{"ID":2918937,"CreatedAt":"2026-06-01T22:54:38.67411846Z","UpdatedAt":"2026-06-01T22:54:38.67411846Z","DeletedAt":null,"paper_url":"https://arxiv.org/abs/1604.03586","arxiv_id":"1604.03586","title":"Late Pop III Star Formation During the Epoch of Reionization: Results from the Renaissance Simulations","abstract":"We present results on the formation of Pop III stars at redshift 7.6 from the Renaissance Simulations, a suite of extremely high-resolution and physics-rich radiation transport hydrodynamics cosmological adaptive-mesh refinement simulations of high redshift galaxy formation performed on the Blue Waters supercomputer. In a survey volume of about 220 comoving Mpc$^3$, we found 14 Pop III galaxies with recent star formation. The surprisingly late formation of Pop III stars is possible due to two factors: (i) the metal enrichment process is local and slow, leaving plenty of pristine gas to exist in the vast volume; and (ii) strong Lyman-Werner radiation from vigorous metal-enriched star formation in early galaxies suppresses Pop III formation in (\"not so\") small primordial halos with mass less than $\\sim$ 3 $\\times$ 10$^7$ M$_\\odot$. We quantify the properties of these Pop III galaxies and their Pop III star formation environments. We look for analogues to the recently discovered luminous Ly $α$ emitter CR7 (Sobral et al. 2015), which has been interpreted as a Pop III star cluster within or near a metal-enriched star forming galaxy. We find and discuss a system similar to this in some respects, however the Pop III star cluster is far less massive and luminous than CR7 is inferred to be.","url_abs":"https://arxiv.org/abs/1604.03586v1","url_pdf":"https://arxiv.org/pdf/1604.03586v1","authors":"Hao Xu, Michael L. Norman, Brian W. O'Shea, John H. Wise","published":"2016-04-12T21:05:34Z","has_code":false}