The Effect of Absorption Systems on Cosmic Reionization

TL;DR

This study uses large-scale simulations to explore how absorption systems influence the morphology and timeline of cosmic reionization, emphasizing the importance of the mean free path in modeling the process accurately.

Contribution

It introduces an efficient 3D smoothing method that accounts for absorption systems, highlighting their critical role in the complex structure of reionization.

Findings

Reionization morphology strongly depends on the mean free path to absorption systems.

Large simulation volumes are necessary to accurately model reionization at low neutral fractions.

Absorption systems significantly increase the complexity of the overlap phase.

Abstract

We use large-scale simulations to investigate the morphology of reionization during the final, overlap phase. Our method uses an efficient three-dimensional smoothing technique which takes into account the finite mean free path due to absorption systems, lambda, by only smoothing over scales R_s<lambda. The large dynamic range of our calculations is necessary to resolve the neutral patches left at the end of reionization within a representative volume; we find that simulation volumes exceeding several hundred Mpc on a side are necessary in order to properly model reionization when the neutral fraction is ~0.01-0.3. Our results indicate a strong dependence of percolation morphology on a large and uncertain region of model parameter space. The single most important parameter is the mean free path to absorption systems, which serve as opaque barriers to ionizing radiation. If these absorption systems were as abundant as some realistic estimates indicate, the spatial structure of the overlap phase is considerably more complex than previously predicted. In view of the lack of constraints on the mean free path at the highest redshifts, current theories that do not include absorption by Lyman-limit systems, and in particular three-dimensional simulations, may underestimate the abundance of neutral clouds at the end of reionization. This affects predictions for the 21 cm signal associated with reionization, interpretation of absorption features in quasar spectra at z ~5-6, the connection between reionization and the local universe, and constraints on the patchiness and duration of reionization from temperature fluctuations measured in the cosmic microwave background arising from the kinetic Sunyaev-Zel'dovich effect.