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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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/2410.16565">arXiv:2410.16565</a> <span> [<a href="https://arxiv.org/pdf/2410.16565">pdf</a>, <a href="https://arxiv.org/format/2410.16565">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> </div> </div> <p class="title is-5 mathjax"> Search for gravitational waves emitted from SN 2023ixf </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1758 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="2410.16565v1-abstract-short" style="display: inline;"> We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19th, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16565v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16565v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16565v1-abstract-full" style="display: none;"> We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19th, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been identified in data when at least two gravitational-wave observatories were operating, which covered $\sim 14\%$ of this five-day window. We report the search detection efficiency for various possible gravitational-wave emission models. Considering the distance to M101 (6.7 Mpc), we derive constraints on the gravitational-wave emission mechanism of core-collapse supernovae across a broad frequency spectrum, ranging from 50 Hz to 2 kHz where we assume the GW emission occurred when coincident data are available in the on-source window. Considering an ellipsoid model for a rotating proto-neutron star, our search is sensitive to gravitational-wave energy $1 \times 10^{-5} M_{\odot} c^2$ and luminosity $4 \times 10^{-5} M_{\odot} c^2/\text{s}$ for a source emitting at 50 Hz. These constraints are around an order of magnitude more stringent than those obtained so far with gravitational-wave data. The constraint on the ellipticity of the proto-neutron star that is formed is as low as $1.04$, at frequencies above $1200$ Hz, surpassing results from SN 2019ejj. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16565v1-abstract-full').style.display = 'none'; document.getElementById('2410.16565v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Main paper: 6 pages, 4 figures and 1 table. Total with appendices: 20 pages, 4 figures, and 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2400125 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.09151">arXiv:2410.09151</a> <span> [<a href="https://arxiv.org/pdf/2410.09151">pdf</a>, <a href="https://arxiv.org/format/2410.09151">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> </div> </div> <p class="title is-5 mathjax"> A search using GEO600 for gravitational waves coincident with fast radio bursts from SGR 1935+2154 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Jodah%2C+A">A. Al-Jodah</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a> , et al. (1758 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="2410.09151v1-abstract-short" style="display: inline;"> The magnetar SGR 1935+2154 is the only known Galactic source of fast radio bursts (FRBs). FRBs from SGR 1935+2154 were first detected by CHIME/FRB and STARE2 in 2020 April, after the conclusion of the LIGO, Virgo, and KAGRA Collaborations' O3 observing run. Here we analyze four periods of gravitational wave (GW) data from the GEO600 detector coincident with four periods of FRB activity detected by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09151v1-abstract-full').style.display = 'inline'; document.getElementById('2410.09151v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.09151v1-abstract-full" style="display: none;"> The magnetar SGR 1935+2154 is the only known Galactic source of fast radio bursts (FRBs). FRBs from SGR 1935+2154 were first detected by CHIME/FRB and STARE2 in 2020 April, after the conclusion of the LIGO, Virgo, and KAGRA Collaborations' O3 observing run. Here we analyze four periods of gravitational wave (GW) data from the GEO600 detector coincident with four periods of FRB activity detected by CHIME/FRB, as well as X-ray glitches and X-ray bursts detected by NICER and NuSTAR close to the time of one of the FRBs. We do not detect any significant GW emission from any of the events. Instead, using a short-duration GW search (for bursts $\leq$ 1 s) we derive 50\% (90\%) upper limits of $10^{48}$ ($10^{49}$) erg for GWs at 300 Hz and $10^{49}$ ($10^{50}$) erg at 2 kHz, and constrain the GW-to-radio energy ratio to $\leq 10^{14} - 10^{16}$. We also derive upper limits from a long-duration search for bursts with durations between 1 and 10 s. These represent the strictest upper limits on concurrent GW emission from FRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09151v1-abstract-full').style.display = 'none'; document.getElementById('2410.09151v1-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> 11 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">15 pages of text including references, 4 figures, 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2400192 </p> </li> <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/astro-ph?searchtype=author&query=Raman%2C+G">Gayathri Raman</a>, <a href="/search/astro-ph?searchtype=author&query=Ronchini%2C+S">Samuele Ronchini</a>, <a href="/search/astro-ph?searchtype=author&query=Delaunay%2C+J">James Delaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">Aaron Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">Jamie A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Parsotan%2C+T">Tyler Parsotan</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+E">Elena Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+M+G">Maria Grazia Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Cusumano%2C+G">Giancarlo Cusumano</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ai%2C+A">Antonino D'Ai</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">Paolo D'Avanzo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Elia%2C+V">Valerio D'Elia</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pasquale%2C+M">Massimiliano De Pasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Dichiara%2C+S">Simone Dichiara</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P">Phil Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">Dieter Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kuin%2C+P">Paul Kuin</a>, <a href="/search/astro-ph?searchtype=author&query=Melandri%2C+A">Andrea Melandri</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+J+P">Julian P. