Population properties of compact objects from the second LIGO–Virgo gravitational-wave transient catalog

Abbott, R. and Angelova, S. V. and Gier, C. and Hill, P. and Reid, Stuart and Wallace, G. S., LIGO Sci Collaboration, Virgo Collaboration (2021) Population properties of compact objects from the second LIGO–Virgo gravitational-wave transient catalog. Astrophysical Journal Letters, 913 (1). L7. ISSN 2041-8205

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    Abstract

    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^(+20.3)_(-9.1) M⊙ or a power law with a Gaussian feature peaking at 33.1^(+4.0)_(-5.6) M⊙ (90% credible interval). While the primary mass distribution must extend to ~65 M⊙ or beyond, only 2.9^(+3.5)_(-1.7)% of systems have primary masses greater than 45 M⊙. 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°, giving rise to a negative effective inspiral spin parameter, χ_(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 |χ_(eff)| > 0.01 are dynamically assembled. Third, we estimate merger rates, finding R_(BBH) = 23.9^(+14.3)_(-8.6) Gpc⁻³yr⁻¹ for BBHs and R_(BNS) = 320^(+490)_(-240) Gpc⁻³yr⁻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.

    ORCID iDs

    Abbott, R., Angelova, S. V., Gier, C., Hill, P. ORCID logoORCID: https://orcid.org/0000-0003-4826-3531, Reid, Stuart and Wallace, G. S.;