  We have observed a sample of 10 white dwarf candidates in the rich open
cluster NGC 2323 (M50) with the Keck Low-Resolution Imaging Spectrometer. The
spectroscopy shows eight to be DA white dwarfs, with six of these having high
S/N appropriate for our analysis. Two of these white dwarfs are consistent with
singly evolved cluster membership, and both are high mass $\sim$1.07 M$_\odot$,
and give equivalent progenitor masses of 4.69 M$_\odot$. To supplement these
new high-mass white dwarfs and analyze the initial-final mass relation (IFMR),
we have also looked at 30 white dwarfs from publicly available data that are
mostly all high-mass ($\gtrsim$0.9 M$_\odot$). These original published data
exhibited significant scatter, and to test if this scatter is true or simply
the result of systematics, we have uniformly analyzed the white dwarf spectra
and have adopted thorough photometric techniques to derive uniform cluster
parameters for their parent clusters. The resulting IFMR scatter is
significantly reduced, arguing that mass-loss rates are not stochastic in
nature and that within the ranges of metallicity and mass analyzed in this work
mass loss is not highly sensitive to variations in metallicity. Lastly, when
adopting cluster ages based on Y$^2$ isochrones, the slope of the high-mass
IFMR remains steep and consistent with that found from intermediate-mass white
dwarfs, giving a linear IFMR from progenitor masses between 3 to 6.5 M$_\odot$.
In contrast, when adopting the slightly younger cluster ages based on PARSEC
isochrones, the high-mass IFMR has a moderate turnover near an initial mass of
4 M$_\odot$.
