Search | arXiv e-print repository

<!DOCTYPE html> <html lang="en"> <head> <meta charset="utf-8"/> <meta name="viewport" content="width=device-width, initial-scale=1"/>  <link rel="apple-touch-icon" sizes="180x180" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-16x16.png"> <link rel="manifest" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/site.webmanifest"> <link rel="mask-icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/safari-pinned-tab.svg" color="#b31b1b"> <link rel="shortcut icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon.ico"> <meta name="msapplication-TileColor" content="#b31b1b"> <meta name="msapplication-config" content="images/icons/browserconfig.xml"> <meta name="theme-color" content="#b31b1b">  <title>Search | arXiv e-print repository</title> <script defer src="https://static.arxiv.org/static/base/1.0.0a5/fontawesome-free-5.11.2-web/js/all.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/base/1.0.0a5/css/arxivstyle.css" /> <script type="text/x-mathjax-config"> MathJax.Hub.Config({ messageStyle: "none", extensions: ["tex2jax.js"], jax: ["input/TeX", "output/HTML-CSS"], tex2jax: { inlineMath: [ ['$','$'], ["\$","\$"] ], displayMath: [ ['$$','$$'], ["\\[","\\]"] ], processEscapes: true, ignoreClass: '.*', processClass: 'mathjax.*' }, TeX: { extensions: ["AMSmath.js", "AMSsymbols.js", "noErrors.js"], noErrors: { inlineDelimiters: ["$","$"], multiLine: false, style: { "font-size": "normal", "border": "" } } }, "HTML-CSS": { availableFonts: ["TeX"] } }); </script> <script src='//static.arxiv.org/MathJax-2.7.3/MathJax.js'></script> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/notification.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/bulma-tooltip.min.css" /> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/search.css" /> <script src="https://code.jquery.com/jquery-3.2.1.slim.min.js" integrity="sha256-k2WSCIexGzOj3Euiig+TlR8gA0EmPjuc79OEeY5L45g=" crossorigin="anonymous"></script> <script src="https://static.arxiv.org/static/search/0.5.6/js/fieldset.js"></script> <style> radio#cf-customfield_11400 { display: none; } </style> </head> <body> <header><a href="#main-container" class="is-sr-only">Skip to main content</a>  <div class="attribution level is-marginless" role="banner"> <div class="level-left"> <a class="level-item" href="https://cornell.edu/"><img src="https://static.arxiv.org/static/base/1.0.0a5/images/cornell-reduced-white-SMALL.svg" alt="Cornell University" width="200" aria-label="logo" /></a> </div> <div class="level-right is-marginless"><p class="sponsors level-item is-marginless"><span id="support-ack-url">We gratefully acknowledge support from<br /> the Simons Foundation, <a href="https://info.arxiv.org/about/ourmembers.html">member institutions</a>, and all contributors. <a href="https://info.arxiv.org/about/donate.html">Donate</a></span></p></div> </div>  <div class="identity level is-marginless"> <div class="level-left"> <div class="level-item"> <a class="arxiv" href="https://arxiv.org/" aria-label="arxiv-logo"> <img src="https://static.arxiv.org/static/base/1.0.0a5/images/arxiv-logo-one-color-white.svg" aria-label="logo" alt="arxiv logo" width="85" style="width:85px;"/> </a> </div> </div> <div class="search-block level-right"> <form class="level-item mini-search" method="GET" action="https://arxiv.org/search"> <div class="field has-addons"> <div class="control"> <input class="input is-small" type="text" name="query" placeholder="Search..." aria-label="Search term or terms" /> <p class="help"><a href="https://info.arxiv.org/help">Help</a> | <a href="https://arxiv.org/search/advanced">Advanced Search</a></p> </div> <div class="control"> <div class="select is-small"> <select name="searchtype" aria-label="Field to search"> <option value="all" selected="selected">All fields</option> <option value="title">Title</option> <option value="author">Author</option> <option value="abstract">Abstract</option> <option value="comments">Comments</option> <option value="journal_ref">Journal reference</option> <option value="acm_class">ACM classification</option> <option value="msc_class">MSC classification</option> <option value="report_num">Report number</option> <option value="paper_id">arXiv identifier</option> <option value="doi">DOI</option> <option value="orcid">ORCID</option> <option value="author_id">arXiv author ID</option> <option value="help">Help pages</option> <option value="full_text">Full text</option> </select> </div> </div> <input type="hidden" name="source" value="header"> <button class="button is-small is-cul-darker">Search</button> </div> </form> </div> </div>  <div class="container"> <div class="user-tools is-size-7 has-text-right has-text-weight-bold" role="navigation" aria-label="User menu"> <a href="https://arxiv.org/login">Login</a> </div> </div> </header> <main class="container" id="main-container"> <div class="level is-marginless"> <div class="level-left"> <h1 class="title is-clearfix"> Showing 1–50 of 116 results for author: <span class="mathjax">Merzougui, M</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/gr-qc" aria-role="search"> Searching in archive <strong>gr-qc</strong>. <a href="/search/?searchtype=author&query=Merzougui%2C+M">Search in all archives.</a> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Merzougui, M"> </div> <div class="select control is-medium"> <label class="is-hidden" for="searchtype">Field</label> <select class="is-medium" id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> </div> <div class="control"> <button class="button is-link is-medium">Search</button> </div> </div> <div class="field"> <div class="control is-size-7"> <label class="radio"> <input checked id="abstracts-0" name="abstracts" type="radio" value="show"> Show abstracts </label> <label class="radio"> <input id="abstracts-1" name="abstracts" type="radio" value="hide"> Hide abstracts </label> </div> </div> <div class="is-clearfix" style="height: 2.5em"> <div class="is-pulled-right"> <a href="/search/advanced?terms-0-term=Merzougui%2C+M&terms-0-field=author&size=50&order=-announced_date_first">Advanced Search</a> </div> </div> <input type="hidden" name="order" value="-announced_date_first"> <input type="hidden" name="size" value="50"> </form> <div class="level breathe-horizontal"> <div class="level-left"> <form method="GET" action="/search/"> <div style="display: none;"> <select id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> <input id="query" name="query" type="text" value="Merzougui, M"> <ul id="abstracts"><li><input checked id="abstracts-0" name="abstracts" type="radio" value="show"> <label for="abstracts-0">Show abstracts</label></li><li><input id="abstracts-1" name="abstracts" type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.12867">arXiv:2407.12867</a> <span> [<a href="https://arxiv.org/pdf/2407.12867">pdf</a>, <a href="https://arxiv.org/format/2407.12867">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Swift-BAT GUANO follow-up of gravitational-wave triggers in the third LIGO-Virgo-KAGRA observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Raman%2C+G">Gayathri Raman</a>, <a href="/search/gr-qc?searchtype=author&query=Ronchini%2C+S">Samuele Ronchini</a>, <a href="/search/gr-qc?searchtype=author&query=Delaunay%2C+J">James Delaunay</a>, <a href="/search/gr-qc?searchtype=author&query=Tohuvavohu%2C+A">Aaron Tohuvavohu</a>, <a href="/search/gr-qc?searchtype=author&query=Kennea%2C+J+A">Jamie A. Kennea</a>, <a href="/search/gr-qc?searchtype=author&query=Parsotan%2C+T">Tyler Parsotan</a>, <a href="/search/gr-qc?searchtype=author&query=Ambrosi%2C+E">Elena Ambrosi</a>, <a href="/search/gr-qc?searchtype=author&query=Bernardini%2C+M+G">Maria Grazia Bernardini</a>, <a href="/search/gr-qc?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/gr-qc?searchtype=author&query=Cusumano%2C+G">Giancarlo Cusumano</a>, <a href="/search/gr-qc?searchtype=author&query=D%27Ai%2C+A">Antonino D'Ai</a>, <a href="/search/gr-qc?searchtype=author&query=D%27Avanzo%2C+P">Paolo D'Avanzo</a>, <a href="/search/gr-qc?searchtype=author&query=D%27Elia%2C+V">Valerio D'Elia</a>, <a href="/search/gr-qc?searchtype=author&query=De+Pasquale%2C+M">Massimiliano De Pasquale</a>, <a href="/search/gr-qc?searchtype=author&query=Dichiara%2C+S">Simone Dichiara</a>, <a href="/search/gr-qc?searchtype=author&query=Evans%2C+P">Phil Evans</a>, <a href="/search/gr-qc?searchtype=author&query=Hartmann%2C+D">Dieter Hartmann</a>, <a href="/search/gr-qc?searchtype=author&query=Kuin%2C+P">Paul Kuin</a>, <a href="/search/gr-qc?searchtype=author&query=Melandri%2C+A">Andrea Melandri</a>, <a href="/search/gr-qc?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/gr-qc?searchtype=author&query=Osborne%2C+J+P">Julian P. Osborne</a>, <a href="/search/gr-qc?searchtype=author&query=Page%2C+K">Kim Page</a>, <a href="/search/gr-qc?searchtype=author&query=Palmer%2C+D+M">David M. Palmer</a>, <a href="/search/gr-qc?searchtype=author&query=Sbarufatti%2C+B">Boris Sbarufatti</a>, <a href="/search/gr-qc?searchtype=author&query=Tagliaferri%2C+G">Gianpiero Tagliaferri</a> , et al. (1797 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.12867v1-abstract-short" style="display: inline;"> We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO-Virgo-KAGRA (LVK) network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received in low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wav… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12867v1-abstract-full').style.display = 'inline'; document.getElementById('2407.12867v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.12867v1-abstract-full" style="display: none;"> We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO-Virgo-KAGRA (LVK) network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received in low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum--likelihood NITRATES pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15-350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10$^{-3}$ Hz, we compute the GW--BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12867v1-abstract-full').style.display = 'none'; document.getElementById('2407.12867v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">50 pages, 10 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.04248">arXiv:2404.04248</a> <span> [<a href="https://arxiv.org/pdf/2404.04248">pdf</a>, <a href="https://arxiv.org/format/2404.04248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad5beb">10.3847/2041-8213/ad5beb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Gravitational Waves from the Coalescence of a $2.5\text{-}4.5~M_\odot$ Compact Object and a Neutron Star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Ak%C3%A7ay%2C+S">S. Ak莽ay</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a> , et al. (1771 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.04248v3-abstract-short" style="display: inline;"> We report the observation of a coalescing compact binary with component masses $2.5\text{-}4.5~M_\odot$ and $1.2\text{-}2.0~M_\odot$ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO-Virgo-KAGRA detector network on 2023 May 29 by the LIGO Livingston Observatory. The primary component of the so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04248v3-abstract-full').style.display = 'inline'; document.getElementById('2404.04248v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04248v3-abstract-full" style="display: none;"> We report the observation of a coalescing compact binary with component masses $2.5\text{-}4.5~M_\odot$ and $1.2\text{-}2.0~M_\odot$ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO-Virgo-KAGRA detector network on 2023 May 29 by the LIGO Livingston Observatory. The primary component of the source has a mass less than $5~M_\odot$ at 99% credibility. We cannot definitively determine from gravitational-wave data alone whether either component of the source is a neutron star or a black hole. However, given existing estimates of the maximum neutron star mass, we find the most probable interpretation of the source to be the coalescence of a neutron star with a black hole that has a mass between the most massive neutron stars and the least massive black holes observed in the Galaxy. We provisionally estimate a merger rate density of $55^{+127}_{-47}~\text{Gpc}^{-3}\,\text{yr}^{-1}$ for compact binary coalescences with properties similar to the source of GW230529_181500; assuming that the source is a neutron star-black hole merger, GW230529_181500-like sources constitute about 60% of the total merger rate inferred for neutron star-black hole coalescences. The discovery of this system implies an increase in the expected rate of neutron star-black hole mergers with electromagnetic counterparts and provides further evidence for compact objects existing within the purported lower mass gap. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04248v3-abstract-full').style.display = 'none'; document.getElementById('2404.04248v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages (10 pages author list, 13 pages main text, 1 page acknowledgements, 13 pages appendices, 8 pages bibliography), 17 figures, 16 tables. Update to match version published in The Astrophysical Journal Letters. Data products available from https://zenodo.org/records/10845779</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2300352 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 970, L34 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.03004">arXiv:2403.03004</a> <span> [<a href="https://arxiv.org/pdf/2403.03004">pdf</a>, <a href="https://arxiv.org/format/2403.03004">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Ultralight vector dark matter search using data from the KAGRA O3GK run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adamcewicz%2C+C">C. Adamcewicz</a>, <a href="/search/gr-qc?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a> , et al. (1778 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.03004v1-abstract-short" style="display: inline;"> Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we prese… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03004v1-abstract-full').style.display = 'inline'; document.getElementById('2403.03004v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.03004v1-abstract-full" style="display: none;"> Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for $U(1)_{B-L}$ gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the $U(1)_{B-L}$ gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation time scale of DM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03004v1-abstract-full').style.display = 'none'; document.getElementById('2403.03004v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2300250 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.08393">arXiv:2304.08393</a> <span> [<a href="https://arxiv.org/pdf/2304.08393">pdf</a>, <a href="https://arxiv.org/format/2304.08393">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Search for gravitational-lensing signatures in the full third observing run of the LIGO-Virgo network </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1670 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.08393v1-abstract-short" style="display: inline;"> Gravitational lensing by massive objects along the line of sight to the source causes distortions of gravitational wave-signals; such distortions may reveal information about fundamental physics, cosmology and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO--Virgo network. We search for repeated… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08393v1-abstract-full').style.display = 'inline'; document.getElementById('2304.08393v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.08393v1-abstract-full" style="display: none;"> Gravitational lensing by massive objects along the line of sight to the source causes distortions of gravitational wave-signals; such distortions may reveal information about fundamental physics, cosmology and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO--Virgo network. We search for repeated signals from strong lensing by 1) performing targeted searches for subthreshold signals, 2) calculating the degree of overlap amongst the intrinsic parameters and sky location of pairs of signals, 3) comparing the similarities of the spectrograms amongst pairs of signals, and 4) performing dual-signal Bayesian analysis that takes into account selection effects and astrophysical knowledge. We also search for distortions to the gravitational waveform caused by 1) frequency-independent phase shifts in strongly lensed images, and 2) frequency-dependent modulation of the amplitude and phase due to point masses. None of these searches yields significant evidence for lensing. Finally, we use the non-detection of gravitational-wave lensing to constrain the lensing rate based on the latest merger-rate estimates and the fraction of dark matter composed of compact objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08393v1-abstract-full').style.display = 'none'; document.getElementById('2304.08393v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2200031 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.03676">arXiv:2302.03676</a> <span> [<a href="https://arxiv.org/pdf/2302.03676">pdf</a>, <a href="https://arxiv.org/format/2302.03676">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acdc9f">10.3847/1538-4365/acdc9f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Open data from the third observing run of LIGO, Virgo, KAGRA and GEO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a>, <a href="/search/gr-qc?