One fundamental goal of the newly born gravitational wave astronomy is discovering the origin of the observed binary black hole mergers. Toward this end, identifying features in the growing wealth of data may help in distinguishing different formation pathways. While large uncertainties still affect the binary formation models, spin-mass relations remain characteristic features of specific classes of channels. By focusing on the effective inspiral spin ${\chi }_{\text{eff}}$, the best reconstructed spin-related merger parameter, we show that current GWTC-3 data support the hypothesis that a fraction of events may display mass-spin correlations similar to one expected by dynamical formation channels of either astrophysical or primordial nature. We quantify the Bayesian evidence in favor of those models, which are substantially preferred when compared to the Gaussian phenomenological model adopted to describe the distribution of ${\chi }_{\text{eff}}$ in the recent LIGO/Virgo/KAGRA population analyses.

• Received 15 February 2022
• Accepted 8 June 2022

DOI:https://doi.org/10.1103/PhysRevD.105.123024