{"topic":"gravitational-waves","sort":"top","limit":25,"offset":0,"count":25,"papers":[{"id":"arxiv:1602.03837","kind":"article","title":"Observation of Gravitational Waves from a Binary Black Hole Merger","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","M. R. Abernathy","F. Acernese","K. Ackley","C. Adams","Thomas Adams","Paolo Addesso","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","B. Allen","A. Allocca","P. A. Altin","S. B. Anderson","Warren G. Anderson","Koji Arai"],"author_count":100,"year":2016,"published":"2016-02-11","venue":"Physical Review Letters","cited_by":14246,"doi":"10.1103/physrevlett.116.061102","arxiv_id":"1602.03837","nct_id":null,"source_url":"https://doi.org/10.1103/physrevlett.116.061102","archive_url":"https://space-kitty.com/papers/arxiv:1602.03837","updated":"2016-02-11","pmid":"26918975","pmcid":null,"openalex_id":"W2252795400","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevLett.116.061102","abstract":"On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of $1.0 \\times 10^{-21}$. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1 σ. The source lies at a luminosity distance of $410^{+160}_{-180}$ Mpc corresponding to a redshift $z = 0.09^{+0.03}_{-0.04}$. In the source frame, the initial black hole masses are $36^{+5}_{-4} M_\\odot$ and $29^{+4}_{-4} M_\\odot$, and the final black hole mass is $62^{+4}_{-4} M_\\odot$, with $3.0^{+0.5}_{-0.5} M_\\odot c^2$ radiated in gravitational waves. All uncertainties define 90% credible intervals.These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1811.12907","kind":"article","title":"GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","G. Allen","A. Allocca","M. Á. Aloy","P. A. Altin","A. Amato","A. Ananyeva","S. B. Anderson","Warren G. Anderson"],"author_count":100,"year":2019,"published":"2019-09-04","venue":"Physical Review X","cited_by":3529,"doi":"10.1103/physrevx.9.031040","arxiv_id":"1811.12907","nct_id":null,"source_url":"https://doi.org/10.1103/physrevx.9.031040","archive_url":"https://space-kitty.com/papers/arxiv:1811.12907","updated":"2019-10-04","pmid":null,"pmcid":null,"openalex_id":"W2971836485","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevX.9.031040","abstract":"We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1$\\mathrm{M}_\\odot$ during the first and second observing runs of the Advanced gravitational-wave detector network. During the first observing run (O1), from September $12^\\mathrm{th}$, 2015 to January $19^\\mathrm{th}$, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November $30^\\mathrm{th}$, 2016 to August $25^\\mathrm{th}$, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818 and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between $18.6_{-0.7}^{+3.2}\\mathrm{M}_\\odot$, and $84.4_{-11.1}^{+15.8} \\mathrm{M}_\\odot$, and range in distance between $320_{-110}^{+120}$ Mpc and $2840_{-1360}^{+1400}$ Mpc. No neutron star - black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of $110\\, -\\, 3840$ $\\mathrm{Gpc}^{-3}\\,\\mathrm{y}^{-1}$ for binary neutron stars and $9.7\\, -\\, 101$ $\\mathrm{Gpc}^{-3}\\,\\mathrm{y}^{-1}$ for binary black holes assuming fixed population distributions, and determine a neutron star - black hole merger rate 90% upper limit of $610$ $\\mathrm{Gpc}^{-3}\\,\\mathrm{y}^{-1}$.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2010.14527","kind":"article","title":"GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo during the First Half of the Third Observing Run","authors":["R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","A. Adams","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","S. Akcay","G. Allen","A. Allocca","P. A. Altin","A. Amato","S. Anand","A. Ananyeva","S. B. Anderson"],"author_count":100,"year":2021,"published":"2021-06-09","venue":"Physical Review X","cited_by":2246,"doi":"10.1103/physrevx.11.021053","arxiv_id":"2010.14527","nct_id":null,"source_url":"https://doi.org/10.1103/physrevx.11.021053","archive_url":"https://space-kitty.com/papers/arxiv:2010.14527","updated":"2021-03-08","pmid":null,"pmcid":null,"openalex_id":"W3094812309","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevX.11.021053","abstract":"We report on gravitational wave discoveries from compact binary coalescences detected by Advanced LIGO and Advanced Virgo in the first half of the third observing run (O3a) between 1 April 2019 15:00 UTC and 1 October 2019 15:00. By imposing a false-alarm-rate threshold of two per year in each of the four search pipelines that constitute our search, we present 39 candidate gravitational wave events. At this threshold, we expect a contamination fraction of less than 10%. Of these, 26 candidate events were reported previously in near real-time through GCN Notices and Circulars; 13 are reported here for the first time. The catalog contains events whose sources are black hole binary mergers up to a redshift of ~0.8, as well as events whose components could not be unambiguously identified as black holes or neutron stars. For the latter group, we are unable to determine the nature based on estimates of the component masses and spins from gravitational wave data alone. The range of candidate events which are unambiguously identified as binary black holes (both objects $\\geq 3~M_\\odot$) is increased compared to GWTC-1, with total masses from $\\sim 14~M_\\odot$ for GW190924_021846 to $\\sim 150~M_\\odot$ for GW190521. For the first time, this catalog includes binary systems with significantly asymmetric mass ratios, which had not been observed in data taken before April 2019. We also find that 11 of the 39 events detected since April 2019 have positive effective inspiral spins under our default prior (at 90% credibility), while none exhibit negative effective inspiral spin. Given the increased sensitivity of Advanced LIGO and Advanced Virgo, the detection of 39 candidate events in ~26 weeks of data (~1.5 per week) is consistent with GWTC-1.