "cat": "astro-ph", "authors": ["P. Giommi", "M. Capalbi", "E. Cavazzuti", "S. Colafrancesco", "S. Cutini", "D. Gasparrini", "E. Massaro", "P. Padovani", "M. Perri", "S. Puccetti"]}, "1785": {"id": "1806.03748v2", "title": "Member stars of the GD1 tidal stream from the SDSS, LAMOST and Gaia surveys", "url": "http://arxiv.org/pdf/1806.03748v2", "date": "2019-04-02 00:11:23", "abs": "With the photometric data from the SDSS survey, the spectroscopic data from\nthe SDSS/SEGUE and the LAMOST surveys, and the astrometric data from the Gaia\nDR2, we have identified 71 highly-probable member stars of the GD-1 cold\nstellar stream spread along almost its entire length (i.e. from 126 to 203\ndegree in Right Ascension). With the accurate spectroscopic (i.e. metallicity\nand line-of-sight velocity) and astrometric (i.e. proper motions) information,\nthe position-velocity diagrams, i.e. $\\phi_{1}$-$\\mu_{\\alpha}$,\n$\\phi_{1}$-$\\mu_{\\delta}$ and $\\phi_{1}$-${v_{\\rm gsr}}$, of the GD-1 stream\nare well mapped. The stream has an average metallicity [Fe/H] $= -1.95 \\pm\n0.23$. The rich information of member stars of the stream now available allow\none not only to model its origin, but also to place strong constraints on the\nmass distribution and the gravitational potential of the Milky Way.", "cat": "astro-ph.GA", "authors": ["Yang Huang", "Xiaowei Liu", "Bingqiu Chen", "Huawei Zhang", "Haibo Yuan", "Maosheng Xiang", "Chun Wang", "Zhijian Tian"]}, "1786": {"id": "1503.04201v1", "title": "To Apply or Not to Apply: A Survey Analysis of Grant Writing Costs and Benefits", "url": "http://arxiv.org/pdf/1503.04201v1", "date": "2015-03-13 20:00:11", "abs": "We surveyed 113 astronomers and 82 psychologists active in applying for\nfederally funded research on their grant-writing history between January, 2009\nand November, 2012. We collected demographic data, effort levels, success\nrates, and perceived non-financial benefits from writing grant proposals. We\nfind that the average proposal takes 116 PI hours and 55 CI hours to write;\nalthough time spent writing was not related to whether the grant was funded.\nEffort did translate into success, however, as academics who wrote more grants\nreceived more funding. Participants indicated modest non-monetary benefits from\ngrant writing, with psychologists reporting a somewhat greater benefit overall\nthan astronomers. These perceptions of non-financial benefits were unrelated to\nhow many grants investigators applied for, the number of grants they received,\nor the amount of time they devoted to writing their proposals. We also explored\nthe number of years an investigator can afford to apply unsuccessfully for\nresearch grants and our analyses suggest that funding rates below approximately\n20%, commensurate with current NIH and NSF funding, are likely to drive at\nleast half of the active researchers away from federally funded research. We\nconclude with recommendations and suggestions for individual investigators and\nfor department heads.", "cat": "physics.soc-ph", "authors": ["Ted von Hippel", "Courtney von Hippel"]}, "1787": {"id": "2203.11242v3", "title": "A survey on GANs for computer vision: Recent research, analysis and taxonomy", "url": "http://arxiv.org/pdf/2203.11242v3", "date": "2024-02-16 12:48:21", "abs": "In the last few years, there have been several revolutions in the field of\ndeep learning, mainly headlined by the large impact of Generative Adversarial\nNetworks (GANs). GANs not only provide an unique architecture when defining\ntheir models, but also generate incredible results which have had a direct\nimpact on society. Due to the significant improvements and new areas of\nresearch that GANs have brought, the community is constantly coming up with new\nresearches that make it almost impossible to keep up with the times. Our survey\naims to provide a general overview of GANs, showing the latest architectures,\noptimizations of the loss functions, validation metrics and application areas\nof the most widely recognized variants. The efficiency of the different\nvariants of the model architecture will be evaluated, as well as showing the\nbest application area; as a vital part of the process, the different metrics\nfor evaluating the performance of GANs and the frequently used loss functions\nwill be analyzed. The final objective of this survey is to provide a summary of\nthe evolution and performance of the GANs which are having better results to\nguide future researchers in the field.", "cat": "cs.LG", "authors": ["Guillermo Iglesias", "Edgar Talavera", "Alberto D\u00edaz-\u00c1lvarez"]}, "1788": {"id": "0902.4103v1", "title": "Quasar Optical Variability in the Palomar-QUEST Survey", "url": "http://arxiv.org/pdf/0902.4103v1", "date": "2009-02-24 09:19:12", "abs": "The ensemble variability properties of nearly 23,000 quasars are studied\nusing the Palomar-QUEST Survey. The survey has covered 15,000 square degrees\nmultiple times over 3.5 years using 7 optical filters, and has been calibrated\nspecifically for variability work. Palomar-QUEST allows for the study of rare\nobjects using multiple epochs of consistently calibrated, homogeneous data,\nobviating the common problem of generating comparable measurements from\ndisparate datasets. A power law fit to the quasar structure function versus\ntime yields an index of 0.432 +/- 0.024 for our best measured sample. We see\nthe commonly reported anticorrelation between average optical variability\namplitude and optical luminosity, and measure the logarithmic decrease in\nvariability amplitude to scale as the logarithm of the luminosity times 0.205\n+/- 0.002. Black hole mass is positively correlated with variability amplitude\nover three orders of magnitude in mass. Quasar variability amplitude is seen to\ndecrease with Eddington ratio as a step function with a transition around\nEddington ratio of 0.5. The higher variability at low Eddington ratios is due\nto excess power at timescales shorter than roughly 300 days. X-ray and radio\nmeasurements exist for subsets of the quasar sample. We observe an\nanticorrelation between optical variability amplitude and X-ray luminosity. No\nsignificant correlation is seen between average optical variability properties\nand radio luminosity. The timescales of quasar fluctuations are suggestive of\naccretion disk instabilities. The relationships seen between variability,\nEddington ratio, and radio and X-ray emission are discussed in terms of a\npossible link between the behavior of quasars and black hole X-ray binaries.", "cat": "astro-ph.CO", "authors": ["Anne Bauer", "Charles Baltay", "Paolo Coppi", "Nancy Ellman", "Jonathan Jerke", "David Rabinowitz", "Richard Scalzo"]}, "1789": {"id": "2108.03640v2", "title": "Angular clustering properties of the DESI QSO target selection using DR9 Legacy Imaging Surveys", "url": "http://arxiv.org/pdf/2108.03640v2", "date": "2022-01-05 14:56:17", "abs": "The quasar target selection for the upcoming survey of the Dark Energy\nSpectroscopic Instrument (DESI) will be fixed for the next five years. The aim\nof this work is to validate the quasar selection by studying the impact of\nimaging systematics as well as stellar and galactic contaminants, and to\ndevelop a procedure to mitigate them. Density fluctuations of quasar targets\nare found to be related to photometric properties such as seeing and depth of\nthe Data Release 9 of the DESI Legacy Imaging Surveys. To model this complex\nrelation, we explore machine learning algorithms (Random Forest and Multi-Layer\nPerceptron) as an alternative to the standard linear regression. Splitting the\nfootprint of the Legacy Imaging Surveys into three regions according to\nphotometric properties, we perform an independent analysis in each region,\nvalidating our method using eBOSS EZ-mocks. The mitigation procedure is tested\nby comparing the angular correlation of the corrected target selection on each\nphotometric region to the angular correlation function obtained using quasars\nfrom the Sloan Digital Sky Survey (SDSS)Data Release 16. With our procedure, we\nrecover a similar level of correlation between DESI quasar targets and SDSS\nquasars in two thirds of the total footprint and we show that the excess of\ncorrelation in the remaining area is due to a stellar contamination which\nshould be removed with DESI spectroscopic data. We derive the Limber parameters\nin our three imaging regions and compare them to previous measurements from\nSDSS and the 2dF QSO Redshift Survey.", "cat": "astro-ph.CO", "authors": ["Edmond Chaussidon", "Christophe Y\u00e8che", "Nathalie Palanque-Delabrouille", "Arnaud de Mattia", "Adam D. Myers", "Mehdi Rezaie", "Ashley J. Ross", "Hee-Jong Seo", "David Brooks", "Enrique Gazta\u00f1aga", "Robert Kehoe", "Michael E. Levi", "Jeffrey A. Newman", "Gregory Tarl\u00e9", "Kai Zhang"]}, "1790": {"id": "2302.04549v1", "title": "Weakly Supervised Anomaly Detection: A Survey", "url": "http://arxiv.org/pdf/2302.04549v1", "date": "2023-02-09 10:27:21", "abs": "Anomaly detection (AD) is a crucial task in machine learning with various\napplications, such as detecting emerging diseases, identifying financial\nfrauds, and detecting fake news. However, obtaining complete, accurate, and\nprecise labels for AD tasks can be expensive and challenging due to the cost\nand difficulties in data annotation. To address this issue, researchers have\ndeveloped AD methods that can work with incomplete, inexact, and inaccurate\nsupervision, collectively summarized as weakly supervised anomaly detection\n(WSAD) methods. In this study, we present the first comprehensive survey of\nWSAD methods by categorizing them into the above three weak supervision\nsettings across four data modalities (i.e., tabular, graph, time-series, and\nimage/video data). For each setting, we provide formal definitions, key\nalgorithms, and potential future directions. To support future research, we\nconduct experiments on a selected setting and release the source code, along\nwith a collection of WSAD methods and data.", "cat": "cs.LG", "authors": ["Minqi Jiang", "Chaochuan Hou", "Ao Zheng", "Xiyang Hu", "Songqiao Han", "Hailiang Huang", "Xiangnan He", "Philip S. Yu", "Yue Zhao"]}, "1791": {"id": "2406.03806v1", "title": "Increasing the detectability of long-period and nulling pulsars in next-generation pulsar surveys", "url": "http://arxiv.org/pdf/2406.03806v1", "date": "2024-06-06 07:27:59", "abs": "Recent discoveries of multiple long-period pulsars (periods ${\\sim}10\\,$s or\nlarger) are starting to challenge the conventional notion that coherent radio\nemission cannot be produced by objects that are below the many theorised death\nlines. Many of the past pulsar surveys and software have been prone to\nselection effects that restricted their sensitivities towards long-period and\nsporadically-emitting objects. Pulsar surveys using new-generation\nlow-frequency facilities are starting to employ longer dwell times, which makes\nthem significantly more sensitive in detecting long-period or nulling pulsars.