  We present a photometric and spectroscopic study of the white dwarf
population of the populous, intermediate-age open cluster M35 (NGC 2168); this
study expands upon our previous study of the white dwarfs in this cluster. We
spectroscopically confirm 14 white dwarfs in the field of the cluster: 12 DAs,
1 hot DQ, and 1 DB star. For each DA, we determine the white dwarf mass and
cooling age, from which we derive the each star's progenitor mass. These data
are then added to the empirical initial-final mass relation (IFMR), where the
M35 WDs contribute significantly to the high-mass end of the relation. The
resulting points are consistent with previously-published linear fits to the
IFMR, modulo moderate systematics introduced by the uncertainty in the star
cluster age. Based on this cluster alone, the observational lower limit on the
maximum mass of white dwarf progenitors is found to be ~5.1-5.2 solar masses at
the 95% confidence level; including data from other young open clusters raises
this limit as high as 7.1 solar masses, depending on the cluster membership of
three massive WDs and the core-composition of the most massive WDs. We find
that the apparent distance modulus and extinction derived solely from the
cluster white dwarfs [(m-M)v=10.45 +/- 0.08 and E(B-V)=0.185 +/- 0.010,
respectively] is fully consistent with that derived from main-sequence fitting
techniques. Four M35 WDs may be massive enough to have oxygen-neon cores; the
assumed core composition does not significantly affect the empirical IFMR.
Finally, the two non-DA WDs in M35 are photometrically consistent with cluster
membership; further analysis is required to determine their memberships.