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2006.12611","kind":"article","title":"GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object","authors":["R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","A. Aich","L. Aiello","A. Ain","P. Ajith","S. Akcay","G. Allen","A. Allocca","P. A. Altin","A. Amato","S. Anand","A. Ananyeva","S. B. Anderson"],"author_count":100,"year":2020,"published":"2020-06-01","venue":"The Astrophysical Journal Letters","cited_by":1830,"doi":"10.3847/2041-8213/ab960f","arxiv_id":"2006.12611","nct_id":null,"source_url":"https://doi.org/10.3847/2041-8213/ab960f","archive_url":"https://space-kitty.com/papers/arxiv:2006.12611","updated":"2020-06-22","pmid":null,"pmcid":null,"openalex_id":"W3036761016","pdf_url":"https://iopscience.iop.org/article/10.3847/2041-8213/ab960f/pdf","abstract":"We report the observation of a compact binary coalescence involving a 22.2 - 24.3 $M_{\\odot}$ black hole and a compact object with a mass of 2.50 - 2.67 $M_{\\odot}$ (all measurements quoted at the 90$\\%$ credible level). The gravitational-wave signal, GW190814, was observed during LIGO's and Virgo's third observing run on August 14, 2019 at 21:10:39 UTC and has a signal-to-noise ratio of 25 in the three-detector network. The source was localized to 18.5 deg$^2$ at a distance of $241^{+41}_{-45}$ Mpc; no electromagnetic counterpart has been confirmed to date. The source has the most unequal mass ratio yet measured with gravitational waves, $0.112^{+0.008}_{-0.009}$, and its secondary component is either the lightest black hole or the heaviest neutron star ever discovered in a double compact-object system. The dimensionless spin of the primary black hole is tightly constrained to $\\leq 0.07$. Tests of general relativity reveal no measurable deviations from the theory, and its prediction of higher-multipole emission is confirmed at high confidence. We estimate a merger rate density of 1-23 Gpc$^{-3}$ yr$^{-1}$ for the new class of binary coalescence sources that GW190814 represents. Astrophysical models predict that binaries with mass ratios similar to this event can form through several channels, but are unlikely to have formed in globular clusters. However, the combination of mass ratio, component masses, and the inferred merger rate for this event challenges all current models for the formation and mass distribution of compact-object binaries.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2001.01761","kind":"article","title":"GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M ⊙","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","G. Allen","A. Allocca","M. Á. Aloy","P. A. Altin","A. Amato","Shreya Anand","A. Ananyeva","S. B. Anderson"],"author_count":100,"year":2020,"published":"2020-03-19","venue":"The Astrophysical Journal Letters","cited_by":1607,"doi":"10.3847/2041-8213/ab75f5","arxiv_id":"2001.01761","nct_id":null,"source_url":"https://doi.org/10.3847/2041-8213/ab75f5","archive_url":"https://space-kitty.com/papers/arxiv:2001.01761","updated":"2020-04-07","pmid":null,"pmcid":null,"openalex_id":"W2999365684","pdf_url":"https://iris.uniss.it/bitstream/11388/353835/1/Abbott_GW190425_2020.pdf","abstract":"On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from 1.12 to 2.52 $M_{\\odot}$ (1.45 to 1.88 $M_{\\odot}$ if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass $1.44^{+0.02}_{-0.02} M_{\\odot}$ and the total mass $3.4^{+0.3}_{-0.1}\\,M_{\\odot}$ of this system are significantly larger than those of any other known binary neutron star system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic binary neutron star population. Under the assumption that the signal was produced by a binary neutron star coalescence, the local rate of neutron star mergers is updated to $250-2810 \\text{Gpc}^{-3}\\text{yr}^{-1}$.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1602.03841","kind":"article","title":"Tests of General Relativity with GW150914","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","M. R. Abernathy","F. Acernese","K. Ackley","C. Adams","Thomas Adams","Paolo Addesso","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","B. Allen","A. Allocca","P. A. Altin","S. B. Anderson","Warren G. Anderson","Koji Arai"],"author_count":100,"year":2016,"published":"2016-05-31","venue":"Physical Review Letters","cited_by":1780,"doi":"10.1103/physrevlett.116.221101","arxiv_id":"1602.03841","nct_id":null,"source_url":"https://doi.org/10.1103/physrevlett.116.221101","archive_url":"https://space-kitty.com/papers/arxiv:1602.03841","updated":"2018-10-23","pmid":"27314708","pmcid":null,"openalex_id":"W2273892807","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevLett.116.221101","abstract":"The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (post-inspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasi-normal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parameterized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a $90\\%$-confidence lower bound of $10^{13}$ km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2009.01075","kind":"article","title":"GW190521: A Binary Black Hole Merger with a Total Mass of 150 M ⊙","authors":["R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","A. Aich","L. Aiello","A. Ain","P. Ajith","Sarp Akçay","G. Allen","A. Allocca","P. A. Altin","A. Amato","Shreya Anand","A. Ananyeva","S. B. Anderson"],"author_count":100,"year":2020,"published":"2020-09-02","venue":"Physical Review Letters","cited_by":1312,"doi":"10.1103/physrevlett.125.101102","arxiv_id":"2009.01075","nct_id":null,"source_url":"https://doi.org/10.1103/physrevlett.125.101102","archive_url":"https://space-kitty.com/papers/arxiv:2009.01075","updated":"2020-09-02","pmid":"32955328","pmcid":null,"openalex_id":"W3081939279","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevLett.125.101102","abstract":"On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of $85^{+21}_{-14} M_{\\odot}$ and $66^{+17}_{-18} M_{\\odot}$ (90 % credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, and has only a 0.32 % probability of being below $65 M_{\\odot}$. We calculate the mass of the remnant to be $142^{+28}_{-16} M_{\\odot}$, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is $5.3^{+2.4}_{-2.6}$ Gpc, corresponding to a redshift of $0.82^{+0.28}_{-0.34}$. The inferred rate of mergers similar to GW190521 is $0.13^{+0.30}_{-0.11}\\,\\mathrm{Gpc}^{-3}\\,\\mathrm{yr}^{-1}$.