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We study the observational consequences of several unknown properties ofPopulation III (Pop III) stars using large-scale cosmological simulations thatinclude a subgrid model to track the unresolved mixing of pollutants. Varyingthe value of the critical metallicity that marks the boundary between Pop IIIand Population II (Pop II) star formation across 2 dex has a negligible effecton the fraction of Pop III stars formed and the subsequent fraction of Pop IIIflux from high-redshift galaxies. However, adopting a log normal initial massfunction (IMF) for Pop III stars, in place of a baseline Salpeter IMF, resultsin a Pop III star formation rate density (SFRD) that is 1/4 of the baselinerate. The flux from high-redshift galaxies modeled with this IMF is highlybimodal, resulting in a tiny fraction of $z \leq 8$ galaxies with more than75\% of their flux coming from Pop III stars. However, at $z=9$, right beforereionization in our simulations, $\approx$ 20\% of galaxies are Pop III-brightwith $m_{\rm UV} \le 31.4$ mag and at least 75\% of their flux generated by PopIII stars . Additionally, the log normal Pop III IMF results in a population ofcarbon enhanced, metal poor stars in reasonable agreement with MW haloobservations. Our analysis supports the conclusion that the Pop III IMF wasdominated by stars in the 20-120$M_{\odot}$ range that generate SN withcarbon-enhanced ejecta.

Following the Cosmic Evolution of Pristine Gas III: The Observational Consequences of the Unknown Properties of Population III Stars