Formation of Pop II star clusters in the aftermath of a pair instability supernova

Abstract

Pop II stars formed a few hundred million years after the Big Bang were key drivers of cosmic reionization and building blocks of high redshift galaxies. How and when these stars formed is a subject of ongoing research. We conduct cosmological radiation hydrodynamical simulations to investigate the formation of Pop II star clusters in dark matter halos forming at $z=10-25$ in the aftermath of a pair instability supernova (PISN). Our simulations model the formation of Pop III and Pop II stars in a self-consistent manner along with their radiative, chemical and SN feedback in halos of $5\times 10^5-7\times 10^7{\mathrm{M}}_{\odot }$. We find that a PISN evacuates the gas from halos $\le 3\times 10^6{\mathrm{M}}_{\odot }$ and thereafter shuts off in situ star formation for at-least 30 Myr. Pop II stellar clusters of $923{\mathrm{M}}_{\odot }$ and $6800{\mathrm{M}}_{\odot }$ form in halos of $3.5\times 10^7{\mathrm{M}}_{\odot }$ and $7.2\times 10^7{\mathrm{M}}_{\odot }$, respectively. The mode of star formation is highly episodic and mainly regulated by Pop II SN feedback. The average star formation rates are $10^{-5}-10^{-4}{\mathrm{M}}_{\odot }/yr$ and the star formation efficiency is less than 1\%.

arXiv commentTo be published in ApJL, comments welcome

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