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2306.16215","kind":"article","title":"Search for an isotropic gravitational-wave background with the Parkes Pulsar Timing Array","authors":["Daniel J. Reardon","Andrew Zic","Ryan M. Shannon","George B. Hobbs","Matthew Bailes","Valentina Di Marco","Agastya Kapur","Axl F. Rogers","Eric Thrane","Jacob Askew","N. D. Ramesh Bhat","Andrew Cameron","Małgorzata Curyło","William A. Coles","Shi Dai","Boris Goncharov","Matthew Kerr","Atharva Kulkarni","Yuri Levin","Marcus E. Lower","Richard N. Manchester","Rami Mandow","Matthew T. Miles","Rowina S. Nathan","Stefan Osłowski"],"author_count":29,"year":2023,"published":"2023-06-28","venue":"The Astrophysical Journal Letters","cited_by":1160,"doi":"10.3847/2041-8213/acdd02","arxiv_id":"2306.16215","nct_id":null,"source_url":"https://arxiv.org/abs/2306.16215","archive_url":"https://space-kitty.com/papers/arxiv:2306.16215","updated":"2023-06-28","pmid":null,"pmcid":null,"openalex_id":"W4382358671","pdf_url":"https://arxiv.org/pdf/2306.16215","abstract":"Pulsar timing arrays aim to detect nanohertz-frequency gravitational waves (GWs). A background of GWs modulates pulsar arrival times and manifests as a stochastic process, common to all pulsars, with a signature spatial correlation. Here we describe a search for an isotropic stochastic gravitational-wave background (GWB) using observations of 30 millisecond pulsars from the third data release of the Parkes Pulsar Timing Array (PPTA), which spans 18 years. Using current Bayesian inference techniques we recover and characterize a common-spectrum noise process. Represented as a strain spectrum $h_c = A(f/1 {\\rm yr}^{-1})^α$, we measure $A=3.1^{+1.3}_{-0.9} \\times 10^{-15}$ and $α=-0.45 \\pm 0.20$ respectively (median and 68% credible interval). For a spectral index of $α=-2/3$, corresponding to an isotropic background of GWs radiated by inspiraling supermassive black hole binaries, we recover an amplitude of $A=2.04^{+0.25}_{-0.22} \\times 10^{-15}$. However, we demonstrate that the apparent signal strength is time-dependent, as the first half of our data set can be used to place an upper limit on $A$ that is in tension with the inferred common-spectrum amplitude using the complete data set. We search for spatial correlations in the observations by hierarchically analyzing individual pulsar pairs, which also allows for significance validation through randomizing pulsar positions on the sky. For a process with $α=-2/3$, we measure spatial correlations consistent with a GWB, with an estimated false-alarm probability of $p \\lesssim 0.02$ (approx. $2σ$). The long timing baselines of the PPTA and the access to southern pulsars will continue to play an important role in the International Pulsar Timing Array.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":false,"peer_reviewed":null,"categories":["astro-ph.HE","astro-ph.CO","astro-ph.GA","gr-qc"],"details":null,"provenance":"arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1606.04856","kind":"article","title":"Binary Black Hole Mergers in the First Advanced LIGO Observing Run","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","M. R. Abernathy","F. Acernese","K. Ackley","C. Adams","Thomas Adams","P. Addesso","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","B. Allen","A. Allocca","P. A. Altin","S. B. Anderson","W. G. Anderson","K. Arai"],"author_count":100,"year":2016,"published":"2016-10-21","venue":"Physical Review X","cited_by":1395,"doi":"10.1103/physrevx.6.041015","arxiv_id":"1606.04856","nct_id":null,"source_url":"https://doi.org/10.1103/physrevx.6.041015","archive_url":"https://space-kitty.com/papers/arxiv:1606.04856","updated":"2018-10-23","pmid":null,"pmcid":null,"openalex_id":"W2423333910","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevX.6.041015","abstract":"The first observational run of the Advanced LIGO detectors, from September 12, 2015 to January 19, 2016, saw the first detections of gravitational waves from binary black hole mergers. In this paper we present full results from a search for binary black hole merger signals with total masses up to $100 M_\\odot$ and detailed implications from our observations of these systems. Our search, based on general-relativistic models of gravitational wave signals from binary black hole systems, unambiguously identified two signals, GW150914 and GW151226, with a significance of greater than $5σ$ over the observing period. It also identified a third possible signal, LVT151012, with substantially lower significance, and with an 87% probability of being of astrophysical origin. We provide detailed estimates of the parameters of the observed systems. Both GW150914 and GW151226 provide an unprecedented opportunity to study the two-body motion of a compact-object binary in the large velocity, highly nonlinear regime. We do not observe any deviations from general relativity, and place improved empirical bounds on several high-order post-Newtonian coefficients. From our observations we infer stellar-mass binary black hole merger rates lying in the range $9-240 \\mathrm{Gpc}^{-3} \\mathrm{yr}^{-1}$. These observations are beginning to inform astrophysical predictions of binary black hole formation rates, and indicate that future observing runs of the Advanced detector network will yield many more gravitational wave detections.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1711.05578","kind":"article","title":"GW170608: Observation of a 19 Solar-mass Binary Black Hole Coalescence","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","F. Acernese","K. Ackley","C. Adams","Thomas Adams","Paolo Addesso","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Afrough","Bhanu Agarwal","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","B. Allen","G. Allen","A. Allocca","P. A. Altin","A. Amato"],"author_count":100,"year":2017,"published":"2017-12-18","venue":"The Astrophysical Journal Letters","cited_by":1231,"doi":"10.3847/2041-8213/aa9f0c","arxiv_id":"1711.05578","nct_id":null,"source_url":"https://doi.org/10.3847/2041-8213/aa9f0c","archive_url":"https://space-kitty.com/papers/arxiv:1711.05578","updated":"2017-11-15","pmid":null,"pmcid":null,"openalex_id":"W2768286292","pdf_url":"https://arxiv.org/pdf/1711.05578","abstract":"On June 8, 2017 at 02:01:16.49 UTC, a gravitational-wave signal from the merger of two stellar-mass black holes was observed by the two Advanced LIGO detectors with a network signal-to-noise ratio of 13. This system is the lightest black hole binary so far observed, with component masses $12^{+7}_{-2}\\,M_\\odot$ and $7^{+2}_{-2}\\,M_\\odot$ (90% credible intervals). These lie in the range of measured black hole masses in low-mass X-ray binaries, thus allowing us to compare black holes detected through gravitational waves with electromagnetic observations. The source's luminosity distance is $340^{+140}_{-140}$ Mpc, corresponding to redshift $0.07^{+0.03}_{-0.03}$. We verify that the signal waveform is consistent with the predictions of general relativity.