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We present forward modeling from the BPASS code suite of the population ofobserved gravitational wave (GW) transients reported by the LIGO/VIRGOconsortium (LVC) during their third observing run, O3(a+b). Specifically, wepredict the expected chirp mass and mass ratio distributions for GW transients,taking account of detector sensitivity to determine how many events should havebeen detected by the current detector network in O3(a+b). We investigate howthese predictions change by alternating between four different remnant massestimation schemes and two supernovae (SNe) kick prescriptions. We find thatnone of the model populations resulting from these variations accurately matchthe whole O3(a+b) GW transient catalog. However, agreement from some models topart of the catalog suggests ways to achieve a more complete fit. These includereducing the number of low mass black holes (BHs) close to the mass gap, whilealso increasing the number of higher mass BHs below the pair-instability SNlimit. Finally, we find that the interaction between the value of the remnantmass from a stellar model and the choice of SN kick is complex and differentkick prescriptions may be required depending on whether a neutron star or BH isformed.

Forward Modelling the O3(a+b) GW transient mass distributions with BPASS by varying compact remnant mass and SNe kick prescriptions