# Fully Coupled Simulation of Cosmic Reionization. III. Stochastic Early Reionization by the Smallest Galaxies

## TL;DR

This paper presents a novel simulation including small, chemically enriched halos that significantly influence early reionization, revealing a stochastic phase driven by intermittent star formation before larger halos dominate.

## Contribution

It introduces a fully-coupled radiation hydrodynamic simulation with inline halo finding and a PDF-based ionizing flux assignment, modeling the impact of small galaxies on reionization.

## Key findings

- Reionization begins earlier with small halos included.
- Early reionization phase is stochastic with small H II regions forming and recombining.
- Reionization completes around redshift 10 dominated by larger halos.

## Abstract

Previously we identified a new class of early galaxy that we estimate contributes up to 30\% of the ionizing photons responsible for reionization. These are low mass halos in the range $M_h =10^{6.5}-10^{8} M_{\odot}$ that have been chemically enriched by supernova ejecta from prior Pop III star formation. Despite their low star formation rates, these Metal Cooling halos (MCs) are significant sources of ionizing radiation, especially at the onset of reionization, due to their high number density and ionizing escape fractions. Here we present a fully-coupled radiation hydrodynamic simulation of reionization that includes these MCs as well the more massive hydrogen atomic line cooling halos. Our method is novel: we perform halo finding inline with the radiation hydrodynamical simulation, and assign escaping ionizing fluxes to halos using a probability distribution function (PDF) measured from the galaxy-resolving Renaissance Simulations. The PDF captures the mass dependence of the ionizing escape fraction as well as the probability that a halo is actively forming stars. With MCs, reionization starts earlier than if only halos of $10^8 M_{\odot}$ and above are included, however the redshift when reionization completes is only marginally affected as this is driven by more massive galaxies. Because star formation is intermittent in MCs, the earliest phase of reionization exhibits a stochastic nature, with small H II regions forming and recombining. Only later, once halos of mass $\sim 10^9 M_{\odot}$ and above begin to dominate the ionizing emissivity, does reionization proceed smoothly in the usual manner deduced from previous studies. This occurs at $z\approx 10$ in our simulation.