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1603.00464","kind":"article","title":"Did LIGO Detect Dark Matter?","authors":["Simeon Bird","Ilias Cholis","Julián B. Muñoz","Yacine Ali-Haïmoud","Marc Kamionkowski","Ely D. Kovetz","Alvise Raccanelli","Adam G. Riess"],"author_count":8,"year":2016,"published":"2016-05-19","venue":"Physical Review Letters","cited_by":1226,"doi":"10.1103/physrevlett.116.201301","arxiv_id":"1603.00464","nct_id":null,"source_url":"https://doi.org/10.1103/physrevlett.116.201301","archive_url":"https://space-kitty.com/papers/arxiv:1603.00464","updated":"2016-05-30","pmid":"27258861","pmcid":null,"openalex_id":"W2289010674","pdf_url":"https://arxiv.org/pdf/1603.00464","abstract":"We consider the possibility that the black-hole (BH) binary detected by LIGO may be a signature of dark matter. Interestingly enough, there remains a window for masses $20\\,M_\\odot \\lesssim M_{\\rm bh} \\lesssim 100\\, M_\\odot$ where primordial black holes (PBHs) may constitute the dark matter. If two BHs in a galactic halo pass sufficiently close, they radiate enough energy in gravitational waves to become gravitationally bound. The bound BHs will rapidly spiral inward due to emission of gravitational radiation and ultimately merge. Uncertainties in the rate for such events arise from our imprecise knowledge of the phase-space structure of galactic halos on the smallest scales. Still, reasonable estimates span a range that overlaps the $2-53$ Gpc$^{-3}$ yr$^{-1}$ rate estimated from GW150914, thus raising the possibility that LIGO has detected PBH dark matter. PBH mergers are likely to be distributed spatially more like dark matter than luminous matter and have no optical nor neutrino counterparts. They may be distinguished from mergers of BHs from more traditional astrophysical sources through the observed mass spectrum, their high ellipticities, or their stochastic gravitational wave background. Next generation experiments will be invaluable in performing these tests.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1710.05835","kind":"article","title":"A gravitational-wave standard siren measurement of the Hubble constant","authors":["B. P. Abbott","R. Abbott","T. M. C. Abbott","F. Acernese","K. Ackley","C. Adams","Thomas Adams","Paolo Addesso","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Afrough","Bhanu Agarwal","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","B. Allen","G. Allen","A. Allocca","P. A. Altin","A. Amato"],"author_count":100,"year":2017,"published":"2017-10-16","venue":"Nature","cited_by":1201,"doi":"10.1038/nature24471","arxiv_id":"1710.05835","nct_id":null,"source_url":"https://doi.org/10.1038/nature24471","archive_url":"https://space-kitty.com/papers/arxiv:1710.05835","updated":"2017-10-16","pmid":"29094696","pmcid":null,"openalex_id":"W2766227262","pdf_url":"https://arxiv.org/pdf/1710.05835","abstract":"The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within $\\sim 10$ arcsec of the galaxy NGC 4993. These multi-messenger observations allow us to use GW170817 as a standard siren, the gravitational-wave analog of an astronomical standard candle, to measure the Hubble constant. This quantity, which represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurement combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using electromagnetic data. This approach does not require any form of cosmic \"distance ladder;\" the gravitational wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be $70.0^{+12.0}_{-8.0} \\, \\mathrm{km} \\, \\mathrm{s}^{-1} \\, \\mathrm{Mpc}^{-1}$ (maximum a posteriori and 68% credible interval). This is consistent with existing measurements, while being completely independent of them. Additional standard-siren measurements from future gravitational-wave sources will provide precision constraints of this important cosmological parameter.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by-nc-nd","is_open_access":true,"peer_reviewed":null,"categories":["Cosmology and Gravitation Theories"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"doi:10.1103/physrevx.13.011048","kind":"article","title":"Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3","authors":["R. Abbott","T. D. Abbott","F. Acernese","K. Ackley","C. Adams","N. Adhikari","R. X. Adhikari","V. B. Adya","C. Affeldt","D. Agarwal","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","Tomotada Akutsu","P. F. de Alarcón","Sarp Akçay","Simone Albanesi","A. Allocca","P. A. Altin","A. Amato","C. Anand"],"author_count":100,"year":2023,"published":"2023-03-29","venue":"Physical Review X","cited_by":890,"doi":"10.1103/physrevx.13.011048","arxiv_id":null,"nct_id":null,"source_url":"https://doi.org/10.1103/physrevx.13.011048","archive_url":"https://space-kitty.com/papers/doi:10.1103/physrevx.13.011048","updated":null,"pmid":null,"pmcid":null,"openalex_id":"W4226083230","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevX.13.011048","abstract":"We report on the population properties of compact binary mergers inferred from gravitational-wave observations of these systems during the first three LIGO-Virgo observing runs. The Gravitational-Wave Transient Catalog 3 (GWTC-3) contains signals consistent with three classes of binary mergers: binary black hole, binary neutron star, and neutron star–black hole mergers. We infer the binary neutron star merger rate to be between 10 and 1700 Gpc − 3 yr − 1 and the neutron star–black hole merger rate to be between 7.8 and 140 Gpc − 3 yr − 1 , assuming a constant rate density in the comoving frame and taking the union of 90% credible intervals for methods used in this work. We infer the binary black hole merger rate, allowing for evolution with redshift, to be between 17.9 and 44 Gpc − 3 yr − 1 at a fiducial redshift ( z = 0.2 ). The rate of binary black hole mergers is observed to increase with redshift at a rate proportional to ( 1 + z ) κ with κ = 2. 9 − 1.8 + 1.7 for z ≲ 1 . Using both binary neutron star and neutron star–black hole binaries, we obtain a broad, relatively flat neutron star mass distribution extending from 1.2 − 0.2 + 0.1 to 2.0 − 0.3 + 0.3 M ⊙ . We confidently determine that the merger rate as a function of mass sharply declines after the expected maximum neutron star mass, but cannot yet confirm or rule out the existence of a lower mass gap between neutron stars and black holes. We also find the binary black hole mass distribution has localized over- and underdensities relative to a power-law distribution, with peaks emerging at chirp masses of 8.3 − 0.5 + 0.3 and 27.9 − 1.8 + 1.9 M ⊙ . While we continue to find that 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 approximately 60 M ⊙ , which would indicate the presence of a upper mass gap. Observed black hole spins are small, with half of spin magnitudes below χ i ≈ 0.25 . While the majority of spins are preferentially aligned with the orbital angular momentum, we infer evidenc","abstract_license":"CC-BY (publisher license, via OpenAlex)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex","attribution":"Abstract of \"Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3\" by R. Abbott, T. D. Abbott, F. Acernese et al., https://doi.org/10.1103/physrevx.13.011048, used under its Creative Commons Attribution license (CC-BY); markup removed, otherwise unmodified."