%0 Generic %1 xu2016formation %A Xu, Hao %A Norman, Michael L. %A O'Shea, Brian W. %A Wise, John H. %D 2016 %K formation metal mixing popIII simulation %T Late Pop III Star Formation During the Epoch of Reionization: Results from the Renaissance Simulations %U http://arxiv.org/abs/1604.03586 %X 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$_ødot$. 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 $\alpha$ 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.

@misc{xu2016formation, 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 $\alpha$ 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.}, added-at = {2016-04-14T10:04:31.000+0200}, author = {Xu, Hao and Norman, Michael L. and O'Shea, Brian W. and Wise, John H.}, biburl = {https://www.bibsonomy.org/bibtex/22acc798e7b5c891b0c4a05c272f7bf7a/miki}, description = {[1604.03586] Late Pop III Star Formation During the Epoch of Reionization: Results from the Renaissance Simulations}, interhash = {8714dfab299ec39186a4552f2227c622}, intrahash = {2acc798e7b5c891b0c4a05c272f7bf7a}, keywords = {formation metal mixing popIII simulation}, note = {cite arxiv:1604.03586Comment: 8 pages, 4 figures, 3 tables. Accepted by ApJ}, timestamp = {2016-04-14T10:04:31.000+0200}, title = {Late Pop III Star Formation During the Epoch of Reionization: Results from the Renaissance Simulations}, url = {http://arxiv.org/abs/1604.03586}, year = 2016 }