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We present deep high resolution (0.03", 200pc) ALMA Band 7 observationscovering the dust continuum and [CII] $\lambda157.7\mu$m emission in four$z\sim4.4-4.8$ sub-millimeter galaxies (SMGs) selected from the ALESS andAS2UDS surveys. The data show that the rest-frame 160$\mu$m (observed 345 GHz)dust emission is consistent with smooth morphologies on kpc scales for three ofthe sources. One source, UDS47.0, displays apparent substructure but this isalso consistent with a smooth morphology, as indicated by simulations showingthat smooth exponential disks can appear clumpy when observed at high angularresolution (0.03") and depth of these observations ($\sigma_{345\text{GHz}}\sim27-47\mu$Jy beam$^{-1}$). The four SMGs are bright [CII] emitters, and weextract [CII] spectra from the high resolution data, and recover $\sim20-100$%of the [CII] flux and $\sim40-80$% of the dust continuum emission, compared tothe previous lower resolution observations. When tapered to 0.2" resolution ourmaps recover $\sim80-100$% of the continuum emission, indicating that $\sim60$%of the emission is resolved out on $\sim200$pc scales. We find that the [CII]emission in high-redshift galaxies is more spatially extended than therest-frame 160$\mu$m dust continuum by a factor of $1.6\pm0.4$. By consideringthe $L_{\text{[CII]}}$/$L_{\text{FIR}}$ ratio as a function of thestar-formation rate surface density ($\Sigma_{\text{SFR}}$) we revisit the[CII] deficit, and suggest that the decline in the$L_{\text{[CII]}}$/$L_{\text{FIR}}$ ratio as a function of$\Sigma_{\text{SFR}}$ is consistent with local processes. We also explore thephysical drivers that may be responsible for these trends and can give rise tothe properties found in the densest regions of SMGs.

astrophysical journal/the astrophysical journal

The dust and [CII] morphologies of redshift ~4.5 sub-millimeter galaxies  at ~200pc resolution: The absence of large clumps in the interstellar medium  of high-redshift galaxies