\nThere have also been software advancements to aid more sensitive searches\ntowards long-period objects. Furthermore, recent discoveries suggest that\nnulling may be a key aspect of the long-period pulsar population. We simulate\nboth long-period and nulling pulsar signals, using the Southern-sky MWA Rapid\nTwo-meter (SMART) survey data as reference, and explore the detection efficacy\nof popular search methods such as the fast Fourier transform (FFT),\nfast-folding algorithm (FFA) and single pulse search (SPS). For FFT-based\nsearch and SPS, we make use of the PRESTO implementation, and for FFA we use\nRIPTIDE. We find RIPTIDE's FFA to be more sensitive; however, it is also the\nslowest algorithm. PRESTO's FFT, although faster than others, also shows some\nunexpected inaccuracies in detection properties. SPS is highly sensitive to\nlong-period and nulling signals, but only for pulses with high intrinsic\nsignal-to-noise ratios. We use these findings to inform current and future\npulsar surveys that aim to uncover a large population of long-period or nulling\nobjects and comment on how to make optimal use of these methods in unison.", "cat": "astro-ph.HE", "authors": ["G. Grover", "N. D. R. Bhat", "S. J. McSweeney"]}, "1792": {"id": "1103.3000v1", "title": "The structure and dynamics of molecular gas in planet-forming zones: A CRIRES spectro-astrometric survey", "url": "http://arxiv.org/pdf/1103.3000v1", "date": "2011-03-15 19:32:40", "abs": "We present a spectro-astrometric survey of molecular gas in the inner regions\nof 16 protoplanetary disks using CRIRES, the high resolution infrared imaging\nspectrometer on the Very Large Telescope. Spectro-astrometry with CRIRES\nmeasures the spatial extent of line emission to sub-milliarcsecond precision,\nor <0.2 AU at the distance of the observed targets. The sample consists of\ngas-rich disks surrounding stars with spectral types ranging from K to A. The\nproperties of the spectro-astrometric signals divide the sources into two\ndistinct phenomenological classes: one that shows clear Keplerian astrometric\nspectra, and one in which the astrometric signatures are dominated by gas with\nstrong non-Keplerian (radial) motions. Similarly to the near-infrared continuum\nemission, as determined by interferometry, we find that the size of the CO line\nemitting region in the Keplerian sources obeys a size-luminosity relation as\n$R_CO L_*^0.5. The non-Keplerian spectro-astrometric signatures are likely\nindicative of the presence of wide-angle disk winds. The central feature of the\nwinds is a strong sub-Keplerian velocity field due to conservation of angular\nmomentum as the wind pressure drives the gas outwards. We construct a\nparametrized 2-dimensional disk+wind model that reproduces the observed\ncharacteristics the observed CO spectra and astrometry. The modeled winds\nindicate mass-loss rates of >10^-10 to 10^-8 Msol/yr. We suggest a unifying\nmodel in which all disks have slow molecular winds, but where the magnitude of\nthe mass-loss rate determines the degree to which the mid-infrared molecular\nlines are dominated by the wind relative to the Keplerian disk surface.", "cat": "astro-ph.EP", "authors": ["Klaus M. Pontoppidan", "Geoffrey A. Blake", "Alain Smette"]}, "1793": {"id": "1601.02630v1", "title": "The SCUBA-2 Cosmology Legacy Survey: Multi-wavelengths counterparts to 10$^3$ submillimeter galaxies in the UKIDSS-UDS field", "url": "http://arxiv.org/pdf/1601.02630v1", "date": "2016-01-11 21:00:10", "abs": "We present multiwavelength identifications for the counterparts of 1088\nsubmillimeter sources detected at 850$\\mu$m in the SCUBA-2 Cosmology Legacy\nSurvey study of the UKIDSS-UDS field. By utilising an ALMA pilot study on a\nsubset of our bright SCUBA-2 sample as a training set, along with the deep\noptical-near-infrared data available in this field, we develop a novel\ntechnique, Optical-IR Triple Color (OIRTC), using $z-K$, $K-[3.6]$,\n$[3.6]-[4.5]$ colors to select the candidate submillimeter galaxy (SMG)\ncounterparts. By combining radio identification and the OIRTC technique, we\nfind counterpart candidates for 80% of the Class = 1 $\\geq4\\,\\sigma$ SCUBA-2\nsample, defined as those that are covered by both radio and OIR imaging and the\nbase sample for our scientific analyses. Based on the ALMA training set, we\nexpect the accuracy of these identifications to be $82\\pm20$%, with a\ncompleteness of $69\\pm16$%, essentially as accurate as the traditional\n$p$-value technique but with higher completeness. We find that the fraction of\nSCUBA-2 sources having candidate counterparts is lower for fainter 850$\\mu$m\nsources, and we argue that for follow-up observations sensitive to SMGs with\n$S_{850}\\gtrsim 1$ mJy across the whole ALMA beam, the fraction with multiple\ncounterparts is likely to be $>40$% for SCUBA-2 sources at $S_{850} \\gtrsim 4$\nmJy. We find that the photometric redshift distribution for the SMGs is well\nfit by a lognormal distribution, with a median redshift of $z=2.3\\pm0.1$. After\naccounting for the sources without any radio and/or OIRTC counterpart, we\nestimate the median redshift to be $z=2.6\\pm0.1$ for SMGs with $S_{850} >1$\nmJy. We also use this new large sample to study the clustering of SMGs and the\nthe far-infrared properties of the unidentified submillimeter sources by\nstacking their Herschel SPIRE far-infrared emission.", "cat": "astro-ph.GA", "authors": ["Chian-Chou Chen", "Ian Smail", "Rob J. Ivison", "Vinodiran Arumugam", "Omar Almaini", "Christopher J. Conselice", "James E. Geach", "Will G. Hartley", "Cheng-Jiun Ma", "Alice Mortlock", "Chris Simpson", "James M. Simpson", "A. Mark Swinbank", "Itziar Aretxaga", "Andrew Blain", "Scott C. Chapman", "James S. Dunlop", "Duncan Farrah", "Mark Halpern", "Micha\u0142 J. Micha\u0142owski", "Paul van der Werf", "Aaron Wilkinson", "Jorge A. Zavala"]}, "1794": {"id": "2407.01576v1", "title": "The Future of Aerial Communications: A Survey of IRS-Enhanced UAV Communication Technologies", "url": "http://arxiv.org/pdf/2407.01576v1", "date": "2024-06-02 09:58:53", "abs": "The advent of Intelligent Reflecting Surfaces (IRS) and Unmanned Aerial\nVehicles (UAVs) is setting a new benchmark in the field of wireless\ncommunications. IRS, with their groundbreaking ability to manipulate\nelectromagnetic waves, have opened avenues for substantial enhancements in\nsignal quality, network efficiency, and spectral usage. These surfaces\ndynamically reconfigure the propagation environment, leading to optimized\nsignal paths and reduced interference. Concurrently, UAVs have emerged as\ndynamic, versatile elements within communication networks, offering high\nmobility and the ability to access and enhance coverage in areas where\ntraditional, fixed infrastructure falls short. This paper presents a\ncomprehensive survey on the synergistic integration of IRS and UAVs in wireless\nnetworks, highlighting how this innovative combination substantially boosts\nnetwork performance, particularly in terms of security, energy efficiency, and\nreliability. The versatility of UAVs, combined with the signal-manipulating\nprowess of IRS, creates a potent solution for overcoming the limitations of\nconventional communication setups, especially in challenging and underserved\nenvironments. Furthermore, the survey delves into the cutting-edge realm of\nMachine Learning (ML), exploring its role in the strategic deployment and\noperational optimization of UAVs equipped with IRS. The paper also underscores\nthe latest research and practical advancements in this field, providing\ninsights into real-world applications and experimental setups. It concludes by\ndiscussing the future prospects and potential directions for this emerging\ntechnology, positioning the IRS-UAV integration as a transformative force in\nthe landscape of next-generation wireless", "cat": "cs.RO", "authors": ["Zina Chkirbene", "Ala Gouissem", "Ridha Hamila", "Devrim Unal"]}, "1795": {"id": "0903.3239v1", "title": "The Santa Fe Light Cone Simulation Project: II. The Prospects for Direct Detection of the WHIM with SZE Surveys", "url": "http://arxiv.org/pdf/0903.3239v1", "date": "2009-03-18 20:53:57", "abs": "Detection of the Warm-Hot Intergalactic Medium (WHIM) using Sunyaev-Zeldovich\neffect (SZE) surveys is an intriguing possibility, and one that may allow\nobservers to quantify the amount of \"missing baryons\" in the WHIM phase. We\nestimate the necessary sensitivity for detecting low density WHIM gas with the\nSouth Pole Telescope (SPT) and Planck Surveyor for a synthetic 100 square\ndegree sky survey. This survey is generated from a very large, high dynamic\nrange adaptive mesh refinement cosmological simulation performed with the Enzo\ncode. We find that for a modest increase in the SPT survey sensitivity (a\nfactor of 2-4), the WHIM gas makes a detectable contribution to the integrated\nsky signal. For a Planck-like satellite, similar detections are possible with a\nmore significant increase in sensitivity (a factor of 8-10). We point out that\nfor the WHIM gas, the kinematic SZE signal can sometimes dominate the thermal\nSZE where the thermal SZE decrement is maximal (150 GHz), and that using the\ncombination of the two increases the chance of WHIM detection using SZE\nsurveys. However, we find no evidence of unique features in the thermal SZE\nangular power spectrum that may aid in its detection. Interestingly, there are\ndifferences in the power spectrum of the kinematic SZE, which may not allow us\nto detect the WHIM directly, but could be an important contaminant in\ncosmological analyses of the kSZE-derived velocity field. Corrections derived\nfrom numerical simulations may be necessary to account for this contamination.", "cat": "astro-ph.CO", "authors": ["Eric J. Hallman", "Brian W. O'Shea", "Britton D. Smith", "Jack O. Burns", "Michael L. Norman"]}, "1796": {"id": "2406.13801v1", "title": "A Census of the Deep Radio Sky with the VLA I: 10GHz Survey of the GOODS-N field", "url": "http://arxiv.org/pdf/2406.13801v1", "date": "2024-06-19 20:06:34", "abs": "We present the first high-resolution, high-frequency radio continuum survey\nthat fully maps an extragalactic deep field: the 10GHz survey of the Great\nObservatories Origins Deep Survey-North (GOODS-N) field. This is a Large\nProgram of the Karl G. Jansky Very Large Array that allocated 380 hours of\nobservations using the X-band ($8-12$GHz) receivers, leading to a 10GHz mosaic\nof the GOODS-field with an average rms noise $\\sigma_{\\rm n}=671\\,\\rm\nnJy\\,beam^{-1}$ and angular resolution $\\theta_{1/2}=0.22$arcsec across 297$\\rm\narcmin^2$. To maximize the brightness sensitivity we also produce a\nlow-resolution mosaic with $\\theta_{1/2}=1.0$arcsec and $\\sigma_{\\rm\nn}=968\\,\\rm nJy\\,beam^{-1}$, from which we derive our master catalog containing\n256 radio sources detected with peak signal-to-noise ratio $\\geq 5$. Radio\nsource size and flux density estimates from the high-resolution mosaic are\nprovided in the master catalog as well. The total fraction of spurious sources\nin the catalog is 0.75%. Monte Carlo simulations are performed to derive\ncompleteness corrections of the catalog. We find that the 10GHz radio source\ncounts in the GOODS-N field agree, in general, with predictions from numerical\nsimulations/models and expectations from 1.4 and 3GHz radio counts.", "cat": "astro-ph.GA", "authors": ["Eric F. Jim\u00e9nez-Andrade", "Eric J. Murphy", "Emmanuel Momjian", "James J. Condon", "Ranga-Ram Chary", "Russ Taylor", "Mark Dickinson"]}, "1797": {"id": "1603.02393v2", "title": "Microprocessor Optimizations for the Internet of Things: A Survey", "url": "http://arxiv.org/pdf/1603.02393v2", "date": "2018-02-20 19:42:53", "abs": "The Internet of Things (IoT) refers to a pervasive presence of interconnected\nand uniquely identifiable physical devices. These devices' goal is to gather\ndata and drive actions in order to improve productivity, and ultimately reduce\nor eliminate reliance on human intervention for data acquisition,\ninterpretation, and use. The proliferation of these connected low-power devices\nwill result in a data explosion that will significantly increase data\ntransmission costs with respect to energy consumption and latency. Edge\ncomputing