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The ALPINE–ALMA [C II] survey. Luminosity function of serendipitous [C II] line emitters at z ∼ 5

Loiacono, Federica and Decarli, Roberto and Gruppioni, Carlotta and Talia, Margherita and Cimatti, Andrea and Zamorani, Gianni and Pozzi, Francesca and Yan, Lin and Lemaux, Brian C. and Riechers, Dominik A. and Le Fèvre, Olivier and Béthermin, Matthieu and Capak, Peter and Cassata, Paolo and Faisst, Andreas and Schaerer, Daniel and Silverman, John D. and Bardelli, Sandro and Boquien, Médéric and Burkutean, Sandra and Dessauges-Zavadsky, Miroslava and Fudamoto, Yoshinobu and Fujimoto, Seiji and Ginolfi, Michele and Hathi, Nimish P. and Jones, Gareth C. and Khusanova, Yana and Koekemoer, Anton M. and Lagache, Guilaine and Lubin, Lori M. and Massardi, Marcella and Oesch, Pascal and Romano, Michael and Vallini, Livia and Vergani, Daniela and Zucca, Elena (2021) The ALPINE–ALMA [C II] survey. Luminosity function of serendipitous [C II] line emitters at z ∼ 5. Astronomy and Astrophysics, 646 . Art. No. A76. ISSN 0004-6361.

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We present the first [C II] 158 μm luminosity function (LF) at z ∼ 5 from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). A study of the 118 ALPINE pointings revealed several serendipitous lines. Based on their fidelity, we selected 14 lines for the final catalog. According to the redshift of their counterparts, we identified eight out of 14 detections as [C II] lines at z ∼ 5, along with two as CO transitions at lower redshifts. The remaining four lines have an elusive identification in the available catalogs and we considered them as [C II] candidates. We used the eight confirmed [C II] and the four [C II] candidates to build one of the first [C II] LFs at z ∼ 5. We found that 11 out of these 12 sources have a redshift very similar to that of the ALPINE target in the same pointing, suggesting the presence of overdensities around the targets. Therefore, we split the sample in two (a “clustered” and “field” subsample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the [C II] LF between z ∼ 5 and z ∼ 0. By converting the [C II] luminosity to the star-formation rate, we evaluated the cosmic star-formation rate density (SFRD) at z ∼ 5. The clustered sample results in a SFRD ∼10 times higher than previous measurements from UV–selected galaxies. On the other hand, from the field sample (likely representing the average galaxy population), we derived a SFRD ∼1.6 higher compared to current estimates from UV surveys but compatible within the errors. Because of the large uncertainties, observations of larger samples will be necessary to better constrain the SFRD at z ∼ 5. This study represents one of the first efforts aimed at characterizing the demography of [C II] emitters at z ∼ 5 using a mm selection of galaxies.

Item Type:Article
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URLURL TypeDescription Paper
Loiacono, Federica0000-0002-8858-6784
Decarli, Roberto0000-0002-2662-8803
Talia, Margherita0000-0003-4352-2063
Cimatti, Andrea0000-0002-4409-5633
Zamorani, Gianni0000-0002-2318-301X
Pozzi, Francesca0000-0002-7412-647X
Yan, Lin0000-0003-1710-9339
Lemaux, Brian C.0000-0002-1428-7036
Riechers, Dominik A.0000-0001-9585-1462
Le Fèvre, Olivier0000-0001-5891-2596
Béthermin, Matthieu0000-0002-3915-2015
Capak, Peter0000-0003-3578-6843
Cassata, Paolo0000-0002-6716-4400
Faisst, Andreas0000-0002-9382-9832
Schaerer, Daniel0000-0001-7144-7182
Silverman, John D.0000-0002-0000-6977
Bardelli, Sandro0000-0002-8900-0298
Boquien, Médéric0000-0003-0946-6176
Dessauges-Zavadsky, Miroslava0000-0003-0348-2917
Fudamoto, Yoshinobu0000-0001-7440-8832
Fujimoto, Seiji0000-0001-7201-5066
Ginolfi, Michele0000-0002-9122-1700
Hathi, Nimish P.0000-0001-6145-5090
Jones, Gareth C.0000-0002-0267-9024
Koekemoer, Anton M.0000-0002-6610-2048
Lagache, Guilaine0000-0003-1492-2519
Lubin, Lori M.0000-0003-4249-5315
Oesch, Pascal0000-0001-5851-6649
Romano, Michael0000-0002-9948-3916
Vallini, Livia0000-0002-3258-3672
Vergani, Daniela0000-0003-0898-2216
Zucca, Elena0000-0002-5845-8132
Additional Information:© 2021 ESO. Article published by EDP Sciences. Received 8 June 2020; Accepted 3 November 2020; Published online 10 February 2021. This paper is dedicated to the memory of Olivier Le Févre, PI of the ALPINE survey. This paper is based on data obtained with the ALMA Observatory, under 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. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This program is supported by the national program Cosmology and Galaxies from the CNRS in France. Some of the material presented in this paper is based upon work supported by the National Science Foundation under Grant No. 1908422. Some of the spectrographic data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank the indigenous Hawaiian community for allowing us to be guests on their sacred mountain, a privilege without which this work would not have been possible. We are most fortunate to be able to conduct observations from this site. F.L., C.G., A.C., F.P., and M.T. acknowledge the support from the grant PRIN MIUR 2017. 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. G.C.J. acknowledges ERC Advanced Grant 695671 “QUENCH” and support by the Science and Technology Facilities Council (STFC). 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)
Funding AgencyGrant Number
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)UNSPECIFIED
Alexander von Humboldt FoundationUNSPECIFIED
European Research Council (ERC)695671
Science and Technology Facilities Council (STFC)UNSPECIFIED
European Research Council (ERC)788212
Aix-Marseille UniversityUNSPECIFIED
Subject Keywords:galaxies: evolution – galaxies: ISM – galaxies: high-redshift – galaxies: luminosity function, mass function – submillimeter: galaxies
Record Number:CaltechAUTHORS:20210210-124713447
Persistent URL:
Official Citation:The ALPINE–ALMA [C II] survey - Luminosity function of serendipitous [C II] line emitters at z ∼ 5. Federica Loiacono, Roberto Decarli, Carlotta Gruppioni, Margherita Talia, Andrea Cimatti, Gianni Zamorani, Francesca Pozzi, Lin Yan, Brian C. Lemaux, Dominik A. Riechers, Olivier Le Fèvre, Matthieu Bèthermin, Peter Capak, Paolo Cassata, Andreas Faisst, Daniel Schaerer, John D. Silverman, Sandro Bardelli, Médéric Boquien, Sandra Burkutean, Miroslava Dessauges-Zavadsky, Yoshinobu Fudamoto, Seiji Fujimoto, Michele Ginolfi, Nimish P. Hathi, Gareth C. Jones, Yana Khusanova, Anton M. Koekemoer, Guilaine Lagache, Lori M. Lubin, Marcella Massardi, Pascal Oesch, Michael Romano, Livia Vallini, Daniela Vergani and Elena Zucca. A&A, 646 (2021) A76; DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:107990
Deposited By: Tony Diaz
Deposited On:10 Feb 2021 22:22
Last Modified:10 Feb 2021 22:22

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