The Initial Mass Function in Star-forming Regions in the Magellanic Clouds

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The stellar Initial Mass Function (IMF) accounts for the distribution of the masses of stars at the time they are formed. The IMF is a very important distribution function, which is directly linked to the formation of stars in individual stellar systems, but also in a galaxy as a whole. There is a lack of information on the low-mass end of the IMF, especially in galaxies other than our own, because of observational constraints, which do not allow us to detect the fainter stars. I will take advantage of high-resolution observations with the Hubble Space Telescope (HST) of the Magellanic Clouds, our neighboring dwarf galaxies, to investigate the IMF of low-mass stars in their low-metallicity environments. These observations include previously taken archived data, and also data already granted to me in STScI Cycle 14. This study will add substantial information on the formation of stars with masses comparable and smaller than the mass of the Sun in active star forming stellar systems, such as stellar associations. Stars, which are not members of any specific system, but belong to the general field population, will also be studied. Furthermore, these observations, coordinated with high-resolution ground-based observations with the most advanced near-infrared detectors will allow the discovery of pre-main-sequence stars, objects which have not started their lives as stars yet, and the study of their IMF. This would open a new field of study for the Magellanic Clouds.