reduces these costs by performing computations at the edge nodes,\nprior to data transmission, to interpret and/or utilize the data. While much\nresearch has focused on the IoT's connected nature and communication\nchallenges, the challenges of IoT embedded computing with respect to device\nmicroprocessors has received much less attention. This paper explores IoT\napplications' execution characteristics from a microarchitectural perspective\nand the microarchitectural characteristics that will enable efficient and\neffective edge computing. To tractably represent a wide variety of\nnext-generation IoT applications, we present a broad IoT application\nclassification methodology based on application functions, to enable quicker\nworkload characterizations for IoT microprocessors. We then survey and discuss\npotential microarchitectural optimizations and computing paradigms that will\nenable the design of right-provisioned microprocessors that are efficient,\nconfigurable, extensible, and scalable. This paper provides a foundation for\nthe analysis and design of a diverse set of microprocessor architectures for\nnext-generation IoT devices.", "cat": "cs.OH", "authors": ["Tosiron Adegbija", "Anita Rogacs", "Chandrakant Patel", "Ann Gordon-Ross"]}, "1798": {"id": "2407.17030v1", "title": "Applications of Multi-Agent Deep Reinforcement Learning Communication in Network Management: A Survey", "url": "http://arxiv.org/pdf/2407.17030v1", "date": "2024-07-24 06:19:30", "abs": "With the advancement of artificial intelligence technology, the automation of\nnetwork management, also known as Autonomous Driving Networks (ADN), is gaining\nwidespread attention. The network management has shifted from traditional\nhomogeneity and centralization to heterogeneity and decentralization.\nMulti-agent deep reinforcement learning (MADRL) allows agents to make decisions\nbased on local observations independently. This approach is in line with the\nneeds of automation and has garnered significant attention from academia and\nindustry. In a distributed environment, information interaction between agents\ncan effectively address the non-stationarity problem of multiple agents and\npromote cooperation. Therefore, in this survey, we first examined the\napplication of MADRL in network management, including specific application\nfields such as traffic engineering, wireless network access, power control, and\nnetwork security. Then, we conducted a detailed analysis of communication\nbehavior between agents, including communication schemes, communication content\nconstruction, communication object selection, message processing, and\ncommunication constraints. Finally, we discussed the open issues and future\nresearch directions of agent communication in MADRL for future network\nmanagement and ADN applications.", "cat": "cs.NI", "authors": ["Yue Pi", "Wang Zhang", "Yong Zhang", "Hairong Huang", "Baoquan Rao", "Yulong Ding", "Shuanghua Yang"]}, "1799": {"id": "1211.1972v1", "title": "Exoplanets from the Arctic: The First Wide-Field Survey at 80 Degrees North", "url": "http://arxiv.org/pdf/1211.1972v1", "date": "2012-11-08 21:00:01", "abs": "Located within 10 degrees of the North Pole, northern Ellesmere Island offers\ncontinuous darkness in the winter months. This capability can greatly enhance\nthe detection efficiency of planetary transit surveys and other time domain\nastronomy programs. We deployed two wide-field cameras at 80 degrees North,\nnear Eureka, Nunavut, for a 152-hour observing campaign in February 2012. The\n16-megapixel-camera systems were based on commercial f/1.2 lenses with 70mm and\n42mm apertures, and they continuously imaged 504 and 1,295 square degrees\nrespectively. In total, the cameras took over 44,000 images and produced\nbetter-than-1% precision light curves for approximately 10,000 stars. We\ndescribe a new high-speed astrometric and photometric data reduction pipeline\ndesigned for the systems, test several methods for the precision flat-fielding\nof images from very-wide-angle cameras, and evaluate the cameras' image\nqualities. We achieved a scintillation-limited photometric precision of 1-2% in\neach 10s exposure. Binning the short exposures into 10-min chunks provided a\nphotometric stability of 2-3 millimagnitudes, sufficient for the detection of\ntransiting exoplanets around the bright stars targeted by our survey. We\nestimate that the cameras, when operated over the full arctic winter, will be\ncapable of discovering several transiting exoplanets around bright (V<9) stars.", "cat": "astro-ph.EP", "authors": ["Nicholas M. Law", "Raymond Carlberg", "Pegah Salbi", "Wai-Hin Wayne Ngan", "Aida Ahmadi", "Eric Steinbring", "Richard Murowinski", "Suresh Sivanandam", "Wolfgang Kerzendorf"]}, "1800": {"id": "1905.03308v1", "title": "Submodular Optimization Problems and Greedy Strategies: A Survey", "url": "http://arxiv.org/pdf/1905.03308v1", "date": "2019-05-08 19:29:43", "abs": "The greedy strategy is an approximation algorithm to solve optimization\nproblems arising in decision making with multiple actions. How good is the\ngreedy strategy compared to the optimal solution? In this survey, we mainly\nconsider two classes of optimization problems where the objective function is\nsubmodular. The first is set submodular optimization, which is to choose a set\nof actions to optimize a set submodular objective function, and the second is\nstring submodular optimization, which is to choose an ordered set of actions to\noptimize a string submodular function. Our emphasis here is on performance\nbounds for the greedy strategy in submodular optimization problems.\nSpecifically, we review performance bounds for the greedy strategy, more\ngeneral and improved bounds in terms of curvature, performance bounds for the\nbatched greedy strategy, and performance bounds for Nash equilibria.", "cat": "math.OC", "authors": ["Yajing Liu", "Edwin K. P. Chong", "Ali Pezeshki", "Zhenliang Zhang"]}, "1801": {"id": "2107.10250v2", "title": "Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-selected clusters from Future CMB Surveys", "url": "http://arxiv.org/pdf/2107.10250v2", "date": "2021-12-28 07:48:38", "abs": "We forecast the number of galaxy clusters that can be detected via the\nthermal Sunyaev-Zeldovich (tSZ) signals by future cosmic microwave background\n(CMB) experiments, primarily the wide area survey of the CMB-S4 experiment but\nalso CMB-S4's smaller delensing survey and the proposed CMB-HD experiment. We\npredict that CMB-S4 will detect 75,000 clusters with its wide survey of $f_{\\rm\nsky}$ = 50% and 14,000 clusters with its deep survey of $f_{\\rm sky}$ = 3%. Of\nthese, approximately 1350 clusters will be at $z \\ge 2$, a regime that is\ndifficult to probe by optical or X-ray surveys. We assume CMB-HD will survey\nthe same sky as the S4-Wide{}, and find that CMB-HD will detect $\\times3$ more\noverall and an order of magnitude more $z \\ge 2$ clusters than CMB-S4. These\nresults include galactic and extragalactic foregrounds along with atmospheric\nand instrumental noise. Using CMB-cluster lensing to calibrate cluster tSZ-mass\nscaling relation, we combine cluster counts with primary CMB to obtain\ncosmological constraints for a two parameter extension of the standard model\n($\\Lambda CDM+\\sum m_{\\nu}+w_{0}$). Besides constraining $\\sigma(w_{0})$ to\n$\\lesssim 1\\%$, we find that both surveys can enable a $\\sim 2.5-4.5\\sigma$\ndetection of $\\sum m_{\\nu}$, substantially strengthening CMB-only constraints.\nWe also study the evolution of intracluster medium by modelling the cluster\nvirialization ${\\rm v}(z)$ and find tight constraints from CMB-S4, with further\nfactors of 3-4 improvement for CMB-HD. The binned cluster counts, Fisher\nmatrices, and other associated products can be downloaded from\nhttps://github.com/sriniraghunathan/tSZ_cluster_forecasts.", "cat": "astro-ph.CO", "authors": ["Srinivasan Raghunathan", "Nathan Whitehorn", "Marcelo A. Alvarez", "Han Aung", "Nicholas Battaglia", "Gilbert P. Holder", "Daisuke Nagai", "Elena Pierpaoli", "Christian L. Reichardt", "Joaquin D. Vieira"]}, "1802": {"id": "1907.07703v1", "title": "Sub-damped Lyman alpha systems in the XQ-100 survey I -- Identification and contribution to the cosmological HI budget", "url": "http://arxiv.org/pdf/1907.07703v1", "date": "2019-07-17 18:17:24", "abs": "Sub-damped Lyman alpha systems (subDLAs; HI column densities of\n19.0<=logN(HI)<20.3) are rarely included in the cosmic HI census performed at\nredshifts z>=1.5, yet are expected to contribute significantly to the overall\nHI mass budget of the Universe. In this paper, we present a blindly selected\nsample of 155 subDLAs found along 100 quasar sightlines (with a redshift path\nlength X=475) in the XQ-100 survey to investigate the contribution of subDLAs\nto the HI mass density of the Universe. The impact of X-Shooter's spectral\nresolution on sub-DLA identification is evaluated, and found to be sufficient\nfor reliably finding absorbers with logN(HI)>=18.9. We compared the\nimplications of searching for subDLAs solely using HI absorption versus the use\nof additional metal lines to confirm the identification, and found that\nmetal-selection techniques would have missed 75 subDLAs. Using a\nbootstrap-Monte Carlo simulation, we computed the column density distribution\nfunction (f(N,X)) and the cosmological HI mass density of subDLAs and compared\nwith our previous work based on the XQ-100 damped Lyman alpha systems. We do\nnot find any significant redshift evolution in f(N,X) or cosmological HI mass\ndensity for subDLAs. However, subDLAs contribute 10-20 per cent of the total\ncosmological HI mass density measured at redshifts 20.1 Gyr. We derived statistical ages\nand distances of field stars, and we separated them in thin and thick disc\npopulations. We studied the time evolution and dependence on metallicity of\nabundance ratios using open clusters and field stars. Using our large and\nhomogeneous sample of open clusters, thin and thick disc stars, spanning an age\nrange larger than 10 Gyr, we confirm an increase towards young ages of\ns-process abundances in the Solar neighbourhood. These trends are well defined\nfor open clusters and stars located nearby the solar position and they may be\nexplained by a late enrichment due to significant contribution to the\nproduction of these elements from long-living low-mass stars. At the same time,\nwe found a strong dependence of the s-process abundance ratios with the\nGalactocentric distance and with the metallicity of the clusters and field\nstars. Our results, derived from the largest and homogeneous sample of\ns-process abundances in the literature, confirm the growth with decreasing\nstellar ages of the s-process abundances in both field and open cluster stars.