},{"id":"arxiv:1811.02042","kind":"article","title":"Bilby: A User-friendly Bayesian Inference Library for Gravitational-wave Astronomy","authors":["Gregory Ashton","Moritz Hübner","Paul D. Lasky","Colm Talbot","Kendall Ackley","S. Biscoveanu","Qi Chu","Atul Divakarla","Paul J. Easter","Boris Goncharov","Francisco Hernandez Vivanco","Jan Harms","Marcus E. Lower","Grant D. Meadors","Denyz Melchor","Ethan Payne","Matthew D. Pitkin","Jade Powell","Nikhil Sarin","Rory J. E. Smith","Eric Thrane"],"author_count":21,"year":2019,"published":"2019-04-01","venue":"The Astrophysical Journal Supplement Series","cited_by":1147,"doi":"10.3847/1538-4365/ab06fc","arxiv_id":"1811.02042","nct_id":null,"source_url":"https://doi.org/10.3847/1538-4365/ab06fc","archive_url":"https://space-kitty.com/papers/arxiv:1811.02042","updated":"2018-11-05","pmid":null,"pmcid":null,"openalex_id":"W2899782607","pdf_url":"https://iopscience.iop.org/article/10.3847/1538-4365/ab06fc/pdf","abstract":"Bayesian parameter estimation is fast becoming the language of gravitational-wave astronomy. It is the method by which gravitational-wave data is used to infer the sources' astrophysical properties. We introduce a user-friendly Bayesian inference library for gravitational-wave astronomy, Bilby. This python code provides expert-level parameter estimation infrastructure with straightforward syntax and tools that facilitate use by beginners. It allows users to perform accurate and reliable gravitational-wave parameter estimation on both real, freely-available data from LIGO/Virgo, and simulated data. We provide a suite of examples for the analysis of compact binary mergers and other types of signal model including supernovae and the remnants of binary neutron star mergers. These examples illustrate how to change the signal model, how to implement new likelihood functions, and how to add new detectors. Bilby has additional functionality to do population studies using hierarchical Bayesian modelling. We provide an example in which we infer the shape of the black hole mass distribution from an ensemble of observations of binary black hole mergers.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1001.5029","kind":"article","title":"Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei","authors":["Brian D. Metzger","Gabriel Martínez-Pinedo","Siva Darbha","Eliot Quataert","Almudena Arcones","Daniel Kasen","R. C. Thomas","P. Nugent","I. V. Panov","Nikolaj Thomas Zinner"],"author_count":10,"year":2010,"published":"2010-06-01","venue":"Monthly Notices of the Royal Astronomical Society","cited_by":1183,"doi":"10.1111/j.1365-2966.2010.16864.x","arxiv_id":"1001.5029","nct_id":null,"source_url":"https://doi.org/10.1111/j.1365-2966.2010.16864.x","archive_url":"https://space-kitty.com/papers/arxiv:1001.5029","updated":"2010-04-23","pmid":null,"pmcid":null,"openalex_id":"W1851157365","pdf_url":"https://arxiv.org/pdf/1001.5029","abstract":"The most promising astrophysical sources of kHz gravitational waves (GWs) are the inspiral and merger of binary neutron star(NS)/black hole systems. Maximizing the scientific return of a GW detection will require identifying a coincident electro-magnetic (EM) counterpart. One of the most likely sources of isotropic EM emission from compact object mergers is a supernova-like transient powered by the radioactive decay of heavy elements synthesized in ejecta from the merger. We present the first calculations of the optical transients from compact object mergers that self-consistently determine the radioactive heating by means of a nuclear reaction network; using this heating rate, we model the light curve with a one dimensional Monte Carlo radiation transfer calculation. For an ejecta mass ~1e-2 M_sun[1e-3 M_sun] the resulting light curve peaks on a timescale ~ 1 day at a V-band luminosity nu L_nu ~ 3e41[1e41] ergs/s (M_V = -15[-14]); this corresponds to an effective \"f\" parameter ~3e-6 in the Li-Paczynski toy model. We argue that these results are relatively insensitive to uncertainties in the relevant nuclear physics and to the precise early-time dynamics and ejecta composition. Due to the rapid evolution and low luminosity of NS merger transients, EM counterpart searches triggered by GW detections will require close collaboration between the GW and astronomical communities. NS merger transients may also be detectable following a short-duration Gamma-Ray Burst or \"blindly\" with present or upcoming optical transient surveys. Because the emission produced by NS merger ejecta is powered by the formation of rare r-process elements, current optical transient surveys can directly constrain the unknown origin of the heaviest elements in the Universe.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Gamma-ray bursts and supernovae"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1304.0670","kind":"article","title":"Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA","authors":["Shubhanshu Tiwari","R. Abbott","T. D. Abbott","et al"],"author_count":4,"year":2020,"published":"2020-10-30","venue":"University of Groningen research database (University of Groningen / Centre for Information Technology)","cited_by":987,"doi":"10.5167/uzh-191285","arxiv_id":"1304.0670","nct_id":null,"source_url":"https://research.rug.nl/en/publications/4829a4f0-ba60-4842-b61e-75a90402ec44","archive_url":"https://space-kitty.com/papers/arxiv:1304.0670","updated":"2020-11-24","pmid":null,"pmcid":null,"openalex_id":"W2975828310","pdf_url":"https://arxiv.org/pdf/1304.0670","abstract":"We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is BNS, NSBH, and BBH systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90\\% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1508.07253","kind":"article","title":"Frequency-domain gravitational waves from nonprecessing black-hole binaries. II. A phenomenological model for the advanced detector era","authors":["S. Khan","S. Husa","Mark Hannam","F. Ohme","M. Pürrer","Xisco Jiménez Forteza","A. Bohé"],"author_count":7,"year":2016,"published":"2016-02-03","venue":"Physical review. D/Physical review. D.","cited_by":1086,"doi":"10.1103/physrevd.93.044007","arxiv_id":"1508.07253","nct_id":null,"source_url":"https://doi.org/10.1103/physrevd.93.044007","archive_url":"https://space-kitty.com/papers/arxiv:1508.07253","updated":"2015-09-25","pmid":null,"pmcid":null,"openalex_id":"W1134494461","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevD.93.044007","abstract":"We present a new frequency-domain phenomenological model of the gravitational-wave signal from the inspiral, merger and ringdown of non-precessing (aligned-spin) black-hole binaries. The model is calibrated to 19 hybrid