Obscured star-formation in bright z ~ 7 Lyman-break galaxies

Abstract

We present Atacama Large Millimeter/Submillimeter Array observations of the rest-frame far-infrared (FIR) dust continuum emission of six bright Lyman-break galaxies (LBGs) at $z\simeq 7$. One LBG is detected ($5.2\sigma$ at peak emission), while the others remain individually undetected at the $3\sigma$ level. The average FIR luminosity of the sample is found to be $L_{\mathrm{FIR}}\simeq 2\times 10^{11}{\mathrm{L}}_{\odot }$, corresponding to an obscured star-formation rate (SFR) that is comparable to that inferred from the unobscured UV emission. In comparison to the infrared excess (IRX$=L_{\mathrm{FIR}}/L_{\mathrm{UV}}$)-$\beta$ relation, our results are consistent with a Calzetti-like attenuation law (assuming a dust temperature of T = 40-50 K). We find a physical offset of 3 kpc between the dust continuum emission and the rest-frame UV light probed by Hubble Space Telescope imaging for galaxy ID65666 at $z=7.17_{-0.06}^{+0.09}$. The offset is suggestive of an inhomogeneous dust distribution, where 75% of the total star formation activity (SFR$\simeq 70{\mathrm{M}}_{\odot }/\mathrm{yr}$) of the galaxy is completely obscured. Our results provide direct evidence that dust obscuration plays a key role in shaping the bright-end of the observed rest-frame UV luminosity function at $z\simeq 7$, in agreement with cosmological galaxy formation simulations. The existence of a heavily-obscured component of galaxy ID65666 indicates that dusty star-forming regions, or even entire galaxies, that are "UV-dark" are significant even in the $z\simeq 7$ galaxy population.

arXiv comment15 pages, 8 figures, 3 tables. Updated to match MNRAS accepted version

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