Gullberg, B. and Swinbank, A. M. and Smail, I. and Biggs, A. D. and Bertoldi, F. and Breuck, C. De 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.', Astrophysical journal., 859 (1). p. 12.
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 (s345 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 /LFIR ratio as a function of the star formation rate surface density (SSFR), we revisit the [C II] deficit and suggest that the decline in the L[ ] C II /LFIR ratio as a function of SSFR 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.
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|Publisher Web site:||https://doi.org/10.3847/1538-4357/aabe8c|
|Publisher statement:||© 2018. The American Astronomical Society. All rights reserved.|
|Date accepted:||09 April 2018|
|Date deposited:||08 June 2018|
|Date of first online publication:||17 May 2018|
|Date first made open access:||08 June 2018|
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