effective-one-body--numerical-relativity waveforms up to mass ratios of 1:18 and black-hole spins of $|a/m| \\sim 0.85$ ($0.98$ for equal-mass systems). The inspiral part of the model consists of an extension of frequency-domain post-Newtonian expressions, using higher-order terms fit to the hybrids. The merger-ringdown is based on a phenomenological ansatz that has been significantly improved over previous models. The model exhibits mismatches of typically less than 1\\% against all 19 calibration hybrids, and an additional 29 verification hybrids, which provide strong evidence that, over the calibration region, the model is sufficiently accurate for all relevant gravitational-wave astronomy applications with the Advanced LIGO and Virgo detectors. Beyond the calibration region the model produces physically reasonable results, although we recommend caution in assuming that \\emph{any} merger-ringdown waveform model is accurate outside its calibration region. As an example, we note that an alternative non-precessing model, SEOBNRv2 (calibrated up to spins of only 0.5 for unequal-mass systems), exhibits mismatch errors of up to 10\\% for high spins outside its calibration region. We conclude that waveform models would benefit most from a larger number of numerical-relativity simulations of high-aligned-spin unequal-mass binaries.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2010.14533","kind":"article","title":"Population Properties of Compact Objects from the Second LIGO–Virgo Gravitational-Wave Transient Catalog","authors":["R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","A. Adams","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","G. Allen","A. Allocca","P. A. Altin","A. Amato","Shreya Anand","A. Ananyeva","S. B. Anderson","Warren G. Anderson"],"author_count":100,"year":2021,"published":"2021-05-01","venue":"The Astrophysical Journal Letters","cited_by":901,"doi":"10.3847/2041-8213/abe949","arxiv_id":"2010.14533","nct_id":null,"source_url":"https://doi.org/10.3847/2041-8213/abe949","archive_url":"https://space-kitty.com/papers/arxiv:2010.14533","updated":"2021-02-25","pmid":null,"pmcid":null,"openalex_id":"W3161193838","pdf_url":"https://iopscience.iop.org/article/10.3847/2041-8213/abe949/pdf","abstract":"We report on the population of the 47 compact binary mergers detected with a false-alarm rate 1/yr in the second LIGO--Virgo Gravitational-Wave Transient Catalog, GWTC-2. We observe several characteristics of the merging binary black hole (BBH) population not discernible until now. First, we find that the primary mass spectrum contains structure beyond a power-law with a sharp high-mass cut-off; it is more consistent with a broken power law with a break at $39.7^{+20.3}_{-9.1}\\,M_\\odot$, or a power law with a Gaussian feature peaking at $33.1^{+4.0}_{-5.6}\\,M_\\odot$ (90\\% credible interval). While the primary mass distribution must extend to $\\sim65\\,M_\\odot$ or beyond, only $2.9^{+3.5}_{1.7}\\%$ of systems have primary masses greater than $45\\,M_\\odot$. Second, we find that a fraction of BBH systems have component spins misaligned with the orbital angular momentum, giving rise to precession of the orbital plane. Moreover, 12% to 44% of BBH systems have spins tilted by more than $90^\\circ$, giving rise to a negative effective inspiral spin parameter $χ_\\mathrm{eff}$. Under the assumption that such systems can only be formed by dynamical interactions, we infer that between 25% and 93% of BBH with non-vanishing $|χ_\\mathrm{eff}| > 0.01$ are dynamically assembled. Third, we estimate merger rates, finding $\\mathcal{R}_\\text{BBH} = 23.9^{+14.3}_{8.6}$ Gpc$^{-3}$ yr$^{-1}$ for BBH and $\\mathcal{R}_\\text{BNS}= 320^{+490}_{-240}$ Gpc$^{-3}$ yr$^{-1}$ for binary neutron stars. We find that the BBH rate likely increases with redshift ($85\\%$ credibility), but not faster than the star-formation rate ($86\\%$ credibility). Additionally, we examine recent exceptional events in the context of our population models, finding that the asymmetric masses of GW190412 and the high component masses of GW190521 are consistent with our models, but the low secondary mass of GW190814 makes it an outlier.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1602.03840","kind":"article","title":"Properties of the Binary Black Hole Merger GW150914","authors":["B. P. Abbott","R. Abbott","T. D. Abbott","M. R. Abernathy","F. Acernese","K. Ackley","C. Adams","Thomas Adams","Paolo Addesso","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","B. Allen","A. Allocca","P. A. Altin","S. B. Anderson","Warren G. Anderson","Koji Arai"],"author_count":100,"year":2016,"published":"2016-06-14","venue":"Physical Review Letters","cited_by":1030,"doi":"10.1103/physrevlett.116.241102","arxiv_id":"1602.03840","nct_id":null,"source_url":"https://doi.org/10.1103/physrevlett.116.241102","archive_url":"https://space-kitty.com/papers/arxiv:1602.03840","updated":"2016-06-20","pmid":"27367378","pmcid":null,"openalex_id":"W2254226187","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevLett.116.241102","abstract":"On September 14, 2015, the Laser Interferometer Gravitational-wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of $36^{+5}_{-4} M_\\odot$ and $29^{+4}_{-4} M_\\odot$; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be $<0.7$ (at 90% probability). The luminosity distance to the source is $410^{+160}_{-180}$ Mpc, corresponding to a redshift $0.09^{+0.03}_{-0.04}$ assuming standard cosmology. The source location is constrained to an annulus section of $610$ deg$^2$, primarily in the southern hemisphere. The binary merges into a black hole of $62^{+4}_{-4} M_\\odot$ and spin $0.67^{+0.05}_{-0.07}$. This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1710.05938","kind":"article","title":"Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817","authors":["Ben Margalit","Brian D. Metzger"],"author_count":2,"year":2017,"published":"2017-11-21","venue":"The Astrophysical Journal Letters","cited_by":916,"doi":"10.3847/2041-8213/aa991c","arxiv_id":"1710.05938","nct_id":null,"source_url":"https://doi.org/10.3847/2041-8213/aa991c","archive_url":"https://space-kitty.com/papers/arxiv:1710.05938","updated":"2017-11-08","pmid":null,"pmcid":null,"openalex_id":"W2766413446","pdf_url":"https://iopscience.iop.org/article/10.3847/2041-8213/aa991c/pdf","abstract":"We combine electromagnetic (EM) and gravitational wave (GW) information on the binary neutron star (NS) merger GW170817 in order to constrain the radii $R_{\\rm ns}$ and maximum mass $M_{\\rm max}$ of NSs. GW170817 was followed by a range of EM counterparts, including a weak gamma-ray burst (GRB), kilonova (KN) emission from the radioactive decay