The spectroscopic study of white dwarfs provides both their mass, cooling age, and intrinsic photometric properties. For a white dwarf that is a member of a star cluster, comparison of its cooling age to the cluster's total age gives the evolutionary timescale of its progenitor star, and hence its initial mass. This initial-final mass relation (IFMR) gives valuable information on how stars evolve. Our work presents a uniform analysis of 85 white dwarfs spanning from progenitor masses of 0.85 to 8.15 M$_odot$. This IFMR helps to constrain AGB mass loss, stellar gas recycling, and chemical evolution. Additionally, the higher-mass white dwarfs in the IFMR can help constrain the supernova mass transition, where white dwarf formation ends and core-collapse supernovae begin. This is valuable is determining Type II supernova rates. The IFMR can also help constrain Type Ia supernova rates by defining production rates of high-mass CO white dwarfs. These stellar feedback processes provide crucial input for our understanding of the characteristics and evolution of the ISM.