Comparison of BBH merger masses from computed model star clusters with those from GWTC. Top panels: primary mass, M₁, versus secondary mass, M₂ (M₁ ≥ M₂), of all BBH mergers from the computed model star clusters of Ba21 (filled circles). These data points are colour-coded according to the merger delay time, t_mrg (left panel), and the parent model cluster’s metallicity, Z (right panel). The GWTC events’ data points (black, filled squares) and their corresponding 90% credible intervals (horizontal and vertical error bars) are indicated where events with FAR ≤1 yr⁻¹ and > 1 yr⁻¹ are distinguished by different shades. The shaded regions over 45 M_samp − 120 M_samp on each panel represent the PSN mass gap. The shadings have been placed in the background so that they do not influence the colours of the data points. Bottom panels: same as the top panels, except that the mergers from the present computed clusters (Table A.1) with King concentration parameters W₀ = 7.0 (filled triangles) and 9.0 (filled circles) are shown.