Main properties of dynamical BBH mergers in our GH and no-GH AGN models. The unfilled solid blue (dashed orange) histogram shows BBHs in the GH (no-GH) AGN scenario. The filled blue (orange) histogram shows the 1g BBHs in the GH (no-GH) AGN scenario. If 1g BHs in the no-GH scenario are identical to the GH scenario, they are not shown. Panels (a) and (b): probability density function (pdf) of the primary and secondary BH mass (m₁ and m₂). Panels (c) and (d): primary and secondary spin magnitudes (χ₁ and χ₂). Panel (e): orbital BBH eccentricity e(10 Hz) when the GW frequency is f_GW = 10 Hz. In gray we show the thermal distribution p(e) = 2e for comparison. Panel (f): timescales of delay time, t_del, between the BBH pair-up and the merger.