期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 913, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/2041-8213/abe949
关键词
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资金
- United States National Science Foundation (NSF)
- Science and Technology Facilities Council (STFC) of the United Kingdom
- Max-Planck-Society (MPS)
- State of Niedersachsen/Germany
- Australian Research Council
- EGO consortium
- Council of Scientific and Industrial Research of 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
- Vicepresidencia i Conselleria d'Innovacio Recerca i Turisme
- Conselleria d'Educacio i Universitat del Govern de les Illes Balears
- Conselleria d'Innovacio Universitats
- Ciencia i Societat Digital de la Generalitat Valenciana
- 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
- National Research Foundation of Korea [2010-0018156] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
The study reveals unique characteristics of the merging binary black hole (BBH) population, including a specific primary mass spectrum and misaligned component spins leading to precession of the orbital plane. The research also estimates merger rates, indicating potential correlation between BBH rate and redshift but not exceeding the star formation rate. Additionally, recent exceptional events are examined in relation to population models, with GW190814 being identified as an outlier due to its low secondary mass.
We report on the population of 47 compact binary mergers detected with a false-alarm rate of <1 yr(-1) in the second LIGO-Virgo Gravitational-Wave.Transient.Catalog. We observe several characteristics of the merging binary.black.hole (BBH) population not discernible until now. First, the primary mass spectrum contains structure beyond a power law with a sharp high-mass cutoff; it is more consistent with a broken.power.law with a break at -.39.7(-9.1)(+20.3) M-circle dot or a power.law with a Gaussian feature peaking at 33.1(-5.6)(+4.0) M-circle dot (90% credible interval). While the primary mass distribution must extend to similar to 65 M-circle dot or beyond, only 2.9(-1.7)(+3.5)% of systems have primary masses greater than 45 M-circle dot. 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%-44% of BBH systems have spins tilted by more than 90 degrees, giving rise to a negative effective inspiral spin parameter, chi(eff). Under the assumption that such systems can only be formed by dynamical interactions, we infer that between.25% and.93% of BBHs with nonvanishing vertical bar chi eff vertical bar > 0.01 are dynamically assembled. Third, we estimate merger rates, finding R-BBH= 23.9(-8.6)(+14.3) Gpc(-3) yr(-1) for BBHs and = R-BNS = 320(-240)(+490) 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.
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