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The initial-final mass relation (IFMR) represents the total mass lost by astar during the entirety of its evolution from the zero age main sequence tothe white dwarf cooling track. The semi-empirical IFMR is largely based onobservations of DA white dwarfs, the most common spectral type of white dwarfand the simplest atmosphere to model. We present a first derivation of thesemi-empirical IFMR for hydrogen deficient white dwarfs (non-DA) in open starclusters. We identify a possible discrepancy between the DA and non-DA IFMRs,with non-DA white dwarfs $\approx 0.07 M_\odot$ less massive at a given initialmass. Such a discrepancy is unexpected based on theoretical models of non-DAformation and observations of field white dwarf mass distributions. If real,the discrepancy is likely due to enhanced mass loss during the final thermalpulse and renewed post-AGB evolution of the star. However, we are dubious thatthe mass discrepancy is physical and instead is due to the small sample size,to systematic issues in model atmospheres of non-DAs, and to the uncertainevolutionary history of Procyon B (spectral type DQZ). A significantly largersample size is needed to test these assertions. In addition, we also presentMonte Carlo models of the correlated errors for DA and non-DA white dwarfs inthe initial-final mass plane. We find the uncertainties in initial-final massdeterminations for individual white dwarfs can be significantly asymmetric, butthe recovered functional form of the IFMR is grossly unaffected by thecorrelated errors.

The Initial-Final Mass Relation for Hydrogen-Deficient White Dwarfs