Comparison of Convective Overshooting Models and Their Impact on
  Abundances from Integrated Light Spectroscopy of Young ($<$ 3 Gyr) Star
  Clusters
  As part of an ongoing program to measure detailed chemical abundances in
nearby galaxies, we use a sample of young to intermediate age clusters in the
Large Magellanic Cloud with ages of 10 Myr to 2 Gyr to evaluate the effect of
isochrone parameters, specifically core convective overshooting, on Fe
abundance results from high resolution, integrated light spectroscopy. In this
work we also obtain fiducial Fe abundances from high resolution spectroscopy of
the cluster individual member stars. We compare the Fe abundance results for
the individual stars to the results from isochrones and integrated light
spectroscopy to determine whether isochrones with convective overshooting
should be used in our integrated light analysis of young to intermediate age
(10 Myr -3 Gyr) star clusters. We find that when using the isochrones from the
Teramo group, we obtain more accurate results for young and intermediate age
clusters over the entire age range when using isochrones without convective
overshooting. While convective overshooting is not the only uncertain aspect of
stellar evolution, it is one of the most readily parametrized ingredients in
stellar evolution models, and thus important to evaluate for the specific
models used in our integrated light analysis. This work demonstrates that our
method for integrated light spectroscopy of star clusters can provide unique
tests for future constraints on stellar evolution models of young and
intermediate age clusters.