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K">Kim Page</a>, <a href="/search/astro-ph?searchtype=author&query=Palmer%2C+D+M">David M. Palmer</a>, <a href="/search/astro-ph?searchtype=author&query=Sbarufatti%2C+B">Boris Sbarufatti</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Abchouyeh%2C+M+A">M. Aghaei Abchouyeh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%C3%A7ay%2C+S">S. Ak莽ay</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abouelfettouh%2C+I">I. Abouelfettouh</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adamcewicz%2C+C">C. Adamcewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?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/2309.07228">arXiv:2309.07228</a> <span> [<a href="https://arxiv.org/pdf/2309.07228">pdf</a>, <a href="https://arxiv.org/format/2309.07228">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/PhysRevLett.132.101401">10.1103/PhysRevLett.132.101401 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling the merger structure of black hole binaries in generic planar orbits </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carullo%2C+G">Gregorio Carullo</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">Simone Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Nagar%2C+A">Alessandro Nagar</a>, <a href="/search/astro-ph?searchtype=author&query=Gamba%2C+R">Rossella Gamba</a>, <a href="/search/astro-ph?searchtype=author&query=Bernuzzi%2C+S">Sebastiano Bernuzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">Tomas Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Trenado%2C+J">Juan Trenado</a> </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="2309.07228v3-abstract-short" style="display: inline;"> The precise modeling of binary black hole coalescences in generic planar orbits is a crucial step to disentangle dynamical and isolated binary formation channels through gravitational-wave observations. The merger regime of such coalescences exhibits a significantly higher complexity compared to the quasicircular case, and cannot be readily described through standard parameterizations in terms of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07228v3-abstract-full').style.display = 'inline'; document.getElementById('2309.07228v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.07228v3-abstract-full" style="display: none;"> The precise modeling of binary black hole coalescences in generic planar orbits is a crucial step to disentangle dynamical and isolated binary formation channels through gravitational-wave observations. The merger regime of such coalescences exhibits a significantly higher complexity compared to the quasicircular case, and cannot be readily described through standard parameterizations in terms of eccentricity and anomaly. In the spirit of the Effective One Body formalism, we build on the study of the test-mass limit, and introduce a new modelling strategy to describe the general-relativistic dynamics of two-body systems in generic orbits. This is achieved through gauge-invariant combinations of the binary energy and angular momentum, such as a dynamical "impact parameter" at merger. These variables reveal simple "quasi-universal" structures of the pivotal merger parameters, allowing to build an accurate analytical representation of generic (bounded and dynamically-bounded) orbital configurations. We demonstrate the validity of these analytical relations using 311 numerical simulations of bounded noncircular binaries with progenitors from the RIT and SXS catalogs, together with a custom dataset of dynamical captures generated using the Einstein Toolkit, and test-mass data in bound orbits. Our modeling strategy lays the foundations of accurate and complete waveform models for systems in arbitrary orbits, bolstering observational explorations of dynamical formation scenarios and the discovery of new classes of gravitational wave sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07228v3-abstract-full').style.display = 'none'; document.getElementById('2309.07228v3-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">v2: extended to spinning case. Matches journal version; v3: fix formatting issue in Suppl. Mat</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> VIR-0804A-23 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 132, 101401 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.13666">arXiv:2308.13666</a> <span> [<a href="https://arxiv.org/pdf/2308.13666">pdf</a>, <a href="https://arxiv.org/format/2308.13666">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> </div> </div> <p class="title is-5 mathjax"> A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-Wave Candidates from the Third Gravitational-wave Observing Run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fletcher%2C+C">C. Fletcher</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+J">J. Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Hamburg%2C+R">R. Hamburg</a>, <a href="/search/astro-ph?searchtype=author&query=Veres%2C+P">P. Veres</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. M. Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Briggs%2C+M+S">M. S. Briggs</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Cleveland%2C+W+H">W. H. Cleveland</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+M+M">M. M. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">A. Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">B. A. Hristov</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">S. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Mailyan%2C+B">B. Mailyan</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">C. Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Poolakkil%2C+S">S. Poolakkil</a>, <a href="/search/astro-ph?searchtype=author&query=von+Kienlin%2C+A">A. von Kienlin</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">C. A. Wilson-Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+T+F+G+B+M">The Fermi Gamma-ray Burst Monitor Team</a>, <a href="/search/astro-ph?searchtype=author&query=Crnogor%C4%8Devi%C4%87%2C+M">M. Crnogor膷evi膰</a>, <a href="/search/astro-ph?searchtype=author&query=DeLaunay%2C+J">J. DeLaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">A. Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Caputo%2C+R">R. Caputo</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a> , et al. (1674 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="2308.13666v1-abstract-short" style="display: inline;"> We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13666v1-abstract-full').style.display = 'inline'; document.getElementById('2308.13666v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.13666v1-abstract-full" style="display: none;"> We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma-rays from binary black hole mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13666v1-abstract-full').style.display = 'none'; document.getElementById('2308.13666v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.03822">arXiv:2308.03822</a> <span> [<a href="https://arxiv.org/pdf/2308.03822">pdf</a>, <a href="https://arxiv.org/format/2308.03822">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> </div> </div> <p class="title is-5 mathjax"> Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abac%2C+A+G">A. G. Abac</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adamcewicz%2C+C">C. Adamcewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+I">I. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a> , et al. (1750 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="2308.03822v1-abstract-short" style="display: inline;"> Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03822v1-abstract-full').style.display = 'inline'; document.getElementById('2308.03822v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.03822v1-abstract-full" style="display: none;"> Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that were already identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total mass $M>70$ $M_\odot$) binaries covering eccentricities up to 0.3 at 15 Hz orbital frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place an upper limit for the merger rate density of high-mass binaries with eccentricities $0 < e \leq 0.3$ at $0.33$ Gpc$^{-3}$ yr$^{-1}$ at 90\% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03822v1-abstract-full').style.display = 'none'; document.getElementById('2308.03822v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">24 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-P2300080 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.08697">arXiv:2307.08697</a> <span> [<a href="https://arxiv.org/pdf/2307.08697">pdf</a>, <a href="https://arxiv.org/format/2307.08697">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> <p class="title is-5 mathjax"> Towards numerical-relativity informed effective-one-body waveforms for dynamical capture black hole binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">Tomas Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Trenado%2C+J">Juan Trenado</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">Simone Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Gamba%2C+R">Rossella Gamba</a>, <a href="/search/astro-ph?searchtype=author&query=Bernuzzi%2C+S">Sebastiano Bernuzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Nagar%2C+A">Alessandro Nagar</a>, <a href="/search/astro-ph?searchtype=author&query=Calderon-Bustillo%2C+J">Juan Calderon-Bustillo</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchis-Gual%2C+N">Nicolas Sanchis-Gual</a>, <a href="/search/astro-ph?searchtype=author&query=Font%2C+J+A">Jose A. Font</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+W">William Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Daszuta%2C+B">Boris Daszuta</a>, <a href="/search/astro-ph?searchtype=author&query=Zappa%2C+F">Francesco Zappa</a>, <a href="/search/astro-ph?searchtype=author&query=Radice%2C+D">David Radice</a> </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="2307.08697v1-abstract-short" style="display: inline;"> Dynamical captures of black holes may take place in dense stellar media due to the emission of gravitational radiation during a close passage. Detection of such events requires detailed modelling, since their phenomenology qualitatively differs from that of quasi-circular binaries. Very few models can deliver such waveforms, and none includes information from Numerical Relativity (NR) simulations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08697v1-abstract-full').style.display = 'inline'; document.getElementById('2307.08697v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08697v1-abstract-full" style="display: none;"> Dynamical captures of black holes may take place in dense stellar media due to the emission of gravitational radiation during a close passage. Detection of such events requires detailed modelling, since their phenomenology qualitatively differs from that of quasi-circular binaries. Very few models can deliver such waveforms, and none includes information from Numerical Relativity (NR) simulations of non quasi-circular