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1719 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.03676v1-abstract-short" style="display: inline;"> The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in April of 2019 and lasting six months, O3b starting in November of 2019 and lasting five months, and O3GK starting in April of 2020 and lasti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.03676v1-abstract-full').style.display = 'inline'; document.getElementById('2302.03676v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.03676v1-abstract-full" style="display: none;"> The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in April of 2019 and lasting six months, O3b starting in November of 2019 and lasting five months, and O3GK starting in April of 2020 and lasting 2 weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main dataset, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.03676v1-abstract-full').style.display = 'none'; document.getElementById('2302.03676v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2200316 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.15634">arXiv:2210.15634</a> <span> [<a href="https://arxiv.org/pdf/2210.15634">pdf</a>, <a href="https://arxiv.org/format/2210.15634">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6382/acdf36">10.1088/1361-6382/acdf36 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Virgo Detector Characterization and Data Quality: tools </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/gr-qc?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/gr-qc?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/gr-qc?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/gr-qc?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/gr-qc?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/gr-qc?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/gr-qc?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/gr-qc?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/gr-qc?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/gr-qc?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/gr-qc?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/gr-qc?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/gr-qc?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/gr-qc?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/gr-qc?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/gr-qc?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/gr-qc?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/gr-qc?searchtype=author&query=Baird%2C+J">J. Baird</a> , et al. (469 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.15634v2-abstract-short" style="display: inline;"> Detector characterization and data quality studies -- collectively referred to as {\em DetChar} activities in this article -- are paramount to the scientific exploitation of the joint dataset collected by the LIGO-Virgo-KAGRA global network of ground-based gravitational-wave (GW) detectors. They take place during each phase of the operation of the instruments (upgrade, tuning and optimization, dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15634v2-abstract-full').style.display = 'inline'; document.getElementById('2210.15634v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.15634v2-abstract-full" style="display: none;"> Detector characterization and data quality studies -- collectively referred to as {\em DetChar} activities in this article -- are paramount to the scientific exploitation of the joint dataset collected by the LIGO-Virgo-KAGRA global network of ground-based gravitational-wave (GW) detectors. They take place during each phase of the operation of the instruments (upgrade, tuning and optimization, data taking), are required at all steps of the dataflow (from data acquisition to the final list of GW events) and operate at various latencies (from near real-time to vet the public alerts to offline analyses). This work requires a wide set of tools which have been developed over the years to fulfill the requirements of the various DetChar studies: data access and bookkeeping; global monitoring of the instruments and of the different steps of the data processing; studies of the global properties of the noise at the detector outputs; identification and follow-up of noise peculiar features (whether they be transient or continuously present in the data); quick processing of the public alerts. The present article reviews all the tools used by the Virgo DetChar group during the third LIGO-Virgo Observation Run (O3, from April 2019 to March 2020), mainly to analyse the Virgo data acquired at EGO. Concurrently, a companion article focuses on the results achieved by the DetChar group during the O3 run using these tools. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15634v2-abstract-full').style.display = 'none'; document.getElementById('2210.15634v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 16 figures. New version, resubmitted to Class. and Quantum Grav. This is the "Tools" part of preprint arXiv:2205.01555 [gr-qc] which has been split into two companion articles: one about the tools and methods, the other about the analyses of the O3 Virgo data</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.15633">arXiv:2210.15633</a> <span> [<a href="https://arxiv.org/pdf/2210.15633">pdf</a>, <a href="https://arxiv.org/format/2210.15633">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6382/acd92d">10.1088/1361-6382/acd92d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Virgo Detector Characterization and Data Quality: results from the O3 run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/gr-qc?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/gr-qc?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/gr-qc?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/gr-qc?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/gr-qc?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/gr-qc?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/gr-qc?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/gr-qc?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/gr-qc?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/gr-qc?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/gr-qc?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/gr-qc?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/gr-qc?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/gr-qc?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/gr-qc?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/gr-qc?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/gr-qc?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/gr-qc?searchtype=author&query=Baird%2C+J">J. Baird</a> , et al. (469 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.15633v2-abstract-short" style="display: inline;"> The Advanced Virgo detector has contributed with its data to the rapid growth of the number of detected gravitational-wave (GW) signals in the past few years, alongside the two Advanced LIGO instruments. First during the last month of the Observation Run 2 (O2) in August 2017 (with, most notably, the compact binary mergers GW170814 and GW170817), and then during the full Observation Run 3 (O3): an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15633v2-abstract-full').style.display = 'inline'; document.getElementById('2210.15633v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.15633v2-abstract-full" style="display: none;"> The Advanced Virgo detector has contributed with its data to the rapid growth of the number of detected gravitational-wave (GW) signals in the past few years, alongside the two Advanced LIGO instruments. First during the last month of the Observation Run 2 (O2) in August 2017 (with, most notably, the compact binary mergers GW170814 and GW170817), and then during the full Observation Run 3 (O3): an 11-months data taking period, between April 2019 and March 2020, that led to the addition of about 80 events to the catalog of transient GW sources maintained by LIGO, Virgo and now KAGRA. These discoveries and the manifold exploitation of the detected waveforms require an accurate characterization of the quality of the data, such as continuous study and monitoring of the detector noise sources. These activities, collectively named {\em detector characterization and data quality} or {\em DetChar}, span the whole workflow of the Virgo data, from the instrument front-end hardware to the final analyses. They are described in details in the following article, with a focus on the results achieved by the Virgo DetChar group during the O3 run. Concurrently, a companion article describes the tools that have been used by the Virgo DetChar group to perform this work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15633v2-abstract-full').style.display = 'none'; document.getElementById('2210.15633v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">57 pages, 18 figures. New version, resubmitted to Class. and Quantum Grav. This is the "Results" part of preprint arXiv:2205.01555 [gr-qc] which has been split into two companion articles: one about the tools and methods, the other about the analyses of the O3 Virgo data</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.02863">arXiv:2209.02863</a> <span> [<a href="https://arxiv.org/pdf/2209.02863">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aca1b0">10.3847/2041-8213/aca1b0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Model-based cross-correlation search for gravitational waves from the low-mass X-ray binary Scorpius X-1 in LIGO O3 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1670 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.02863v2-abstract-short" style="display: inline;"> We present the results of a model-based search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1 using LIGO detector data from the third observing run of Advanced LIGO, Advanced Virgo and KAGRA. This is a semicoherent search which uses details of the signal model to coherently combine data separated by less than a specified coherence time, which can be adjusted to bala… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02863v2-abstract-full').style.display = 'inline'; document.getElementById('2209.02863v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.02863v2-abstract-full" style="display: none;"> We present the results of a model-based search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1 using LIGO detector data from the third observing run of Advanced LIGO, Advanced Virgo and KAGRA. This is a semicoherent search which uses details of the signal model to coherently combine data separated by less than a specified coherence time, which can be adjusted to balance sensitivity with computing cost. The search covered a range of gravitational-wave frequencies from 25Hz to 1600Hz, as well as ranges in orbital speed, frequency and phase determined from observational constraints. No significant detection candidates were found, and upper limits were set as a function of frequency. The most stringent limits, between 100Hz and 200Hz, correspond to an amplitude h0 of about 1e-25 when marginalized isotropically over the unknown inclination angle of the neutron star's rotation axis, or less than 4e-26 assuming the optimal orientation. The sensitivity of this search is now probing amplitudes predicted by models of torque balance equilibrium. For the usual conservative model assuming accretion at the surface of the neutron star, our isotropically-marginalized upper limits are close to the predicted amplitude from about 70Hz to 100Hz; the limits assuming the neutron star spin is aligned with the most likely orbital angular momentum are below the conservative torque balance predictions from 40Hz to 200Hz. Assuming a broader range of accretion models, our direct limits on gravitational-wave amplitude delve into the relevant parameter space over a wide range of frequencies, to 500Hz or more. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02863v2-abstract-full').style.display = 'none'; document.getElementById('2209.02863v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, Open Access Journal PDF</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100110-v13 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 941, L30 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.01555">arXiv:2205.01555</a> <span> [<a href="https://arxiv.org/pdf/2205.01555">pdf</a>, <a href="https://arxiv.org/format/2205.01555">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Virgo Detector Characterization and Data Quality during the O3 run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/gr-qc?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/gr-qc?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/gr-qc?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/gr-qc?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/gr-qc?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/gr-qc?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/gr-qc?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/gr-qc?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/gr-qc?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/gr-qc?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/gr-qc?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/gr-qc?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/gr-qc?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/gr-qc?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/gr-qc?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/gr-qc?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/gr-qc?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/gr-qc?searchtype=author&query=Baird%2C+J">J. Baird</a> , et al. (469 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.01555v2-abstract-short" style="display: inline;"> The Advanced Virgo detector has contributed with its data to the rapid growth of the number of detected gravitational-wave signals in the past few years, alongside the two LIGO instruments. First, during the last month of the Observation Run 2 (O2) in August 2017 (with, most notably, the compact binary mergers GW170814 and GW170817) and then during the full Observation Run 3 (O3): an 11 months dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.01555v2-abstract-full').style.display = 'inline'; document.getElementById('2205.01555v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.01555v2-abstract-full" style="display: none;"> The Advanced Virgo detector has contributed with its data to the rapid growth of the number of detected gravitational-wave signals in the past few years, alongside the two LIGO instruments. First, during the last month of the Observation Run 2 (O2) in August 2017 (with, most notably, the compact binary mergers GW170814 and GW170817) and then during the full Observation Run 3 (O3): an 11 months data taking period, between April 2019 and March 2020, that led to the addition of about 80 events to the catalog of transient gravitational-wave sources maintained by LIGO, Virgo and KAGRA. These discoveries and the manifold exploitation of the detected waveforms require an accurate characterization of the quality of the data, such as continuous study and monitoring of the detector noise. These activities, collectively named {\em detector characterization} or {\em DetChar}, span the whole workflow of the Virgo data, from the instrument front-end to the final analysis. They are described in details in the following article, with a focus on the associated tools, the results achieved by the Virgo DetChar group during the O3 run and the main prospects for future data-taking periods with an improved detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.01555v2-abstract-full').style.display = 'none'; document.getElementById('2205.01555v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">86 pages, 33 figures. This paper has been divided into two articles which supercede it and have been posted to arXiv on October 2022. Please use these new preprints as references: arXiv:2210.15634 (tools and methods) and arXiv:2210.15633 (results from the O3 run)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.04523">arXiv:2204.04523</a> <span> [<a href="https://arxiv.org/pdf/2204.04523">pdf</a>, <a href="https://arxiv.org/format/2204.04523">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.106.042003">10.1103/PhysRevD.106.042003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO--Virgo data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1645 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.04523v1-abstract-short" style="display: inline;"> We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO--Virgo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04523v1-abstract-full').style.display = 'inline'; document.getElementById('2204.04523v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.04523v1-abstract-full" style="display: none;"> We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO--Virgo run in the detector frequency band $[10,2000]\rm~Hz$ have been used. No significant detection was found and 95$\%$ confidence level upper limits on the signal strain amplitude were computed, over the full search band, with the deepest limit of about $7.6\times 10^{-26}$ at $\simeq 142\rm~Hz$. These results are significantly more constraining than those reported in previous searches. We use these limits to put constraints on the fiducial neutron star ellipticity and r-mode amplitude. These limits can be also translated into constraints in the black hole mass -- boson mass plane for a hypothetical population of boson clouds around spinning black holes located in the GC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04523v1-abstract-full').style.display = 'none'; document.getElementById('2204.04523v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.04014">arXiv:2203.04014</a> <span> [<a href="https://arxiv.org/pdf/2203.04014">pdf</a>, <a href="https://arxiv.org/format/2203.04014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6382/ac776a">10.1088/1361-6382/ac776a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Virgo O3 run and the impact of the environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/gr-qc?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/gr-qc?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/gr-qc?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/gr-qc?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/gr-qc?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/gr-qc?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/gr-qc?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/gr-qc?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/gr-qc?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/gr-qc?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/gr-qc?