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The study of young massive clusters can provide key information for theformation of globular clusters, as they are often considered analogues. Acurrently unanswered question in this field is how long these massive clustersremain embedded in their natal gas, with important implications for theformation of multiple populations that have been used to explain phenomenaobserved in globular clusters. We present an analysis of ages and masses of theyoung massive cluster population of M83. Through visual inspection of theclusters, and comparison of their SEDs and position in colour-colour space, theclusters are all exposed (no longer embedded) by < 4 Myr, most likely less,indicating that current proposed age spreads within older clusters areunlikely. We also present several methods of constraining the ages of veryyoung massive clusters. This can often be difficult using SED fitting due to alack of information to disentangle age-extinction degeneracies and possibleinaccurate assumptions in the models used for the fitting. The individualmorphology of the Halpha around each cluster has a significant effect on themeasured fluxes, which contributes to inaccuracies in the age estimates forclusters younger than 10 Myr using SED fitting. This is due to modeluncertainties and aperture effects. Our methods to help constrain ages of youngclusters include using the near-infrared and spectral features, such asWolf-Rayet stars.

Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories