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Journal Article

The [C II] emission as a molecular gas mass tracer in galaxies at low and high redshifts

MPS-Authors

Zanella,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Daddi,  E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Magdis,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Diaz Santos,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cormier,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Liu,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cibinel,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gobat,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dickinson,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sargent,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Popping,  G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Madden,  S. C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bethermin,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hughes,  T. M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Valentino,  F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rujopakarn,  W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pannella,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bournaud,  F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Walter,  F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Elbaz,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Coogan,  R. T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018MNRAS.481.1976Z
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Citation

Zanella, A., Daddi, E., Magdis, G., Diaz Santos, T., Cormier, D., Liu, D., et al. (2018). The [C II] emission as a molecular gas mass tracer in galaxies at low and high redshifts. Monthly Notices of the Royal Astronomical Society, 481, 1976-1999.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CA26-D
Abstract
We present ALMA Band 9 observations of the [C II]158 μm emission for a sample of 10 main-sequence galaxies at redshift z ̃ 2, with typical stellar masses (log M⋆/M☉ ̃ 10.0-10.9) and star formation rates (̃35-115 M☉ yr-1). Given the strong and well-understood evolution of the interstellar medium from the present to z = 2, we investigate the behaviour of the [C II] emission and empirically identify its primary driver. We detect [C II] from six galaxies (four secure and two tentative) and estimate ensemble averages including non-detections. The [C II]-to-infrared luminosity ratio ([C II]/LIR) of our sample is similar to that of local main- sequence galaxies (̃2 × 10-3), and ̃10 times higher than that of starbursts. The [C II] emission has an average spatial extent of 4-7 kpc, consistent with the optical size. Complementing our sample with literature data, we find that the [C II] luminosity correlates with galaxies' molecular gas mass, with a mean absolute deviation of 0.2 dex and without evident systematics: the [C II]-to-H2 conversion factor (α _[C II] ̃ 30 M☉/L☉) is largely independent of galaxies' depletion time, metallicity, and redshift. [C II] seems therefore a convenient tracer to estimate galaxies' molecular gas content regardless of their starburst or main-sequence nature, and extending to metal-poor galaxies at low and high redshifts. The dearth of [C II] emission reported for z > 6-7 galaxies might suggest either a high star formation efficiency or a small fraction of ultraviolet light from star formation reprocessed by dust.