Quantifying Lyman-$\alpha$ emissions from reionization fronts

TL;DR

This paper quantifies the Ly$ ext{a}$ emission from intergalactic ionization fronts during reionization using high-resolution simulations, providing a model to predict emission based on I-front speed and spectral properties.

Contribution

It introduces a parameterization of Ly$ ext{a}$ emission efficiency from I-fronts, enabling sub-grid modeling in reionization simulations and aiding observational efforts.

Findings

Ly$ ext{a}$ production efficiency depends mainly on I-front speed and spectral index.

Density fluctuations cause scatter but do not significantly increase mean efficiency.

Maximum Ly$ ext{a}$ flux occurs with high incident flux, hard spectrum, and slow I-fronts.

Abstract

During reionization, intergalactic ionization fronts (I-fronts) are sources of Ly$\alpha$ line radiation produced by collisional excitation of hydrogen atoms within the fronts. In principle, detecting this emission could provide direct evidence for a reionizing intergalactic medium (IGM). In this paper, we use a suite of high-resolution one-dimensional radiative transfer simulations run on cosmological density fields to quantify the parameter space of I-front Ly$\alpha$ emission. We find that the Ly$\alpha$ production efficiency -- the ratio of emitted Ly$\alpha$ flux to incident ionizing flux driving the front -- depends mainly on the I-front speed and the spectral index of the ionizing radiation. IGM density fluctuations on scales smaller than the typical I-front width produce scatter in the efficiency, but they do not significantly boost its mean value. The Ly$\alpha$ flux emitted by an I-front is largest if 3 conditions are met simultaneously: (1) the incident ionizing flux is large; (2) the incident spectrum is hard, consisting of more energetic photons; (3) the I-front is traveling through a cosmological over-density, which causes it to propagate more slowly. We present a convenient parameterization of the efficiency in terms of I-front speed and incident spectral index. We make these results publicly available as an interpolation table and we provide a simple fitting function for a representative ionizing background spectrum. Our results can be applied as a sub-grid model for I-front Ly$\alpha$ emissions in reionization simulations with spatial and/or temporal resolutions too coarse to resolve I-front structure. In a companion paper, we use our results to explore the possibility of directly imaging Ly$\alpha$ emission around neutral islands during the last phases of reionization.