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/gr-qc?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/gr-qc?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/gr-qc?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/gr-qc?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/gr-qc?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/gr-qc?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/gr-qc?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a> , et al. (464 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.04014v2-abstract-short" style="display: inline;"> Sources of geophysical noise (such as wind, sea waves and earthquakes) or of anthropogenic noise impact ground-based gravitational-wave interferometric detectors, causing transient sensitivity worsening and gaps in data taking. During the one year-long third Observing Run (O3: from April 01, 2019 to March 27, 2020), the Virgo Collaboration collected a statistically significant dataset, used in thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04014v2-abstract-full').style.display = 'inline'; document.getElementById('2203.04014v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.04014v2-abstract-full" style="display: none;"> Sources of geophysical noise (such as wind, sea waves and earthquakes) or of anthropogenic noise impact ground-based gravitational-wave interferometric detectors, causing transient sensitivity worsening and gaps in data taking. During the one year-long third Observing Run (O3: from April 01, 2019 to March 27, 2020), the Virgo Collaboration collected a statistically significant dataset, used in this article to study the response of the detector to a variety of environmental conditions. We correlated environmental parameters to global detector performance, such as observation range, duty cycle and control losses. Where possible, we identified weaknesses in the detector that will be used to elaborate strategies in order to improve Virgo robustness against external disturbances for the next data taking period, O4, currently planned to start at the end of 2022. The lessons learned could also provide useful insights for the design of the next generation of ground-based interferometers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04014v2-abstract-full').style.display = 'none'; document.getElementById('2203.04014v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 27 figures. Published in Classical and Quantum Grav</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.01270">arXiv:2203.01270</a> <span> [<a href="https://arxiv.org/pdf/2203.01270">pdf</a>, <a href="https://arxiv.org/format/2203.01270">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/ptep/ptac073">10.1093/ptep/ptac073 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First joint observation by the underground gravitational-wave detector, KAGRA, with GEO600 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1647 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.01270v2-abstract-short" style="display: inline;"> We report the results of the first joint observation of the KAGRA detector with GEO600. KAGRA is a cryogenic and underground gravitational-wave detector consisting of a laser interferometer with three-kilometer arms, and located in Kamioka, Gifu, Japan. GEO600 is a British--German laser interferometer with 600 m arms, and located near Hannover, Germany. GEO600 and KAGRA performed a joint observing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.01270v2-abstract-full').style.display = 'inline'; document.getElementById('2203.01270v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.01270v2-abstract-full" style="display: none;"> We report the results of the first joint observation of the KAGRA detector with GEO600. KAGRA is a cryogenic and underground gravitational-wave detector consisting of a laser interferometer with three-kilometer arms, and located in Kamioka, Gifu, Japan. GEO600 is a British--German laser interferometer with 600 m arms, and located near Hannover, Germany. GEO600 and KAGRA performed a joint observing run from April 7 to 20, 2020. We present the results of the joint analysis of the GEO--KAGRA data for transient gravitational-wave signals, including the coalescence of neutron-star binaries and generic unmodeled transients. We also perform dedicated searches for binary coalescence signals and generic transients associated with gamma-ray burst events observed during the joint run. No gravitational-wave events were identified. We evaluate the minimum detectable amplitude for various types of transient signals and the spacetime volume for which the network is sensitive to binary neutron-star coalescences. We also place lower limits on the distances to the gamma-ray bursts analysed based on the non-detection of an associated gravitational-wave signal for several signal models, including binary coalescences. These analyses demonstrate the feasibility and utility of KAGRA as a member of the global gravitational-wave detector network. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.01270v2-abstract-full').style.display = 'none'; document.getElementById('2203.01270v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Matches with published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100286 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Progress of Theoretical and Experimental Physics, Volume 2022, Issue 6, 063F01 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.10104">arXiv:2201.10104</a> <span> [<a href="https://arxiv.org/pdf/2201.10104">pdf</a>, <a href="https://arxiv.org/format/2201.10104">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.106.062002">10.1103/PhysRevD.106.062002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for gravitational waves from Scorpius X-1 with a hidden Markov model in O3 LIGO data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1647 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.10104v1-abstract-short" style="display: inline;"> Results are presented for a semi-coherent search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1, using a hidden Markov model (HMM) to allow for spin wandering. This search improves on previous HMM-based searches of Laser Interferometer Gravitational-wave Observatory (LIGO) data by including the orbital period in the search template grid, and by analyzing data from t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10104v1-abstract-full').style.display = 'inline'; document.getElementById('2201.10104v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.10104v1-abstract-full" style="display: none;"> Results are presented for a semi-coherent search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1, using a hidden Markov model (HMM) to allow for spin wandering. This search improves on previous HMM-based searches of Laser Interferometer Gravitational-wave Observatory (LIGO) data by including the orbital period in the search template grid, and by analyzing data from the latest (third) observing run (O3). In the frequency range searched, from 60 to 500 Hz, we find no evidence of gravitational radiation. This is the most sensitive search for Scorpius X-1 using a HMM to date. For the most sensitive sub-band, starting at $256.06$Hz, we report an upper limit on gravitational wave strain (at $95 \%$ confidence) of $h_{0}^{95\%}=6.16\times10^{-26}$, assuming the orbital inclination angle takes its electromagnetically restricted value $喂=44^{\circ}$. The upper limits on gravitational wave strain reported here are on average a factor of $\sim 3$ lower than in the O2 HMM search. This is the first Scorpius X-1 HMM search with upper limits that reach below the indirect torque-balance limit for certain sub-bands, assuming $喂=44^{\circ}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10104v1-abstract-full').style.display = 'none'; document.getElementById('2201.10104v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100405 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.00697">arXiv:2201.00697</a> <span> [<a href="https://arxiv.org/pdf/2201.00697">pdf</a>, <a href="https://arxiv.org/format/2201.00697">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.106.102008">10.1103/PhysRevD.106.102008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-sky search for continuous gravitational waves from isolated neutron stars using Advanced LIGO and Advanced Virgo O3 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1645 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.00697v1-abstract-short" style="display: inline;"> We present results of an all-sky search for continuous gravitational waves which can be produced by spinning neutron stars with an asymmetry around their rotation axis, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. Four different analysis methods are used to search in a gravitational-wave frequency band from 10 to 2048 Hz and a first frequency derivativ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.00697v1-abstract-full').style.display = 'inline'; document.getElementById('2201.00697v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.00697v1-abstract-full" style="display: none;"> We present results of an all-sky search for continuous gravitational waves which can be produced by spinning neutron stars with an asymmetry around their rotation axis, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. Four different analysis methods are used to search in a gravitational-wave frequency band from 10 to 2048 Hz and a first frequency derivative from $-10^{-8}$ to $10^{-9}$ Hz/s. No statistically-significant periodic gravitational-wave signal is observed by any of the four searches. As a result, upper limits on the gravitational-wave strain amplitude $h_0$ are calculated. The best upper limits are obtained in the frequency range of 100 to 200 Hz and they are ${\sim}1.1\times10^{-25}$ at 95\% confidence-level. The minimum upper limit of $1.10\times10^{-25}$ is achieved at a frequency 111.5 Hz. We also place constraints on the rates and abundances of nearby planetary- and asteroid-mass primordial black holes that could give rise to continuous gravitational-wave signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.00697v1-abstract-full').style.display = 'none'; document.getElementById('2201.00697v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 main text pages, 17 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100367 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.10990">arXiv:2112.10990</a> <span> [<a href="https://arxiv.org/pdf/2112.10990">pdf</a>, <a href="https://arxiv.org/format/2112.10990">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac6ad0">10.3847/1538-4357/ac6ad0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Narrowband searches for continuous and long-duration transient gravitational waves from known pulsars in the LIGO-Virgo third observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1636 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.10990v2-abstract-short" style="display: inline;"> Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully-coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.10990v2-abstract-full').style.display = 'inline'; document.getElementById('2112.10990v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.10990v2-abstract-full" style="display: none;"> Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully-coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow the frequency and frequency time-derivative of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search we look in O3 data for long-duration (hours-months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.10990v2-abstract-full').style.display = 'none'; document.getElementById('2112.10990v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 9 figures, submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100267 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 932, 133 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.06861">arXiv:2112.06861</a> <span> [<a href="https://arxiv.org/pdf/2112.06861">pdf</a>, <a href="https://arxiv.org/format/2112.06861">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Tests of General Relativity with GWTC-3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=de+Alarc%C3%B3n%2C+P+F">P. F. de Alarc贸n</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1657 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.06861v1-abstract-short" style="display: inline;"> The ever-increasing number of detections of gravitational waves (GWs) from compact binaries by the Advanced LIGO and Advanced Virgo detectors allows us to perform ever-more sensitive tests of general relativity (GR) in the dynamical and strong-field regime of gravity. We perform a suite of tests of GR using the compact binary signals observed during the second half of the third observing run of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06861v1-abstract-full').style.display = 'inline'; document.getElementById('2112.06861v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.06861v1-abstract-full" style="display: none;"> The ever-increasing number of detections of gravitational waves (GWs) from compact binaries by the Advanced LIGO and Advanced Virgo detectors allows us to perform ever-more sensitive tests of general relativity (GR) in the dynamical and strong-field regime of gravity. We perform a suite of tests of GR using the compact binary signals observed during the second half of the third observing run of those detectors. We restrict our analysis to the 15 confident signals that have false alarm rates $\leq 10^{-3}\, {\rm yr}^{-1}$. In addition to signals consistent with binary black hole (BH) mergers, the new events include GW200115_042309, a signal consistent with a neutron star--BH merger. We find the residual power, after subtracting the best fit waveform from the data for each event, to be consistent with the detector noise. Additionally, we find all the post-Newtonian deformation coefficients to be consistent with the predictions from GR, with an improvement by a factor of ~2 in the -1PN parameter. We also find that the spin-induced quadrupole moments of the binary BH constituents are consistent with those of Kerr BHs in GR. We find no evidence for dispersion of GWs, non-GR modes of polarization, or post-merger echoes in the events that were analyzed. We update the bound on the mass of the graviton, at 90% credibility, to $m_g \leq 1.27 \times 10^{-23} \mathrm{eV}/c^2$. The final mass and final spin as inferred from the pre-merger and post-merger parts of the waveform are consistent with each other. The studies of the properties of the remnant BHs, including deviations of the quasi-normal mode frequencies and damping times, show consistency with the predictions of GR. In addition to considering signals individually, we also combine results from the catalog of GW signals to calculate more precise population constraints. We find no evidence in support of physics beyond GR. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06861v1-abstract-full').style.display = 'none'; document.getElementById('2112.06861v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100275 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.15116">arXiv:2111.15116</a> <span> [<a href="https://arxiv.org/pdf/2111.15116">pdf</a>, <a href="https://arxiv.org/format/2111.15116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.082005">10.1103/PhysRevD.105.082005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search of the Early O3 LIGO Data for Continuous Gravitational Waves from the Cassiopeia A and Vela Jr. Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+C">C. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1389 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.15116v2-abstract-short" style="display: inline;"> We present directed searches for continuous gravitational waves from the neutron stars in the Cassiopeia A (Cas A) and Vela Jr. supernova remnants. We carry out the searches in the LIGO data from the first six months of the third Advanced LIGO and Virgo observing run, using the Weave semi-coherent method, which sums matched-filter detection-statistic values over many time segments spanning the obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.15116v2-abstract-full').style.display = 'inline'; document.getElementById('2111.15116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.15116v2-abstract-full" style="display: none;"> We present directed searches for continuous gravitational waves from the neutron stars in the Cassiopeia A (Cas A) and Vela Jr. supernova remnants. We carry out the searches in the LIGO data from the first six months of the third Advanced LIGO and Virgo observing run, using the Weave semi-coherent method, which sums matched-filter detection-statistic values over many time segments spanning the observation period. No gravitational wave signal is detected in the search band of 20--976 Hz for assumed source ages greater than 300 years for Cas A and greater than 700 years for Vela Jr. Estimates from simulated continuous wave signals indicate we achieve the most sensitive results to date across the explored parameter space volume, probing to strain magnitudes as low as ~$6.3\times10^{-26}$ for Cas A and ~$5.6\times10^{-26}$ for Vela Jr. at frequencies near 166 Hz at 95% efficiency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.15116v2-abstract-full').style.display = 'none'; document.getElementById('2111.15116v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 8 figures. To appear in Physical Review D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100298-v8 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.13106">arXiv:2111.13106</a> <span> [<a href="https://arxiv.org/pdf/2111.13106">pdf</a>, <a href="https://arxiv.org/format/2111.13106">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac6acf">10.3847/1538-4357/ac6acf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1672 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.13106v2-abstract-short" style="display: inline;"> We present a targeted search for continuous gravitational waves (GWs) from 236 pulsars using data from the third observing run of LIGO and Virgo (O3) combined with data from the second observing run (O2). Searches were for emission from the $l=m=2$ mass quadrupole mode with a frequency at only twice the pulsar rotation frequency (single harmonic) and the $l=2, m=1,2$ modes with a frequency of both… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.13106v2-abstract-full').style.display = 'inline'; document.getElementById('2111.13106v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.13106v2-abstract-full" style="display: none;"> We present a targeted search for continuous gravitational waves (GWs) from 236 pulsars using data from the third observing run of LIGO and Virgo (O3) combined with data from the second observing run (O2). Searches were for emission from the $l=m=2$ mass quadrupole mode with a frequency at only twice the pulsar rotation frequency (single harmonic) and the $l=2, m=1,2$ modes with a frequency of both once and twice the rotation frequency (dual harmonic). No evidence of GWs was found so we present 95\% credible upper limits on the strain amplitudes $h_0$ for the single harmonic search along with limits on the pulsars' mass quadrupole moments $Q_{22}$ and ellipticities $\varepsilon$. Of the pulsars studied, 23 have strain amplitudes that are lower than the limits calculated from their electromagnetically measured spin-down rates. These pulsars include the millisecond pulsars J0437\textminus4715 and J0711\textminus6830 which have spin-down ratios of 0.87 and 0.57 respectively. For nine pulsars, their spin-down limits have been surpassed for the first time. For the Crab and Vela pulsars our limits are factors of $\sim 100$ and $\sim 20$ more constraining than their spin-down limits, respectively. For the dual harmonic searches, new limits are placed on the strain amplitudes $C_{21}$ and $C_{22}$. For 23 pulsars we also present limits on the emission amplitude assuming dipole radiation as predicted by Brans-Dicke theory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.13106v2-abstract-full').style.display = 'none'; document.getElementById('2111.13106v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100049 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.03634">arXiv:2111.03634</a> <span> [<a href="https://arxiv.org/pdf/2111.03634">pdf</a>, <a href="https://arxiv.org/format/2111.03634">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> The population of merging compact binaries inferred using gravitational waves through GWTC-3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1612 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.03634v4-abstract-short" style="display: inline;"> We report on the population properties of 76 compact binary mergers detected with gravitational waves below a false alarm rate of 1 per year through GWTC-3. The catalog contains three classes of binary mergers: BBH, BNS, and NSBH mergers. We infer the BNS merger rate to be between 10 $\rm{Gpc^{-3} yr^{-1}}$ and 1700 $\rm{Gpc^{-3} yr^{-1}}$ and the NSBH merger rate to be between 7.8… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03634v4-abstract-full').style.display = 'inline'; document.getElementById('2111.03634v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.03634v4-abstract-full" style="display: none;"> We report on the population properties of 76 compact binary mergers detected with gravitational waves below a false alarm rate of 1 per year through GWTC-3. The catalog contains three classes of binary mergers: BBH, BNS, and NSBH mergers. We infer the BNS merger rate to be between 10 $\rm{Gpc^{-3} yr^{-1}}$ and 1700 $\rm{Gpc^{-3} yr^{-1}}$ and the NSBH merger rate to be between 7.8 $\rm{Gpc^{-3}\, yr^{-1}}$ and 140 $\rm{Gpc^{-3} yr^{-1}}$ , assuming a constant rate density versus comoving volume and taking the union of 90% credible intervals for methods used in this work. Accounting for the BBH merger rate to evolve with redshift, we find the BBH merger rate to be between 17.9 $\rm{Gpc^{-3}\, yr^{-1}}$ and 44 $\rm{Gpc^{-3}\, yr^{-1}}$ at a fiducial redshift (z=0.2). We obtain a broad neutron star mass distribution extending from $1.2^{+0.1}_{-0.2} M_\odot$ to $2.0^{+0.3}_{-0.3} M_\odot$. We can confidently identify a rapid decrease in merger rate versus component mass between neutron star-like masses and black-hole-like masses, but there is no evidence that the merger rate increases again before 10 $M_\odot$. We also find the BBH mass distribution has localized over- and under-densities relative to a power law distribution. While we continue to find the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above $\sim 60 M_\odot$. The rate of BBH mergers is observed to increase with redshift at a rate proportional to $(1+z)^魏$ with $魏= 2.9^{+1.7}_{-1.8}$ for $z\lesssim 1$. Observed black hole spins are small, with half of spin magnitudes below $蠂_i \simeq 0.25$. We observe evidence of negative aligned spins in the population, and an increase in spin magnitude for systems with more unequal mass ratio. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03634v4-abstract-full').style.display = 'none'; document.getElementById('2111.03634v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">v2: minor edits, most to Table 1 and caption; v3: rerun with public data; Data release: https://zenodo.org/record/5655785; v4: update Fig 14</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100239 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.03608">arXiv:2111.03608</a> <span> [<a href="https://arxiv.org/pdf/2111.03608">pdf</a>, <a href="https://arxiv.org/format/2111.03608">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac532b">10.3847/1538-4357/ac532b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift During the LIGO-Virgo Run O3b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1610 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.03608v1-abstract-short" style="display: inline;"> We search for gravitational-wave signals associated with gamma-ray bursts detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (1 November 2019 15:00 UTC-27 March 2020 17:00 UTC).We conduct two independent searches: a generic gravitational-wave transients search to analyze 86 gamma-ray bursts and an analysis to target bina… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03608v1-abstract-full').style.display = 'inline'; document.getElementById('2111.03608v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.03608v1-abstract-full" style="display: none;"> We search for gravitational-wave signals associated with gamma-ray bursts detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (1 November 2019 15:00 UTC-27 March 2020 17:00 UTC).We conduct two independent searches: a generic gravitational-wave transients search to analyze 86 gamma-ray bursts and an analysis to target binary mergers with at least one neutron star as short gamma-ray burst progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these gamma-ray bursts. A weighted binomial test of the combined results finds no evidence for sub-threshold gravitational wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each gamma-ray burst. Finally, we constrain the population of low luminosity short gamma-ray bursts using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03608v1-abstract-full').style.display = 'none'; document.getElementById('2111.03608v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 6 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2100091 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.03606">arXiv:2111.03606</a> <span> [<a href="https://arxiv.org/pdf/2111.03606">pdf</a>, <a href="https://arxiv.org/format/2111.03606">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevX.13.041039">10.1103/PhysRevX.13.041039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1637 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.03606v3-abstract-short" style="display: inline;"> The third Gravitational-Wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. There ar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03606v3-abstract-full').style.display = 'inline'; document.getElementById('2111.03606v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.03606v3-abstract-full" style="display: none;"> The third Gravitational-Wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. There are 35 compact binary coalescence candidates identified by at least one of our search algorithms with a probability of astrophysical origin $p_\mathrm{astro} > 0.5$. Of these, 18 were previously reported as low-latency public alerts, and 17 are reported here for the first time. Based upon estimates for the component masses, our O3b candidates with $p_\mathrm{astro} > 0.5$ are consistent with gravitational-wave signals from binary black holes or neutron star-black hole binaries, and we identify none from binary neutron stars. However, from the gravitational-wave data alone, we are not able to measure matter effects that distinguish whether the binary components are neutron stars or black holes. The range of inferred component masses is similar to that found with previous catalogs, but the O3b candidates include the first confident observations of neutron star-black hole binaries. Including the 35 candidates from O3b in addition to those from GWTC-2.1, GWTC-3 contains 90 candidates found by our analysis with $p_\mathrm{astro} > 0.5$ across the first three observing runs. These observations of compact binary coalescences present an unprecedented view of the properties of black holes and neutron stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03606v3-abstract-full').style.display = 'none'; document.getElementById('2111.03606v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">88 pages (10 pages author list, 31 pages main text, 1 page acknowledgements, 24 pages appendices, 22 pages bibliography), 17 figures, 16 tables. Update to match version to be published in Physical Review X. Data products available from https://gwosc.org/GWTC-3/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000318 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. X; 13(4):041039; 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.03604">arXiv:2111.03604</a> <span> [<a href="https://arxiv.org/pdf/2111.03604">pdf</a>, <a href="https://arxiv.org/format/2111.03604">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac74bb">10.3847/1538-4357/ac74bb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the cosmic expansion history from GWTC-3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1654 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.03604v2-abstract-short" style="display: inline;"> We use 47 gravitational-wave sources from the Third LIGO-Virgo-KAGRA Gravitational-Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter $H(z)$, including its current value, the Hubble constant $H_0$. Each gravitational-wave (GW) signal provides the luminosity distance to the source and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03604v2-abstract-full').style.display = 'inline'; document.getElementById('2111.03604v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.03604v2-abstract-full" style="display: none;"> We use 47 gravitational-wave sources from the Third LIGO-Virgo-KAGRA Gravitational-Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter $H(z)$, including its current value, the Hubble constant $H_0$. Each gravitational-wave (GW) signal provides the luminosity distance to the source and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and $H(z)$. The source mass distribution displays a peak around $34\, {\rm M_\odot}$, followed by a drop-off. Assuming this mass scale does not evolve with redshift results in a $H(z)$ measurement, yielding $H_0=68^{+12}_{-7} {\rm km\,s^{-1}\,Mpc^{-1}}$ ($68\%$ credible interval) when combined with the $H_0$ measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the $H_0$ estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of $H_0=68^{+8}_{-6} {\rm km\,s^{-1}\,Mpc^{-1}}$ with the galaxy catalog method, an improvement of 42% with respect to our GWTC-1 result and 20% with respect to recent $H_0$ studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about $H_0$) is the well-localized event GW190814. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.03604v2-abstract-full').style.display = 'none'; document.getElementById('2111.03604v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Main paper: 30 pages, 15 figure, 7 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100185-v6 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.09834">arXiv:2110.09834</a> <span> [<a href="https://arxiv.org/pdf/2110.09834">pdf</a>, <a href="https://arxiv.org/format/2110.09834">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.122001">10.1103/PhysRevD.105.122001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-sky, all-frequency directional search for persistent gravitational-waves from Advanced LIGO's and Advanced Virgo's first three observing runs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1605 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.09834v1-abstract-short" style="display: inline;"> We present the first results from an all-sky all-frequency (ASAF) search for an anisotropic stochastic gravitational-wave background using the data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. Upper limit maps on broadband anisotropies of a persistent stochastic background were published for all observing runs of the LIGO-Virgo detectors. However, a broadb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.09834v1-abstract-full').style.display = 'inline'; document.getElementById('2110.09834v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.09834v1-abstract-full" style="display: none;"> We present the first results from an all-sky all-frequency (ASAF) search for an anisotropic stochastic gravitational-wave background using the data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. Upper limit maps on broadband anisotropies of a persistent stochastic background were published for all observing runs of the LIGO-Virgo detectors. However, a broadband analysis is likely to miss narrowband signals as the signal-to-noise ratio of a narrowband signal can be significantly reduced when combined with detector output from other frequencies. Data folding and the computationally efficient analysis pipeline, {\tt PyStoch}, enable us to perform the radiometer map-making at every frequency bin. We perform the search at 3072 {\tt{HEALPix}} equal area pixels uniformly tiling the sky and in every frequency bin of width $1/32$~Hz in the range $20-1726$~Hz, except for bins that are likely to contain instrumental artefacts and hence are notched. We do not find any statistically significant evidence for the existence of narrowband gravitational-wave signals in the analyzed frequency bins. Therefore, we place $95\%$ confidence upper limits on the gravitational-wave strain for each pixel-frequency pair, the limits are in the range $(0.030 - 9.6) \times10^{-24}$. In addition, we outline a method to identify candidate pixel-frequency pairs that could be followed up by a more sensitive (and potentially computationally expensive) search, e.g., a matched-filtering-based analysis, to look for fainter nearly monochromatic coherent signals. The ASAF analysis is inherently independent of models describing any spectral or spatial distribution of power. We demonstrate that the ASAF results can be appropriately combined over frequencies and sky directions to successfully recover the broadband directional and isotropic results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.09834v1-abstract-full').style.display = 'none'; document.getElementById('2110.09834v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 6 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100292 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.12197">arXiv:2109.12197</a> <span> [<a href="https://arxiv.org/pdf/2109.12197">pdf</a>, <a href="https://arxiv.org/format/2109.12197">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.129.061104">10.1103/PhysRevLett.129.061104 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for subsolar-mass binaries in the first half of Advanced LIGO and Virgo's third observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1612 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.12197v1-abstract-short" style="display: inline;"> We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2 $M_\odot$ and 1.0 $M_\odot$ in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.12197v1-abstract-full').style.display = 'inline'; document.getElementById('2109.12197v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.12197v1-abstract-full" style="display: none;"> We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2 $M_\odot$ and 1.0 $M_\odot$ in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio $q \geq 0.1$. We do not report any gravitational-wave candidates. The most significant trigger has a false alarm rate of 0.14 $\mathrm{yr}^{-1}$. This implies an upper limit on the merger rate of subsolar binaries in the range $[220-24200] \mathrm{Gpc}^{-3} \mathrm{yr}^{-1}$, depending on the chirp mass of the binary. We use this upper limit to derive astrophysical constraints on two phenomenological models that could produce subsolar-mass compact objects. One is an isotropic distribution of equal-mass primordial black holes. Using this model, we find that the fraction of dark matter in primordial black holes is $f_\mathrm{PBH} \equiv 惟_\mathrm{PBH} / 惟_\mathrm{DM} \lesssim 6\%$. The other is a dissipative dark matter model, in which fermionic dark matter can collapse and form black holes. The upper limit on the fraction of dark matter black holes depends on the minimum mass of the black holes that can be formed: the most constraining result is obtained at $M_\mathrm{min}=1 M_\odot$, where $f_\mathrm{DBH} \equiv 惟_\mathrm{PBH} / 惟_\mathrm{DM} \lesssim 0.003\%$. These are the tightest limits on spinning subsolar-mass binaries to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.12197v1-abstract-full').style.display = 'none'; document.getElementById('2109.12197v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100163-v8 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.09255">arXiv:2109.09255</a> <span> [<a