\nAt the same time, taking advantage of the abundances of open clusters located\nin a wide Galactocentric range, they open a new view on the dependence of the\ns-process evolution on the metallicity and star formation history, pointing to\ndifferent behaviours at various Galactocentric distances.", "cat": "astro-ph.GA", "authors": ["L. Magrini", "L. Spina", "S. Randich", "E. Friel", "G. Kordopatis", "C. Worley", "E. Pancino", "A. Bragaglia", "P. Donati", "G. Tautvaivsiene", "V. Bagdonas", "E. Delgado-Mena", "V. Adibekyan", "S. G. Sousa", "F. M. Jimenez-Esteban", "N. Sanna", "V. Roccatagliata", "R. Bonito", "L. Sbordone", "S. Duffau", "G. Gilmore", "S. Feltzing", "R. D. Jeffries", "A. Vallenari", "E. J. Alfaro", "T. Bensby", "P. Francois", "S. Koposov", "A. J. Korn", "A. Recio-Blanco", "R. Smiljanic", "A. Bayo", "G. Carraro", "A. R. Casey", "M. T. Costado", "F. Damiani", "E. Franciosini", "A. Frasca", "A. Hourihane", "P. Jofre", "P. de Laverny", "J. Lewis", "T. Masseron", "L. Monaco", "L. Morbidelli", "L. Prisinzano", "G. Sacco", "S. Zaggia"]}, "1804": {"id": "2309.11799v1", "title": "WALLABY Pre-Pilot Survey: Ultra-Diffuse Galaxies in the Eridanus Supergroup", "url": "http://arxiv.org/pdf/2309.11799v1", "date": "2023-09-21 06:11:21", "abs": "We present a pilot study of the atomic neutral hydrogen gas (HI) content of\nultra-diffuse galaxy (UDG) candidates. In this paper, we use the pre-pilot\nEridanus field data from the Widefield ASKAP L-band Legacy All-sky Blind Survey\n(WALLABY) to search for HI in UDG candidates found in the Systematically\nMeasuring Ultra-diffuse Galaxies survey (SMUDGes). We narrow down to 78 SMUDGes\nUDG candidates within the maximum radial extents of the Eridanus subgroups for\nthis study. Most SMUDGes UDGs candidates in this study have effective radii\nsmaller than 1.5 kpc and thus fail to meet the defining size threshold. We only\nfind one HI detection, which we classify as a low-surface-brightness dwarf. Six\nputative UDGs are HI-free. We show the overall distribution of SMUDGes UDG\ncandidates on the size-luminosity relation and compare them with low-mass\ndwarfs on the atomic gas fraction versus stellar mass scaling relation. There\nis no correlation between gas-richness and colour indicating that colour is not\nthe sole parameter determining their HI content. The evolutionary paths that\ndrive galaxy morphological changes and UDG formation channels are likely the\nadditional factors to affect the HI content of putative UDGs. The actual\nnumbers of UDGs for the Eridanus and NGC 1332 subgroups are consistent with the\npredicted abundance of UDGs and the halo virial mass relation, except for the\nNGC 1407 subgroup, which has a smaller number of UDGs than the predicted\nnumber. Different group environments suggest that these putative UDGs are\nlikely formed via the satellite accretion scenario.", "cat": "astro-ph.GA", "authors": ["B. -Q. For", "K. Spekkens", "L. Staveley-Smith", "K. Bekki", "A. Karunakaran", "B. Catinella", "B. S. Koribalski", "K. Lee-Waddell", "J. P. Madrid", "C. Murugeshan", "J. Rhee", "T. Westmeier", "O. I. Wong", "D. Zaritsky", "R. Donnerstein"]}, "1805": {"id": "2311.09680v5", "title": "Trustworthy Large Models in Vision: A Survey", "url": "http://arxiv.org/pdf/2311.09680v5", "date": "2024-02-01 05:15:52", "abs": "The rapid progress of Large Models (LMs) has recently revolutionized various\nfields of deep learning with remarkable grades, ranging from Natural Language\nProcessing (NLP) to Computer Vision (CV). However, LMs are increasingly\nchallenged and criticized by academia and industry due to their powerful\nperformance but untrustworthy behavior, which urgently needs to be alleviated\nby reliable methods. Despite the abundance of literature on trustworthy LMs in\nNLP, a systematic survey specifically delving into the trustworthiness of LMs\nin CV remains absent. In order to mitigate this gap, we summarize four relevant\nconcerns that obstruct the trustworthy usage in vision of LMs in this survey,\nincluding 1) human misuse, 2) vulnerability, 3) inherent issue and 4)\ninterpretability. By highlighting corresponding challenge, countermeasures, and\ndiscussion in each topic, we hope this survey will facilitate readers'\nunderstanding of this field, promote alignment of LMs with human expectations\nand enable trustworthy LMs to serve as welfare rather than disaster for human\nsociety.", "cat": "cs.CV", "authors": ["Ziyan Guo", "Li Xu", "Jun Liu"]}, "1806": {"id": "1704.06274v2", "title": "Kinematics of the local disk from the RAVE survey and the Gaia first data release", "url": "http://arxiv.org/pdf/1704.06274v2", "date": "2017-05-22 11:40:21", "abs": "We attempt to constrain the kinematics of the thin and thick disks using the\nBesancon population synthesis model together with RAVE DR4 and Gaia first data\nrelease (TGAS). The RAVE fields were simulated by applying a detailed target\nselection function and the kinematics was computed using velocity ellipsoids\ndepending on age in order to study the secular evolution. We accounted for the\nasymmetric drift computed from fitting a Stackel potential to orbits. Model\nparameters such as velocity dispersions, mean motions, and velocity gradients\nwere adjusted using an ABC-MCMC method. We made use of the metallicity to\nenhance the separation between thin and thick disks. We show that this model is\nable to reproduce the kinematics of the local disks in great detail. The disk\nfollows the expected secular evolution, in very good agreement with previous\nstudies of the thin disk. The new asymmetric drift formula, fitted to our\npreviously described St\\\"ackel potential, fairly well reproduces the velocity\ndistribution in a wide solar neighborhood. The U and W components of the solar\nmotion determined with this method agree well with previous studies. However,\nwe find a smaller V component than previously thought, essentially because we\ninclude the variation of the asymmetric drift with distance to the plane. The\nthick disk is represented by a long period of formation (at least 2 Gyr),\nduring which, as we show, the mean velocity increases with time while the scale\nheight and scale length decrease, very consistently with a collapse phase with\nconservation of angular momentum. This new Galactic dynamical model is able to\nreproduce the observed velocities in a wide solar neighborhood at the quality\nlevel of the TGAS-RAVE sample, allowing us to constrain the thin and thick disk\ndynamical evolution, as well as determining the solar motion.", "cat": "astro-ph.GA", "authors": ["Annie C. Robin", "Olivier Bienaym\u00e9", "Jos\u00e9 G. Fern\u00e1ndez-Trincado", "C\u00e9line Reyl\u00e9"]}, "1807": {"id": "2104.11092v1", "title": "Survey on Modeling Intensity Function of Hawkes Process Using Neural Models", "url": "http://arxiv.org/pdf/2104.11092v1", "date": "2021-04-22 14:23:38", "abs": "The event sequence of many diverse systems is represented as a sequence of\ndiscrete events in a continuous space. Examples of such an event sequence are\nearthquake aftershock events, financial transactions, e-commerce transactions,\nsocial network activity of a user, and the user's web search pattern. Finding\nsuch an intricate pattern helps discover which event will occur in the future\nand when it will occur. A Hawkes process is a mathematical tool used for\nmodeling such time series discrete events. Traditionally, the Hawkes process\nuses a critical component for modeling data as an intensity function with a\nparameterized kernel function. The Hawkes process's intensity function involves\ntwo components: the background intensity and the effect of events' history.\nHowever, such parameterized assumption can not capture future event\ncharacteristics using past events data precisely due to bias in modeling kernel\nfunction. This paper explores the recent advancement using novel deep\nlearning-based methods to model kernel function to remove such parametrized\nkernel function. In the end, we will give potential future research directions\nto improve modeling using the Hawkes process.", "cat": "cs.LG", "authors": ["Jayesh Malaviya"]}, "1808": {"id": "2112.03842v1", "title": "A Survey on Intrinsic Images: Delving Deep Into Lambert and Beyond", "url": "http://arxiv.org/pdf/2112.03842v1", "date": "2021-12-07 17:26:35", "abs": "Intrinsic imaging or intrinsic image decomposition has traditionally been\ndescribed as the problem of decomposing an image into two layers: a\nreflectance, the albedo invariant color of the material; and a shading,\nproduced by the interaction between light and geometry. Deep learning\ntechniques have been broadly applied in recent years to increase the accuracy\nof those separations. In this survey, we overview those results in context of\nwell-known intrinsic image data sets and relevant metrics used in the\nliterature, discussing their suitability to predict a desirable intrinsic image\ndecomposition. Although the Lambertian assumption is still a foundational basis\nfor many methods, we show that there is increasing awareness on the potential\nof more sophisticated physically-principled components of the image formation\nprocess, that is, optically accurate material models and geometry, and more\ncomplete inverse light transport estimations. We classify these methods in\nterms of the type of decomposition, considering the priors and models used, as\nwell as the learning architecture and methodology driving the decomposition\nprocess. We also provide insights about future directions for research, given\nthe recent advances in neural, inverse and differentiable rendering techniques.", "cat": "cs.CV", "authors": ["Elena Garces", "Carlos Rodriguez-Pardo", "Dan Casas", "Jorge Lopez-Moreno"]}, "1809": {"id": "0904.3459v1", "title": "XMM-Newton observations of Seyfert galaxies from the Palomar spectroscopic survey: the X-ray absorption distribution", "url": "http://arxiv.org/pdf/0904.3459v1", "date": "2009-04-22 13:17:31", "abs": "We present XMM-Newton spectral analysis of all 38 Seyfert galaxies from the\nPalomar spectroscopic sample of galaxies. These are found at distances of up to\n67 Mpc and cover the absorbed 2-10 keV luminosity range ~10^38-10^43 ergs/s.\nOur aim is to determine the distribution of the X-ray absorption in the local\nUniverse. Three of these are Compton-thick with column densities just above\n10^24 cm^-2 and high equivalent width FeKa lines (>700 eV). Five more sources\nhave low values of the X-ray to [OIII] flux ratio suggesting that they could be\nassociated with obscured nuclei. Their individual spectra show neither high\nabsorbing columns nor flat spectral indices. However, their stacked spectrum\nreveals an absorbing column density of N_H~10^23 cm^-2. Therefore the fraction\nof absorbed sources (>10^22 cm^-2 could be as high as 55+/-12%. A number of\nSeyfert-2 appear to host unabsorbed nuclei. These are associated with\nlow-luminosity sources Lx < 3x10^41 ergs/s. Their stacked spectrum again shows\nno absorption while inspection of the \\chandra images, where available, shows\nthat contamination from nearby sources does not affect the {\\it XMM-Newton}\nspectra in most cases. Nevertheless, such low luminosity sources are not\ncontributing significantly to the X-ray background flux. When we consider only\nthe brighter, $>10^{41}$ \\lunits, 21 sources, we find that the fraction of\nabsorbed nuclei rises to $75\\pm19 $ % while that of Compton-thick sources to\n15-20%. The fraction of Compton-thick AGN is lower than that predicted by the\nX-ray background synthesis model in the same luminosity and redshift range.}", "cat": "astro-ph.CO", "authors": ["A. Akylas", "I. Georgantopoulos"]}, "1810": {"id": "2403.07078v1", "title": "Improving deep learning with prior knowledge and cognitive models: A survey on enhancing explainability, adversarial robustness and zero-shot learning", "url": "http://arxiv.org/pdf/2403.07078v1", "date": "2024-03-11 18:11:00", "abs": "We review current and emerging knowledge-informed and brain-inspired\ncognitive systems for realizing adversarial defenses, eXplainable Artificial\nIntelligence (XAI), and zero-shot or few-short learning. Data-driven deep\nlearning models have achieved remarkable performance and demonstrated\ncapabilities surpassing human experts in many applications. Yet, their\ninability to exploit domain knowledge leads to serious performance limitations\nin practical applications. In particular, deep learning systems are exposed to\nadversarial attacks, which can trick them into making glaringly incorrect\ndecisions. Moreover, complex data-driven models typically lack interpretability\nor explainability, i.e., their decisions cannot be understood by human\nsubjects. Furthermore, models are usually trained on standard datasets with a\nclosed-world assumption. Hence, they struggle to generalize to unseen cases\nduring inference in practical open-world environments, thus, raising the zero-\nor few-shot generalization problem. Although many conventional solutions exist,\nexplicit domain knowledge, brain-inspired neural network and cognitive\narchitectures offer powerful new dimensions towards alleviating these problems.