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Galactic outflows in star-forming galaxies at z ∼ 6 studied with deep UV spectra and ALMA emission line

Published online by Cambridge University Press:  10 June 2020

Yuma Sugahara
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba277-8582, Japan email: sugayu@icrr.u-tokyo.ac.jp Department of Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo, 113-0033, Japan
Masami Ouchi
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba277-8582, Japan email: sugayu@icrr.u-tokyo.ac.jp Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba277-8583, Japan
Yuichi Harikane
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba277-8582, Japan email: sugayu@icrr.u-tokyo.ac.jp Department of Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo, 113-0033, Japan
Nicolas Bouché
Affiliation:
Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis-Laval, France
Peter D. Mitchell
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands
Jérémy Blaizot
Affiliation:
Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis-Laval, France
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Abstract

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We present a velocity of galactic outflows in star-forming galaxies at the highest redshift, z ∼ 6, so far studied with metal absorption lines. Absorption-line studies of galactic outflows need well-determined redshifts, but there are few strong emission lines in the observed-frame optical spectra of galaxies at high redshifts. In this work, we use the systemic redshifts determined by the ALMA [CII]158 μm emission lines. The sample consists of seven Lyman break galaxies at 5.1 < z < 5.7 whose Keck/DEIMOS and ALMA data are available in the archive. The outflow maximum velocity (νmax) is estimated by a fitting of line profiles to metal absorption lines in a composite spectrum. We find that νmax monotonically increases from z ∼ 0 to 6 and that νmax tightly correlates with the halo circular velocity estimated from the stellar mass.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

References

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