href="https://arxiv.org/pdf/2109.09255">pdf</a>, <a href="https://arxiv.org/format/2109.09255">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.022002">10.1103/PhysRevD.105.022002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for continuous gravitational waves from 20 accreting millisecond X-ray pulsars in O3 LIGO data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+C">C. Anand</a> , et al. (1612 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.09255v2-abstract-short" style="display: inline;"> Results are presented of searches for continuous gravitational waves from 20 accreting millisecond X-ray pulsars with accurately measured spin frequencies and orbital parameters, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. The search algorithm uses a hidden Markov model, where the transition probabilities allow the frequency to wander according to an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.09255v2-abstract-full').style.display = 'inline'; document.getElementById('2109.09255v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.09255v2-abstract-full" style="display: none;"> Results are presented of searches for continuous gravitational waves from 20 accreting millisecond X-ray pulsars with accurately measured spin frequencies and orbital parameters, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. The search algorithm uses a hidden Markov model, where the transition probabilities allow the frequency to wander according to an unbiased random walk, while the $\mathcal{J}$-statistic maximum-likelihood matched filter tracks the binary orbital phase. Three narrow sub-bands are searched for each target, centered on harmonics of the measured spin frequency. The search yields 16 candidates, consistent with a false alarm probability of 30% per sub-band and target searched. These candidates, along with one candidate from an additional target-of-opportunity search done for SAX J1808.4$-$3658, which was in outburst during one month of the observing run, cannot be confidently associated with a known noise source. Additional follow-up does not provide convincing evidence that any are a true astrophysical signal. When all candidates are assumed non-astrophysical, upper limits are set on the maximum wave strain detectable at 95% confidence, $h_0^{95\%}$. The strictest constraint is $h_0^{95\%} = 4.7\times 10^{-26}$ from IGR J17062$-$6143. Constraints on the detectable wave strain from each target lead to constraints on neutron star ellipticity and $r$-mode amplitude, the strictest of which are $蔚^{95\%} = 3.1\times 10^{-7}$ and $伪^{95\%} = 1.8\times 10^{-5}$ respectively. This analysis is the most comprehensive and sensitive search of continuous gravitational waves from accreting millisecond X-ray pulsars to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.09255v2-abstract-full').style.display = 'none'; document.getElementById('2109.09255v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 6 figures. This version contains minor typographical revisions to match published article</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100221 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 105, 022002 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.01045">arXiv:2108.01045</a> <span> [<a href="https://arxiv.org/pdf/2108.01045">pdf</a>, <a href="https://arxiv.org/format/2108.01045">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+C">C. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1407 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.01045v2-abstract-short" style="display: inline;"> The second Gravitational-Wave Transient Catalog reported on 39 compact binary coalescences observed by the Advanced LIGO and Advanced Virgo detectors between 1 April 2019 15:00 UTC and 1 October 2019 15:00 UTC. We present GWTC-2.1, which reports on a deeper list of candidate events observed over the same period. We analyze the final version of the strain data over this period with improved calibra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01045v2-abstract-full').style.display = 'inline'; document.getElementById('2108.01045v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.01045v2-abstract-full" style="display: none;"> The second Gravitational-Wave Transient Catalog reported on 39 compact binary coalescences observed by the Advanced LIGO and Advanced Virgo detectors between 1 April 2019 15:00 UTC and 1 October 2019 15:00 UTC. We present GWTC-2.1, which reports on a deeper list of candidate events observed over the same period. We analyze the final version of the strain data over this period with improved calibration and better subtraction of excess noise, which has been publicly released. We employ three matched-filter search pipelines for candidate identification, and estimate the astrophysical probability for each candidate event. While GWTC-2 used a false alarm rate threshold of 2 per year, we include in GWTC-2.1, 1201 candidates that pass a false alarm rate threshold of 2 per day. We calculate the source properties of a subset of 44 high-significance candidates that have an astrophysical probability greater than 0.5. Of these candidates, 36 have been reported in GWTC-2. If the 8 additional high-significance candidates presented here are astrophysical, the mass range of events that are unambiguously identified as binary black holes (both objects $\geq 3M_\odot$) is increased compared to GWTC-2, with total masses from $\sim 14 M_\odot$ for GW190924_021846 to $\sim 182 M_\odot$ for GW190426_190642. The primary components of two new candidate events (GW190403_051519 and GW190426_190642) fall in the mass gap predicted by pair instability supernova theory. We also expand the population of binaries with significantly asymmetric mass ratios reported in GWTC-2 by an additional two events (the mass ratio is less than $0.65$ and $0.44$ at $90\%$ probability for GW190403_051519 and GW190917_114630 respectively), and find that 2 of the 8 new events have effective inspiral spins $蠂_\mathrm{eff} > 0$ (at $90\%$ credibility), while no binary is consistent with $蠂_\mathrm{eff} < 0$ at the same significance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01045v2-abstract-full').style.display = 'none'; document.getElementById('2108.01045v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 figures, 8 tables, including updates to parameter estimates of events from GWTC-1 and GWTC-2 in an Appendix</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100063 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.13796">arXiv:2107.13796</a> <span> [<a href="https://arxiv.org/pdf/2107.13796">pdf</a>, <a href="https://arxiv.org/format/2107.13796">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.102001">10.1103/PhysRevD.104.102001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1605 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.13796v1-abstract-short" style="display: inline;"> After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well-suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into "short" $ \lesssim 1~$\,s and "long" $ \gtrsim 1~$\,s duration signals, these signals are expected from a var… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13796v1-abstract-full').style.display = 'inline'; document.getElementById('2107.13796v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.13796v1-abstract-full" style="display: none;"> After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well-suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into "short" $ \lesssim 1~$\,s and "long" $ \gtrsim 1~$\,s duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgo's third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of $2~\text{--}~ 500$~s in duration and a frequency band of $24 - 2048$ Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude $h_{\mathrm{rss}}$ as a function of waveform morphology. These $h_{\mathrm{rss}}$ limits improve upon the results from the second observing run by an average factor of 1.8. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13796v1-abstract-full').style.display = 'none'; document.getElementById('2107.13796v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2100063 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.03701">arXiv:2107.03701</a> <span> [<a href="https://arxiv.org/pdf/2107.03701">pdf</a>, <a href="https://arxiv.org/format/2107.03701">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.122004">10.1103/PhysRevD.104.122004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-sky search for short gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1608 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.03701v1-abstract-short" style="display: inline;"> This paper presents the results of a search for generic short-duration gravitational-wave transients in data from the third observing run of Advanced LIGO and Advanced Virgo. Transients with durations of milliseconds to a few seconds in the 24--4096 Hz frequency band are targeted by the search, with no assumptions made regarding the incoming signal direction, polarization or morphology. Gravitatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03701v1-abstract-full').style.display = 'inline'; document.getElementById('2107.03701v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.03701v1-abstract-full" style="display: none;"> This paper presents the results of a search for generic short-duration gravitational-wave transients in data from the third observing run of Advanced LIGO and Advanced Virgo. Transients with durations of milliseconds to a few seconds in the 24--4096 Hz frequency band are targeted by the search, with no assumptions made regarding the incoming signal direction, polarization or morphology. Gravitational waves from compact binary coalescences that have been identified by other targeted analyses are detected, but no statistically significant evidence for other gravitational wave bursts is found. Sensitivities to a variety of signals are presented. These include updated upper limits on the source rate-density as a function of the characteristic frequency of the signal, which are roughly an order of magnitude better than previous upper limits. This search is sensitive to sources radiating as little as $\sim$10$^{-10} M_{\odot} c^2$ in gravitational waves at $\sim$70 Hz from a distance of 10~kpc, with 50\% detection efficiency at a false alarm rate of one per century. The sensitivity of this search to two plausible astrophysical sources is estimated: neutron star f-modes, which may be excited by pulsar glitches, as well as selected core-collapse supernova models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03701v1-abstract-full').style.display = 'none'; document.getElementById('2107.03701v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2100045 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.03294">arXiv:2107.03294</a> <span> [<a href="https://arxiv.org/pdf/2107.03294">pdf</a>, <a href="https://arxiv.org/format/2107.03294">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6382/ac3c8e">10.1088/1361-6382/ac3c8e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of Advanced Virgo and reconstruction of detector strain h(t) during the Observing Run O3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Virgo+Collaboration"> Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/gr-qc?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/gr-qc?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/gr-qc?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/gr-qc?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/gr-qc?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/gr-qc?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/gr-qc?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/gr-qc?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/gr-qc?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/gr-qc?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/gr-qc?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/gr-qc?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/gr-qc?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/gr-qc?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/gr-qc?searchtype=author&query=Ballardin%2C+G">G. Ballardin</a>, <a href="/search/gr-qc?searchtype=author&query=Baltus%2C+G">G. Baltus</a>, <a href="/search/gr-qc?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a> , et al. (422 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.03294v3-abstract-short" style="display: inline;"> The three Advanced Virgo and LIGO gravitational wave detectors participated to the third observing run (O3) between 1 April 2019 15:00 UTC and 27 March 2020 17:00 UTC,leading to several gravitational wave detections per month. This paper describes the Advanced Virgo detector calibration and the reconstruction of the detector strain $h(t)$ during O3, as well as the estimation of the associated unce… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03294v3-abstract-full').style.display = 'inline'; document.getElementById('2107.03294v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.03294v3-abstract-full" style="display: none;"> The three Advanced Virgo and LIGO gravitational wave detectors participated to the third observing run (O3) between 1 April 2019 15:00 UTC and 27 March 2020 17:00 UTC,leading to several gravitational wave detections per month. This paper describes the Advanced Virgo detector calibration and the reconstruction of the detector strain $h(t)$ during O3, as well as the estimation of the associated uncertainties. For the first time, the photon calibration technique as been used as reference for Virgo calibration, which allowed to cross-calibrate the strain amplitude of the Virgo and LIGO detectors. The previous reference, so-called free swinging Michelson technique, has still been used but as an independent cross-check. $h(t)$ reconstruction and noise subtraction were processed online, with good enough quality to prevent the need for offline reprocessing, except for the two last weeks of September 2019. The uncertainties for the reconstructed $h(t)$ strain, estimated in this paper in a 20-2000~Hz frequency band, are frequency independent: 5% in amplitude, 35 mrad in phase and 10 $渭$s in timing, with the exception of larger uncertainties around 50 Hz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03294v3-abstract-full').style.display = 'none'; document.getElementById('2107.03294v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">50 pages, 30 figures. Submitted to Class. and Quantum Grav.. Includes revision after referee's comments (resubmitted Nov. 2021)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Class. Quantum Grav. 39 045006 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.00600">arXiv:2107.00600</a> <span> [<a href="https://arxiv.org/pdf/2107.00600">pdf</a>, <a href="https://arxiv.org/format/2107.00600">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.082004">10.1103/PhysRevD.104.082004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-sky Search for Continuous Gravitational Waves from Isolated Neutron Stars in the Early O3 LIGO Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1566 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.00600v2-abstract-short" style="display: inline;"> We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000\,Hz and with a frequency time derivative in the range of $[-1.0, +0.1]\times10^{-8}$\,Hz/s. Such a signal could be produced by a nearby, spinning and slightly non-axisymmetric isolated neutron star in our galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Vi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00600v2-abstract-full').style.display = 'inline'; document.getElementById('2107.00600v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.00600v2-abstract-full" style="display: none;"> We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000\,Hz and with a frequency time derivative in the range of $[-1.0, +0.1]\times10^{-8}$\,Hz/s. Such a signal could be produced by a nearby, spinning and slightly non-axisymmetric isolated neutron star in our galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95\%\ confidence-level (CL) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude $h_0$ are $~1.7\times10^{-25}$ near 200\,Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are $\sim6.3\times10^{-26}$. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95\%\ CL upper limits on the strain amplitude are $\sim1.\times10^{-25}$. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of $\sim$2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00600v2-abstract-full').style.display = 'none'; document.getElementById('2107.00600v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000334-v9 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 104, 082004 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13085">arXiv:2105.13085</a> <span> [<a href="https://arxiv.org/pdf/2105.13085">pdf</a>, <a href="https://arxiv.org/format/2105.13085">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.105.063030">10.1103/PhysRevD.105.063030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on dark photon dark matter using data from LIGO's and Virgo's third observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1605 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.13085v3-abstract-short" style="display: inline;"> We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo's third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13085v3-abstract-full').style.display = 'inline'; document.getElementById('2105.13085v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13085v3-abstract-full" style="display: none;"> We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo's third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors. The excess power method optimizes the Fourier Transform coherence time as a function of frequency, to account for the expected signal width due to Doppler modulations. We do not find any evidence of dark photon dark matter with a mass between $m_{\rm A} \sim 10^{-14}-10^{-11}$ eV/$c^2$, which corresponds to frequencies between 10-2000 Hz, and therefore provide upper limits on the square of the minimum coupling of dark photons to baryons, i.e. $U(1)_{\rm B}$ dark matter. For the cross-correlation method, the best median constraint on the squared coupling is $\sim2.65\times10^{-46}$ at $m_{\rm A}\sim4.31\times10^{-13}$ eV/$c^2$; for the other analysis, the best constraint is $\sim 2.4\times 10^{-47}$ at $m_{\rm A}\sim 5.7\times 10^{-13}$ eV/$c^2$. These limits improve upon those obtained in direct dark matter detection experiments by a factor of $\sim100$ for $m_{\rm A}\sim [2-4]\times 10^{-13}$ eV/$c^2$, and are, in absolute terms, the most stringent constraint so far in a large mass range $m_A\sim$ $2\times 10^{-13}-8\times 10^{-12}$ eV/$c^2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13085v3-abstract-full').style.display = 'none'; document.getElementById('2105.13085v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 7 figures; In the latest version, we integrated the changes reported in the published erratum (DOI: https://doi.org/10.1103/PhysRevD.109.089902). Essentially, we overestimated the sensitivity of the cross-correlation search to a dark photon dark matter signal and have corrected this, making the BSD limits the most stringent in this search at most dark photon masses</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100098 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 105, 063030, 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.06384">arXiv:2105.06384</a> <span> [<a href="https://arxiv.org/pdf/2105.06384">pdf</a>, <a href="https://arxiv.org/format/2105.06384">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac23db">10.3847/1538-4357/ac23db <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for lensing signatures in the gravitational-wave observations from the first half of LIGO-Virgo's third observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1356 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.06384v3-abstract-short" style="display: inline;"> We search for signatures of gravitational lensing in the gravitational-wave signals from compact binary coalescences detected by Advanced LIGO and Advanced Virgo during O3a, the first half of their third observing run. We study: 1) the expected rate of lensing at current detector sensitivity and the implications of a non-observation of strong lensing or a stochastic gravitational-wave background o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06384v3-abstract-full').style.display = 'inline'; document.getElementById('2105.06384v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.06384v3-abstract-full" style="display: none;"> We search for signatures of gravitational lensing in the gravitational-wave signals from compact binary coalescences detected by Advanced LIGO and Advanced Virgo during O3a, the first half of their third observing run. We study: 1) the expected rate of lensing at current detector sensitivity and the implications of a non-observation of strong lensing or a stochastic gravitational-wave background on the merger-rate density at high redshift; 2) how the interpretation of individual high-mass events would change if they were found to be lensed; 3) the possibility of multiple images due to strong lensing by galaxies or galaxy clusters; and 4) possible wave-optics effects due to point-mass microlenses. Several pairs of signals in the multiple-image analysis show similar parameters and, in this sense, are nominally consistent with the strong lensing hypothesis. However, taking into account population priors, selection effects, and the prior odds against lensing, these events do not provide sufficient evidence for lensing. Overall, we find no compelling evidence for lensing in the observed gravitational-wave signals from any of these analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06384v3-abstract-full').style.display = 'none'; document.getElementById('2105.06384v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages and 6 figures. Accepted by the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000400 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.14417">arXiv:2104.14417</a> <span> [<a href="https://arxiv.org/pdf/2104.14417">pdf</a>, <a href="https://arxiv.org/format/2104.14417">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac0d52">10.3847/1538-4357/ac0d52 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints from LIGO O3 data on gravitational-wave emission due to r-modes in the glitching pulsar PSR J0537-6910 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1574 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.14417v2-abstract-short" style="display: inline;"> We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J0537-6910 using data from the LIGO-Virgo Collaboration observing run O3. PSR J0537-6910 is a young energetic X-ray pulsar and is the most frequent glitcher known. The inter-glitch braking index of the pulsar suggests that gravitational-wave emission due to r-mode oscillations may play an important role… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.14417v2-abstract-full').style.display = 'inline'; document.getElementById('2104.14417v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.14417v2-abstract-full" style="display: none;"> We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J0537-6910 using data from the LIGO-Virgo Collaboration observing run O3. PSR J0537-6910 is a young energetic X-ray pulsar and is the most frequent glitcher known. The inter-glitch braking index of the pulsar suggests that gravitational-wave emission due to r-mode oscillations may play an important role in the spin evolution of this pulsar. Theoretical models confirm this possibility and predict emission at a level that can be probed by ground-based detectors. In order to explore this scenario, we search for r-mode emission in the epochs between glitches by using a contemporaneous timing ephemeris obtained from NICER data. We do not detect any signals in the theoretically expected band of 86-97 Hz, and report upper limits on the amplitude of the gravitational waves. Our results improve on previous amplitude upper limits from r-modes in J0537-6910 by a factor of up to 3 and place stringent constraints on theoretical models for r-mode driven spin-down in PSR J0537-6910, especially for higher frequencies at which our results reach below the spin-down limit defined by energy conservation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.14417v2-abstract-full').style.display = 'none'; document.getElementById('2104.14417v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 19 figures, accepted in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100069 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 922 71 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.08520">arXiv:2103.08520</a> <span> [<a href="https://arxiv.org/pdf/2103.08520">pdf</a>, <a href="https://arxiv.org/format/2103.08520">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.022005">10.1103/PhysRevD.104.022005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo's first three observing runs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1568 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.08520v4-abstract-short" style="display: inline;"> We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called {\tt PyStoch} on data folded over one sidereal day. We use gravitational-wave radiometry (broadban… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.08520v4-abstract-full').style.display = 'inline'; document.getElementById('2103.08520v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.08520v4-abstract-full" style="display: none;"> We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called {\tt PyStoch} on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitational-wave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95\% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from $F_{伪, 螛} < {\rm (0.013 - 7.6)} \times 10^{-8} {\rm erg \, cm^{-2} \, s^{-1} \, Hz^{-1}},$ and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from $惟_{伪, 螛} < {\rm (0.57 - 9.3)} \times 10^{-9} \, {\rm sr^{-1}}$, depending on direction ($螛$) and spectral index ($伪$). These limits improve upon previous limits by factors of $2.9 - 3.5$. We also set 95\% confidence level upper limits on the frequency-dependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from $h_0 < {\rm (1.7-2.1)} \times 10^{-25},$ a factor of $\geq 2.0$ improvement compared to previous stochastic radiometer searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.08520v4-abstract-full').style.display = 'none'; document.getElementById('2103.08520v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 Pages, 9 Figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000500 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 104, 022005 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.12248">arXiv:2101.12248</a> <span> [<a href="https://arxiv.org/pdf/2101.12248">pdf</a>, <a href="https://arxiv.org/format/2101.12248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.126.241102">10.1103/PhysRevLett.126.241102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on cosmic strings using data from the third Advanced LIGO-Virgo observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1565 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.12248v1-abstract-short" style="display: inline;"> We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 data set. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks and, for the first time, kink-kink collisions.cA template-based search for short-duration transient signals does not yield a detection. We also use the stochastic gravit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12248v1-abstract-full').style.display = 'inline'; document.getElementById('2101.12248v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.12248v1-abstract-full" style="display: none;"> We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 data set. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks and, for the first time, kink-kink collisions.cA template-based search for short-duration transient signals does not yield a detection. We also use the stochastic gravitational-wave background energy density upper limits derived from the O3 data to constrain the cosmic string tension, $G渭$, as a function of the number of kinks, or the number of cusps, for two cosmic string loop distribution models.cAdditionally, we develop and test a third model which interpolates between these two models. Our results improve upon the previous LIGO-Virgo constraints on $G渭$ by one to two orders of magnitude depending on the model which is tested. In particular, for one loop distribution model, we set the most competitive constraints to date, $G渭\lesssim 4\times 10^{-15}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12248v1-abstract-full').style.display = 'none'; document.getElementById('2101.12248v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000506 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 126, 241102 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.12130">arXiv:2101.12130</a> <span> [<a href="https://arxiv.org/pdf/2101.12130">pdf</a>, <a href="https://arxiv.org/format/2101.12130">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.104.022004">10.1103/PhysRevD.104.022004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Upper Limits on the Isotropic Gravitational-Wave Background from Advanced LIGO's and Advanced Virgo's Third Observing Run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1566 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.12130v1-abstract-short" style="display: inline;"> We report results of a search for an isotropic gravitational-wave background (GWB) using data from Advanced LIGO's and Advanced Virgo's third observing run (O3) combined with upper limits from the earlier O1 and O2 runs. Unlike in previous observing runs in the advanced detector era, we include Virgo in the search for the GWB. The results are consistent with uncorrelated noise, and therefore we pl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12130v1-abstract-full').style.display = 'inline'; document.getElementById('2101.12130v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.12130v1-abstract-full" style="display: none;"> We report results of a search for an isotropic gravitational-wave background (GWB) using data from Advanced LIGO's and Advanced Virgo's third observing run (O3) combined with upper limits from the earlier O1 and O2 runs. Unlike in previous observing runs in the advanced detector era, we include Virgo in the search for the GWB. The results are consistent with uncorrelated noise, and therefore we place upper limits on the strength of the GWB. We find that the dimensionless energy density $惟_{\rm GW}\leq 5.8\times 10^{-9}$ at the 95% credible level for a flat (frequency-independent) GWB, using a prior which is uniform in the log of the strength of the GWB, with 99% of the sensitivity coming from the band 20-76.6 Hz; $\leq 3.4 \times 10^{-9}$ at 25 Hz for a power-law GWB with a spectral index of 2/3 (consistent with expectations for compact binary coalescences), in the band 20-90.6 Hz; and $\leq 3.9 \times 10^{-10}$ at 25 Hz for a spectral index of 3, in the band 20-291.6 Hz. These upper limits improve over our previous results by a factor of 6.0 for a flat GWB. We also search for a GWB arising from scalar and vector modes, which are predicted by alternative theories of gravity; we place upper limits on the strength of GWBs with these polarizations. We demonstrate that there is no evidence of correlated noise of magnetic origin by performing a Bayesian analysis that allows for the presence of both a GWB and an effective magnetic background arising from geophysical Schumann resonances. We compare our upper limits to a fiducial model for the GWB from the merger of compact binaries. Finally, we combine our results with observations of individual mergers andshow that, at design sensitivity, this joint approach may yield stronger constraints on the merger rate of binary black holes at $z \lesssim 2$ than can be achieved with individually resolved mergers alone. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12130v1-abstract-full').style.display = 'none'; document.getElementById('2101.12130v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 7 figures, Abstract abridged for arxiv submission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-DCC-P2000314 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 104, 022004 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.12926">arXiv:2012.12926</a> <span> [<a href="https://arxiv.org/pdf/2012.12926">pdf</a>, <a href="https://arxiv.org/format/2012.12926">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/abffcd">10.3847/2041-8213/abffcd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Diving below the spin-down limit: Constraints on gravitational waves from the energetic young pulsar PSR J0537-6910 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1568 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.12926v2-abstract-short" style="display: inline;"> We present a search for continuous gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537-6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using NICER data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537-6910 has the larges… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12926v2-abstract-full').style.display = 'inline'; document.getElementById('2012.12926v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12926v2-abstract-full" style="display: none;"> We present a search for continuous gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537-6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using NICER data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537-6910 has the largest spin-down luminosity of any pulsar and is highly active with regards to glitches. Analyses of its long-term and inter-glitch braking indices provided intriguing evidence that its spin-down energy budget may include gravitational-wave emission from a time-varying mass quadrupole moment. Its 62 Hz rotation frequency also puts its possible gravitational-wave emission in the most sensitive band of LIGO/Virgo detectors. Motivated by these considerations, we search for gravitational-wave emission at both once and twice the rotation frequency. We find no signal, however, and report our upper limits. Assuming a rigidly rotating triaxial star, our constraints reach below the gravitational-wave spin-down limit for this star for the first time by more than a factor of two and limit gravitational waves from the $l=m=2$ mode to account for less than 14% of the spin-down energy budget. The fiducial equatorial ellipticity is limited to less than about 3e-5, which is the third best constraint for any young pulsar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12926v2-abstract-full').style.display = 'none'; document.getElementById('2012.12926v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 5 figures, published in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000407 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.12128">arXiv:2012.12128</a> <span> [<a href="https://arxiv.org/pdf/2012.12128">pdf</a>, <a href="https://arxiv.org/format/2012.12128">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.103.064017">10.1103/PhysRevD.103.064017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-sky search in early O3 LIGO data for continuous gravitational-wave signals from unknown neutron stars in binary systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Aleman%2C+K+M">K. M. Aleman</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a> , et al. (1347 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.12128v2-abstract-short" style="display: inline;"> Rapidly spinning neutron stars are promising sources of persistent, continuous gravitational waves. Detecting such a signal would allow probing of the physical properties of matter under extreme conditions. A significant fraction of the known pulsar population belongs to binary systems. Searching for unknown neutron stars in binary systems requires specialized algorithms to address unknown orbital… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12128v2-abstract-full').style.display = 'inline'; document.getElementById('2012.12128v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12128v2-abstract-full" style="display: none;"> Rapidly spinning neutron stars are promising sources of persistent, continuous gravitational waves. Detecting such a signal would allow probing of the physical properties of matter under extreme conditions. A significant fraction of the known pulsar population belongs to binary systems. Searching for unknown neutron stars in binary systems requires specialized algorithms to address unknown orbital frequency modulations. We present a search for continuous gravitational waves emitted by neutron stars in binary systems in early data from the third observing run of the Advanced LIGO and Advanced Virgo detectors using the semicoherent, GPU-accelerated, BinarySkyHough pipeline. The search analyzes the most sensitive frequency band of the LIGO detectors, 50 - 300 Hz. Binary orbital parameters are split into four regions, comprising orbital periods of 3 - 45 days and projected semimajor axes of 2 - 40 light-seconds. No detections are reported. We estimate the sensitivity of the search using simulated continuous wave signals, achieving the most sensitive results to date across the analyzed parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12128v2-abstract-full').style.display = 'none'; document.getElementById('2012.12128v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 12 figures, 7 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000298 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 064017 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14550">arXiv:2010.14550</a> <span> [<a href="https://arxiv.org/pdf/2010.14550">pdf</a>, <a href="https://arxiv.org/format/2010.14550">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abee15">10.3847/1538-4357/abee15 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift During the LIGO-Virgo Run O3a </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aich%2C+A">A. Aich</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Ananyeva%2C+A">A. Ananyeva</a> , et al. (1228 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14550v3-abstract-short" style="display: inline;"> We search for gravitational-wave transients associated with gamma-ray bursts detected by the Fermi and Swift satellites during the first part of the third observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC - 1 October 2019 15:00 UTC). 