Total intrinsic (not weighted by merger rate or by detection probability) merger-mass distribution for two progenitor stellar populations of different metallicity. Models with (M10) and without (M1) pair-instability pulsation supernovae and pair-instability supernovae are shown. Bottom panel: at high metallicity, (Z = 10% Z_⊙ and higher) models are indistinguishable. Top panel: at low metallicity (e.g., Z = 0.5% Z_⊙), pair-instability pulsation supernovae and pair-instability supernovae do not allow for high mass-merger formation (M_tot ≲ 80 M_⊙). We note that the model that does not take into account pair-instability pulsation supernovae and pair-instability supernovae allows for the formation of high mass mergers (M_tot> 80 M_⊙).