Studying dark gaps in Ly-$\alpha$ forest transmission with large reionization simulations

TL;DR

This study uses large-scale simulations to analyze Ly-$eta$ forest dark gaps, providing insights into the IGM conditions during the final stages of cosmic reionization around redshift 5-6.

Contribution

It introduces a large-volume simulation framework to compare dark-gap distributions with observations, constraining reionization timing and IGM properties.

Findings

Models with later reionization ($z ext{~}5.4$) best match observed data.

Short mean free path models are disfavored at lower redshifts.

Simulations cannot yet reproduce large-scale flux correlations.

Abstract

The physical conditions of the intergalactic medium (IGM) during the final stages of cosmic reionization ($z\sim5.0-6.0$) are not yet fully understood. Recent reports of unexpectedly large-scale ($\ge 150 h^{-1}\mathrm{cMpc}$) correlation in Ly-$\alpha$ transmission flux using extended XQR-30 quasar spectra pose interesting challenges on the reionization end stages. In this work, we investigate the Ly-$\alpha$ forest dark-gap distribution (defined as regions with transmitted flux below 0.05) as another sensitive tracer of the IGM, using an efficient, large-volume ($\sim 1 ~\mathrm{Gpc}$) simulation framework. By constructing a suite of physically motivated model variants (i.e, varying the reionization redshift, IGM temperature, and ionizing-photon mean free path), we generate synthetic sightlines and compare their predicted cumulative distribution of dark gaps with that of observed spectra (at redshift intervals of $\Delta z=0.2$). We find that most of the models achieve qualitatively consistent agreement with the data. The scenario involving a slightly later reionization completion ($z\sim 5.4$) provides the closest match, while a short constant mean free path model is disfavored by the data at lower redshifts. These findings give qualitative support for the emerging scenario of reionization end extending to $z\le5.7$, although they can not rule out a slightly early reionization with enhanced post-ionization ultraviolet (UV) background fluctuations. A similar conclusion arises from the redshift distribution of long dark gap ($L\ge 30 ~h^{-1}\mathrm{cMpc}$) fraction. However, the model variants are still not able to reproduce the observed strong flux correlations at unusually large scales, which remains open for further investigations.