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What drives the [CII]/FIR deficit in submillimeter galaxies?

Published online by Cambridge University Press:  04 June 2020

Matus Rybak Open the ORCID record for Matus Rybak [Opens in a new window] ,
J. A. Hodge ,
G. Calistro Rivera  and
ALESS Collaboration
Matus Rybak
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CALeiden, the Netherlands email: mrybak@strw.leidenuniv.nl
J. A. Hodge
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CALeiden, the Netherlands email: mrybak@strw.leidenuniv.nl
G. Calistro Rivera
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CALeiden, the Netherlands email: mrybak@strw.leidenuniv.nl
ALESS Collaboration
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CALeiden, the Netherlands email: mrybak@strw.leidenuniv.nl
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Abstract

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Submillimeter galaxies at redshift z⩾1 show a pronounced [CII]/FIR deficit down to sub-kpc scales; however, the physical origin of this deficit remains poorly understood. We use resolved ALMA observations of the [CII], FIR and CO(3–2) emission in two z = 3 SMGs to distinguish between the different proposed scenarios; the thermal saturation of the [CII] emission is the most likely explanation.

Keywords

galaxies: high-redshiftgalaxies: ISMsubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S352: Uncovering Early Galaxy Evolution in the ALMA and JWST Era , June 2019 , pp. 293 - 294
Copyright
© International Astronomical Union 2020

References

Calistro-Rivera, G.et al. 2019, ApJ, 863, 5610.3847/1538-4357/aacffaCrossRefGoogle Scholar
Díaz-Santos, T.et al. 2017, ApJ, 846, 3210.3847/1538-4357/aa81d7CrossRefGoogle Scholar
Gullberg, B.et al. 2015, MNRAS, 449, 288310.1093/mnras/stv372CrossRefGoogle Scholar
Gullberg, B.et al. 2018, ApJ, 859, 1210.3847/1538-4357/aabe8cCrossRefGoogle Scholar
Kaufman, M. J.et al. 2008, ApJ, 644, 28310.1086/503596CrossRefGoogle Scholar
Lamarche, C.et al. 2018, ApJ, 867, 140CrossRefGoogle Scholar
Litke, K. C.et al. 2019, ApJ, 870, 8010.3847/1538-4357/aaf057CrossRefGoogle Scholar
Muñoz, J. A. & Oh, S. P. 2016, MNRAS, 463, 208510.1093/mnras/stw2102CrossRefGoogle Scholar
Pound, M. W. & Wolfire, M. G. 2008, ASPCS, 394, 654Google Scholar
Rybak, M.et al. 2019, ApJ, 876, 11210.3847/1538-4357/ab0e0fCrossRefGoogle Scholar
Smith, J. D.et al. 2017, ApJ, 834, 510.3847/1538-4357/834/1/5CrossRefGoogle Scholar
Wardlow, J.et al. 2017, ApJ, 837, 1210.3847/1538-4357/837/1/12CrossRefGoogle Scholar