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Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

The Astrophysical Journal Letters · 2021 · Vol. 915(1) · pp. L5–L5
R. Abbott✉T. D. AbbottS. AbrahamF. AcerneseK. AckleyA. AdamsC. AdamsR. X. AdhikariV. B. AdyaC. AffeldtD. AgarwalM. AgathosK. AgatsumaN. AggarwalO. D. AguiarL. AielloA. AinP. AjithT. AkutsuK. M. AlemanG. AllenA. AlloccaP. A. AltinA. AmatoS. AnandA. AnanyevaS. B. AndersonW. G. AndersonM. AndoS. V. AngelovaS. AnsoldiJ. M. AntelisS. AntierS. AppertKoya AraiKoji AraiY. AraiS. ArakiA. ArayaM. C. ArayaJ. S. AreedaM. ArèneN. AritomiN. ArnaudS. M. AronsonK. G. ArunH. AsadaY. AsaliG. AshtonY. AsoS. M. AstonP. AstoneF. AubinP. AufmuthK. AultONealC. AustinS. BabakF. BadaraccoM. K. M. BaderS. BaeY. BaeA. M. BaerS. BagnascoY. BaiL. BaiottiJ. BairdR. BajpaiM. BallG. BallardinS. W. BallmerM. BalsA. BalsamoG. BaltusS. BanagiriD. BankarR. S. BankarJ. C. BarayogaC. BarbieriB. C. BarishD. BarkerP. BarneoF. BaroneB. BarrL. BarsottiM. BarsugliaD. BartaJ. BartlettM. A. BartonI. BartosR. BassiriA. BastiM. BawajJ. C. BayleyA. C. BaylorM. BazzanB. BécsyV. M. BedakihaleM. BejgerI. BelahceneV. BenedettoD. 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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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>8</mml:mn> <mml:mo>.</mml:mo> <mml:msubsup> <mml:mn>9</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> <mml:mo>.</mml:mo> <mml:mn>5</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.</mml:mn> <mml:mn>2</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>1.</mml:mn> <mml:msubsup> <mml:mn>9</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.</mml:mn> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.</mml:mn> <mml:mn>3</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mi>M</mml:mi> <mml:mo>⊙</mml:mo> </mml:msub> </mml:math> , whereas the source of GW200115 has component masses <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>5.</mml:mn> <mml:msubsup> <mml:mn>7</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> <mml:mo>.</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.</mml:mn> <mml:mn>8</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>1.</mml:mn> <mml:msubsup> <mml:mn>5</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.</mml:mn> <mml:mn>3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.</mml:mn> <mml:mn>7</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mi>M</mml:mi> <mml:mo>⊙</mml:mo> </mml:msub> </mml:math> (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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>280</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>110</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>110</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>300</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>100</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>150</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mi>Mpc</mml:mi> </mml:math> , 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 the spin or tidal deformation of the secondary component for either event. We infer an NSBH merger rate density of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>45</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>33</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>75</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi>Gpc</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi>yr</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> when assuming that GW200105 and GW200115 are representative of the NSBH population or <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>130</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>69</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>112</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi>Gpc</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <m

Pulsars and Gravitational Waves ResearchAstrophysical Phenomena and ObservationsRelativity and Gravitational TheoryLIGONeutron starGravitational waveLuminosityComponent (thermodynamics)Binary numberGravitational-wave observatory

Funding

  • National Science Foundation
  • U.S. Department of Energy
  • Centres de Recerca de Catalunya
  • Institut des Origines de Lyon
  • Leverhulme Trust
  • Scottish Funding Council
  • Scottish Universities Physics Alliance
  • European Commission
  • Cardiff University
  • National Research Foundation
  • Council of Scientific and Industrial Research, India
  • Abdus Salam International Centre for Theoretical Physics
  • Ministry of Education, Culture, Sports, Science and Technology
  • Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung
  • Swinburne University of Technology
  • National Natural Science Foundation of China
  • Academia Sinica
  • Fundacja na rzecz Nauki Polskiej
  • Russian Foundation for Basic Research
  • Fonds De La Recherche Scientifique - FNRS
  • Generalitat de Catalunya
  • Fonds Wetenschappelijk Onderzoek
  • Generalitat Valenciana
  • Hungarian Scientific Research Fund
  • Korea Institute of Science and Technology Information
  • National Research Foundation of Korea
  • Max-Planck-Gesellschaft
  • Ministry of Education, India
  • Centre National de la Recherche Scientifique
  • National Astronomical Observatory of Japan
  • Russian Science Foundation
  • Nemzeti Kutatási Fejlesztési és Innovációs Hivatal
  • Vlaamse regering
  • Istituto Nazionale di Fisica Nucleare
  • ICTP South American Institute for Fundamental Research
  • Govern de les Illes Balears
  • Science and Technology Facilities Council
  • Japan Society for the Promotion of Science
  • Science and Engineering Research Board
  • European Regional Development Fund
  • Agencia Estatal de Investigación
  • Institute for Cosmic Ray Research, University of Tokyo
  • National Research, Development and Innovation Office
  • Great Southern Development Commission, Government of Western Australia
  • Division of Human Resource Development
Citations
708
FWCI
89.76
field-weighted impact
References
239
Percentile
100%
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Citations per year
Cited by
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