2020MNRAS.499.5136C

ALMA observations have revealed that [C II] 158 µm line emission in high-z galaxies is ≃2-3 x more extended than the UV continuum emission. Here we explore whether surface brightness dimming (SBD) of the [C II] line is responsible for the reported [C II] deficit, and the large L_[O III]_/L[C II]_ luminosity ratio measured in early galaxies. We first analyse archival ALMA images of nine z > 6 galaxies observed in both [C II] and [O III]. After performing several uv-tapering experiments to optimize the identification of extended line emission, we detect [C II] emission in the whole sample, with an extent systematically larger than the [O III] emission. Next, we use interferometric simulations to study the effect of SBD on the line luminosity estimate. About 40 per cent of the extended [C II] component might be missed at an angular resolution of 0.8 arcsec, implying that L_[C II]_ is underestimated by a factor ≃2 in data at low (<7) signal-to-noise ratio. By combining these results, we conclude that L_[C II]_ of z > 6 galaxies lies, on average, slightly below the local L_[C II]_ - SFR relation (Δ^z=6–9 = -0.07 ± 0.3), but within the intrinsic dispersion of the relation. SBD correction also yields L_[O III]_/L[C II]_< 10, i.e. more in line with current hydrodynamical simulations.