coalescences. In this study we present a first step towards a fully NR-informed Effective One Body (EOB) model of dynamical captures. We perform 14 new simulations of single and double encounter mergers, and use this data to inform the merger-ringdown model of the TEOBResumS-Dali approximant. We keep the initial energy approximately fixed to the binary mass, and vary the mass-rescaled, dimensionless angular momentum in the range $(0.6, 1.1)$, the mass ratio in $(1, 2.15)$ and aligned dimensionless spins in $(-0.5, 0.5)$. We find that the model is able to match NR to $97%$, improving previous performances, without the need of modifying the base-line template. Upon NR informing the model, this improves to $99%$ with the exception of one outlier corresponding to a direct plunge. The maximum EOBNR phase difference at merger for the uninformed model is of $0.15$ radians, which is reduced to $0.1$ radians after the NR information is introduced. We outline the steps towards a fully informed EOB model of dynamical captures, and discuss future improvements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08697v1-abstract-full').style.display = 'none'; document.getElementById('2307.08697v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">21 pages, 15 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/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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/2212.01477">arXiv:2212.01477</a> <span> [<a href="https://arxiv.org/pdf/2212.01477">pdf</a>, <a href="https://arxiv.org/format/2212.01477">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="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/10.1093/mnras/stad3120">10.1093/mnras/stad3120 <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 black hole binaries in the second part of Advanced LIGO's and Advanced Virgo's third observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a> , et al. (1680 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="2212.01477v2-abstract-short" style="display: inline;"> We describe a search for gravitational waves from compact binaries with at least one component with mass 0.2 $M_\odot$ -- $1.0 M_\odot$ and mass ratio $q \geq 0.1$ in Advanced LIGO and Advanced Virgo data collected between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. No signals were detected. The most significant candidate has a false alarm rate of 0.2 $\mathrm{yr}^{-1}$. We estimate t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.01477v2-abstract-full').style.display = 'inline'; document.getElementById('2212.01477v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.01477v2-abstract-full" style="display: none;"> We describe a search for gravitational waves from compact binaries with at least one component with mass 0.2 $M_\odot$ -- $1.0 M_\odot$ and mass ratio $q \geq 0.1$ in Advanced LIGO and Advanced Virgo data collected between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. No signals were detected. The most significant candidate has a false alarm rate of 0.2 $\mathrm{yr}^{-1}$. We estimate the sensitivity of our search over the entirety of Advanced LIGO's and Advanced Virgo's third observing run, and present the most stringent limits to date on the merger rate of binary black holes with at least one subsolar-mass component. We use the upper limits to constrain two fiducial scenarios that could produce subsolar-mass black holes: primordial black holes (PBH) and a model of dissipative dark matter. The PBH model uses recent prescriptions for the merger rate of PBH binaries that include a rate suppression factor to effectively account for PBH early binary disruptions. If the PBHs are monochromatically distributed, we can exclude a dark matter fraction in PBHs $f_\mathrm{PBH} \gtrsim 0.6$ (at 90% confidence) in the probed subsolar-mass range. However, if we allow for broad PBH mass distributions we are unable to rule out $f_\mathrm{PBH} = 1$. For the dissipative model, where the dark matter has chemistry that allows a small fraction to cool and collapse into black holes, we find an upper bound $f_{\mathrm{DBH}} < 10^{-5}$ on the fraction of atomic dark matter collapsed into black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.01477v2-abstract-full').style.display = 'none'; document.getElementById('2212.01477v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">https://dcc.ligo.org/P2200139</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.15634">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/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/astro-ph?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/astro-ph?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/astro-ph?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/astro-ph?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/astro-ph?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/astro-ph?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/astro-ph?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/astro-ph?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/astro-ph?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/astro-ph?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/astro-ph?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/astro-ph?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/astro-ph?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/astro-ph?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/astro-ph?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/astro-ph?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/astro-ph?