of the merger ejecta, and X-ray/radio emission consistent with being the synchrotron afterglow of a more powerful off-axis jet. The type of compact remnant produced in the immediate merger aftermath, and its predicted EM signal, depend sensitively on the high-density NS equation of state (EOS). For a soft EOS which supports a low $M_{\\rm max}$, the merger undergoes a prompt collapse accompanied by a small quantity of shock-heated or disk wind ejecta, inconsistent with the large quantity $\\gtrsim 10^{-2}M_{\\odot}$ of lanthanide-free ejecta inferred from the KN. On the other hand, if $M_{\\rm max}$ is sufficiently large, then the merger product is a rapidly-rotating supramassive NS (SMNS), which must spin-down before collapsing into a black hole. A fraction of the enormous rotational energy necessarily released by the SMNS during this process is transferred to the ejecta, either into the GRB jet (energy $E_{\\rm GRB}$) or the KN ejecta (energy $E_{\\rm ej}$), also inconsistent with observations. By combining the total binary mass of GW170817 inferred from the GW signal with conservative upper limits on $E_{\\rm GRB}$ and $E_{\\rm ej}$ from EM observations, we constrain the likelihood probability of a wide-range of previously-allowed EOS. These two constraints delineate an allowed region of the $M_{\\rm max}-R_{\\rm ns}$ parameter space, which once marginalized over NS radius places an upper limit of $M_{\\rm max} \\lesssim 2.17M_{\\odot}$ (90\\%), which is tighter or arguably less model-dependent than other current constraints.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"other-oa","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1602.03847","kind":"article","title":"GW150914: Implications for the stochastic gravitational wave background from binary black holes","authors":["The LIGO Scientific Collaboration","the Virgo Collaboration"],"author_count":2,"year":2016,"published":"2016-02-11","venue":"Phys. Rev. Lett. 116, 131102 (2016)","cited_by":382,"doi":"10.1103/physrevlett.116.131102","arxiv_id":"1602.03847","nct_id":null,"source_url":"https://arxiv.org/abs/1602.03847","archive_url":"https://space-kitty.com/papers/arxiv:1602.03847","updated":"2016-03-20","pmid":"27081965","pmcid":null,"openalex_id":"W2256095203","pdf_url":"https://arxiv.org/pdf/1602.03847","abstract":"The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses $\\gtrsim 30\\, \\text{M}_\\odot$, suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO/Virgo band for stochastic backgrounds (near 25 Hz), we predict $Ω_\\text{GW}(f=25 Hz) = 1.1_{-0.9}^{+2.7} \\times 10^{-9}$ with 90\\% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO/Virgo detectors operating at their projected final sensitivity.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"other-oa","is_open_access":true,"peer_reviewed":null,"categories":["gr-qc","astro-ph.CO","astro-ph.HE"],"details":null,"provenance":"arxiv+openalex","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1602.04531","kind":"article","title":"The first gravitational-wave source from the isolated evolution of two stars in the 40–100 solar mass range","authors":["Krzysztof Belczyński","DANIEL E. HOLZ","T. Bulik","Richard W O'Shaughnessy"],"author_count":4,"year":2016,"published":"2016-06-22","venue":"Nature","cited_by":908,"doi":"10.1038/nature18322","arxiv_id":"1602.04531","nct_id":null,"source_url":"https://doi.org/10.1038/nature18322","archive_url":"https://space-kitty.com/papers/arxiv:1602.04531","updated":"2016-06-22","pmid":"27337338","pmcid":null,"openalex_id":"W2462805925","pdf_url":"https://arxiv.org/pdf/1602.04531","abstract":"The merger of two massive 30 Msun black holes has been detected in gravitational waves (1,GW150914). This discovery validates recent predictions (2-4) that massive binary black holes would constitute the first detection. However, previous calculations have not sampled the relevant binary black hole progenitors---massive, low-metallicity binary stars---with sufficient accuracy and input physics to enable robust predictions to better than several orders of magnitude (5-10). Here we report a suite of high-precision numerical simulations of binary black hole formation via the evolution of isolated binary stars, providing a framework to interpret GW150914 and predict the properties of subsequent binary black hole gravitational-wave events. Our models imply that these events form in an environment where the metallicity is less than 10 percent of solar; have initial masses of 40-100 Msun; and interact through mass transfer and a common envelope phase. Their progenitors likely form either at 2 Gyr, or somewhat less likely, at 11 Gyr after the Big Bang. Most binary black holes form without supernova explosions, and their spins are nearly unchanged since birth, but do not have to be parallel. The classical field formation of binary black holes proposed in this study, with low natal kicks and restricted common envelope evolution, produces 40 times more binary black holes than dynamical formation channels involving globular clusters (11) and is comparable to the rate from homogeneous evolution channels (12-15). Our calculations predict detections of about 1,000 black hole mergers per year with total mass of 20-80 Msun once second generation ground-based gravitational wave observatories reach full sensitivity.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:1710.05841","kind":"article","title":"A kilonova as the electromagnetic counterpart to a gravitational-wave source","authors":["Stephen J. Smartt","T. W. Chen","Anders Jerkstrand","M. W. Coughlin","E. Kankare","Stuart A. Sim","M. Fraser","C. Inserra","K. Maguire","K. C. Chambers","M. E. Huber","T. Kruehler","G. Leloudas","M. Magee","Luke Jeremy Shingles","K. Smith","David R. Young","John L. Tonry","Rubina Kotak","Avishay Gal‐Yam","J. D. Lyman","D. S. Homan","C. Agliozzo","Joseph P. Anderson","C. R. Angus"],"author_count":100,"year":2017,"published":"2017-10-16","venue":"Nature","cited_by":868,"doi":"10.1038/nature24303","arxiv_id":"1710.05841","nct_id":null,"source_url":"https://doi.org/10.1038/nature24303","archive_url":"https://space-kitty.com/papers/arxiv:1710.05841","updated":"2017-10-17","pmid":"29094693","pmcid":null,"openalex_id":"W2765180549","pdf_url":"https://www.nature.com/articles/nature24303.pdf","abstract":"Gravitational waves were discovered with the detection of binary black hole mergers and they should also be detectable from lower mass neutron star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal called a kilonova. The gravitational wave source GW170817 arose from a binary neutron star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC4993, which is spatially