Revised Simulations of the Planetary Nebulae Luminosity Function
  We describe a revised procedure for the numerical simulation of planetary
nebulae luminosity functions (PNLF), improving on previous work (M\'endez &
Soffner 1997). The procedure now is based on new H-burning post-AGB
evolutionary tracks (Miller Bertolami 2016). For a given stellar mass, the new
central stars are more luminous and evolve faster. We have slightly changed the
distribution of the [OIII] 5007 intensities relative to those of H$\beta$ and
the generation of absorbing factors, while still basing their numerical
modeling on empirical information extracted from studies of galactic planetary
nebulae (PNs) and their central stars. We argue that the assumption of PNs
being completely optically thick to H-ionizing photons leads to conflicts with
observations and show that to account for optically thin PNs is necessary. We
then use the new simulations to estimate a maximum final mass, clarifying its
meaning, and discuss the effect of internal dust extinction as a possible way
of explaining the persistent discrepancy between PNLF and surface brightness
fluctuation (SBF) distances. By adjusting the range of minimum to maximum final
mass, it is also possible to explain the observed variety of PNLF shapes at
intermediate magnitudes. The new PN formation rates are calculated to be
slightly lower than suggested by previous simulations based on older post-AGB
evolutionary tracks.
