IMPACT OF H₂-BASED STAR FORMATION MODEL ON THEz⩾ 6 LUMINOSITY FUNCTION AND THE IONIZING PHOTON BUDGET FOR REIONIZATION

We present the results of a numerical study examining the effect of an H 2 -based star formation (SF) model on the rest-frame UV luminosity function and star formation rate function (SFRF) of z ⩾ 6 galaxies, and the implications for reionization. Using cosmological hydrodynamical simulations outfitted with an H 2 -SF model, we find good agreement with our previous results (non-H 2 SF model) and observations at M uv ⩽ −18. However, at M uv > −18, we find that the LF deviates from both our previous work and current observational extrapolations, producing significantly fewer low-luminosity galaxies and exhibiting additional turnover at the faint end. We constrain the redshift evolution of this turnover point using a modified Schechter function that includes additional terms to quantify the turnover magnitude ( ) and subsequent slope (β). We find that evolves from (at z = 8) to −15.38 ( z = 6), while β becomes shallower by Δβ = 0.22 during the same epoch. This occurs in an M uv range that will be observable by James Webb Space Telescope . By integrating the SFRF, we determine that even though the H 2 -SF model significantly reduces the number density of low-luminosity galaxies at M uv > −18, it does not suppress the total SFR density enough to affect the capability of SF to maintain reionization.