\nPrior knowledge is represented in appropriate forms and incorporated in deep\nlearning frameworks to improve performance. Brain-inspired cognition methods\nuse computational models that mimic the human mind to enhance intelligent\nbehavior in artificial agents and autonomous robots. Ultimately, these models\nachieve better explainability, higher adversarial robustness and data-efficient\nlearning, and can, in turn, provide insights for cognitive science and\nneuroscience-that is, to deepen human understanding on how the brain works in\ngeneral, and how it handles these problems.", "cat": "cs.LG", "authors": ["Fuseinin Mumuni", "Alhassan Mumuni"]}, "1811": {"id": "2101.02039v1", "title": "A survey of the European Union's artificial intelligence ecosystem", "url": "http://arxiv.org/pdf/2101.02039v1", "date": "2020-12-28 18:51:05", "abs": "Compared to other global powers, the European Union (EU) is rarely considered\na leading player in the development of artificial intelligence (AI). Why is\nthis, and does this in fact accurately reflect the activities of the EU? What\nwould it take for the EU to take a more leading role in AI? This report surveys\ncore components of the current AI ecosystem of the EU, providing the crucial\nbackground context for answering these questions.", "cat": "cs.CY", "authors": ["Charlotte Stix"]}, "1812": {"id": "2207.10574v2", "title": "Co-Located Human-Human Interaction Analysis using Nonverbal Cues: A Survey", "url": "http://arxiv.org/pdf/2207.10574v2", "date": "2023-10-04 07:52:19", "abs": "Automated co-located human-human interaction analysis has been addressed by\nthe use of nonverbal communication as measurable evidence of social and\npsychological phenomena. We survey the computing studies (since 2010) detecting\nphenomena related to social traits (e.g., leadership, dominance, personality\ntraits), social roles/relations, and interaction dynamics (e.g., group\ncohesion, engagement, rapport). Our target is to identify the nonverbal cues\nand computational methodologies resulting in effective performance. This survey\ndiffers from its counterparts by involving the widest spectrum of social\nphenomena and interaction settings (free-standing conversations, meetings,\ndyads, and crowds). We also present a comprehensive summary of the related\ndatasets and outline future research directions which are regarding the\nimplementation of artificial intelligence, dataset curation, and\nprivacy-preserving interaction analysis. Some major observations are: the most\noften used nonverbal cue, computational method, interaction environment, and\nsensing approach are speaking activity, support vector machines, and meetings\ncomposed of 3-4 persons equipped with microphones and cameras, respectively;\nmultimodal features are prominently performing better; deep learning\narchitectures showed improved performance in overall, but there exist many\nphenomena whose detection has never been implemented through deep models. We\nalso identified several limitations such as the lack of scalable benchmarks,\nannotation reliability tests, cross-dataset experiments, and explainability\nanalysis.", "cat": "cs.HC", "authors": ["Cigdem Beyan", "Alessandro Vinciarelli", "Alessio Del Bue"]}, "1813": {"id": "1801.03181v3", "title": "The Dark Energy Survey Data Release 1", "url": "http://arxiv.org/pdf/1801.03181v3", "date": "2019-04-23 14:53:02", "abs": "We describe the first public data release of the Dark Energy Survey, DES DR1,\nconsisting of reduced single epoch images, coadded images, coadded source\ncatalogs, and associated products and services assembled over the first three\nyears of DES science operations. DES DR1 is based on optical/near-infrared\nimaging from 345 distinct nights (August 2013 to February 2016) by the Dark\nEnergy Camera mounted on the 4-m Blanco telescope at Cerro Tololo\nInter-American Observatory in Chile. We release data from the DES wide-area\nsurvey covering ~5,000 sq. deg. of the southern Galactic cap in five broad\nphotometric bands, grizY. DES DR1 has a median delivered point-spread function\nof g = 1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.90 arcsec FWHM, a\nphotometric precision of < 1% in all bands, and an astrometric precision of 151\nmas. The median coadded catalog depth for a 1.95\" diameter aperture at S/N = 10\nis g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 mag. DES DR1\nincludes nearly 400M distinct astronomical objects detected in ~10,000 coadd\ntiles of size 0.534 sq. deg. produced from ~39,000 individual exposures.\nBenchmark galaxy and stellar samples contain ~310M and ~ 80M objects,\nrespectively, following a basic object quality selection. These data are\naccessible through a range of interfaces, including query web clients, image\ncutout servers, jupyter notebooks, and an interactive coadd image visualization\ntool. DES DR1 constitutes the largest photometric data set to date at the\nachieved depth and photometric precision.", "cat": "astro-ph.IM", "authors": ["T. M. C. Abbott", "F. B. Abdalla", "S. Allam", "A. Amara", "J. Annis", "J. Asorey", "S. Avila", "O. Ballester", "M. Banerji", "W. Barkhouse", "L. Baruah", "M. Baumer", "K. Bechtol", "M . R. Becker", "A. Benoit-L\u00e9vy", "G. M. Bernstein", "E. Bertin", "J. Blazek", "S. Bocquet", "D. Brooks", "D. Brout", "E. Buckley-Geer", "D. L. Burke", "V. Busti", "R. Campisano", "L. Cardiel-Sas", "A. C arnero Rosell", "M. Carrasco Kind", "J. Carretero", "F. J. Castander", "R. Cawthon", "C. Chang", "X. Chen", "C. Conselice", "G. Costa", "M. Crocce", "C. E. Cunha", "C. B. D'Andrea", "L. N. da Costa", "R. Das", "G. Daues", "T. M. Davis", "C. Davis", "J. De Vicente", "D. L. DePoy", "J. DeRose", "S. Desai", "H. T. Diehl", "J. P. Dietrich", "S. Dodelson", "P. Doel", "A. Drlica-Wagner", "T. F. Eifler", "A. E. Elliott", "A. E. Evrard", "A. Farahi", "A. Fausti Neto", "E. Fernandez", "D. A. Finley", "M. Fitzpatrick", "B. Flaugher", "R. J. Foley", "P. Fosalba", "D. N. Friedel", "J. Frieman", "J. Garc\u00eda-Bellido", "E. Gaz tanaga", "D. W. Gerdes", "T. Giannantonio", "M. S. S. Gill", "K. Glazebrook", "D. A. Goldstein", "M. Gower", "D. Gruen", "R. A. Gruendl", "J. Gschwend", "R. R. Gupta", "G. Gutierrez", "S. Hamilton", "W. G. Hartley", "S. R. Hinton", "J. M. Hislop", "D. Hollowood", "K. Honscheid", "B. Hoyle", "D. Huterer", "B. Jain", "D. J. James", "T. Jeltema", "M. W. G. Johnson", "M. D. Johnson", "S. Juneau", "T. Kacprzak", "S. Kent", "G. Khullar", "M. Klein", "A. Kovacs", "A. M. G. Koziol", "E. Krause", "A. Kremin", "R. Kron", "K. Kuehn", "S. Kuhlmann", "N. Kuropatkin", "O. Lahav", "J. Lasker", "T. S. Li", "R. T. Li", "A. R. Liddle", "M. Lima", "H. Lin", "P. L\u00f3pez-Reyes", "N. MacCrann", "M. A. G. Maia", "J. D. Maloney", "M. Manera", "M. March", "J. Marriner", "J. L. Marshall", "P. Martini", "T. McClintock", "T. McKay", "R . G. McMahon", "P. Melchior", "F. Menanteau", "C. J. Miller", "R. Miquel", "J. J. Mohr", "E. Morganson", "J. Mould", "E. Neilsen", "R. C. Nichol", "D. Nidever", "R. Nikutta", "F. Nogueira", "B. Nord", "P. Nugent", "L. Nunes", "R. L. C. Ogando", "L. Old", "K. Olsen", "A. B. Pace", "A. Palmese", "F. Paz-Chinch\u00f3n", "H. V. Peiris", "W. J. Percival", "D. Petravick", "A. A. Plazas", "J. Poh", "C. Pond", "A. Por redon", "A. Pujol", "A. Refregier", "K. Reil", "P. M. Ricker", "R. P. Rollins", "A. K. Romer", "A. Roodman", "P. Rooney", "A. J. Ross", "E. S. Rykoff", "M. Sako", "E. Sanchez", "M. L. Sanchez", "B. Santiago", "A. Saro", "V. Scarpine", "D. Scolnic", "A. Scott", "S. Serrano", "I. Sevilla-Noarbe", "E. Sheldon", "N. Shipp", "M. L. Silveira", "R. C. Smith", "J. A. Smith", "M. Smith", "M. Soares-Santos", "F. Sobre ira", "J. Song", "A. Stebbins", "E. Suchyta", "M. Sullivan", "M. E. C. Swanson", "G. Tarle", "J. Thaler", "D. Thomas", "R. C. Thomas", "M. A. Troxel", "D. L. Tucker", "V. Vikram", "A. K. Vivas", "A. R. Wal ker", "R. H. Wechsler", "J. Weller", "W. Wester", "R. C. Wolf", "H. Wu", "B. Yanny", "A. Zenteno", "Y. Zhang", "J. Zuntz"]}, "1814": {"id": "1505.07423v1", "title": "Halpha3: an Halpha imaging survey of HI selected galaxies from ALFALFA. V: The Coma Supercluster survey completion", "url": "http://arxiv.org/pdf/1505.07423v1", "date": "2015-05-27 18:09:16", "abs": "Neutral hydrogen represents the major observable baryonic constituent of\ngalaxies that fuels the formation of stars through the transformation in\nmolecular hydrogen. The emission of the hydrogen recombination line Halpha is\nthe most direct tracer of the process that transforms gas (fuel) into stars. We\ncontinue to present Halpha3 (acronym for Halpha-alpha-alpha), an extensive\nHalpha+[NII] narrow-band imaging campaign of galaxies selected from the HI\nArecibo Legacy Fast ALFA Survey (ALFALFA), using the instrumentation available\nat the San Pedro Martir observatory (Mexico). In only four years since 2011 we\nwere able to complete in 48 nights the Halpha imaging observations of 724\ngalaxies in the region of the Coma supercluster 10^h < R.A. <16^h; 24^o < Dec.\n<28^o and 3900 -0.5 and 1.2 +/- 0.2 % have\nalpha > 0. By combining this spectral index distribution with 1.4 GHz source\ncounts we predict 31 GHz source counts in the range 1 mJy < S_31 < 4 mJy,\nN(>S_31) = (16.7 +/- 1.7) deg^2 (S_31/1 mJy)^(-0.80 +/- 0.07). We also assess\nthe contribution of mJy-level (S_1.4 < 3.4 mJy) radio sources to the 31 GHz CMB\npower spectrum, finding a mean power of ell (ell+1) C^src_ell/(2 pi) = 44 +/-\n14 micro-Kelvin^2 and a 95% upper limit of 80 micro-Kelvin^2 at ell = 2500.