The ALMA REBELS Survey: the dust content of $z\sim 7$ Lyman Break Galaxies

Abstract

We include a fully coupled treatment of metal and dust enrichment into the Delphi semi-analytic model of galaxy formation to explain the dust content of 13 Lyman Break Galaxies (LBGs) detected by the Atacama Large millimetre Array (ALMA) REBELS Large Program at $z\simeq 7$. We find that the galaxy dust mass, $M_d$, is regulated by the combination of SNII dust production, astration, shock destruction, and ejection in outflows; grain growth (with a standard timescale ${\tau }_0=30$ Myr) plays a negligible role. The model predicts a dust-to-stellar mass ratio of $\sim 0.07-0.1\%$ and a UV-to-total star formation rate relation such that $log({\psi }_{\mathrm{UV}})=-0.05[log(\psi ){]}^2+0.86log(\psi )-0.05$ (implying that 55-80\% of the star formation is obscured) for REBELS galaxies with stellar mass $M_{\ast }=10^{9-10}{M}_{\odot }$. This relation reconciles the intrinsic UV luminosity of LBGs with their observed luminosity function at $z=7$. However, 2 out of the 13 systems show dust-to-stellar mass ratios ($\sim 0.94-1.1\%$) that are up to $18\times$ larger than expected from the fiducial relation. Due to the physical coupling between dust and metal enrichment, even decreasing ${\tau }_0$ to very low values (0.3 Myr) only increases the dust-to-stellar mass ratio by a factor $\sim 2$. Given that grain growth is not a viable explanation for such high observed ratios of the dust-to-stellar mass, we propose alternative solutions.

arXiv commentAccepted to MNRAS

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