The vast majority of our knowledge of star formation is deduced from observations of near-solar, Galactic star forming regions. This neglects the how differing galactic properties such as metallicity and large scale tidal forces affect star formation on small scales. At distances of 50kpc and 60kpc, respectively the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) allow the study of star formation on both a galactic scale and on the scale of individual stars at lower metalicities than the Milky Way.

Spitzer and Herschel large scale surveys lack the spatial resolution to fully resolve YSOs. We present SINFONI K-band integral field spectroscopy of 23 YSO targets (20 in the SMC and 3 in N113 in the LMC) selected using Spitzer photometry and spectroscopy. This provides a resolution of 0.1”, giving spatial resolutions of ∼0.024pc in the LMC and ∼0.029pc in the SMC.

With resolutions improved by an order of magnitude compared to Spitzer observations, we resolve significantly more continuum sources (30 in the SMC, 6 in N113). We find that whilst many of the properties of the YSOs appear to be similar to Galactic samples, the detection rates of emission lines differ significantly from those of the MW. We also find extensive evidence of strong stellar feedback associated with the star formation process in the Magellanic Clouds.

This is the first study to utilise NIR integral field spectroscopy to obtain high spatial and spectral resolution observations of a significant sample of Magellanic YSOs.