Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 896, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8213/ab960f
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Funding
- Council of Scientific and Industrial Research of India
- Department of Science and Technology, India
- Science & Engineering Research Board (SERB), India
- Ministry of Human Resource Development, India
- Spanish Agencia Estatal de Investigacion, Spain
- Vicepresidencia i Conselleria d'Innovacio Recerca i Turisme, Spain
- Conselleria d'Educacio i Universitat del Govern de les Illes Balears, Spain
- Conselleria d'Innovacio Universitats, Spain
- Ciencia i Societat Digital de la Generalitat Valenciana, Spain
- CERCA Programme Generalitat de Catalunya, Spain
- National Science Centre of Poland
- Swiss National Science Foundation (SNSF)
- Russian Foundation for Basic Research
- Russian Science Foundation
- European Commission
- European Regional Development Funds (ERDF)
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- French Lyon Institute of Origins (LIO)
- Belgian Fonds de la Recherche Scientifique (FRS-FNRS)
- Actions de Recherche Concertees (ARC)
- Fonds Wetenschappelijk Onderzoek-Vlaanderen (FWO), Belgium
- Paris Ile-de-France Region
- National Research, Development and Innovation Office Hungary (NKFIH)
- National Research Foundation of Korea
- Industry Canada
- Province of Ontario through the Ministry of Economic Development and Innovation
- Natural Science and Engineering Research Council Canada
- Canadian Institute for Advanced Research
- Brazilian Ministry of Science, Technology, Innovations, and Communications
- International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)
- Research Grants Council of Hong Kong
- National Natural Science Foundation of China (NSFC)
- Leverhulme Trust
- Research Corporation
- Ministry of Science and Technology (MOST), Taiwan
- Kavli Foundation
- NSF
- STFC
- INFN
- CNRS
- STFC [ST/V001337/1, ST/T000325/1, ST/S000550/1, ST/P000673/1, ST/K000845/1, ST/T00049X/1, ST/N005422/1, ST/S000305/1, ST/T000333/1, ST/R00045X/1, ST/V001167/1, ST/N000072/1, ST/N000633/1, ST/V001396/1, ST/I006269/1, ST/V001019/1, ST/N005430/1, ST/T000147/1] Funding Source: UKRI
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We report the observation of a compact binary coalescence involving a 22.2-24.3 M-circle dot black hole and a compact object with a mass of 2.50-2.67 M-circle dot (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 2019 August 14 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(-0.009)(+0.008), 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 <= 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 of the formation and mass distribution of compact-object binaries.
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