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With the remarkable success of the LVK consortium in detecting binary blackhole mergers, it has become possible to use the population properties toconstrain our understanding of the progenitor stars' evolution. The moststriking features of the observed primary black hole mass distributions are theextended tail up to 100M$_\odot$ and an excess of masses at 35M$_\odot$.Currently, isolated binary population synthesis have difficulty explainingthese features. Using the well-tested BPASS detailed stellar binary evolutionmodels to determine mass transfer stability, accretion rates, and remnantmasses, we postulate that stable mass transfer with super-Eddington accretionis responsible for the extended tail. Furthermore, that the excess is not dueto pulsation-pair instability, as previously thought, but due to stable masstransfer. These systems are able to merge within the Hubble time due to morestable mass transfer with extreme mass ratios that allows the orbits to shrinksufficiently to allow for a merger. These finding are at odds with those fromother population synthesis codes but in agreement with other recent studiesusing detailed binary evolution models.

Understanding the high-mass binary black hole population from stable mass transfer and super-Eddington accretion in BPASS