  The goal of the present study is twofold. First, we employ new HST/STIS
spectra and photoionization modeling techniques to determine the progenitor
masses of eight planetary nebulae (IC 2165, IC 3568, NGC 2440, NGC 3242, NGC
5315, NGC 5882, NGC 7662 and PB6). Second, for the first time we are able to
compare each object's observed nebular abundances of helium, carbon and
nitrogen with abundance predictions of these same elements by a stellar model
that is consistent with each object's progenitor mass. Important results
include the following: 1) the mass range of our objects' central stars matches
well with the mass distribution of other PN central stars and white dwarfs; 2)
He/H is above solar in all of our objects, in most cases likely due to the
predicted effects of first dredge up; 3) most of our objects show negligible C
enrichment, probably because their low masses preclude 3rd dredge-up; 4) C/O
versus O/H for our objects appears to be inversely correlated, perhaps
consistent with the conclusion of theorists that the extent of atmospheric
carbon enrichment from first dredge-up is sensitive to a parameter whose value
increases as metallicity declines; 5) stellar model predictions of nebular C
and N enrichment are consistent with observed abundances for progenitor star
masses <=1.5 Msun. Finally, we present the first published photoionization
models of NGC 5315 and NGC 5882.