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/2210.10931">arXiv:2210.10931</a> <span> [<a href="https://arxiv.org/pdf/2210.10931">pdf</a>, <a href="https://arxiv.org/format/2210.10931">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> </div> </div> <p class="title is-5 mathjax"> Search for gravitational-wave transients associated with magnetar bursts in Advanced LIGO and Advanced Virgo data from the third observing run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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="2210.10931v1-abstract-short" style="display: inline;"> Gravitational waves are expected to be produced from neutron star oscillations associated with magnetar giant flares and short bursts. We present the results of a search for short-duration (milliseconds to seconds) and long-duration ($\sim$ 100 s) transient gravitational waves from 13 magnetar short bursts observed during Advanced LIGO, Advanced Virgo and KAGRA's third observation run. These 13 bu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10931v1-abstract-full').style.display = 'inline'; document.getElementById('2210.10931v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.10931v1-abstract-full" style="display: none;"> Gravitational waves are expected to be produced from neutron star oscillations associated with magnetar giant flares and short bursts. We present the results of a search for short-duration (milliseconds to seconds) and long-duration ($\sim$ 100 s) transient gravitational waves from 13 magnetar short bursts observed during Advanced LIGO, Advanced Virgo and KAGRA's third observation run. These 13 bursts come from two magnetars, SGR 1935$+$2154 and Swift J1818.0$-$1607. We also include three other electromagnetic burst events detected by Fermi GBM which were identified as likely coming from one or more magnetars, but they have no association with a known magnetar. No magnetar giant flares were detected during the analysis period. We find no evidence of gravitational waves associated with any of these 16 bursts. We place upper bounds on the root-sum-square of the integrated gravitational-wave strain that reach $2.2 \times 10^{-23}$ $/\sqrt{\text{Hz}}$ at 100 Hz for the short-duration search and $8.7 \times 10^{-23}$ $/\sqrt{\text{Hz}}$ at $450$ Hz for the long-duration search, given a detection efficiency of 50%. For a ringdown signal at 1590 Hz targeted by the short-duration search the limit is set to $1.8 \times 10^{-22}$ $/\sqrt{\text{Hz}}$. Using the estimated distance to each magnetar, we derive upper bounds on the emitted gravitational-wave energy of $3.2 \times 10^{43}$ erg ($7.3 \times 10^{43}$ erg) for SGR 1935$+$2154 and $8.2 \times 10^{42}$ erg ($2.8 \times 10^{43}$ erg) for Swift J1818.0$-$1607, for the short-duration (long-duration) search. Assuming isotropic emission of electromagnetic radiation of the burst fluences, we constrain the ratio of gravitational-wave energy to electromagnetic energy for bursts from SGR 1935$+$2154 with available fluence information. The lowest of these ratios is $3 \times 10^3$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10931v1-abstract-full').style.display = 'none'; document.getElementById('2210.10931v1-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, 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">30 pages with appendices, 5 figures, 10 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P2100387 </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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhicary%2C+S">S. Adhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=All%C3%A9n%C3%A9%2C+C">C. All茅n茅</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/astro-ph?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/astro-ph?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/astro-ph?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/astro-ph?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/astro-ph?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/astro-ph?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/astro-ph?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/astro-ph?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/2203.12038">arXiv:2203.12038</a> <span> [<a href="https://arxiv.org/pdf/2203.12038">pdf</a>, <a href="https://arxiv.org/format/2203.12038">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> </div> </div> <p class="title is-5 mathjax"> Search for Gravitational Waves Associated with Fast Radio Bursts Detected by CHIME/FRB During the LIGO--Virgo Observing Run O3a </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+t+C">the CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1633 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="2203.12038v1-abstract-short" style="display: inline;"> We search for gravitational-wave transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB), during the first part of the third observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC-1 Oct 2019 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets compact binary coal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12038v1-abstract-full').style.display = 'inline'; document.getElementById('2203.12038v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.12038v1-abstract-full" style="display: none;"> We search for gravitational-wave transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB), during the first part of the third observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC-1 Oct 2019 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets compact binary coalescences with at least one neutron star component. A targeted search for generic gravitational-wave transients was conducted on 40 FRBs. We find no significant evidence for a gravitational-wave association in either search. Given the large uncertainties in the distances of the FRBs inferred from the dispersion measures in our sample, however, this does not conclusively exclude any progenitor models that include emission of a gravitational wave of the types searched for from any of these FRB events. We report $90\%$ confidence lower bounds on the distance to each FRB for a range of gravitational-wave progenitor models. By combining the inferred maximum distance information for each FRB with the sensitivity of the gravitational-wave searches, we set upper limits on the energy emitted through gravitational waves for a range of emission scenarios. We find values of order $10^{51}$-$10^{57}$ erg for a range of different emission models with central gravitational wave frequencies in the range 70-3560 Hz. Finally, we also found no significant coincident detection of gravitational waves with the repeater, FRB 20200120E, which is the closest known extragalactic FRB. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12038v1-abstract-full').style.display = 'none'; document.getElementById('2203.12038v1-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">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">35 pages, 6 figures, 8 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2100124 </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/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9s-Carcasona%2C+M">M. Andr茅s-Carcasona</a>, <a href="/search/astro-ph?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/astro-ph?searchtype=author&query=Apostolatos%2C+T">T. Apostolatos</a>, <a href="/search/astro-ph?searchtype=author&query=Appavuravther%2C+E+Z">E. Z. Appavuravther</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/astro-ph?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/astro-ph?searchtype=author&query=Melo%2C+S+A+d+S">S. Assis de Souza Melo</a>, <a href="/search/astro-ph?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/astro-ph?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/astro-ph?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/2201.00697">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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=de+Alarc%C3%B3n%2C+P+F">P. F. de Alarc贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?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/2111.15507">arXiv:2111.15507</a> <span> [<a href="https://arxiv.org/pdf/2111.15507">pdf</a>, <a href="https://arxiv.org/format/2111.15507">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> </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.105.102001">10.1103/PhysRevD.105.102001 <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 gravitational wave emission from scalar boson clouds around spinning black holes in LIGO O3 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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="2111.15507v2-abstract-short" style="display: inline;"> This paper describes the first all-sky search for long-duration, quasi-monochromatic gravitational-wave signals emitted by ultralight scalar boson clouds around spinning black holes using data from the third observing run of Advanced LIGO. We analyze the frequency range from 20~Hz to 610~Hz, over a small frequency derivative range around zero, and use multiple frequency resolutions to be robust to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.15507v2-abstract-full').style.display = 'inline'; document.getElementById('2111.15507v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.15507v2-abstract-full" style="display: none;"> This paper describes the first all-sky search for long-duration, quasi-monochromatic gravitational-wave signals emitted by ultralight scalar boson clouds around spinning black holes using data from the third observing run of Advanced LIGO. We analyze the frequency range from 20~Hz to 610~Hz, over a small frequency derivative range around zero, and use multiple frequency resolutions to be robust towards possible signal frequency wanderings. Outliers from this search are followed up using two different methods, one more suitable for nearly monochromatic signals, and the other more robust towards frequency fluctuations. We do not find any evidence for such signals and set upper limits on the signal strain amplitude, the most stringent being $\approx10^{-25}$ at around 130~Hz. We interpret these upper limits as both an "exclusion region" in the boson mass/black hole mass plane and the maximum detectable distance for a given boson mass, based on an assumption of the age of the black hole/boson cloud system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.15507v2-abstract-full').style.display = 'none'; document.getElementById('2111.15507v2-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 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">28 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2100343 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 105, 102001, 2022 </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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akcay%2C+S">S. Akcay</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+V+K">V. K. Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaidi%2C+R+A">R. A. Alfaidi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?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/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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/astro-ph?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/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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=Virgo+Collaboration"> Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+A">A. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Andres%2C+N">N. Andres</a>, <a href="/search/astro-ph?searchtype=author&query=Andri%C4%87%2C+T">T. Andri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A8ne%2C+M">M. Ar猫ne</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaud%2C+N">N. Arnaud</a>, <a href="/search/astro-ph?searchtype=author&query=Assiduo%2C+M">M. Assiduo</a>, <a href="/search/astro-ph?searchtype=author&query=Astone%2C+P">P. Astone</a>, <a href="/search/astro-ph?searchtype=author&query=Aubin%2C+F">F. Aubin</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Badaracco%2C+F">F. Badaracco</a>, <a href="/search/astro-ph?searchtype=author&query=Bader%2C+M+K+M">M. K. M. Bader</a>, <a href="/search/astro-ph?searchtype=author&query=Bagnasco%2C+S">S. Bagnasco</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardin%2C+G">G. Ballardin</a>, <a href="/search/astro-ph?searchtype=author&query=Baltus%2C+G">G. Baltus</a>, <a href="/search/astro-ph?