2024ApJ...977..220A

A pair-instability supernova (PISN) prevents black hole (BH) formation from stellar collapse within the approximate mass range M ∈ [65, 130]M_⊙. However, such BHs may form hierarchically through merging ancestral BHs, whose properties determine those of the “child” one: mass, spin, and recoil velocity. Crucially, the child will leave its host environment if its birth recoil exceeds the corresponding escape velocity, preventing further mergers. We exploit relations between the final recoil and spin of quasi-circular BH mergers to obtain posterior probability distributions for the hypothetical ancestral masses, spins, and birth recoils of the component BHs of GW190521. To this, we present a Bayesian framework applicable to existing estimates for the components of BH merger observations. We consider both the quasi-circular (generically spinning) analysis performed by the LIGO-Virgo-KAGRA collaboration and the eccentric (aligned-spin) one performed by Romero-Shaw et al. We evaluate the probability p_2g that the GW190521 components inferred by these analyses formed from the merger of stellar-origin BHs and were retained by their environment. For the primary component, which populates the PISN gap, such scenario is strongly suppressed if GW190521 happened in a globular cluster with p_2g ∼ 10^–3 unless it was quasi circular and its ancestors had aligned spins, uncharacteristic of hierarchical formation channels, or small spins, which yields p_2g ≃ 10^–2. If GW190521 was eccentric, we obtain p_2g ≃ 0.1 for any host other than an active galactic nucleus, and zero for a globular cluster. If GW190521 was quasi circular, a nuclear star cluster origin is possible with p_2g ∈ (∼0.4, ∼0.8).