Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 900, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8213/aba493
Keywords
Astrophysical black holes; High energy astrophysics; Gravitational collapse; Gravitation; Gravitational wave astronomy; Gravitational wave sources; LIGO; Stellar mass black holes; Stellar populations; Intermediate-mass black holes
Categories
Funding
- Council of Scientific and Industrial Research, India
- Department of Science and Technology, India
- Science AMP
- Engineering Research Board (SERB), India
- Ministry of Human Resource Development, India
- Spanish Agencia Estatal de Investigacion del Govern de les Illes Balears
- Vicepresidencia i Conselleria d'Innovacio Recerca i Turisme del Govern de les Illes Balears
- Conselleria d'Educacio i Universitat del Govern de les Illes Balears
- Conselleria d'Innovacio Universitats, 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), Belgium
- Actions de Recherche Concertees (ARC), Belgium
- 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
- Industry Canada
- STFC [ST/N000633/1, ST/R00045X/1, ST/T00049X/1, ST/V001167/1, ST/V001396/1, ST/N00003X/1, ST/T000333/1, ST/N000072/1, ST/S000550/1, ST/V001337/1, ST/V001019/1, ST/I006269/1, ST/P000673/1, ST/N005430/1, ST/T000147/1, ST/K000845/1, ST/N005422/1, 1947165, ST/S000305/1] Funding Source: UKRI
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The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, M and M, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65-120 M. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger ( M) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be . We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary.
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