The Evolution of the Lyman-Alpha Luminosity Function During Reionization
arXiv:2101.01205 · doi:10.3847/1538-4357/ac1104
Abstract
The time frame in which hydrogen reionization occurred is highly uncertain, but can be constrained by observations of Lyman-alpha (Ly) emission from distant sources. Neutral hydrogen in the intergalactic medium (IGM) attenuates Ly~photons emitted by galaxies. As reionization progressed the IGM opacity decreased, increasing Ly~visibility. The galaxy Ly~luminosity function (LF) is thus a useful tool to constrain the timeline of reionization. In this work, we model the Ly~LF as a function of redshift, , and average IGM neutral hydrogen fraction, $\overline{x}_\textsc{hi}$. We combine the Ly~luminosity probability distribution obtained from inhomogeneous reionization simulations with a model for the UV LF to model the Ly~LF. As the neutral fraction increases, the average number density of Ly~emitting galaxies decreases, and are less luminous, though for $\overline{x}_\textsc{hi} \lesssim 0.4$ there is only a small decrease of the Ly~LF. We use our model to infer the IGM neutral fraction at from observed Ly~LFs. We conclude that there is a significant increase in the neutral fraction with increasing redshift: $\overline{x}_\textsc{hi}(z=6.6)=0.08^{+ 0.08}_{- 0.05}, \, \overline{x}_\textsc{hi}(z=7.0)=0.28 \pm 0.05$ and $\overline{x}_\textsc{hi}(z=7.3)=0.83^{+ 0.06}_{- 0.07}$. We predict trends in the Ly~luminosity density and Schechter parameters as a function of redshift and the neutral fraction. We find that the Ly~luminosity density decreases as the universe becomes more neutral. Furthermore, as the neutral fraction increases, the faint-end slope of the Ly~LF steepens, and the characteristic Ly~luminosity shifts to lower values, concluding that the evolving shape of the Ly~LF -- not just its integral -- is an important tool to study reionization.
arXiv comment20 pages, 10 figures, submitted to ApJ
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