coincident with GW170817 and a weak short gamma-ray burst. The transient has physical parameters broadly matching the theoretical predictions of blue kilonovae from neutron star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 +/- 0.01 Msol, with an opacity of kappa <= 0.5 cm2/gm at a velocity of 0.2 +/- 0.1c. The power source is constrained to have a power law slope of beta = -1.2 +/- 0.3, consistent with radioactive powering from r-process nuclides. We identify line features in the spectra that are consistent with light r-process elements (90 < A < 140). As it fades, the transient rapidly becomes red, and emission may have contribution by a higher opacity, lanthanide-rich ejecta component. This indicates that neutron star mergers produce gravitational waves, radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Gamma-ray bursts and supernovae"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2106.15163","kind":"article","title":"Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences","authors":["R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","A. Adams","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","D. Agarwal","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","T. Akutsu","K. M. Aleman","G. Allen","A. Allocca","P. A. Altin","A. Amato","S. Anand"],"author_count":100,"year":2021,"published":"2021-06-29","venue":"The Astrophysical Journal Letters","cited_by":769,"doi":"10.3847/2041-8213/ac082e","arxiv_id":"2106.15163","nct_id":null,"source_url":"https://doi.org/10.3847/2041-8213/ac082e","archive_url":"https://space-kitty.com/papers/arxiv:2106.15163","updated":"2021-06-29","pmid":null,"pmcid":null,"openalex_id":"W3173762688","pdf_url":"https://arxiv.org/pdf/2106.15163","abstract":"We report the observation of gravitational waves from two compact binary coalescences in LIGO's and Virgo's third observing run with properties consistent with neutron star-black hole (NSBH) binaries. The two events are named GW200105_162426 and GW200115_042309, abbreviated as GW200105 and GW200115; the first was observed by LIGO Livingston and Virgo, and the second by all three LIGO-Virgo detectors. The source of GW200105 has component masses $8.9^{+1.2}_{-1.5}\\,M_\\odot$ and $1.9^{+0.3}_{-0.2}\\,M_\\odot$, whereas the source of GW200115 has component masses $5.7^{+1.8}_{-2.1}\\,M_\\odot$ and $1.5^{+0.7}_{-0.3}\\,M_\\odot$ (all measurements quoted at the 90% credible level). The probability that the secondary's mass is below the maximal mass of a neutron star is 89%-96% and 87%-98%, respectively, for GW200105 and GW200115, with the ranges arising from different astrophysical assumptions. The source luminosity distances are $280^{+110}_{-110}$ Mpc and $300^{+150}_{-100}$ Mpc, respectively. The magnitude of the primary spin of GW200105 is less than 0.23 at the 90% credible level, and its orientation is unconstrained. For GW200115, the primary spin has a negative spin projection onto the orbital angular momentum at 88% probability. We are unable to constrain spin or tidal deformation of the secondary component for either event. We infer a NSBH merger rate density of $45^{+75}_{-33}\\,\\mathrm{Gpc}^{-3} \\mathrm{yr}^{-1}$ when assuming GW200105 and GW200115 are representative of the NSBH population, or $130^{+112}_{-69}\\,\\mathrm{Gpc}^{-3} \\mathrm{yr}^{-1}$ under the assumption of a broader distribution of component masses.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":"cc-by","is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."},{"id":"arxiv:2010.14529","kind":"article","title":"Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational-wave transient catalog","authors":["R. Abbott","T. D. Abbott","S. Abraham","F. Acernese","K. Ackley","A. Adams","C. Adams","R. X. Adhikari","V. B. Adya","C. Affeldt","M. Agathos","K. Agatsuma","Nancy Aggarwal","O. D. Aguiar","L. Aiello","A. Ain","P. Ajith","Sarp Akçay","G. Allen","A. Allocca","P. A. Altin","A. Amato","Shreya Anand","A. Ananyeva","S. B. Anderson"],"author_count":100,"year":2021,"published":"2021-06-15","venue":"Physical review. D/Physical review. D.","cited_by":761,"doi":"10.1103/physrevd.103.122002","arxiv_id":"2010.14529","nct_id":null,"source_url":"https://doi.org/10.1103/physrevd.103.122002","archive_url":"https://space-kitty.com/papers/arxiv:2010.14529","updated":"2025-09-10","pmid":null,"pmcid":null,"openalex_id":"W3096163345","pdf_url":"http://link.aps.org/pdf/10.1103/PhysRevD.103.122002","abstract":"Gravitational waves enable tests of general relativity in the highly dynamical and strong-field regime. Using events detected by LIGO-Virgo up to 1 October 2019, we evaluate the consistency of the data with predictions from the theory. We first establish that residuals from the best-fit waveform are consistent with detector noise, and that the low- and high-frequency parts of the signals are in agreement. We then consider parametrized modifications to the waveform by varying post-Newtonian and phenomenological coefficients, improving past constraints by factors of ${\\sim}2$; we also find consistency with Kerr black holes when we specifically target signatures of the spin-induced quadrupole moment. Looking for gravitational-wave dispersion, we tighten constraints on Lorentz-violating coefficients by a factor of ${\\sim}2.6$ and bound the mass of the graviton to $m_g \\leq 3.09 \\times 10^{-23} \\mathrm{eV}/c^2$ with 90% credibility. We also analyze the properties of the merger remnants by measuring ringdown frequencies and damping times, constraining fractional deviations away from the Kerr frequency to $δ\\hat{f}_{220} = 0.03^{+0.38}_{-0.35}$ for the fundamental quadrupolar mode, and $δ\\hat{f}_{221} = 0.02^{+0.29}_{-0.33}$ for the first overtone; additionally, we find no evidence for postmerger echoes. Finally, we determine that our data are consistent with tensorial polarizations through a template-independent method. When possible, we assess the validity of general relativity based on collections of events analyzed jointly. We find no evidence for new physics beyond general relativity, for black hole mimickers, or for any unaccounted systematics.","abstract_license":"CC0-1.0 (arXiv descriptive metadata)","license":null,"is_open_access":true,"peer_reviewed":null,"categories":["Pulsars and Gravitational Waves Research"],"details":null,"provenance":"openalex+arxiv","attribution":"Abstract: arXiv descriptive metadata (CC0). Thank you to arXiv for use of its open access interoperability. This service was not reviewed or approved by, nor does it necessarily express or reflect the policies or opinions of, arXiv."}],"next":"https://space-kitty.com/api/v1/topics/gravitational-waves/papers?sort=top&limit=25&offset=25"}