On the Likely Dynamical Origin of GW191109 and Binary Black Hole Mergers with Negative Effective Spin

With the growing number of binary black hole (BBH) mergers detected by LIGO/Virgo/KAGRA, several systems have become difficult to explain via isolated binary evolution, having components in the pair-instability mass gap, high orbital eccentricities, and/or spin-orbit misalignment. Here we focus on GW191109_010717, a BBH merger with component masses of ${65}_{-11}^{+11}$ and ${47}_{-13}^{+15}$ M _⊙ and an effective spin of $-{0.29}_{-0.31}^{+0.42}$ , which could imply a spin-orbit misalignment of more than π/2 rad for at least one of its components. Besides its component masses being in the pair-instability mass gap, we show that isolated binary evolution is unlikely to reproduce the proposed spin-orbit misalignment of GW191109 with high confidence. On the other hand, we demonstrate that BBHs dynamically assembled in dense star clusters would naturally reproduce the spin-orbit misalignment and masses of GW191109 and the rates of GW191109-like events if at least one of the components were to be a second-generation BH. Finally, we generalize our results to all events with a measured negative effective spin, arguing that GW200225 also has a likely dynamical origin.