Inhomogeneous recombinations during cosmic reionization

By depleting the ionizing photon budget available to expand cosmic H ii regions, recombining systems (or Lyman limit systems) can have a large impact during (and following) cosmic reionization. Unfortunately, directly resolving such structures in large-scale reionization simulations is computationally impractical. Instead, here we implement a subgrid prescription for tracking inhomogeneous recombinations in the intergalactic medium. Building on previous work parametrizing photoheating feedback on star formation, we present large-scale, seminumeric reionization simulations which self-consistently track the local (subgrid) evolution of both sources and sinks of ionizing photons. Our simple, single-parameter model naturally results in both an extended reionization and a modest, slowly evolving emissivity, consistent with observations. Recombinations are instrumental in slowing the growth of large H ii regions, and damping the rapid rise of the ionizing background in the late stages of (and following) reionization. As a result, typical H ii regions are smaller by factors of similar to 2 to 3 throughout reionization. The large-scale (k less than or similar to 0.2 Mpc(-1)) ionization power spectrum is suppressed by factors of greater than or similar to 2-3 in the second half of reionization. Therefore properly modelling recombinations is important in interpreting virtually all reionization observables, including upcoming interferometry with the redshifted 21cm line. Consistent with previous works, we find the clumping factor of ionized gas to be C (H ii) similar to 4 at the end of reionization.