105 gamma-ray bursts were analyzed using a search for generic gravitational-wave transients; 32 gamma-ray bursts were analyzed with a search t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14550v3-abstract-full').style.display = 'inline'; document.getElementById('2010.14550v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14550v3-abstract-full" style="display: none;"> We search for gravitational-wave transients associated with gamma-ray bursts detected by the Fermi and Swift satellites during the first part of the third observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC - 1 October 2019 15:00 UTC). 105 gamma-ray bursts were analyzed using a search for generic gravitational-wave transients; 32 gamma-ray bursts were analyzed with a search that specifically targets neutron star binary mergers as short gamma-ray burst progenitors. We describe a method to calculate the probability that triggers from the binary merger targeted search are astrophysical and apply that method to the most significant gamma-ray bursts in that search. We find no significant evidence for gravitational-wave signals associated with the gamma-ray bursts that we followed up, nor for a population of unidentified subthreshold signals. We consider several source types and signal morphologies, and report for these lower bounds on the distance to each gamma-ray burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14550v3-abstract-full').style.display = 'none'; document.getElementById('2010.14550v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 5 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000040 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. J. 915, 86 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14533">arXiv:2010.14533</a> <span> [<a href="https://arxiv.org/pdf/2010.14533">pdf</a>, <a href="https://arxiv.org/format/2010.14533">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/abe949">10.3847/2041-8213/abe949 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Population Properties of Compact Objects from the Second LIGO-Virgo Gravitational-Wave Transient Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Ananyeva%2C+A">A. Ananyeva</a> , et al. (1316 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14533v2-abstract-short" style="display: inline;"> We report on the population of the 47 compact binary mergers detected with a false-alarm rate 1/yr in the second LIGO--Virgo Gravitational-Wave Transient Catalog, GWTC-2. We observe several characteristics of the merging binary black hole (BBH) population not discernible until now. First, we find that the primary mass spectrum contains structure beyond a power-law with a sharp high-mass cut-off; i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14533v2-abstract-full').style.display = 'inline'; document.getElementById('2010.14533v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14533v2-abstract-full" style="display: none;"> We report on the population of the 47 compact binary mergers detected with a false-alarm rate 1/yr in the second LIGO--Virgo Gravitational-Wave Transient Catalog, GWTC-2. We observe several characteristics of the merging binary black hole (BBH) population not discernible until now. First, we find that the primary mass spectrum contains structure beyond a power-law with a sharp high-mass cut-off; it is more consistent with a broken power law with a break at $39.7^{+20.3}_{-9.1}\,M_\odot$, or a power law with a Gaussian feature peaking at $33.1^{+4.0}_{-5.6}\,M_\odot$ (90\% credible interval). While the primary mass distribution must extend to $\sim65\,M_\odot$ or beyond, only $2.9^{+3.5}_{1.7}\%$ of systems have primary masses greater than $45\,M_\odot$. Second, we find that a fraction of BBH systems have component spins misaligned with the orbital angular momentum, giving rise to precession of the orbital plane. Moreover, 12% to 44% of BBH systems have spins tilted by more than $90^\circ$, giving rise to a negative effective inspiral spin parameter $蠂_\mathrm{eff}$. Under the assumption that such systems can only be formed by dynamical interactions, we infer that between 25% and 93% of BBH with non-vanishing $|蠂_\mathrm{eff}| > 0.01$ are dynamically assembled. Third, we estimate merger rates, finding $\mathcal{R}_\text{BBH} = 23.9^{+14.3}_{8.6}$ Gpc$^{-3}$ yr$^{-1}$ for BBH and $\mathcal{R}_\text{BNS}= 320^{+490}_{-240}$ Gpc$^{-3}$ yr$^{-1}$ for binary neutron stars. We find that the BBH rate likely increases with redshift ($85\%$ credibility), but not faster than the star-formation rate ($86\%$ credibility). Additionally, we examine recent exceptional events in the context of our population models, finding that the asymmetric masses of GW190412 and the high component masses of GW190521 are consistent with our models, but the low secondary mass of GW190814 makes it an outlier. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14533v2-abstract-full').style.display = 'none'; document.getElementById('2010.14533v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">53 pages, including 24 pages main text, 18 pages appendix, 30 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000077 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14529">arXiv:2010.14529</a> <span> [<a href="https://arxiv.org/pdf/2010.14529">pdf</a>, <a href="https://arxiv.org/format/2010.14529">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.103.122002">10.1103/PhysRevD.103.122002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Ananyeva%2C+A">A. Ananyeva</a> , et al. (1322 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14529v2-abstract-short" style="display: inline;"> Gravitational waves enable tests of general relativity in the highly dynamical and strong-field regime. Using events detected by LIGO-Virgo up to 1 October 2019, we evaluate the consistency of the data with predictions from the theory. We first establish that residuals from the best-fit waveform are consistent with detector noise, and that the low- and high-frequency parts of the signals are in ag… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14529v2-abstract-full').style.display = 'inline'; document.getElementById('2010.14529v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14529v2-abstract-full" style="display: none;"> Gravitational waves enable tests of general relativity in the highly dynamical and strong-field regime. Using events detected by LIGO-Virgo up to 1 October 2019, we evaluate the consistency of the data with predictions from the theory. We first establish that residuals from the best-fit waveform are consistent with detector noise, and that the low- and high-frequency parts of the signals are in agreement. We then consider parametrized modifications to the waveform by varying post-Newtonian and phenomenological coefficients, improving past constraints by factors of ${\sim}2$; we also find consistency with Kerr black holes when we specifically target signatures of the spin-induced quadrupole moment. Looking for gravitational-wave dispersion, we tighten constraints on Lorentz-violating coefficients by a factor of ${\sim}2.6$ and bound the mass of the graviton to $m_g \leq 1.76 \times 10^{-23} \mathrm{eV}/c^2$ with 90% credibility. We also analyze the properties of the merger remnants by measuring ringdown frequencies and damping times, constraining fractional deviations away from the Kerr frequency to $未\hat{f}_{220} = 0.03^{+0.38}_{-0.35}$ for the fundamental quadrupolar mode, and $未\hat{f}_{221} = 0.04^{+0.27}_{-0.32}$ for the first overtone; additionally, we find no evidence for postmerger echoes. Finally, we determine that our data are consistent with tensorial polarizations through a template-independent method. When possible, we assess the validity of general relativity based on collections of events analyzed jointly. We find no evidence for new physics beyond general relativity, for black hole mimickers, or for any unaccounted systematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14529v2-abstract-full').style.display = 'none'; document.getElementById('2010.14529v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages + appendices, 19 figures; journal version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000091 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 122002 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14527">arXiv:2010.14527</a> <span> [<a href="https://arxiv.org/pdf/2010.14527">pdf</a>, <a href="https://arxiv.org/format/2010.14527">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevX.11.021053">10.1103/PhysRevX.11.021053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Ananyeva%2C+A">A. Ananyeva</a>, <a href="/search/gr-qc?searchtype=author&query=Anderson%2C+S+B">S. B. Anderson</a> , et al. (1327 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14527v3-abstract-short" style="display: inline;"> We report on gravitational wave discoveries from compact binary coalescences detected by Advanced LIGO and Advanced Virgo in the first half of the third observing run (O3a) between 1 April 2019 15:00 UTC and 1 October 2019 15:00. By imposing a false-alarm-rate threshold of two per year in each of the four search pipelines that constitute our search, we present 39 candidate gravitational wave event… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14527v3-abstract-full').style.display = 'inline'; document.getElementById('2010.14527v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14527v3-abstract-full" style="display: none;"> We report on gravitational wave discoveries from compact binary coalescences detected by Advanced LIGO and Advanced Virgo in the first half of the third observing run (O3a) between 1 April 2019 15:00 UTC and 1 October 2019 15:00. By imposing a false-alarm-rate threshold of two per year in each of the four search pipelines that constitute our search, we present 39 candidate gravitational wave events. At this threshold, we expect a contamination fraction of less than 10%. Of these, 26 candidate events were reported previously in near real-time through GCN Notices and Circulars; 13 are reported here for the first time. The catalog contains events whose sources are black hole binary mergers up to a redshift of ~0.8, as well as events whose components could not be unambiguously identified as black holes or neutron stars. For the latter group, we are unable to determine the nature based on estimates of the component masses and spins from gravitational wave data alone. The range of candidate events which are unambiguously identified as binary black holes (both objects $\geq 3~M_\odot$) is increased compared to GWTC-1, with total masses from $\sim 14~M_\odot$ for GW190924_021846 to $\sim 150~M_\odot$ for GW190521. For the first time, this catalog includes binary systems with significantly asymmetric mass ratios, which had not been observed in data taken before April 2019. We also find that 11 of the 39 events detected since April 2019 have positive effective inspiral spins under our default prior (at 90% credibility), while none exhibit negative effective inspiral spin. Given the increased sensitivity of Advanced LIGO and Advanced Virgo, the detection of 39 candidate events in ~26 weeks of data (~1.5 per week) is consistent with GWTC-1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14527v3-abstract-full').style.display = 'none'; document.getElementById('2010.14527v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This version updates with minor revisions to typographical errors. We would also like to call attention to the updated parameter estimation samples data release here: https://dcc.ligo.org/LIGO-P2000223/public</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2000061 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. X 11, 021053 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.01190">arXiv:2009.01190</a> <span> [<a href="https://arxiv.org/pdf/2009.01190">pdf</a>, <a href="https://arxiv.org/format/2009.01190">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aba493">10.3847/2041-8213/aba493 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Properties and astrophysical implications of the 150 Msun binary black hole merger GW190521 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aich%2C+A">A. Aich</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1233 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.01190v1-abstract-short" style="display: inline;"> The gravitational-wave signal GW190521 is consistent with a binary black hole merger source at redshift 0.8 with unusually high component masses, $85^{+21}_{-14}\,M_{\odot}$ and $66^{+17}_{-18}\,M_{\odot}$, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01190v1-abstract-full').style.display = 'inline'; document.getElementById('2009.01190v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.01190v1-abstract-full" style="display: none;"> The gravitational-wave signal GW190521 is consistent with a binary black hole merger source at redshift 0.8 with unusually high component masses, $85^{+21}_{-14}\,M_{\odot}$ and $66^{+17}_{-18}\,M_{\odot}$, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range $65 - 120\,M_{\odot}$. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger $(142^{+28}_{-16}\,M_{\odot})$ classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular binary black hole coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be $0.13^{+0.30}_{-0.11}\,{\rm Gpc}^{-3}\,\rm{yr}^{-1}$. We discuss the astrophysical implications of GW190521 for stellar collapse, and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescence, or via hierarchical merger of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01190v1-abstract-full').style.display = 'none'; document.getElementById('2009.01190v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">39 pages, 13 figures; data available at https://dcc.ligo.org/P2000158-v4/public</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000021 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. J. Lett. 900, L13 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.01075">arXiv:2009.01075</a> <span> [<a href="https://arxiv.org/pdf/2009.01075">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.125.101102">10.1103/PhysRevLett.125.101102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GW190521: A Binary Black Hole Merger with a Total Mass of $150 ~ M_{\odot}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aich%2C+A">A. Aich</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1232 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.01075v1-abstract-short" style="display: inline;"> On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of tw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01075v1-abstract-full').style.display = 'inline'; document.getElementById('2009.01075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.01075v1-abstract-full" style="display: none;"> On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of $85^{+21}_{-14} M_{\odot}$ and $66^{+17}_{-18} M_{\odot}$ (90 % credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, and has only a 0.32 % probability of being below $65 M_{\odot}$. We calculate the mass of the remnant to be $142^{+28}_{-16} M_{\odot}$, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is $5.3^{+2.4}_{-2.6}$ Gpc, corresponding to a redshift of $0.82^{+0.28}_{-0.34}$. The inferred rate of mergers similar to GW190521 is $0.13^{+0.30}_{-0.11}\,\mathrm{Gpc}^{-3}\,\mathrm{yr}^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01075v1-abstract-full').style.display = 'none'; document.getElementById('2009.01075v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Supplementary Material at https://dcc.ligo.org/LIGO-P2000020/Public</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 125, 101102 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.14251">arXiv:2007.14251</a> <span> [<a href="https://arxiv.org/pdf/2007.14251">pdf</a>, <a href="https://arxiv.org/format/2007.14251">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/abb655">10.3847/2041-8213/abb655 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational-wave constraints on the equatorial ellipticity of millisecond pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+A">A. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Ananyeva%2C+A">A. Ananyeva</a> , et al. (1311 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.14251v2-abstract-short" style="display: inline;"> We present a search for continuous gravitational waves from five radio pulsars, comprising three recycled pulsars (PSR J0437-4715, PSR J0711-6830, and PSR J0737-3039A) and two young pulsars: the Crab pulsar (J0534+2200) and the Vela pulsar (J0835-4510). We use data from the third observing run of Advanced LIGO and Virgo combined with data from their first and second observing runs. For the first t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.14251v2-abstract-full').style.display = 'inline'; document.getElementById('2007.14251v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.14251v2-abstract-full" style="display: none;"> We present a search for continuous gravitational waves from five radio pulsars, comprising three recycled pulsars (PSR J0437-4715, PSR J0711-6830, and PSR J0737-3039A) and two young pulsars: the Crab pulsar (J0534+2200) and the Vela pulsar (J0835-4510). We use data from the third observing run of Advanced LIGO and Virgo combined with data from their first and second observing runs. For the first time we are able to match (for PSR J0437-4715) or surpass (for PSR J0711-6830) the indirect limits on gravitational-wave emission from recycled pulsars inferred from their observed spin-downs, and constrain their equatorial ellipticities to be less than $10^{-8}$. For each of the five pulsars, we perform targeted searches that assume a tight coupling between the gravitational-wave and electromagnetic signal phase evolution. We also present constraints on PSR J0711-6830, the Crab pulsar and the Vela pulsar from a search that relaxes this assumption, allowing the gravitational-wave signal to vary from the electromagnetic expectation within a narrow band of frequencies and frequency derivatives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.14251v2-abstract-full').style.display = 'none'; document.getElementById('2007.14251v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 6 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2000029 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2020 ApJL 902 L21 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.12611">arXiv:2006.12611</a> <span> [<a href="https://arxiv.org/pdf/2006.12611">pdf</a>, <a href="https://arxiv.org/format/2006.12611">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab960f">10.3847/2041-8213/ab960f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GW190814: Gravitational Waves from the Coalescence of a 23 M$_\odot$ Black Hole with a 2.6 M$_\odot$ Compact Object </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aich%2C+A">A. Aich</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1232 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.12611v1-abstract-short" style="display: inline;"> We report the observation of a compact binary coalescence involving a 22.2 - 24.3 $M_{\odot}$ black hole and a compact object with a mass of 2.50 - 2.67 $M_{\odot}$ (all measurements quoted at the 90$\%$ credible level). The gravitational-wave signal, GW190814, was observed during LIGO's and Virgo's third observing run on August 14, 2019 at 21:10:39 UTC and has a signal-to-noise ratio of 25 in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.12611v1-abstract-full').style.display = 'inline'; document.getElementById('2006.12611v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.12611v1-abstract-full" style="display: none;"> We report the observation of a compact binary coalescence involving a 22.2 - 24.3 $M_{\odot}$ black hole and a compact object with a mass of 2.50 - 2.67 $M_{\odot}$ (all measurements quoted at the 90$\%$ credible level). The gravitational-wave signal, GW190814, was observed during LIGO's and Virgo's third observing run on August 14, 2019 at 21:10:39 UTC and has a signal-to-noise ratio of 25 in the three-detector network. The source was localized to 18.5 deg$^2$ at a distance of $241^{+41}_{-45}$ Mpc; no electromagnetic counterpart has been confirmed to date. The source has the most unequal mass ratio yet measured with gravitational waves, $0.112^{+0.008}_{-0.009}$, and its secondary component is either the lightest black hole or the heaviest neutron star ever discovered in a double compact-object system. The dimensionless spin of the primary black hole is tightly constrained to $\leq 0.07$. Tests of general relativity reveal no measurable deviations from the theory, and its prediction of higher-multipole emission is confirmed at high confidence. We estimate a merger rate density of 1-23 Gpc$^{-3}$ yr$^{-1}$ for the new class of binary coalescence sources that GW190814 represents. Astrophysical models predict that binaries with mass ratios similar to this event can form through several channels, but are unlikely to have formed in globular clusters. However, the combination of mass ratio, component masses, and the inferred merger rate for this event challenges all current models for the formation and mass distribution of compact-object binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.12611v1-abstract-full').style.display = 'none'; document.getElementById('2006.12611v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 8 figures, accepted by ApJ Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P190814 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.08342">arXiv:2004.08342</a> <span> [<a href="https://arxiv.org/pdf/2004.08342">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.102.043015">10.1103/PhysRevD.102.043015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aich%2C+A">A. Aich</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1232 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.08342v3-abstract-short" style="display: inline;"> We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO's and Virgo's third observing run. The signal was recorded on April 12, 2019 at 05:30:44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ~30 solar mass blac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.08342v3-abstract-full').style.display = 'inline'; document.getElementById('2004.08342v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.08342v3-abstract-full" style="display: none;"> We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO's and Virgo's third observing run. The signal was recorded on April 12, 2019 at 05:30:44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ~30 solar mass black hole merged with a ~8 solar mass black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein's general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.08342v3-abstract-full').style.display = 'none'; document.getElementById('2004.08342v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 12 figures; data available under https://doi.org/10.7935/20yv-ka61 posterior samples available under https://dcc.ligo.org/P190412/public</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P190412 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 043015 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.01761">arXiv:2001.01761</a> <span> [<a href="https://arxiv.org/pdf/2001.01761">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab75f5">10.3847/2041-8213/ab75f5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GW190425: Observation of a Compact Binary Coalescence with Total Mass $\sim 3.4 M_{\odot}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+B+P">B. P. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Aloy%2C+M+A">M. A. Aloy</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a> , et al. (1177 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.01761v3-abstract-short" style="display: inline;"> On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from 1.12 to 2.52 $M_{\odot}$ (1.45 to 1.88 $M_{\odot}$ if w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.01761v3-abstract-full').style.display = 'inline'; document.getElementById('2001.01761v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.01761v3-abstract-full" style="display: none;"> On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from 1.12 to 2.52 $M_{\odot}$ (1.45 to 1.88 $M_{\odot}$ if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass $1.44^{+0.02}_{-0.02} M_{\odot}$ and the total mass $3.4^{+0.3}_{-0.1}\,M_{\odot}$ of this system are significantly larger than those of any other known binary neutron star system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic binary neutron star population. Under the assumption that the signal was produced by a binary neutron star coalescence, the local rate of neutron star mergers is updated to $250-2810 \text{Gpc}^{-3}\text{yr}^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.01761v3-abstract-full').style.display = 'none'; document.getElementById('2001.01761v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 19 figures, published in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P190425 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal Letters 892 (2020) L3 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.11716">arXiv:1912.11716</a> <span> [<a href="https://arxiv.org/pdf/1912.11716">pdf</a>, <a href="https://arxiv.org/format/1912.11716">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.softx.2021.100658">10.1016/j.softx.2021.100658 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/gr-qc?searchtype=author&query=Abraham%2C+S">S. Abraham</a>, <a href="/search/gr-qc?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/gr-qc?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/gr-qc?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/gr-qc?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/gr-qc?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/gr-qc?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/gr-qc?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/gr-qc?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/gr-qc?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/gr-qc?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/gr-qc?searchtype=author&query=Aich%2C+A">A. Aich</a>, <a href="/search/gr-qc?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/gr-qc?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/gr-qc?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/gr-qc?searchtype=author&query=Allen%2C+G">G. Allen</a>, <a href="/search/gr-qc?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/gr-qc?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/gr-qc?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/gr-qc?searchtype=author&query=Anand%2C+S">S. Anand</a>, <a href="/search/gr-qc?searchtype=author&query=Ananyeva%2C+A">A. Ananyeva</a> , et al. (1223 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1912.11716v2-abstract-short" style="display: inline;"> Advanced LIGO and Advanced Virgo are actively monitoring the sky and collecting gravitational-wave strain data with sufficient sensitivity to detect signals routinely. In this paper we describe the data recorded by these instruments during their first and second observing runs. The main data products are the gravitational-wave strain arrays, released as time series sampled at 16384 Hz. The dataset… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.11716v2-abstract-full').style.display = 'inline'; document.getElementById('1912.11716v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.11716v2-abstract-full" style="display: none;"> Advanced LIGO and Advanced Virgo are actively monitoring the sky and collecting gravitational-wave strain data with sufficient sensitivity to detect signals routinely. In this paper we describe the data recorded by these instruments during their first and second observing runs. The main data products are the gravitational-wave strain arrays, released as time series sampled at 16384 Hz. The datasets that include this strain measurement can be freely accessed through the Gravitational Wave Open Science Center at http://gw-openscience.org, together with data-quality information essential for the analysis of LIGO and Virgo data, documentation, tutorials, and supporting software. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.11716v2-abstract-full').style.display = 'none'; document.getElementById('1912.11716v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">42 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P1900206 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SoftwareX 13 (2021) 100658 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.03701">arXiv:1911.03701</a> <span> [<a href="https://arxiv.org/pdf/1911.03701">pdf</a>, <a href="https://arxiv.org/format/1911.03701">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6382/aba80e">10.1088/1361-6382/aba80e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ELGAR -- a European Laboratory for Gravitation and Atom-interferometric Research </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/gr-qc?searchtype=author&query=Canuel%2C+B">B. Canuel</a>, <a href="/search/gr-qc?searchtype=author&query=Abend%2C+S">S. Abend</a>, <a href="/search/gr-qc?searchtype=author&query=Amaro-Seoane%2C+P">P. Amaro-Seoane</a>, <a href="/search/gr-qc?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/gr-qc?searchtype=author&query=Beaufils%2C+Q">Q. Beaufils</a>, <a href="/search/gr-qc?searchtype=author&query=Bertoldi%2C+A">A. Bertoldi</a>, <a href="/search/gr-qc?searchtype=author&query=Bongs%2C+K">K. Bongs</a>, <a href="/search/gr-qc?searchtype=author&query=Bouyer%2C+P">P. Bouyer</a>, <a href="/search/gr-qc?searchtype=author&query=Braxmaier%2C+C">C. Braxmaier</a>, <a href="/search/gr-qc?searchtype=author&query=Chaibi%2C+W">W. Chaibi</a>, <a href="/search/gr-qc?searchtype=author&query=Christensen%2C+N">N. Christensen</a>, <a href="/search/gr-qc?searchtype=author&query=Fitzek%2C+F">F. Fitzek</a>, <a href="/search/gr-qc?searchtype=author&query=Flouris%2C+G">G. Flouris</a>, <a href="/search/gr-qc?searchtype=author&query=Gaaloul%2C+N">N. Gaaloul</a>, <a href="/search/gr-qc?searchtype=author&query=Gaffet%2C+S">S. Gaffet</a>, <a href="/search/gr-qc?searchtype=author&query=Alzar%2C+C+L+G">C. L. Garrido Alzar</a>, <a href="/search/gr-qc?searchtype=author&query=Geiger%2C+R">R. Geiger</a>, <a href="/search/gr-qc?searchtype=author&query=Guellati-Khelifa%2C+S">S. Guellati-Khelifa</a>, <a href="/search/gr-qc?searchtype=author&query=Hammerer%2C+K">K. Hammerer</a>, <a href="/search/gr-qc?searchtype=author&query=Harms%2C+J">J. Harms</a>, <a href="/search/gr-qc?searchtype=author&query=Hinderer%2C+J">J. Hinderer</a>, <a href="/search/gr-qc?searchtype=author&query=Junca%2C+J">J. Junca</a>, <a href="/search/gr-qc?searchtype=author&query=Katsanevas%2C+S">S. Katsanevas</a>, <a href="/search/gr-qc?searchtype=author&query=Klempt%2C+C">C. Klempt</a>, <a href="/search/gr-qc?searchtype=author&query=Kozanitis%2C+C">C. Kozanitis</a> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.03701v1-abstract-short" style="display: inline;"> Gravitational Waves (GWs) were observed for the first time in 2015, one century after Einstein predicted their existence. There is now growing interest to extend the detection bandwidth to low frequency. The scientific potential of multi-frequency GW astronomy is enormous as it would enable to obtain a more complete picture of cosmic events and mechanisms. This is a unique and entirely new opportu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.03701v1-abstract-full').style.display = 'inline'; document.getElementById('1911.03701v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.03701v1-abstract-full" style="display: none;"> Gravitational Waves (GWs) were observed for the first time in 2015, one century after Einstein predicted their existence. There is now growing interest to extend the detection bandwidth to low frequency. The scientific potential of multi-frequency GW astronomy is enormous as it would enable to obtain a more complete picture of cosmic events and mechanisms. This is a unique and entirely new opportunity for the future of astronomy, the success of which depends upon the decisions being made on existing and new infrastructures. The prospect of combining observations from the future space-based instrument LISA together with third generation ground based detectors will open the way towards multi-band GW astronomy, but will leave the infrasound (0.1 Hz to 10 Hz) band uncovered. GW detectors based on matter wave interferometry promise to fill such a sensitivity gap. We propose the European Laboratory for Gravitation and Atom-interferometric Research (ELGAR), an underground infrastructure based on the latest progress in atomic physics, to study space-time and gravitation with the primary goal of detecting GWs in the infrasound band. ELGAR will directly inherit from large research facilities now being built in Europe for the study of large scale atom interferometry and will drive new pan-European synergies from top research centers developing quantum sensors. ELGAR will measure GW radiation in the infrasound band with a peak strain sensitivity of $4.1 \times 10^{-22}/\sqrt{\text{Hz}}$ at 1.7 Hz. The antenna will have an impact on diverse fundamental and applied research fields beyond GW astronomy, including gravitation, general relativity, and geology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.03701v1-abstract-full').style.display = 'none'; document.getElementById('1911.03701v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Class. Quantum Grav. 37 225017 (2020) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Merzougui%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

CINXE.COM

Search | arXiv e-print repository