Star Formation in External Galaxies
The conversion of gas into stars is one of the key physical processes that governs the evolution of galaxies through cosmic times. While simple in concept, this process has a high degree of complexity, owing to its multi-scale nature, for the sizes of individual stars to those of galaxy groups and Clusters. My research interests aim at understanding star formation on the scales of galaxies, using information provided by a variety of both space-borne (Hubble, Spitzer, Herschel, etc.) and ground-based telescopes, at wavelengths that range from the ultraviolet to the radio.
Questions that my research specifically addresses are: how to derive unbiased measures of star formation from the data, how to remove or mitigate effects of dust attenuation at UV and optical wavelengths, how to leverage the observed emission from the dust itself to derive star formation rates, how individual stars are linked to the large star-forming structures observed in galaxies, how the gas is linked to star formation, and how the feedback from evolving stars and star clusters affects the gas and its ability to form new generations of stars.