Neutral hydrogen in and around galaxies during the Epoch of Reionization

JWST spectra revealing Lyman-$α$ (Ly$α$) absorption in z~ 5-14 galaxies offer a unique probe of reionization's earliest stages. However, disentangling absorption by the increasingly neutral intergalactic medium (IGM) from that in galaxies' interstellar and circumgalactic medium (ISM, CGM) remains challenging due to the poorly constrained nature of neutral hydrogen (HI) in and around galaxies at these redshifts. We use the SERRA high-resolution cosmological zoom-in simulations to characterize the HI distribution and its evolution along sightlines to star-forming regions during reionization, to interpret the contribution of local HI (ISM+CGM) to Ly$α$ absorption in $z>5$ spectra. We analyze ~ 100 $z=6-9.5$ galaxies, generating mock sightlines from each galaxy's star formation peak. We study the sightline distribution of HI column densities (NHI) and its variation with radius, halo mass and redshift. We find broad sightline variation in NHI (0.5-1.5dex) due to complex ISM morphology driven by bursty star formation, with median log(NHI/ cm⁻²) 21-22. Dense ISM gas is the dominant origin of damped Ly$α$ absorption (DLA) systems along sightlines towards star-forming regions, outweighing gas in the CGM, filaments and proximate absorbers. Median NHI increases with halo mass, scaling roughly with the virial radius, as expected due to larger potentials and more extended CGM, but shows negligible redshift evolution at fixed halo mass. This suggests post-reionization NHI distributions may provide useful priors to interpret IGM damping wings at higher redshifts. To interpret strong $z>5$ DLA candidates found by JWST, we investigate NHI>10²² cm⁻² sightlines. These trace dense, metal-enriched ISM within <1 kpc of massive halos, a scenario testable with higher-resolution spectroscopy.