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/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/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P+A">P. A. Altin</a>, <a href="/search/astro-ph?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/1601.03396">arXiv:1601.03396</a> <span> [<a href="https://arxiv.org/pdf/1601.03396">pdf</a>, <a href="https://arxiv.org/ps/1601.03396">ps</a>, <a href="https://arxiv.org/format/1601.03396">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.3847/0004-637X/819/2/131">10.3847/0004-637X/819/2/131 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> He II $位$4686 emission from the massive binary system in $畏$ Car: constraints to the orbital elements and the nature of the periodic minima </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Teodoro%2C+M">M. Teodoro</a>, <a href="/search/astro-ph?searchtype=author&query=Damineli%2C+A">A. Damineli</a>, <a href="/search/astro-ph?searchtype=author&query=Heathcote%2C+B">B. Heathcote</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+N+D">N. D. Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Moffat%2C+A+F+J">A. F. J. Moffat</a>, <a href="/search/astro-ph?searchtype=author&query=St-Jean%2C+L">L. St-Jean</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+C">C. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Gull%2C+T+R">T. R. Gull</a>, <a href="/search/astro-ph?searchtype=author&query=Madura%2C+T+I">T. I. Madura</a>, <a href="/search/astro-ph?searchtype=author&query=Pollard%2C+K+R">K. R. Pollard</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Coimbra%2C+A">A. Coimbra</a>, <a href="/search/astro-ph?searchtype=author&query=Prates%2C+R">R. Prates</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Laj%C3%BAs%2C+E">E. Fern谩ndez-Laj煤s</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R+C">R. C. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Hickel%2C+G">G. Hickel</a>, <a href="/search/astro-ph?searchtype=author&query=Henrique%2C+W">W. Henrique</a>, <a href="/search/astro-ph?searchtype=author&query=Navarete%2C+F">F. Navarete</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+T">T. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonski%2C+F">F. Jablonski</a>, <a href="/search/astro-ph?searchtype=author&query=Luckas%2C+P">P. Luckas</a>, <a href="/search/astro-ph?searchtype=author&query=Locke%2C+M">M. Locke</a>, <a href="/search/astro-ph?searchtype=author&query=Powles%2C+J">J. Powles</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlsen%2C+T">T. Bohlsen</a>, <a href="/search/astro-ph?searchtype=author&query=Chini%2C+R">R. Chini</a> , et al. (5 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="1601.03396v1-abstract-short" style="display: inline;"> 畏 Carinae is an extremely massive binary system in which rapid spectrum variations occur near periastron. Most notably, near periastron the He II $位4686$ line increases rapidly in strength, drops to a minimum value, then increases briefly before fading away. To understand this behavior, we conducted an intense spectroscopic monitoring of the He II $位4686$ emission line across the 2014.6 periastron… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.03396v1-abstract-full').style.display = 'inline'; document.getElementById('1601.03396v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.03396v1-abstract-full" style="display: none;"> 畏 Carinae is an extremely massive binary system in which rapid spectrum variations occur near periastron. Most notably, near periastron the He II $位4686$ line increases rapidly in strength, drops to a minimum value, then increases briefly before fading away. To understand this behavior, we conducted an intense spectroscopic monitoring of the He II $位4686$ emission line across the 2014.6 periastron passage using ground- and space-based telescopes. Comparison with previous data confirmed the overall repeatability of EW(He II $位4686$), the line radial velocities, and the timing of the minimum, though the strongest peak was systematically larger in 2014 than in 2009 by 26%. The EW(He II $位4686$) variations, combined with other measurements, yield an orbital period $2022.7\pm0.3$ d. The observed variability of the EW(He II $位4686$) was reproduced by a model in which the line flux primarily arises at the apex of the wind-wind collision and scales inversely with the square of the stellar separation, if we account for the excess emission as the companion star plunges into the hot inner layers of the primary's atmosphere, and including absorption from the disturbed primary wind between the source and the observer. This model constrains the orbital inclination to $135^\circ$-$153^\circ$, and the longitude of periastron to $234^\circ$-$252^\circ$. It also suggests that periastron passage occurred on $T_0 = 2456874.4\pm1.3$ d. Our model also reproduced EW(He II $位4686$) variations from a polar view of the primary star as determined from the observed He II $位4686$ emission scattered off the Homunculus nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.03396v1-abstract-full').style.display = 'none'; document.getElementById('1601.03396v1-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </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">The article contains 23 pages and 17 figures. It has been accepted for publication in ApJ</span> </p> </li> </ol> <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>

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