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Population III stars forming in minihalos tend to be relatively inefficient,with each minihalo hosting one or a small number of stars which are moremassive than local stars but still challenging to observe directly at highredshift. Here we explore a possible mechanisms for the generation of largerclusters of such stars: a nearby ionizing source which ionizes a late forminghalo, delaying its collapse until the halo is sufficiently large that the corecan self-shield and suffer runaway collapse. We use simulations with a simplebut accurate model for the radiative ionizing flux and confirm the basicpredictions of previous work: higher ionizing fluxes can delay the collapse tolower redshifts and higher masses, up to an order of magnitude above the atomiccooling limit. In a limited number of runs we also examine the fragmentation ofthe cores at even higher resolution, using both simple estimates and sinkparticles to show that the number of fragments is generally small, at most ahandful, 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 descenton the main sequence (and hence the suppression of accretion) is delayed untilthe stellar masses are of order $100-1000$ M$_\odot$, but not high enough toproduce direct collapse black holes of mass $\sim 10^5$ M$_{\odot}$. Theresulting clusters are larger than those produced in minihalos, but are stilllikely to fall short of being easily detectable in JWST blind fields.

Fragmentation in Population III Galaxies formed through Ionizing Radiation