Gullberg, B. and Swinbank, A. M. and Smail, I. and Biggs, A. D. and Bertoldi, F. and De Breuck, C. and Chapman, S. C. and Chen, C.-C. and Cooke, E. A. and Coppin, K. E. K. and Cox, P. and Dannerbauer, H. and Dunlop, J. S. and Edge, A. C. and Farrah, D. and Geach, J. E. and Greve, T. R. and Hodge, J. and Ibar, E. and Ivison, R. J. and Karim, A. and Schinnerer, E. and Scott, D. and Simpson, J. M. and Stach, S. M. and Thomson, A. P. and van der Werf, P. and Walter, F. and Wardlow, J. L. and Weiss, A. (2018) The Dust and [C II] Morphologies of Redshift ˜4.5 Sub-millimeter Galaxies at ˜200 pc Resolution : The Absence of Large Clumps in the Interstellar Medium at High-redshift. The Astrophysical Journal, 859 (1): 12. ISSN 0004-637X
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Abstract
We present deep, high-resolution (0.″03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C II] λ157.7 μm emission in four z ˜ 4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 μm (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology—as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0.″03) and depth of these observations ({σ }345{GHz}˜ 27{--}47 μJy beam-1). The four SMGs are bright [C II] emitters. We extract [C II] spectra from the high-resolution data, and recover ˜20%-100% of the [C II] flux and ˜40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0.″2 resolution, our maps recover ˜80%-100% of the continuum emission, indicating that ˜60% of the emission is resolved out on ˜200 pc scales. We find that the [C II] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 μm dust continuum by a factor of 1.6 ± 0.4. By considering the {L}[{{C}{{II}}]}/{L}FIR} ratio as a function of the star formation rate surface density ({{{Σ }}}SFR}), we revisit the [C II] deficit and suggest that the decline in the {L}[{{C}{{II}}]}/{L}FIR} ratio as a function of {{{Σ }}}SFR} is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.