ALMA observations have revealed that [C II] 158 μm line emission in high-z galaxies is ≈2–3 × 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[OIII]/L[CII] 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[CII] is underestimated by a factor ≈2 in data at low (<7) signal-to-noise ratio. By combining these results, we conclude that L[CII] of z > 6 galaxies lies, on average, slightly below the local L[CII]−SFR relation (Δz = 6–9 = −0.07 ± 0.3), but within the intrinsic dispersion of the relation. SBD correction also yields L[OIII]/L[CII]<10, i.e. more in line with current hydrodynamical simulations.
Missing [C ii] emission from early galaxies
A Lupi;
2020-01-01
Abstract
ALMA observations have revealed that [C II] 158 μm line emission in high-z galaxies is ≈2–3 × 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[OIII]/L[CII] 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[CII] is underestimated by a factor ≈2 in data at low (<7) signal-to-noise ratio. By combining these results, we conclude that L[CII] of z > 6 galaxies lies, on average, slightly below the local L[CII]−SFR relation (Δz = 6–9 = −0.07 ± 0.3), but within the intrinsic dispersion of the relation. SBD correction also yields L[OIII]/L[CII]<10, i.e. more in line with current hydrodynamical simulations.
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