The first generation of stars to have formed in the universe were likely very different than the stars we observe today. These Population III stars formed from pristine gas with no metals, and their formation was crucial to the early evolution of galaxies. While we have yet to observe a Population III star forming halo directly, we may be able to see them indirectly through their supernovae or their effect on the cosmological 21-cm background. I will present a set of semi-analytic models studying the formation of these Population III stars and the transition of their halos to metal-enriched star formation. I will also discuss the prospects of observing this mode of star formation, focusing on their effect on the cosmological 21-cm background and comparing our results to the recent claimed detection of a 21-cm signal by the EDGES experiment.
Speaker: Rick Mebane, UCLA
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