\nIncluding an estimated contribution of 12 micro-Kelvin^2 from the population of\nsources responsible for the turn-up in counts below S_1.4 = 1 mJy this amounts\nto 21 +/- 7 % of what is needed to explain the CBI high-ell excess signal, 275\n+/- 63 micro-Kelvin^2. These results are consistent with other measurements of\nthe 31 GHz point source foreground.", "cat": "astro-ph.CO", "authors": ["B. S. Mason", "L. C. Weintraub", "J. L. Sievers", "J. R. Bond", "S. T. Myers", "T. J. Pearson", "A. C. S. Readhead", "M. C. Shepherd"]}, "1828": {"id": "1802.00878v1", "title": "DECam Survey for Low-Mass Stars and Substellar Objects in the UCL and LCC Subgroups of the Sco-Cen OB Association (SCOCENSUS)", "url": "http://arxiv.org/pdf/1802.00878v1", "date": "2018-02-02 23:42:59", "abs": "Using images taken with the Dark Energy Camera (DECam), the first extensive\nsurvey of low mass and substellar objects is made in the 15-20 Myr Upper\nCentaurus Lupus (UCL) and Lower Centaurus Crux (LCC) subgroups of the Scorpius\nCentaurus OB Association (Sco-Cen). Due to the size of our dataset (>2Tb) we\ndeveloped an extensive open source set of python libraries to reduce our\nimages, including astrometry, coaddition, and PSF photometry. Our survey\nconsists of 29$\\times$3 deg$^2$ fields in the UCL and LCC subgroups of Sco-Cen\nand the creation of a catalog with over 11 million point sources. We create a\nprioritized list of candidate for members in UCL and LCC, with 118 \\emph{best}\nand another 348 \\emph{good} candidates. We show that the luminosity and mass\nfunctions of our low mass and substellar candidates are consistent with\nmeasurements for the younger Upper Scorpius subgroup and estimates of a\nuniversal IMF, with spectral types ranging from M1 down to L1.", "cat": "astro-ph.SR", "authors": ["Fred E. Moolekamp", "Eric E. Mamajek", "David J. James", "Kevin L. Luhman", "Mark J. Pecaut", "Stanmir A. Metchev", "Cameron P. M. Bell", "Sara R. Denbo"]}, "1829": {"id": "1609.08690v1", "title": "Large collaboration in observational astronomy: the Gemini Planet Imager exoplanet survey case", "url": "http://arxiv.org/pdf/1609.08690v1", "date": "2016-09-27 22:20:18", "abs": "The Gemini Planet Imager (GPI) is a next-generation high-contrast imager\nbuilt for the Gemini Observatory. The GPI exoplanet survey (GPIES) consortium\nis made up of 102 researchers from 28 institutions in North and South America\nand Europe. In November 2014, we launched a search for young Jovian planets and\ndebris disks. In this paper, we discuss how we have coordinated the work done\nby this large team to improve the technical and scientific productivity of the\ncampaign, and describe lessons we have learned that could be useful for future\ninstrumentation-based astronomical surveys. The success of GPIES lies mostly on\nits decentralized structure, clear definition of policies that are signed by\neach member, and the heavy use of modern tools for communicating, exchanging\ninformation, and processing data.", "cat": "astro-ph.IM", "authors": ["Franck Marchis", "Paul G. Kalas", "Marshall D. Perrin", "Quinn M. Konopacky", "Dmitry Savransky", "Bruce Macintosh", "Christian Marois", "James R. Graham"]}, "1830": {"id": "1504.07051v3", "title": "The XMM-Newton serendipitous survey. VII. The third XMM-Newton serendipitous source catalogue", "url": "http://arxiv.org/pdf/1504.07051v3", "date": "2016-02-09 09:52:49", "abs": "Thanks to the large collecting area (3 x ~1500 cm$^2$ at 1.5 keV) and wide\nfield of view (30' across in full field mode) of the X-ray cameras on board the\nEuropean Space Agency X-ray observatory XMM-Newton, each individual pointing\ncan result in the detection of hundreds of X-ray sources, most of which are\nnewly discovered. Recently, many improvements in the XMM-Newton data reduction\nalgorithms have been made. These include enhanced source characterisation and\nreduced spurious source detections, refined astrometric precision, greater net\nsensitivity and the extraction of spectra and time series for fainter sources,\nwith better signal-to-noise. Further, almost 50\\% more observations are in the\npublic domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science\nCentre (XMM-SSC) to produce a much larger and better quality X-ray source\ncatalogue. The XMM-SSC has developed a pipeline to reduce the XMM-Newton data\nautomatically and using improved calibration a new catalogue version has been\nproduced from XMM-Newton data made public by 2013 Dec. 31 (13 years of data).\nManual screening ensures the highest data quality. This catalogue is known as\n3XMM. In the latest release, 3XMM-DR5, there are 565962 X-ray detections\ncomprising 396910 unique X-ray sources. For the 133000 brightest sources,\nspectra and lightcurves are provided. For all detections, the positions on the\nsky, a measure of the quality of the detection, and an evaluation of the X-ray\nvariability is provided, along with the fluxes and count rates in 7 X-ray\nenergy bands, the total 0.2-12 keV band counts, and four hardness ratios. To\nidentify the detections, a cross correlation with 228 catalogues is also\nprovided for each X-ray detection. 3XMM-DR5 is the largest X-ray source\ncatalogue ever produced. Thanks to the large array of data products, it is an\nexcellent resource in which to find new and extreme objects.", "cat": "astro-ph.HE", "authors": ["S. R. Rosen", "N. A. Webb", "M. G. Watson", "J. Ballet", "D. Barret", "V. Braito", "F. J. Carrera", "M. T. Ceballos", "M. Coriat", "R. Della Ceca", "G. Denkinson", "P. Esquej", "S. A. Farrell", "M. Freyberg", "F. Gris\u00e9", "P. Guillout", "L. Heil", "F. Koliopanos", "D. Law-Green", "G. Lamer", "D. Lin", "R. Martino", "L. Michel", "C. Motch", "A. Nebot Gomez-Moran", "C. G. Page", "K. Page", "M. Page", "M. W. Pakull", "J. Pye", "A. Read", "P. Rodriguez", "M. Sakano", "R. Saxton", "A. Schwope", "A. E. Scott", "R. Sturm", "I. Traulsen", "V. Yershov", "I. Zolotukhin"]}, "1831": {"id": "1710.03773v1", "title": "The MUSE Hubble Ultra Deep Field Survey: II. Spectroscopic redshifts and comparisons to color selections of high-redshift galaxies", "url": "http://arxiv.org/pdf/1710.03773v1", "date": "2017-10-10 18:16:07", "abs": "We have conducted a two-layered spectroscopic survey (1'x1' ultra deep and\n3'x3' deep regions) in the Hubble Ultra Deep Field (HUDF) with the Multi Unit\nSpectroscopic Explorer (MUSE). The combination of a large field of view, high\nsensitivity, and wide wavelength coverage provides an order of magnitude\nimprovement in spectroscopically confirmed redshifts in the HUDF; i.e., 1206\nsecure spectroscopic redshifts for HST continuum selected objects, which\ncorresponds to 15% of the total (7904). The redshift distribution extends well\nbeyond z>3 and to HST/F775W magnitudes as faint as ~30 mag (AB, 1-sigma). In\naddition, 132 secure redshifts were obtained for sources with no HST\ncounterparts that were discovered in the MUSE data cubes by a blind search for\nemission-line features. In total, we present 1338 high quality redshifts, which\nis a factor of eight increase compared with the previously known spectroscopic\nredshifts in the same field. We assessed redshifts mainly with the spectral\nfeatures [OII] at z<1.5 (473 objects) and Lya at 2.9~20% up to\n28-29 mag and ~27 mag, respectively. We used the determined redshifts to test\ncontinuum color selection (dropout) diagrams of high-z galaxies. The selection\ncondition for F336W dropouts successfully captures ~80% of the targeted z~2.7\ngalaxies. However, for higher redshift selections (F435W, F606W, and F775W\ndropouts), the success rates decrease to ~20-40%. We empirically redefine the\nselection boundaries to make an attempt to improve them to ~60%. The revised\nboundaries allow bluer colors that capture Lya emitters with high Lya\nequivalent widths falling in the broadbands used for the color-color selection.\nAlong with this paper, we release the redshift and line flux catalog.", "cat": "astro-ph.GA", "authors": ["H. Inami", "R. Bacon", "J. Brinchmann", "J. Richard", "T. Contini", "S. Conseil", "S. Hamer", "M. Akhlaghi", "N. Bouche", "B. Clement", "G. Desprez", "A. B. Drake", "T. Hashimoto", "F. Leclercq", "M. Maseda", "L. Michel-Dansac", "M. Paalvast", "L. Tresse", "E. Ventou", "W. Kollatschny", "L. A. Boogaard", "H. Finley", "R. A. Marino", "J. Schaye", "L. Wisotzki"]}, "1832": {"id": "1502.02460v1", "title": "A skewer survey of the Galactic halo from deep CFHT and INT images", "url": "http://arxiv.org/pdf/1502.02460v1", "date": "2015-02-09 12:32:46", "abs": "We study the density profile and shape of the Galactic halo using deep\nmulticolour images from the MENeaCS and CCCP projects, over 33 fields selected\nto avoid overlap with the Galactic plane. Using multicolour selection and PSF\nhomogenization techniques we obtain catalogues of F stars (near-main sequence\nturnoff stars) out to Galactocentric distances up to 60kpc. Grouping nearby\nlines of sight, we construct the stellar density profiles through the halo in\neight different directions by means of photometric parallaxes. Smooth halo\nmodels are then fitted to these profiles. We find clear evidence for a\nsteepening of the density profile power law index around R=20 kpc, from -2.50\n+- 0.04 to -4.85 +- 0.04, and for a flattening of the halo towards the poles\nwith best-fit axis ratio 0.63 +- 0.02. Furthermore, we cannot rule out a mild\ntriaxiality (w>=0.8). We recover the signatures of well-known substructure and\nstreams that intersect our lines of sight. These results are consistent with\nthose derived from wider but shallower surveys, and augur well for upcoming,\nwide-field surveys of comparable depth to our pencil beam surveys.", "cat": "astro-ph.GA", "authors": ["B. Pila-D\u00edez", "J. T. A. de Jong", "K. Kuijken", "R. F. J. van der Burg", "H. Hoekstra"]}, "1833": {"id": "2208.06625v1", "title": "Airborne Radiometric Surveys and Machine Learning Algorithms for Revealing Soil Texture", "url": "http://arxiv.org/pdf/2208.06625v1", "date": "2022-08-13 11:04:49", "abs": "Soil texture is key information in agriculture for improving soil knowledge\nand crop performance, so the accurate mapping of this crucial feature is\nimperative for rationally planning cultivations and for targeting\ninterventions. We studied the relationship between radioelements and soil\ntexture in the Mezzano Lowland (Italy), a 189 $km^2$ agricultural plain\ninvestigated through a ded-icated airborne gamma-ray spectroscopy survey. The K\nand Th abundances were used to retrieve the clay and sand content by means of a\nmulti-approach method. Linear (simple and multiple) and non-linear (machine\nlearning algorithms with deep neural networks) predictive models were trained\nand tested adopting a 1:50,000 scale soil texture map. The comparison of these\napproaches highlighted that the non-linear model introduces significant\nimprovements in the prediction of soil texture fractions. The predicted maps of\nthe clay and of the sand content were compared with the regional soil maps.\nAlthough the macro-structures were equally present, the airborne gam-ma-ray\ndata permits us shedding light on finer features. Map areas with higher clay\ncontent were coincident with paleo-channels crossing the Mezzano Lowland in\nEtruscan and Roman periods, confirmed by the hydrographic setting of historical\nmaps and by the geo-morphological features of the study area.", "cat": "physics.geo-ph", "authors": ["Andrea Maino", "Matteo Alberi", "Emiliano Anceschi", "Enrico Chiarelli", "Luca Cicala", "Tommaso Colonna", "Mario De Cesare", "Enrico Guastaldi", "Nicola Lopane", "Fabio Mantovani", "Maurizio Marcialis", "Nicola Martini", "Michele Montuschi", "Silvia Piccioli", "Kassandra Giulia Cristina Raptis", "Antonio Russo", "Filippo Semenza", "Virginia Strati"]}, "1834": {"id": "1102.3193v2", "title": "White Dwarfs in the SuperCOSMOS Sky Survey: the Thin Disk, Thick Disk and Spheroid Luminosity Functions", "url": "http://arxiv.org/pdf/1102.3193v2", "date": "2011-04-20 08:41:54", "abs": "We present a magnitude and proper motion limited catalogue of ~10,000 white\ndwarf candidates, obtained from the SuperCOSMOS Sky Survey by means of reduced\nproper motion selection. This catalogue extends to magnitudes r~19.75 and\nproper motions as low as mu ~0.05\"/yr, and covers nearly three quarters of the\nsky. Photometric parallaxes provide distance estimates accurate to ~50%. This\ncatalogue is used to measure the luminosity functions for disk and spheroid\nwhite dwarfs, using strict velocity cuts to isolate subsamples belonging to\neach population. Disk luminosity functions measured in this manner are really a\nconglomerate of thin and thick disk objects, due to the significant velocity\noverlap between these populations. We introduce a new statistical approach to\nthe stellar luminosity function for nearby objects that succesfully untangles\nthe contributions from the different kinematic populations, without the need\nfor stringent velocity cuts. This improves the statistical power by allowing\nall stars to contribute to the luminosity function, even at tangential\nvelocities where the populations are indistinguishable. This method is\nparticularly suited to white dwarfs, for which population discrimination by\nchemical tagging is not possible. We use this technique to obtain the first\nmeasurement of the thick disk white dwarf luminosity function, while also\nimproving constraint on both the thin disk and spheroid luminosity functions.\nWe find that the thin disk, thick disk and spheroid populations contribute to\nthe local white dwarf density in roughly 79%/16%/5% proportions.", "cat": "astro-ph.GA", "authors": ["Nicholas Rowell", "Nigel Hambly"]}, "1835": {"id": "1907.02491v1", "title": "An International Survey of Front-End Receivers and Observing Performance of Telescopes for Radio Astronomy", "url": "http://arxiv.org/pdf/1907.02491v1", "date": "2019-07-04 17:04:21", "abs": "This paper presents a survey of microwave front-end receivers installed at\nradio telescopes throughout the World. This unprecedented analysis was\nconducted as part of a review of front-end developments for Italian radio\ntelescopes, initiated by the Italian National Institute for Astrophysics in\n2016. Fifteen international radio telescopes have been selected to be\nrepresentative of the instrumentation used for radio astronomical observations\nin the frequency domain from 300 MHz to 116 GHz. A comprehensive description of\nthe existing receivers is presented and their characteristics are compared and\ndiscussed. The observing performances of the complete receiving chains are also\npresented. An overview of on-going developments illustrates and anticipates\nfuture trends in front-end projects to meet the most ambitious scientific\nresearch goals.", "cat": "astro-ph.IM", "authors": ["P. Bolli", "A. Orfei", "A. Zanichelli", "R. Prestage", "S. J. Tingay", "M. Beltr\u00e1n", "M. Burgay", "C. Contavalle", "M. Honma", "A. Kraus", "M. Lindqvist", "J. Lopez Perez", "P. Marongiu", "T. Minamidani", "S. Navarro", "T. Pisanu", "Z. -Q. Shen", "B. W. Sohn", "C. Stanghellini", "T. Tzioumis", "G. Zacchiroli"]}, "1836": {"id": "2001.09584v1", "title": "Gravitational microlensing events from the first year of the northern Galactic plane survey by the Zwicky Transient Facility", "url": "http://arxiv.org/pdf/2001.09584v1", "date": "2020-01-27 04:37:06", "abs": "The Zwicky Transient Facility (ZTF) is currently surveying the entire\nnorthern sky, including dense Galactic plane fields. Here, we present\npreliminary results of the search for gravitational microlensing events in the\nZTF data collected from the beginning of the survey (March 20, 2018) through\nJune 30, 2019.", "cat": "astro-ph.SR", "authors": ["P. Mroz", "R. A. Street", "E. Bachelet", "E. O. Ofek", "E. C. Bellm", "R. Dekany", "D. A. Duev", "A. Gal-Yam", "M. J. Graham", "F. J. Masci", "M. Porter", "B. Rusholme", "R. M. Smith", "M. T. Soumagnac", "J. Zolkower"]}, "1837": {"id": "1602.06255v1", "title": "The UV-bright Quasar Survey (UVQS): DR1", "url": "http://arxiv.org/pdf/1602.06255v1", "date": "2016-02-19 19:16:29", "abs": "We present the first data release (DR1) from our UV-bright Quasar Survey\n(UVQS) for new $z \\sim 1$ active galactic nuclei (AGN) across the sky. Using\nsimple GALEX UV and WISE near-IR color selection criteria, we generated a list\nof 1450 primary candidates with $FUV < 18.5$ mag. We obtained discovery\nspectra, primarily on 3m-class telescopes, for 1040 of these candidates and\nconfirmed 86% as AGN with redshifts generally at $z>0.5$. Including a small set\nof observed secondary candidates, we report the discovery of 217 AGN with $FUV\n< 18$ mag that had no previously reported spectroscopic redshift. These are\nexcellent potential targets for UV spectroscopy before the end of the {\\it\nHubble Space Telescope} mission. The main data products are publicly released\nthrough the Mikulski Archive for Space Telescopes.", "cat": "astro-ph.GA", "authors": ["TalaWanda R. Monroe", "J. Xavier Prochaska", "N. Tejos", "G. Worseck", "Joseph F. Hennawi", "Tobias Schmidt", "Jason Tumlinson", "Yue Shen"]}, "1838": {"id": "2208.10463v1", "title": "Survey of Machine Learning Techniques To Predict Heartbeat Arrhythmias", "url": "http://arxiv.org/pdf/2208.10463v1", "date": "2022-08-22 17:33:59", "abs": "Many works in biomedical computer science research use machine learning\ntechniques to give accurate results. However, these techniques may not be\nfeasible for real-time analysis of data pulled from live hospital feeds. In\nthis project, different machine learning techniques are compared from various\nsources to find one that provides not only high accuracy but also low latency\nand memory overhead to be used in real-world health care systems.", "cat": "cs.LG", "authors": ["Samuel Armstrong"]}, "1839": {"id": "2207.00196v3", "title": "The miniJPAS Survey: Detection of double-core Ly\u03b1 morphology of two high-redshift (z>3) QSOs", "url": "http://arxiv.org/pdf/2207.00196v3", "date": "2022-10-29 05:57:06", "abs": "The Ly$\\alpha$ emission is an important tracer of neutral gas in a\ncircum-galactic medium (CGM) around high-z QSOs. The origin of Lya emission\naround QSOs is still under debate which has significant implications for galaxy\nformation and evolution. In this paper, we study Ly$\\alpha$ nebulae around two\nhigh redshift QSOs, SDSS J141935.58+525710.7 at $z=3.218$ (hereafter QSO1) and\nSDSS J141813.40+525240.4 at $z=3.287$ (hereafter QSO2), from the miniJPAS\nsurvey within the AEGIS field. Using the contiguous narrow-band (NB) images\nfrom the miniJPAS survey and SDSS spectra, we analyzed their morphology,\nnature, and origin. We report the serendipitous detection of double-core Ly\\al\\\nmorphology around two QSOs which is rarely seen among other QSOs. The\nseparations of the two Ly\\al~cores are 11.07 $\\pm$ 2.26 kpcs (1.47 $\\pm$\n0.3$^{\\prime\\prime}$) and 9.73 $\\pm$ 1.55 kpcs (1.31 $\\pm$\n0.21$^{\\prime\\prime}$) with Ly$\\alpha$~line luminosities of $\\sim$ 3.35 $\\times\n10^{44}$ erg s $^{-1} $ and $\\sim$ 6.99 $\\times$ 10$^{44}$ erg s $^{-1}$ for\nQSO1 and QSO2, respectively. The miniJPAS NB images show evidence of extended\nLy$\\alpha$ and CIV morphology for both QSOs and extended HeII morphology for\nQSO1. These two QSOs may be potential candidates for the new enormous Lyman\nalpha nebula (ELAN) found from the miniJPAS survey due to their extended\nmorphology in the shallow depth and relatively high Ly$\\alpha$ luminosities. We\nsuggest that galactic outflows are the major powering mechanism for the\ndouble-core Ly$\\alpha$ morphology. Considering the relatively shallow exposures\nof miniJPAS, the objects found here could be the tip of the iceberg of a\npromising number of such objects that will be uncovered in the upcoming full\nJ-PAS survey and deep IFU observations with 8-10m telescopes will be essential\nfor constraining the underlying physical mechanism that is responsible for the\ndouble-cored morphology.", "cat": "astro-ph.GA", "authors": ["P. T. Rahna", "Zhen-Ya Zheng", "Ana L. Chies-Santos", "Zheng Cai", "Daniele Spinoso", "Isabel Marquez", "Roderik Overzier", "L. Raul Abramo", "Silvia Bonoli", "Carolina Kehrig", "L. A. Diaz-Garcia", "Mirjana Povic", "Roberto Soria", "Jose M. Diego", "Tom Broadhurst", "Rosa M. Gonzalez Delgado", "Jailson Alcaniz", "Narciso Benitez", "Saulo. Carneiro", "A. Javier Cenarro", "David Cristobal-Hornillos", "Renato A. Dupke", "Alessandro Ederoclite", "Antonio Hernan-Caballero", "Carlos Lopez-Sanjuan", "Antonio Marin-Franch", "Claudia Mendes de Oliveira", "Mariano Moles", "Laerte Sodre Jr.", "Keith Taylor", "Jesus Varela", "Hector Vazquez Ramio", "JPAS team"]}, "1840": {"id": "1404.3218v1", "title": "A Deep Chandra ACIS Survey of M83", "url": "http://arxiv.org/pdf/1404.3218v1", "date": "2014-04-11 20:18:21", "abs": "We have obtained a series of deep X-ray images of the nearby galaxy M83 using\nChandra, with a total exposure of 729 ks. Combining the new data with earlier\narchival observations totaling 61 ks, we find 378 point sources within the D25\ncontour of the galaxy. We find 80 more sources, mostly background AGN, outside\nof the D25 contour. Of the X-ray sources, 47 have been detected in a new radio\nsurvey of M83 obtained using the Australia Telescope Compact Array. Of the\nX-ray sources, at least 87 seem likely to be supernova remnants (SNRs), based\non a combination of their properties in X-rays and at other wavelengths. We\nattempt to classify the point source population of M83 through a combination of\nspectral and temporal analysis. As part of this effort, we carry out an initial\nspectral analysis of the 29 brightest X-ray sources. The soft X-ray sources in\nthe disk, many of which are SNRs, are associated with the spiral arms, while\nthe harder X-ray sources, mostly X-ray binaries (XRBs), do not appear to be.\nAfter eliminating AGN, foreground stars and identified SNRs from the sample, we\nconstruct the cumulative luminosity function (CLF) of XRBs brighter than 8\n10$^{35}$ ergs/s. Despite M83's relatively high star formation rate, the CLF\nindicates that most of the XRBs in the disk are low mass XRBs.", "cat": "astro-ph.GA", "authors": ["Knox S. Long", "Kip D. Kuntz", "William P. Blair", "Leith Godfrey", "Paul P. Plucinsky", "Roberto Soria", "Christopher Stockdale", "P. Frank Winkler"]}, "1841": {"id": "1512.05444v2", "title": "Finite Blaschke products: a survey", "url": "http://arxiv.org/pdf/1512.05444v2", "date": "2016-07-07 13:11:09", "abs": "A finite Blaschke product is a product of finitely many automorphisms of the\nunit disk. This brief survey covers some of the main topics in the area,\nincluding characterizations of finite Blaschke products, approximation\ntheorems, derivatives and residues of finite Blaschke products, geometric\nlocalization of zeros, and selected other topics.", "cat": "math.CV", "authors": ["Stephan Ramon Garcia", "Javad Mashreghi", "William T. Ross"]}, "1842": {"id": "1105.3470v1", "title": "The Hubble Space Telescope Cluster Supernova Survey: V. Improving the Dark Energy Constraints Above z>1 and Building an Early-Type-Hosted Supernova Sample", "url": "http://arxiv.org/pdf/1105.3470v1", "date": "2011-05-17 19:56:59", "abs": "We present ACS, NICMOS, and Keck AO-assisted photometry of 20 Type Ia\nsupernovae SNe Ia from the HST Cluster Supernova Survey. The SNe Ia were\ndiscovered over the redshift interval 0.623 < z < 1.415. Fourteen of these SNe\nIa pass our strict selection cuts and are used in combination with the world's\nsample of SNe Ia to derive the best current constraints on dark energy. Ten of\nour new SNe Ia are beyond redshift $z=1$, thereby nearly doubling the\nstatistical weight of HST-discovered SNe Ia beyond this redshift. Our detailed\nanalysis corrects for the recently identified correlation between SN Ia\nluminosity and host galaxy mass and corrects the NICMOS zeropoint at the count\nrates appropriate for very distant SNe Ia. Adding these supernovae improves the\nbest combined constraint on the dark energy density \\rho_{DE}(z) at redshifts\n1.0 < z < 1.6 by 18% (including systematic errors). For a LambdaCDM universe,\nwe find \\Omega_\\Lambda = 0.724 +0.015/-0.016 (68% CL including systematic\nerrors). For a flat wCDM model, we measure a constant dark energy\nequation-of-state parameter w = -0.985 +0.071/-0.077 (68% CL). Curvature is\nconstrained to ~0.7% in the owCDM model and to ~2% in a model in which dark\nenergy is allowed to vary with parameters w_0 and w_a. Tightening further the\nconstraints on the time evolution of dark energy will require several\nimprovements, including high-quality multi-passband photometry of a sample of\nseveral dozen z>1 SNe Ia. We describe how such a sample could be efficiently\nobtained by targeting cluster fields with WFC3 on