Himiko is one of the most luminous Lyμ emitters at z = 6.595. It has three star-forming clumps detected in the rest-frame UV, with a total SFR = 20 M o yr-1. We report the Atacama Large Millimeter/submillimeter Array (ALMA) detection of the [C ii]158 μm line emission in this Galaxy with a significance of 8σ. The total [C ii] luminosity (L [C ii] = 1.2 × 108 L o) is fully consistent with the local L [C ii]-SFR relation. The ALMA high-angular resolution reveals that the [C ii] emission is made of two distinct components. The brightest [C ii] clump is extended over 4 kpc and is located on the peak of the Lyμ nebula, which is spatially offset by 1 kpc relative to the brightest UV clump. The second [C ii] component is spatially unresolved (size <2 kpc) and coincident with one of the three UV clumps. While the latter component is consistent with the local L [C ii]-SFR relation, the other components are scattered above and below the local relation. We shortly discuss the possible origin of the [C ii] components and their relation with the star-forming clumps traced by the UV emission.

ALMA Detection of Extended [C II] Emission in Himiko at z = 6.6

Carniani S.
;
Maiolino R.;
2018

Abstract

Himiko is one of the most luminous Lyμ emitters at z = 6.595. It has three star-forming clumps detected in the rest-frame UV, with a total SFR = 20 M o yr-1. We report the Atacama Large Millimeter/submillimeter Array (ALMA) detection of the [C ii]158 μm line emission in this Galaxy with a significance of 8σ. The total [C ii] luminosity (L [C ii] = 1.2 × 108 L o) is fully consistent with the local L [C ii]-SFR relation. The ALMA high-angular resolution reveals that the [C ii] emission is made of two distinct components. The brightest [C ii] clump is extended over 4 kpc and is located on the peak of the Lyμ nebula, which is spatially offset by 1 kpc relative to the brightest UV clump. The second [C ii] component is spatially unresolved (size <2 kpc) and coincident with one of the three UV clumps. While the latter component is consistent with the local L [C ii]-SFR relation, the other components are scattered above and below the local relation. We shortly discuss the possible origin of the [C ii] components and their relation with the star-forming clumps traced by the UV emission.
Settore FIS/05 - Astronomia e Astrofisica
galaxies: evolution; galaxies: formation; galaxies: high-redshift; infrared: ISM
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11384/89540
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