Population Properties of Compact Objects from the Second LIGO–Virgo Gravitational-Wave Transient Catalog

Abstract

GW190413_052954 33.4 +12.4 −7.4 23.4 +6.7 −6.3 7.2 × 10 −2 GW190413_134308 45.4 +13.6 −9.6 30.9 +10.2 −9.6 4.4 × 10 −2 GW190421_213856 40.6 +10.4 −6.631.4 +7.5 −8.2 7.7 × 10 −4 GW190424_180648 39.5 +10.9 −6.9 31.0 +7.428.5 +7.5 −7.9 1.0 × 10 −5 GW190512_180714 23.0 +5.4 −5.7 12.5 +3.5 −2.5

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

“…However, there is considerable uncertainty in the astrophysical mass priors of such systems, and different prior assumptions can affect the component mass posteriors for detections with moderate S/N. To illustrate the impact of population assumptions, we consider three alternative priors: one based on Salpeter mass distributions, p(m) ∼ m −2.3 (Salpeter 1955), independently for each component; one based on an extrapolation of the BBH mass model BROKEN POWER LAW from Abbott et al (2021d) down to 0.5 M e for both components; and another based on a similar extrapolation of the POWER LAW + PEAK BBH mass model from the same study. We marginalize over the uncertainties in the latter two models, which are fit to the BBH population from Abbott et al (2021b), including the outlier event GW190814 with a secondary component mass below 3 M e (Abbott et al 2020c).…”

Importance of tidal resonances in extreme-mass-ratio inspirals

“…For l ¼ 2, allowed values for azimuthal number m are −l to l. However, the m ¼ 0 mode is excluded from the metric. 3 For simplicity, we restrict the position of the tidal perturber to the equatorial plane. Under this restriction, the Newmann-Penrose scalar ψ 0 [see Eq.…”

“…Note that there is an overall factor of two missing in h αβ in[50]; see footnote 17 in[52] for details. After correcting for this factor, dL z =dt agrees in the slow spin limit with dL z =dt for h αβ given in[51] 3. These modes are included in the slow-spin limit metric given by Poisson[51].…”

“…The three observation runs by gravitational-wave (GW) observatories LIGO and VIRGO have unveiled an exciting number of detections [1,2], thereby allowing probes of binary dynamics in the strongly gravitating regime and discovering more about binary formation channels [3,4]. By the early 2030s, the Laser Interferometer Space Antenna (LISA) and Taiji/TianQin will probe the cosmos at lower frequencies (∼mHz range) [5][6][7].…”

Neutrino Emission from Supermassive Binary Black Hole Mergers

“…3 contains the stellar mass binary black hole (BBH) merger rates, since these black holes can possess a strong relativistic jet and merge partially with a spin-flip as well [13], as the data from the Gravitational-Wave Transient Catalogue GWTC-2 shows [14]. We compared two reference merger rates of BBHs: the inferred merging BBH detection rate by the LIGO and Virgo Collaborations with 90 % confidence level [15] and an estimation for this rate by radio observations by [13]. Since the Pierre Auger Collaboration anisotropy study of ultra-high energy cosmic rays hints that 10 % originate from starburst galaxies and the rest from AGN [16], we weighted the neutrino fraction from GW energy in stellar mass BBH mergers BBH with 0.1 and the fraction in SMBBH mergers with 0.9.…”