Bursty or heavy? The surprise of bright Population III systems in the Reionization era

TL;DR

This paper explores the surprising brightness of Population III star systems observed by JWST during the Epoch of Reionization, proposing models with late formation in larger halos or bursty star formation to explain these findings.

Contribution

It introduces two novel models—late-time formation in massive halos and bursty star formation—to explain unexpectedly bright Pop III systems observed at high redshift.

Findings

Pop III stars may form in larger halos than previously thought.

Highly bursty star formation can account for bright Pop III sources.

Models suggest Pop III systems are heavier or more active than assumed.

Abstract

The nature of the first, so-called Population III (Pop III) stars has for long remained largely unconstrained. However, the James Webb Space Telescope (JWST) finally opened new concrete prospects for their detection during the Epoch of Reionization (EoR), notably providing promising observational constraints on the Pop III ultra-violet luminosity function (UVLF) at $z \approx 5.6 - 6.6$. These preliminary data hint towards an unexpected population of UV-bright Pop III sources, which challenges the prevailing view that Pop III star formation is confined to molecular-cooling mini-halos. Here we show that there are two families of models that can explain these surprising observations, either by allowing for late-time Pop III formation within massive, atomic-cooling halos (with halo masses up to $M^\mathrm{III}_\mathrm{up} \gtrsim 10^{10} \, \mathrm{M_\odot}$) or by invoking a highly bursty Pop III star-formation activity (with a stochasticity parameter $\sigma^\mathrm{III}_\mathrm{UV} \gtrsim 1.5$). In these scenarios, Pop III systems would have to be either heavier or burstier than usually assumed, underscoring the need to reconsider common assumptions about Pop III star-formation sites, and the potential implications of JWST candidates for current and future observations.