Population of merging compact binaries inferred using gravitational waves through GWTC3
Abbott, R. and Ben Yaala, M. and Talbot, C. J., The Virgo Collaboration, LIGO Scientific Collaboration, KAGRA Collaboration (2023) Population of merging compact binaries inferred using gravitational waves through GWTC3. Physical Review X, 13 (1). 011048. ISSN 21603308 (https://doi.org/10.1103/PhysRevX.13.011048)
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Abstract
We report on the population properties of compact binary mergers inferred from gravitationalwave observations of these systems during the first three LIGOVirgo observing runs. The GravitationalWave Transient Catalog 3 (GWTC3) 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−3 yr−1 at 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 with κ=2.9+1.7−1.8 for z≲1. Using both binary neutron star and neutron star–black hole binaries, we obtain a broad, relatively flat neutron star mass distribution extending from 1.2+0.1−0.2 to 2.0+0.3−0.3M⊙. 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 powerlaw distribution, with peaks emerging at chirp masses of 8.3+0.3−0.5 and 27.9+1.9−1.8M⊙. 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 approximately 60M⊙, which would indicate the presence of a upper mass gap. Observed black hole spins are small, with half of spin magnitudes below χi≈0.25. While the majority of spins are preferentially aligned with the orbital angular momentum, we infer evidence of antialigned spins among the binary population. We observe an increase in spin magnitude for systems with more unequalmass ratio. We also observe evidence of misalignment of spins relative to the orbital angular momentum.
ORCID iDs
Abbott, R., Ben Yaala, M. ORCID: https://orcid.org/0000000267540875 and Talbot, C. J.;

Item type: Article ID code: 86583 Dates: DateEvent29 March 2023Published19 December 2022AcceptedSubjects: Science > Physics > Optics. Light
Science > PhysicsDepartment: Faculty of Engineering > Biomedical Engineering Depositing user: Pure Administrator Date deposited: 29 Aug 2023 10:03 Last modified: 11 Sep 2024 02:51 URI: https://strathprints.strath.ac.uk/id/eprint/86583