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We investigate how the hydrostatic suppression of baryonic accretion affectsthe growth rate of dark matter halos during the Epoch of Reionization. Bycomparing halo properties in a simplistic hydrodynamic simulation in which gasonly cools adiabatically, with its collisionless equivalent, we find that halogrowth is slowed as hydrostatic forces prevent gas from collapsing. In oursimulations, at the high redshifts relevant for reionization (between ${\sim}6$and ${\sim}11$), halos that host dwarf galaxies ($\lesssim 10^{9}\mathrm{M_\odot}$) can be reduced by up to a factor of 2 in mass due to thehydrostatic pressure of baryons. Consequently, the inclusion of baryoniceffects reduces the amplitude of the low mass tail of the halo mass function byfactors of 2 to 4. In addition, we find that the fraction of baryons in darkmatter halos hosting dwarf galaxies at high redshift never exceeds ${\sim}90\%$of the cosmic baryon fraction. When implementing baryonic processes, includingcooling, star formation, supernova feedback and reionization, the suppressioneffects become more significant with further reductions of ${\sim}30\%$ to60\%. Although convergence tests suggest that the suppression may become weakerin higher resolution simulations, this suppressed growth will be important forsemi-analytic models of galaxy formation, in which the halo mass inherited froman underlying N-body simulation directly determines galaxy properties. Based onthe adiabatic simulation, we provide tables to account for these effects inN-body simulations, and present a modification of the halo mass function alongwith explanatory analytic calculations.

Dark-ages Reionization & Galaxy Formation Simulation VIII. Suppressed growth of dark matter halos during the Epoch of Reionization