Metallicities of Young Massive Clusters in NGC 5236 (M83)
  We present integrated-light spectra of 8 Young Massive Clusters (YMCs) in the
metal-rich spiral galaxy NGC 5236 (M 83). The observations were taken with the
X-Shooter spectrograph on the ESO Very Large Telescope. Through the use of
theoretical isochrones and synthetic integrated-light (IL) spectra we derive
metallicities and study the radial metallicity gradient observed through these
young populations. For the inner regions of the galaxy we observe a relatively
shallow metallicity gradient of $-$0.37 $\pm$0.29 dex R$_{25}^{-1}$, agreeing
with chemical evolution models with an absence of infall material and a
relatively low mass loss due to winds in the inner parts of the disk. We
estimate a central metallicity of [$Z$] = $+$0.17 $\pm$ 0.12 dex, finding
excellent agreement with that obtained via other methods (e.g. blue supergiants
and J-band). We infer a metallicity of 12+log(O/H) = 8.75 $\pm$ 0.08 dex at
R/R$_{25}$ = 0.4, which fits the stellar mass-metallicity relation (MZR)
compilation of blue supergiants and IL studies.
