  Thermally-Pulsing Asymptotic Giant Branch (TP-AGB) stars are relatively short
lived (less than a few Myr), yet their cool effective temperatures, high
luminosities, efficient mass-loss and dust production can dramatically effect
the chemical enrichment histories and the spectral energy distributions of
their host galaxies. The ability to accurately model TP-AGB stars is critical
to the interpretation of the integrated light of distant galaxies, especially
in redder wavelengths. We continue previous efforts to constrain the evolution
and lifetimes of TP-AGB stars by modeling their underlying stellar populations.
Using Hubble Space Telescope (HST) optical and near-infrared photometry taken
of 12 fields of 10 nearby galaxies imaged via the ACS Nearby Galaxy Survey
Treasury and the near-infrared HST/SNAP follow-up campaign, we compare the
model and observed TP-AGB luminosity functions as well as the number ratio of
TP-AGB to red giant branch stars. We confirm the best-fitting mass-loss
prescription, introduced by Rosenfield et al. 2014, in which two different wind
regimes are active during the TP-AGB, significantly improves models of many
galaxies that show evidence of recent star formation. This study extends
previous efforts to constrain TP-AGB lifetimes to metallicities ranging -1.59 <
[Fe/H] < -0.56 and initial TP-AGB masses up to ~ 4 Msun, which include TP-AGB
stars that undergo hot-bottom burning.
