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The population of merging compact binaries inferred using gravitational waves through GWTC-3
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The population of merging compact binaries inferred using gravitational waves through GWTC-3

The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, R Abbott, T. D Abbott, F Acernese, K Ackley, C Adams, N Adhikari, R. X Adhikari, …
05/11/2021

摘要

Physics - General Relativity and Quantum Cosmology Physics - High Energy Astrophysical Phenomena
Physical Review X 13, 011048 (2023) 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 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 ⁻³yr ⁻¹at 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)withκ=2.9^(+1.7)_(-1.8)forz≲1 . Using both binary neutron star and neutron star-black hole binaries, we obtain a broad, relatively flat neutron star mass distribution extending from1.2^(+0.1)_(-0.2)to2.0^(+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 of8.3^(+0.3)_(-0.5)and27.9^(+1.9)_(-1.8) 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 approximately60 M_(⊙)[abridged]

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