HST.", "cat": "astro-ph.CO", "authors": ["N. Suzuki", "D. Rubin", "C. Lidman", "G. Aldering", "R. Amanullah", "K. Barbary", "L. F. Barrientos", "J. Botyanszki", "M. Brodwin", "N. Connolly", "K. S. Dawson", "A. Dey", "M. Doi", "M. Donahue", "S. Deustua", "P. Eisenhardt", "E. Ellingson", "L. Faccioli", "V. Fadeyev", "H. K. Fakhouri", "A. S. Fruchter", "D. G. Gilbank", "M. D. Gladders", "G. Goldhaber", "A. H. Gonzalez", "A. Goobar", "A. Gude", "T. Hattori", "H. Hoekstra", "E. Hsiao", "X. Huang", "Y. Ihara", "M. J. Jee", "D. Johnston", "N. Kashikawa", "B. Koester", "K. Konishi", "M. Kowalski", "E. V. Linder", "L. Lubin", "J. Melbourne", "J. Meyers", "T. Morokuma", "F. Munshi", "C. Mullis", "T. Oda", "N. Panagia", "S. Perlmutter", "M. Postman", "T. Pritchard", "J. Rhodes", "P. Ripoche", "P. Rosati", "D. J. Schlegel", "A. Spadafora", "S. A. Stanford", "V. Stanishev", "D. Stern", "M. Strovink", "N. Takanashi", "K. Tokita", "M. Wagner", "L. Wang", "N. Yasuda", "H. K. C. Yee"]}, "1843": {"id": "2408.04380v3", "title": "Deep Generative Models in Robotics: A Survey on Learning from Multimodal Demonstrations", "url": "http://arxiv.org/pdf/2408.04380v3", "date": "2024-08-21 15:54:54", "abs": "Learning from Demonstrations, the field that proposes to learn robot behavior\nmodels from data, is gaining popularity with the emergence of deep generative\nmodels. Although the problem has been studied for years under names such as\nImitation Learning, Behavioral Cloning, or Inverse Reinforcement Learning,\nclassical methods have relied on models that don't capture complex data\ndistributions well or don't scale well to large numbers of demonstrations. In\nrecent years, the robot learning community has shown increasing interest in\nusing deep generative models to capture the complexity of large datasets. In\nthis survey, we aim to provide a unified and comprehensive review of the last\nyear's progress in the use of deep generative models in robotics. We present\nthe different types of models that the community has explored, such as\nenergy-based models, diffusion models, action value maps, or generative\nadversarial networks. We also present the different types of applications in\nwhich deep generative models have been used, from grasp generation to\ntrajectory generation or cost learning. One of the most important elements of\ngenerative models is the generalization out of distributions. In our survey, we\nreview the different decisions the community has made to improve the\ngeneralization of the learned models. Finally, we highlight the research\nchallenges and propose a number of future directions for learning deep\ngenerative models in robotics.", "cat": "cs.RO", "authors": ["Julen Urain", "Ajay Mandlekar", "Yilun Du", "Mahi Shafiullah", "Danfei Xu", "Katerina Fragkiadaki", "Georgia Chalvatzaki", "Jan Peters"]}, "1844": {"id": "1406.5790v1", "title": "Optimization of Survey Strategies for Detecting Slow Radio Transients", "url": "http://arxiv.org/pdf/1406.5790v1", "date": "2014-06-23 01:59:00", "abs": "We investigate the optimal tradeoff between sensitivity and field of view in\nsurveys for slow radio transients using the event detection rate as the survey\nmetric. We investigate (i) a survey in which the events are distributed\nhomogeneously throughout a volume centred on the Earth, (ii) a survey in which\nthe events are homogeneously distributed, but are only detectable beyond a\ncertain minimum distance, and (iii) a survey in which all the events occur at\nan identical distance, as is appropriate for a targetted survey of a particular\nfield which subtends N_point telescope pointings. For a survey of fixed\nduration, T_obs, we determine the optimal tradeoff between number of telescope\npointings, N, and integration time per field. We consider a population in which\nthe event luminosity distribution follows a power law with index -\\alpha, and\nt_slew is the slewing time between fields or, for a drift scan, the time taken\nfor the telescope drift by one beamwidth. Several orders of magnitude\nimprovement in detection rate is possible by optimization of the survey\nparameters. The optimal value of N for case (i) is N_max ~ T_obs/4 t_slew,\nwhile for case (iii) we find N_max = (L_max/L_0)^2 [ (3 -\\alpha)/2\n]^{2/(\\alpha-1)}, where L_max is the maximum luminosity of a transient event\nand L_0 is the minimum luminosity event detectable in an integration of\nduration T_obs. For a telescope field of view, \\Omega, and a minimum detectable\nflux density, S_0, the detection rate scales as N \\Omega S_0^{-3/2} for\nhomogeneously distributed events, while for targetted events (iii) it scales as\nN \\Omega S_0^{1-\\alpha}. The quantity \\Omega S_0^{-2} is often used as the\nmetric of telescope performance in the SKA transients literature, but only\nunder special circumstances is it the metric that optimizes the event detection\nrate. [abstract abbreviated]", "cat": "astro-ph.HE", "authors": ["Jean-Pierre Macquart"]}, "1845": {"id": "2007.08564v1", "title": "Age of Information: An Introduction and Survey", "url": "http://arxiv.org/pdf/2007.08564v1", "date": "2020-07-16 19:00:24", "abs": "We summarize recent contributions in the broad area of age of information\n(AoI). In particular, we describe the current state of the art in the design\nand optimization of low-latency cyberphysical systems and applications in which\nsources send time-stamped status updates to interested recipients. These\napplications desire status updates at the recipients to be as timely as\npossible; however, this is typically constrained by limited system resources.\nWe describe AoI timeliness metrics and present general methods of AoI\nevaluation analysis that are applicable to a wide variety of sources and\nsystems. Starting from elementary single-server queues, we apply these AoI\nmethods to a range of increasingly complex systems, including energy harvesting\nsensors transmitting over noisy channels, parallel server systems, queueing\nnetworks, and various single-hop and multi-hop wireless networks. We also\nexplore how update age is related to MMSE methods of sampling, estimation and\ncontrol of stochastic processes. The paper concludes with a review of efforts\nto employ age optimization in cyberphysical applications.", "cat": "cs.IT", "authors": ["Roy D. Yates", "Yin Sun", "D. Richard Brown III", "Sanjit K. Kaul", "Eytan Modiano", "Sennur Ulukus"]}, "1846": {"id": "1905.07441v1", "title": "Peak sets and boundary interpolation sets for the unit disc: a survey", "url": "http://arxiv.org/pdf/1905.07441v1", "date": "2019-05-17 18:53:58", "abs": "This paper surveys results concerning peak sets and boundary interpolation\nsets for the unit disc. It includes hitherto unpublished results proved by\nDavid C. Ullrich on peak sets for the Zygmund class.", "cat": "math.CV", "authors": ["Alan Noell"]}, "1847": {"id": "2406.16937v1", "title": "A Complete Survey on LLM-based AI Chatbots", "url": "http://arxiv.org/pdf/2406.16937v1", "date": "2024-06-17 09:39:34", "abs": "The past few decades have witnessed an upsurge in data, forming the\nfoundation for data-hungry, learning-based AI technology. Conversational\nagents, often referred to as AI chatbots, rely heavily on such data to train\nlarge language models (LLMs) and generate new content (knowledge) in response\nto user prompts. With the advent of OpenAI's ChatGPT, LLM-based chatbots have\nset new standards in the AI community. This paper presents a complete survey of\nthe evolution and deployment of LLM-based chatbots in various sectors. We first\nsummarize the development of foundational chatbots, followed by the evolution\nof LLMs, and then provide an overview of LLM-based chatbots currently in use\nand those in the development phase. Recognizing AI chatbots as tools for\ngenerating new knowledge, we explore their diverse applications across various\nindustries. We then discuss the open challenges, considering how the data used\nto train the LLMs and the misuse of the generated knowledge can cause several\nissues. Finally, we explore the future outlook to augment their efficiency and\nreliability in numerous applications. By addressing key milestones and the\npresent-day context of LLM-based chatbots, our survey invites readers to delve\ndeeper into this realm, reflecting on how their next generation will reshape\nconversational AI.", "cat": "cs.CL", "authors": ["Sumit Kumar Dam", "Choong Seon Hong", "Yu Qiao", "Chaoning Zhang"]}, "1848": {"id": "1607.01217v3", "title": "Identification of block-oriented nonlinear systems starting from linear approximations: A survey", "url": "http://arxiv.org/pdf/1607.01217v3", "date": "2018-01-09 10:27:23", "abs": "Block-oriented nonlinear models are popular in nonlinear system\nidentification because of their advantages of being simple to understand and\neasy to use. Many different identification approaches were developed over the\nyears to estimate the parameters of a wide range of block-oriented nonlinear\nmodels. One class of these approaches uses linear approximations to initialize\nthe identification algorithm. The best linear approximation framework and the\n$\\epsilon$-approximation framework, or equivalent frameworks, allow the user to\nextract important information about the system, guide the user in selecting\ngood candidate model structures and orders, and prove to be a good starting\npoint for nonlinear system identification algorithms. This paper gives an\noverview of the different block-oriented nonlinear models that can be\nidentified using linear approximations, and of the identification algorithms\nthat have been developed in the past. A non-exhaustive overview of the most\nimportant other block-oriented nonlinear system identification approaches is\nalso provided throughout this paper.", "cat": "cs.SY", "authors": ["Maarten Schoukens", "Koen Tiels"]}, "1849": {"id": "2312.13137v1", "title": "LDIC Survey 2023: Feeling Welcome in the Community", "url": "http://arxiv.org/pdf/2312.13137v1", "date": "2023-12-20 15:57:38", "abs": "We review the level of welcomeness that members of the lattice field theory\ncommunity feel based on the results of a survey performed in May and June 2023.\nWhile respondents reported generally high levels of feeling welcome at the\nlattice conference, women and people with diverse gender identities, sexual\norientations, ethnic backgrounds and religious affiliations feel less included\nand have more negative experiences at the lattice conference than their peers.\nRespondents report that they are actively informing themselves about inequities\nin the community, however a large fraction of survey participants underestimate\nthe severity of the problem, as was found in previous surveys. The survey data\nindicate that this situation can be most effectively improved by organizing\ntalks and events about issues of diversity and inclusion within the lattice\ncommunity. Respondents also reported that individual readings of scientific\npapers on equity and inclusion are effective in giving people agency in making\na change and hence it may be helpful to collate a collection of important\narticles on these topics.", "cat": "hep-lat", "authors": ["Christopher Aubin", "Bipasha Chakraborty", "Will Detmold", "Sofie Martins", "Nilmani Mathur", "Tereza Mendes", "Finn M. Stokes"]}, "1850": {"id": "1810.01447v2", "title": "The Sloan Digital Sky Survey Reverberation Mapping Project: Sample Characterization", "url": "http://arxiv.org/pdf/1810.01447v2", "date": "2019-04-11 19:19:51", "abs": "We present a detailed characterization of the 849 broad-line quasars from the\nSloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project. Our quasar\nsample covers a redshift range of 0.1