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Published September 1, 2020 | Submitted + Published
Journal Article Open

The ALPINE–ALMA [C ii] Survey: Size of Individual Star-forming Galaxies at z = 4–6 and Their Extended Halo Structure

Abstract

We present the physical extent of [C ii] 158 μm line-emitting gas from 46 star-forming galaxies at z = 4–6 from the ALMA Large Program to INvestigate C ii at Early Times (ALPINE). Using exponential profile fits, we measure the effective radius of the [C ii] line (r_(e,C ii) for individual galaxies and compare them with the rest-frame ultraviolet (UV) continuum r_(e,UV) from Hubble Space Telescope images. The effective radius r_(e,C ii) exceeds r_(e,UV) by factors of ~2–3, and the ratio of r_(e,C ii)/r_(e,UV) increases as a function of M_(star). We do not find strong evidence that the [C ii] line, rest-frame UV, and far-infrared (FIR) continuum are always displaced over ≃1 kpc scale from each other. We identify 30% of isolated ALPINE sources as having an extended [C ii] component over 10 kpc scales detected at 4.1σ–10.9σ beyond the size of rest-frame UV and FIR continuum. One object has tentative rotating features up to ~10 kpc, where the 3D model fit shows the rotating [C ii]-gas disk spread over 4 times larger than the rest-frame UV-emitting region. Galaxies with the extended [C ii] line structure have high star formation rate, high stellar mass (M_(star)), low Lyα equivalent width, and more blueshifted (redshifted) rest-frame UV metal absorption (Lyα line), as compared to galaxies without such extended [C ii] structures. Although we cannot rule out the possibility that a selection bias toward luminous objects may be responsible for such trends, the star-formation-driven outflow also explains all these trends. Deeper observations are essential to test whether the extended [C ii] line structures are ubiquitous to high-z star-forming galaxies.

Additional Information

© 2020 The American Astronomical Society. Received 2020 February 27; revised 2020 May 16; accepted 2020 May 18; published 2020 August 27. This paper is dedicated to the memory of Olivier Le Fèvre, PI of the ALPINE survey. We thank Tanio Díaz-Santos, Andrea Ferrara, Simona Gallerani, Akio Inoue, Sinclaire Manning, Hiroshi Nagai, Kentaro Nagamine, Kimihiko Nakajima, Masami Ouchi, Takatoshi Shibuya, and Francesco Valentino (in alphabetical order) for useful comments and suggestions. This paper makes use of the ALMA data: ADS/JAO. ALMA #2017.1.00428.L. ALMA is a partnership of the ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ. This work is based on observations and archival data made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, along with archival data from the NASA/ESA Hubble Space Telescope. This research also made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work is based in part on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data center, Laboratoire d'Astrophysique de Marseille, France. This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Furthermore, this work is based on data from the W. M. Keck Observatory and the Canada–France–Hawaii Telescope, as well as collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at the National Astronomical Observatory of Japan. Finally, we would also like to recognize the contributions from all of the members of the COSMOS Team who helped in obtaining and reducing the large amount of multiwavelength data that are now publicly available through IRSA at http://irsa.ipac.caltech.edu/Missions/cosmos.html. This study is supported by the NAOJ ALMA Scientific Research grant No. 2016-01A. S.F. acknowledges support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. J.D.S. was supported by the JSPS KAKENHI grant No. JP18H04346 and the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. E.I. acknowledges partial support from FONDECYT through grant No. 1171710. A.C., C.G., F.L., F.P., and M.T. acknowledge the support from grant PRINMIUR 2017-20173ML3WW_001. L.V. acknowledges funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 746119. G.C.J. and R.M. acknowledge ERC Advanced Grant 695671 "QUENCH" and support by the Science and Technology Facilities Council (STFC).

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Submitted - 2003.00013.pdf

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Created:
August 22, 2023
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