Reaching the low-mass content in Young Massive Star Clusters Using Multi Conjugate Adaptive Optics

How massive star clusters form and what the Initial Mass Function is of their stellar population are fundamental to address for us to understand star formation. However, these objects are hard to study due to their rarity and hence large distances from the sun, their compactness and they are deeply embedded in their early phases. High spatial resolution near-infrared imaging is key to resolve the individual stars. WFC3 onboard HST has been instrumental but is lacking crucial K band observations that are necessary to penetrate the extinction and to identify circumstellar disks. Due to the good relative of the system the data obtained now can further be used to measure the proper motion of Galactic Young Massive Clusters. Ground-based Multi Conjugate Adaptive Optics observations in the K band are ideal to complement the shorter wavelength HST data. Here we present recent results on several Young Massive Star Clusters in the Galaxy and the Large Magellanic Cloud. We discuss the low-mass IMF where with the K band data we reach deeper than previously possible and the derived fraction of cluster members with circumstellar disks. Further, we discuss the stellar content of a embedded cluster in the Large Magellanic Clouds that may be a super star cluster in the making.