# Fragmentation in Population III Galaxies formed through Ionizing Radiation

## TL;DR

This study investigates how ionizing radiation can delay the collapse of Population III star-forming halos, leading to larger stellar clusters with a small number of massive stars, but not enough to form direct collapse black holes.

## Contribution

It demonstrates through simulations that ionizing radiation can produce larger Population III clusters with limited fragmentation, expanding understanding of early star formation mechanisms.

## Key findings

- Higher ionizing flux delays collapse to larger masses.
- Clusters formed are larger than in minihalos but still faint for JWST detection.
- Fragmentation results in a few massive stars with high accretion rates.

## Abstract

Population III stars forming in minihalos tend to be relatively inefficient, with each minihalo hosting one or a small number of stars which are more massive than local stars but still challenging to observe directly at high redshift. Here we explore a possible mechanisms for the generation of larger clusters of such stars: a nearby ionizing source which ionizes a late forming halo, delaying its collapse until the halo is sufficiently large that the core can self-shield and suffer runaway collapse. We use simulations with a simple but accurate model for the radiative ionizing flux and confirm the basic predictions of previous work: higher ionizing fluxes can delay the collapse to lower redshifts and higher masses, up to an order of magnitude above the atomic cooling limit. In a limited number of runs we also examine the fragmentation of the cores at even higher resolution, using both simple estimates and sink particles to show that the number of fragments is generally small, at most a handful, and that the mass accretion rate on the fragments is of order $10^{-3}$ M$_\odot$ yr$^{-1}$. This rate is sufficiently high that the descent on the main sequence (and hence the suppression of accretion) is delayed until the stellar masses are of order $100-1000$ M$_\odot$, but not high enough to produce direct collapse black holes of mass $\sim 10^5$ M$_{\odot}$. The resulting clusters are larger than those produced in minihalos, but are still likely to fall short of being easily detectable in JWST blind fields.