Feedback-regulated star formation and escape of LyC photons from mini-haloes during reionisation

Abstract

Reionisation in the early Universe is likely driven by dwarf galaxies. Using cosmological radiation-hydrodynamic simulations, we study star formation and the escape of Lyman continuum (LyC) photons from mini-haloes with $M_{\mathrm{halo}}\le 10^8{M}_{\odot }$. Our simulations include a new thermo-turbulent star formation model, non-equilibrium chemistry, and relevant stellar feedback processes (photoionisation by young massive stars, radiation pressure, and mechanical supernova explosions). We find that feedback reduces star formation very efficiently in mini-haloes, resulting in the stellar mass consistent with the slope and normalisation reported in Kimm \& Cen and the empirical stellar mass-to-halo mass relation derived in the local Universe. Because star formation is stochastic and dominated by a few gas clumps, the escape fraction in mini-haloes is generally determined by radiation feedback (heating due to photo-ionisation), rather than supernova explosions. We also find that the photon number-weighted mean escape fraction in mini-haloes is higher ($\sim 20$-$40\%$) than that in atomic-cooling haloes, although the instantaneous fraction in individual haloes varies significantly. The escape fraction from Pop III stars is found to be significant ($\ge 10\%$) only when the mass is greater than $\sim$100\,\msun. Based on simple analytic calculations, we show that LyC photons from mini-haloes are, despite their high escape fractions, of minor importance for reionisation due to inefficient star formation. We confirm previous claims that stars in atomic-cooling haloes with masses $10^8{M}_{\odot }\le M_{\mathrm{halo}}\le 10^{11}{M}_{\odot }$ are likely to be the most important source of reionisation.

22 pages, 15 figures, Accepted for the publication in MNRAS

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