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JWST observations of galaxies at z 8 suggest that they are more luminous and clumpier than predicted by most models, prompting several proposals on the physics of star formation and feedback in the first galaxies. In this paper, we focus on the role of ultraviolet (UV) radiation in regulating star formation by performing a set of cosmological radiation hydrodynamics simulations of one galaxy at sub-pc resolution with different radiative feedback models. We find that the suppression of cooling by far UV (FUV) radiation (i. e. , H₂ dissociating radiation) from Pop II stars is the main physical process triggering the formation of compact and massive star clusters and is responsible for the bursty star formation observed in metal-poor galaxies at z 10. Indeed, artificially suppressing FUV radiation leads to a less intense continuous mode of star formation distributed into numerous, but low-mass open star clusters. Due to the intense FUV field, low-metallicity clouds remain warm (10⁴\, K) until they reach a relatively high density (10³\, cm^-3), before becoming self-shielded and transitioning to a colder (100\, K), partially molecular phase. As a result, star formation is delayed until the clouds accumulate enough mass to become gravitationally unstable. At this point, the clouds undergo rapid star formation converting gas into stars with high efficiency. We, therefore, observe exceptionally bright galaxies (ten times brighter than for continuous star formation) and subsequent quenched "dead" galaxies that did not form stars for tens of Myrs.
Sugimura et al. (Thu,) studied this question.