GW190711_030756 and GW200114_020818: astrophysical interpretation of two asymmetric binary black hole mergers in the IAS catalog

Abstract

We provide a comprehensive analysis of GW190711_030756 and GW200114_020818, two of the most significant binary black hole merger candidates in the IAS catalog, with probabilities of astrophysical origin $p_{\mathrm{astro}}=0.99$ and $0.71$, respectively, and signal-to-noise ratios of approximately $10.0$ and $13.4$. We employ numerical relativity surrogate models to infer both the source properties and the remnant properties of these two candidates. We find that both GW190711_030756 and GW200114_020818 are asymmetric-mass binaries, with inferred mass ratios of $0.35_{-0.15}^{+0.32}$ and $\le 0.20$. In addition, GW200114_020818 is inferred to have a source-frame total mass of approximately $220M_{\odot }$ and highly spinning black holes, with primary (secondary) dimensionless spin magnitudes of $0.96_{-0.07}^{+0.03}$ ($0.84_{-0.34}^{+0.13}$), closely resembling GW231123_135430. We further find that GW200114\_020818 has a confidently negative effective inspiral spin of ${\chi }_{\mathrm{eff}}=-0.60_{-0.13}^{+0.22}$ and exhibits strong spin precession, characterized by an effective precession parameter of ${\chi }_{\mathrm{p}}=0.60_{-0.19}^{+0.21}$. GW200114_020818 (when considered alongside GW231123_135430) points towards an emerging population of massive, rapidly spinning BBH mergers. While GW231123_135430 is consistent with mergers in globular clusters, producing systems like GW200114_020818 in such environments remains difficult even under hierarchical merger scenarios. The probability that the remnant black hole of GW190711_030756 (GW200114_020818) is retained in its host environment is $0.079$ ($0.0002$), $0.62$ ($0.965$), and $0.997$ ($1$) if the merger occurred in a globular cluster, a nuclear star cluster, or an elliptical galaxy, respectively.

18 pages, 11 figures