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The ALPINE-ALMA [C II] survey. Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6

Le Fèvre, O. and Béthermin, M. and Faisst, A. and Jones, G. C. and Capak, P. and Cassata, P. and Silverman, J. D. and Schaerer, D. and Yan, L. and Amorin, R. and Bardelli, S. and Boquien, M. and Cimatti, A. and Dessauges-Zavadsky, M. and Giavalisco, M. and Hathi, N. P. and Fudamoto, Y. and Fujimoto, S. and Ginolfi, M. and Gruppioni, C. and Hemmati, S. and Ibar, E. and Koekemoer, A. and Khusanova, Y. and Lagache, G. and Lemaux, B. C. and Loiacono, F. and Maiolino, R. and Mancini, C. and Narayanan, D. and Morselli, L. and Méndez-Hernández, Hugo and Oesch, P. A. and Pozzi, F. and Romano, M. and Riechers, D. and Scoville, N. and Talia, M. and Tasca, L. A. M. and Thomas, R. and Toft, S. and Vallini, L. and Vergani, D. and Walter, F. and Zamorani, G. and Zucca, E. (2020) The ALPINE-ALMA [C II] survey. Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6. Astronomy and Astrophysics, 643 . Art. No. A1. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20201028-104133930

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Abstract

The ALMA-ALPINE [C II] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [C II]-158 μm line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 4 <  z <  6. We present the survey science goals, the observational strategy, and the sample selection of the 118 galaxies observed with ALMA, with an average beam minor axis of about 0.85″, or ∼5 kpc at the median redshift of the survey. The properties of the sample are described, including spectroscopic redshifts derived from the UV-rest frame, stellar masses, and star-formation rates obtained from a spectral energy distribution (SED) fitting. The observed properties derived from the ALMA data are presented and discussed in terms of the overall detection rate in [C II] and FIR continuum, with the observed signal-to-noise distribution. The sample is representative of the SFG population in the main sequence at these redshifts. The overall detection rate in [C II] is 64% for a signal-to-noise ratio (S/N) threshold larger than 3.5 corresponding to a 95% purity (40% detection rate for S/N > 5). Based on a visual inspection of the [C II] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4 <  z <  6, a key epoch in galaxy assembly, which is ideally suited for studies with future facilities, such as the James Webb Space Telescope (JWST) and the Extremely Large Telescopes (ELTs).


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201936965DOIArticle
https://arxiv.org/abs/1910.09517arXivDiscussion Paper
ORCID:
AuthorORCID
Le Fèvre, O.0000-0001-5891-2596
Béthermin, M.0000-0002-3915-2015
Faisst, A.0000-0002-9382-9832
Jones, G. C.0000-0002-0267-9024
Capak, P.0000-0003-3578-6843
Cassata, P.0000-0002-6716-4400
Silverman, J. D.0000-0002-0000-6977
Schaerer, D.0000-0001-7144-7182
Yan, L.0000-0003-1710-9339
Amorin, R.0000-0001-5758-1000
Bardelli, S.0000-0002-8900-0298
Boquien, M.0000-0003-0946-6176
Cimatti, A.0000-0002-4409-5633
Dessauges-Zavadsky, M.0000-0003-0348-2917
Giavalisco, M.0000-0002-7831-8751
Hathi, N. P.0000-0001-6145-5090
Fudamoto, Y.0000-0001-7440-8832
Fujimoto, S.0000-0001-7201-5066
Ginolfi, M.0000-0002-8231-821X
Gruppioni, C.0000-0002-5836-4056
Hemmati, S.0000-0003-2226-5395
Koekemoer, A.0000-0002-6610-2048
Khusanova, Y.0000-0002-7220-397X
Lagache, G.0000-0003-1492-2519
Lemaux, B. C.0000-0002-1428-7036
Loiacono, F.0000-0002-8858-6784
Maiolino, R.0000-0002-4985-3819
Mancini, C.0000-0002-4297-0561
Narayanan, D.0000-0002-7064-4309
Morselli, L.0000-0003-0753-2571
Méndez-Hernández, Hugo0000-0003-3057-9677
Oesch, P. A.0000-0001-5851-6649
Pozzi, F.0000-0002-7412-647X
Romano, M.0000-0002-9948-3916
Riechers, D.0000-0001-9585-1462
Scoville, N.0000-0002-0438-3323
Talia, M.0000-0003-4352-2063
Toft, S.0000-0003-3631-7176
Vallini, L.0000-0002-3258-3672
Vergani, D.0000-0003-0898-2216
Walter, F.0000-0003-4793-7880
Zamorani, G.0000-0002-2318-301X
Zucca, E.0000-0002-5845-8132
Additional Information:© O. Le Fèvre et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Received 21 October 2019; Accepted 4 June 2020; Published online 27 October 2020. This paper is based on data obtained with the ALMA Observatory, under the Large Program 2017.1.00428.L. ALMA is a partnership of 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 ESO, AUI/NRAO and NAOJ. This program receives funding from the CNRS national program Cosmology and Galaxies. AC, FP, MT, CG acknowledge the support from grant PRIN MIUR 2017. G.C.J. and R.M. acknowledge ERC Advanced Grant 695671 “QUENCH” and support by the Science and Technology Facilities Council (STFC). E.I. acknowledges partial support from FONDECYT through grant No 1171710. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. S.T. acknowledges support from the ERC Consolidator Grant funding scheme (project Context, grant No. 648179). LV acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie Grant agreement No. 746119. D.R. acknowledges support from the National Science Foundation under grant numbers AST-1614213 and AST-1910107 and from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. JDS was supported by the JSPS KAKENHI Grant Number JP18H04346, and the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. GL acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project CONCERTO, grant agreement No 788212) and from the Excellence Initiative of Aix-Marseille University-A*Midex, a French “Investissements d’Avenir” programme.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)UNSPECIFIED
European Research Council (ERC)695671
Science and Technology Facilities Council (STFC)UNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1171710
Danish National Research Foundation140
European Research Council (ERC)648179
Marie Curie Fellowship746119
NSFAST-1614213
NSFAST-1910107
Alexander von Humboldt FoundationUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP18H04346
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
European Research Council (ERC)788212
Aix-Marseille UniversityUNSPECIFIED
Investissements d’Avenir programUNSPECIFIED
Subject Keywords:galaxies: evolution – galaxies: star formation – galaxies: formation
Record Number:CaltechAUTHORS:20201028-104133930
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20201028-104133930
Official Citation:The ALPINE-ALMA [C II] survey - Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6. O. Le Fèvre, M. Béthermin, A. Faisst, G. C. Jones, P. Capak, P. Cassata, J. D. Silverman, D. Schaerer, L. Yan, R. Amorin, S. Bardelli, M. Boquien, A. Cimatti, M. Dessauges-Zavadsky, M. Giavalisco, N. P. Hathi, Y. Fudamoto, S. Fujimoto, M. Ginolfi, C. Gruppioni, S. Hemmati, E. Ibar, A. Koekemoer, Y. Khusanova, G. Lagache, B. C. Lemaux, F. Loiacono, R. Maiolino, C. Mancini, D. Narayanan, L. Morselli, Hugo Méndez-Hernàndez, P. A. Oesch, F. Pozzi, M. Romano, D. Riechers, N. Scoville, M. Talia, L. A. M. Tasca, R. Thomas, S. Toft, L. Vallini, D. Vergani, F. Walter, G. Zamorani and E. Zucca. A&A, 643 (2020) A1; DOI: https://doi.org/10.1051/0004-6361/201936965
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:106329
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:29 Oct 2020 18:21
Last Modified:29 Oct 2020 18:21

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