  The study of young massive clusters can provide key information for the
formation of globular clusters, as they are often considered analogues. A
currently unanswered question in this field is how long these massive clusters
remain embedded in their natal gas, with important implications for the
formation of multiple populations that have been used to explain phenomena
observed in globular clusters. We present an analysis of ages and masses of the
young massive cluster population of M83. Through visual inspection of the
clusters, and comparison of their SEDs and position in colour-colour space, the
clusters are all exposed (no longer embedded) by < 4 Myr, most likely less,
indicating that current proposed age spreads within older clusters are
unlikely. We also present several methods of constraining the ages of very
young massive clusters. This can often be difficult using SED fitting due to a
lack of information to disentangle age-extinction degeneracies and possible
inaccurate assumptions in the models used for the fitting. The individual
morphology of the Halpha around each cluster has a significant effect on the
measured fluxes, which contributes to inaccuracies in the age estimates for
clusters younger than 10 Myr using SED fitting. This is due to model
uncertainties and aperture effects. Our methods to help constrain ages of young
clusters include using the near-infrared and spectral features, such as
Wolf-Rayet stars.
