Baseline metal enrichment from Population III star formation in cosmological volume simulations

We utilize the hydrodynamic and N-body code { GIZMO} coupled with our newly developed sub-grid Population~III (Pop~III) Legacy model, designed specifically for cosmological volume simulations, to study the baseline metal enrichment from Pop~III star formation at $z>7$. In this idealized numerical experiment, we only consider Pop~III star formation. We find that our model Pop~III star formation rate density (SFRD), which peaks at ~ 10⁻³\ M_ yr⁻¹ Mpc⁻¹ near z~10, agrees well with previous numerical studies and is consistent with the observed estimates for Pop~II SFRDs. The mean Pop~III metallicity rises smoothly from $z=25-7$, but does not reach the critical metallicity value, Zcrit=10⁻⁴\ Z_, required for the Pop~III to Pop~II transition in star formation mode until z7. This suggests that, while individual halos can suppress in-situ Pop~III star formation, the external enrichment is insufficient to globally terminate Pop~III star formation. The maximum enrichment from Pop~III star formation in star forming dark matter halos is Z~10⁻²\ Z_, whereas the minimum found in externally enriched haloes is Z10⁻⁷\ Z_. Finally, mock observations of our simulated IGM enriched with Pop~III metals produce equivalent widths similar to observations of an extremely metal poor damped Lyman alpha (DLA) system at $z=7.04$, which is thought to be enriched by Pop~III star formation only.