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Lyman Limit Systems (LLSs) are dense hydrogen clouds with high enough HIcolumn densities ($N_{\rm HI}$) to absorb Lyman continuum photons emitted fromdistant quasars. Their high column densities imply an origin in denseenvironments; however, the statistics and distribution of LLSs at highredshifts still remain uncertain. In this paper, we use self-consistentradiative transfer cosmological simulations from the "Cosmic Reionization OnComputers" (CROC) project to study the physical properties of LLSs at the tailend of cosmic reionization at $z\sim6$. We generate 3000 synthetic quasarsightlines to obtain a large number of LLS samples in the simulations. Inaddition, with the high physical fidelity and resolution of CROC, we are ableto quantify the association between these LLS samples and nearby galaxies. Ourresults show that a higher fraction of higher column density LLSs are spatiallyassociated with nearby galaxies. Moreover, we find that LLSs that are not nearany galaxy typically reside in filamentary structures connecting neighboringgalaxies in the intergalactic medium (IGM). This quantification of thedistribution and associations of LLSs to large scale structures informs ourunderstanding of the IGM-galaxy connection during the Epoch of Reionization,and provides a theoretical basis for interpreting future observations.

Cosmic Reionization On Computers: Statistics, Physical Properties and Environment of Lyman Limit Systems at $z\sim6$