Metal-Free Gas Supply at the Edge of Reionization: Late-Epoch Population III Star Formation

TL;DR

This paper investigates the persistence of metal-free gas pockets at the end of reionization, predicting the formation and detectability of Population III stars and supernovae at redshift z~6 through cosmological simulations and analytical models.

Contribution

It demonstrates that metal-free gas can still exist at z~6 and estimates the formation and supernova rates of Population III stars, guiding observational search strategies.

Findings

Metal-free halos form at a rate >10^{-9} Mpc^{-3}yr^{-1} at z=6.

Expected supernova rate is approximately 2.6x10^{-3} deg^{-2}yr^{-1}.

Large area surveys are necessary to detect Population III supernovae at high redshift.

Abstract

While the average metallicity of the intergalactic medium rises above Z~10^{-3} Zsun by the end of the reionization, pockets of metal-free gas can still exist at later times. We quantify the presence of a long tail in the formation rate of metal-free halos during late stages of reionization (redshift z~6), which might offer the best window to detect Population III stars. Using cosmological simulations for the growth of dark matter halos, coupled with analytical recipes for the metal enrichment of their interstellar medium, we show that pockets of metal-free gas exist at z~6 even under the assumption of high efficiency in metal pollution via winds. A comoving metal-free halo formation rate d^2n/dtdV > 10^{-9} Mpc^{-3}yr^{-1} is expected at z=6 for halos with virial temperature T_{vir}~10^4 K (mass ~10^8 Msun), sufficient to initiate cooling even with strong negative radiative feedback. Under the assumption of a single Population III supernova formed per metal-free halo, we expect an observed supernova rate of 2.6x10^{-3} deg^{-2}yr^{-1} in the same redshift range. These metal-free stars and their supernovae will be isolated and outside galaxies (at distances >150 h^{-1} kpc) and thus significantly less biased than the general population of ~10^8 Msun halos at z~6. Supernova searches for metal-free explosions must thus rely on large area surveys. If metal-free stars produce very luminous supernovae, like SN2006gy, then a multi-epoch survey reaching m_AB =27 at 1 micron is sufficient for detecting them at z=6. While the Large Synoptic Survey Telescope will not reach this depth in the z band, it will be able to detect several tens of Population III supernovae in the i and r bands at z <5.5, when their observed rate is down to 3-8x10^{-4} deg^{-2} yr^{-1}.