http://arxiv.org/abs/2208.08243
Cosmic dust is an essential component shaping both the evolution of galaxies and their observational signatures. How quickly dust builds up in the early Universe remains an open question that requires deep observations at (sub-)millimeter wavelengths to resolve. Here we use Atacama Large Millimeter Array observations of 45 galaxies from the Reionization Era Bright Emission Line Survey (REBELS) and its pilot programs, designed to target [CII] and dust emission in UV-selected galaxies at $z\sim7$, to investigate the dust content of high-redshift galaxies through a stacking analysis. We find that the typical fraction of obscured star formation $f_\mathrm{obs} = \mathrm{SFR}\mathrm{IR} / \mathrm{SFR}\mathrm{UV + IR}$ depends on stellar mass, similar to what is observed at lower redshift, and ranges from $f_\mathrm{obs} \approx 0.3 – 0.6$ for galaxies with $\log_{10}\left(M_\star / M_\odot\right) = 9.4 – 10.4$. We further adopt the $z\sim7$ stellar mass function from the literature to extract the cosmic star formation rate density from the REBELS survey. Our results suggest only a relatively modest decrease in the cosmic star formation rate density from $z\gtrsim3$ onward, with dust-obscured star formation still contributing $\sim30-50\%$ at $z\sim7$. While we extensively discuss potential caveats, our analysis suggests that dust-obscured star formation at high redshift may be more important than previously expected.
H. Algera, H. Inami, P. Oesch, et. al.
Thu, 18 Aug 22
33/45
Comments: 16 pages, 7 figures, submitted to MNRAS
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