Reionization Bias in High Redshift Quasar Near-Zones

TL;DR

This paper presents a model for the ionization state evolution of the IGM around high-redshift quasars, explaining observed Ly-alpha forest features and near-zone size evolution during reionization.

Contribution

The model uniquely accounts for biased dense regions near quasars and matches multiple observational constraints of reionization at z~4-6.

Findings

Ionization state evolution near quasars precedes that in typical regions by 0.3 redshift units.

Near-zone sizes are more sensitive to background ionization and temperature than neutral hydrogen fraction.

Rapid evolution of near-zone sizes is driven by the completion of reionization overlap.

Abstract

Absorption spectra of high redshift quasars exhibit an increasingly thick Ly-alpha forest towards z~6. However, the interpretation of these spectra is complicated by the fact that the Ly-alpha optical depth is already large for neutral hydrogen fractions in excess of 10^-4, and also because quasars are expected to reside in dense regions of the IGM. We present a model for the evolution of the ionization state of the IGM which is applicable to the dense, biased regions around high-redshift quasars as well as more typical regions in the IGM, and combine this with numerical radiative transfer simulations. Our model is able to simultaneously reproduce the observed Ly-alpha forest opacity at 4<z<6, the ionizing photon mean-free-path at z~4 and the rapid evolution of highly ionized near-zone sizes around high-redshift quasars at 5.8<z<6.4. We find that within 5 physical Mpc of a high redshift quasar, the evolution of the ionization state of the IGM precedes that in more typical regions by around 0.3 redshift units. More importantly, when combined with the rapid increase in the ionizing photon mean-free-path expected shortly after overlap, this offset results in an ionizing background near the quasar which exceeds the value in the rest of the IGM by a factor of ~2-3. We further find that in the post-overlap phase of reionization the size of the observed quasar near-zones is not directly sensitive to the neutral hydrogen fraction of the IGM. Instead, these sizes probe the level of the background ionization rate and the temperature of the surrounding IGM. The observed rapid evolution of the quasar near-zone sizes at 5.8<z<6.4 can thus be explained by the rapid evolution of the ionizing background, which in our model is caused by the completion of overlap at the end of reionization by 6<z<7.