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The properties of Population III (Pop III) stars impact many aspects ofprimeval structure formation such as the onset of cosmological reionization andearly chemical enrichment. However, in spite of over twenty years of numericalsimulations and attempts to constrain the Pop III initial mass function (IMF)by stellar archaelogy, little is known of the masses of the first stars forcertain. Here, we model the effect of Pop III IMF on the properties of primevalgalaxies with a suite of high-resolution radiation-hydrodynamical simulationswith ENZO. We find that a top-heavy Pop III IMF results in earlier starformation but dimmer galaxies than a more conventional Salpeter-type IMFbecause explosions of massive Pop III stars produce more turbulence thatsuppresses high-mass second-generation star formation. Our models suggest thatthe Pop III IMF could therefore be inferred from detections of primordialgalaxies, which will be principal targets of the James Webb Space Telescope andextremely large telecopes on the ground in the coming decade.

How the Population III Initial Mass Function Governs the Properties of the First Galaxies