TY - JOUR
T1 - The ALPINE-ALMA [C ii] Survey
T2 - Size of Individual Star-forming Galaxies at z = 4-6 and Their Extended Halo Structure
AU - Fujimoto, Seiji
AU - Silverman, John D.
AU - Bethermin, Matthieu
AU - Ginolfi, Michele
AU - Jones, Gareth C.
AU - Le F vre, Olivier
AU - Dessauges-Zavadsky, Miroslava
AU - Rujopakarn, Wiphu
AU - Faisst, Andreas L.
AU - Fudamoto, Yoshinobu
AU - Cassata, Paolo
AU - Morselli, Laura
AU - Maiolino, Roberto
AU - Schaerer, Daniel
AU - Capak, Peter
AU - Yan, Lin
AU - Vallini, Livia
AU - Toft, Sune
AU - Loiacono, Federica
AU - Zamorani, Gianni
AU - Talia, Margherita
AU - Narayanan, Desika
AU - Hathi, Nimish P.
AU - Lemaux, Brian C.
AU - Boquien, Médéric
AU - Amorin, Ricardo
AU - Ibar, Edo
AU - Koekemoer, Anton M.
AU - Méndez-Hernández, Hugo
AU - Bardelli, Sandro
AU - Vergani, Daniela
AU - Zucca, Elena
AU - Romano, Michael
AU - Cimatti, Andrea
N1 - Funding Information:
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).
Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved.
PY - 2020/9/1
Y1 - 2020/9/1
N2 - 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 () for individual galaxies and compare them with the rest-frame ultraviolet (UV) continuum () from Hubble Space Telescope images. The effective radius exceeds by factors of ∼2-3, and the ratio of 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.
AB - 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 () for individual galaxies and compare them with the rest-frame ultraviolet (UV) continuum () from Hubble Space Telescope images. The effective radius exceeds by factors of ∼2-3, and the ratio of 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.
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U2 - 10.3847/1538-4357/ab94b3
DO - 10.3847/1538-4357/ab94b3
M3 - Article
AN - SCOPUS:85091141667
SN - 0004-637X
VL - 900
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 1
ER -