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We present a photometric and spectroscopic study of the white dwarfpopulation of the populous, intermediate-age open cluster M35 (NGC 2168); thisstudy expands upon our previous study of the white dwarfs in this cluster. Wespectroscopically 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 andcooling age, from which we derive the each star's progenitor mass. These dataare then added to the empirical initial-final mass relation (IFMR), where theM35 WDs contribute significantly to the high-mass end of the relation. Theresulting points are consistent with previously-published linear fits to theIFMR, modulo moderate systematics introduced by the uncertainty in the starcluster age. Based on this cluster alone, the observational lower limit on themaximum mass of white dwarf progenitors is found to be ~5.1-5.2 solar masses atthe 95% confidence level; including data from other young open clusters raisesthis limit as high as 7.1 solar masses, depending on the cluster membership ofthree massive WDs and the core-composition of the most massive WDs. We findthat the apparent distance modulus and extinction derived solely from thecluster 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 fittingtechniques. Four M35 WDs may be massive enough to have oxygen-neon cores; theassumed core composition does not significantly affect the empirical IFMR.Finally, the two non-DA WDs in M35 are photometrically consistent with clustermembership; further analysis is required to determine their memberships.

astrophysical journal/the astrophysical journal

Probing The Lower Mass Limit for Supernova Progenitors and the High-Mass  End of the Initial-Final Mass Relation from White Dwarfs in the Open Cluster  M35 (NGC 2168)