One of the main projects during my PhD was to study the effect of variations on the pulsational pair instability supernova (PPISN) routines on the primary mass distribution of observed binary black hole systems.
Current observations of merging binary black holes are uncovering structure and details in the distribution of properties of these black holes. One interesting feature is a relatively high rate of observations of systems where the primary mass has \(\sim35M_{\odot}\).