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Binary black holes (BBHs) detected by gravitational wave (GW) observationscould be broadly divided into two formation channels: those formed throughfield binary evolution and those assembled dynamically in dense stellarsystems. Each of these formation channels, and their sub-channels, populate adistinct region in the effective spin-mass ($\chi_{\rm eff}-M$) plane.Depending on the branching ratio of different channels, an ensemble of BBHscould show a trend in this plane. Here we fit a mass-dependent distribution for$\chi_{\rm eff}$ to the GWTC-1 BBHs from the first and second observing runs ofAdvanced LIGO and Advanced Virgo. We find a negative correlation between massand the mean effective spin ($\bar{\chi}_{\mathrm{eff}}$), and positivecorrelation with its dispersion ($\sigma_{\chi_\mathrm{eff}}$) at 75\% and 80\%confidence. This trend is robust against the choice of mass variable, but mostpronounced when the mass variable is taken to be the chirp mass of the binary.The result is consistent with significant contributions from both dynamicallyassembled and field binaries in the GWTC-1 catalog. The upcoming LIGO O3a datarelease will critically test this interpretation.

A trend in the effective spin distribution of LIGO binary black holes with mass