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

TL;DR

This study investigates the age, mass, and embedded state of young massive clusters in M83, revealing they are typically exposed within 4 million years, and discusses methods to improve age estimation accuracy for these clusters.

Contribution

The paper provides new insights into the rapid emergence of young massive clusters from their natal gas and introduces improved methods for constraining their ages.

Findings

Clusters are exposed within less than 4 Myr.

SED fitting inaccuracies are caused by morphology and aperture effects.

Near-infrared and spectral features can better constrain young cluster ages.

Abstract

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.