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We study the impact of inhomogeneous hydrogen reionization on the thermalevolution of the intergalactic medium (IGM) using hydrodynamic + radiativetransfer simulations where reionization is completed either early (z ~ 9) orlate (z ~ 6). In general, we find that low-density gas near large-scaleoverdensities is ionized and heated earlier than gas in the large-scale,underdense voids. Furthermore, at a later time the IGM temperature is inverselyrelated to the reionization redshift because gas that is heated earlier hasmore time to cool through adiabatic expansion and Compton scattering. Thus, atthe end of reionization the median temperature-density relation is an invertedpower-law with slope gamma-1 ~ -0.2, in both models. However, at fixed density,there is up to order unity scatter in the temperature due to the distributionof reionization redshifts. Because of the complex equation-of-state, theevolved IGM temperature-density relations for the redshift range 4 < z < 6 canstill have significant curvature and scatter. These features must be taken intoaccount when interpreting the Lyman alpha absorption in high redshift quasarspectra.

Imprint of Inhomogeneous Hydrogen Reionization on the Temperature Distribution of the Intergalactic Medium