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The ALPINE-ALMA [C II] Survey: [C II] 158 micron Emission Line Luminosity Functions at z ∼ 4−6

Yan, Lin and Sajina, A. and Loiacono, F. and Lagache, G. and Béthermin, M. and Faisst, A. and Ginolfi, M. and Le Fèvre, O. and Gruppioni, C. and Capak, P. L. and Cassata, P. and Schaerer, D. and Silverman, J. D. and Bardelli, S. and Dessauges-Zavadsky, M. and Cimatti, A. and Hathi, N. P. and Lemaux, B. C. and Ibar, E. and Jones, G. C. and Koekemoer, A. M. and Oesch, P. A. and Talia, M. and Pozzi, F. and Riechers, D. A. and Tasca, L. A. and Toft, S. and Vallini, L. and Vergani, D. and Zamorani, G. and Zucca, E. (2020) The ALPINE-ALMA [C II] Survey: [C II] 158 micron Emission Line Luminosity Functions at z ∼ 4−6. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20200824-123559194

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Abstract

We present the [CII]158μm line luminosity functions (LFs) at z ∼ 4−6 using the ALMA observations of 118 sources, which are selected to have UV luminosity M_(1500A) < −20.2 and optical spectroscopic redshifts in COSMOS and ECDF-S. Of the 118 targets, 75 have significant [C II] detections and 43 are upper limits. With this UV-selected sample, we set stringent lower bounds to the volume density of [C II] emitters at z ∼ 4−6. Our derived LFs are consistent with the z ∼ 0 [C II] LF at ≤ 10⁹ L_⊙, but show a hint of an excess of [C II] emitters at the luminous end (>10⁹ L_⊙) compared to z∼0. This excess is consistent with a potential population of [C II]-bright UV-faint sources that are largely excluded from the ALPINE target selection. To further constrain such sources, in a companion analysis, Loiacono et al. (2020) estimate the [C II] LF based on serendipitous [C II] sources in the ALPINE maps. Their resulting single data point is consistent with the excess we observe at high-L. Combined, these studies suggest possible redshift evolution in the [C II] LFs at high luminosity between z ∼ 5 and 0. This conclusion is further supported by the inferred [C II] LFs from the far-IR and CO LFs at z ∼ 4−6. Integrating our estimate on the best-fit [C II] LF, we set a constraint on molecular gas mass density at z ∼ 4−6, with ρ_(mol) ∼ (2−7)×10⁷ M_⊙ Mpc⁻³. This is broadly consistent with previous studies, although the uncertainties span more than an order of magnitude. Finally, we find that available model predictions tend to underestimate the number densities of [C II] emitters at z ∼ 5.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
https://arxiv.org/abs/2006.04835arXivDiscussion Paper
ORCID:
AuthorORCID
Yan, Lin0000-0003-1710-9339
Sajina, A.0000-0002-1917-1200
Loiacono, F.0000-0002-8858-6784
Lagache, G.0000-0003-1492-2519
Béthermin, M.0000-0002-3915-2015
Faisst, A.0000-0002-9382-9832
Ginolfi, M.0000-0002-8231-821X
Le Fèvre, O.0000-0001-5891-2596
Gruppioni, C.0000-0002-5836-4056
Capak, P. L.0000-0003-3578-6843
Cassata, P.0000-0002-6716-4400
Schaerer, D.0000-0001-7144-7182
Silverman, J. D.0000-0002-0000-6977
Bardelli, S.0000-0002-8900-0298
Dessauges-Zavadsky, M.0000-0003-0348-2917
Cimatti, A.0000-0002-4409-5633
Hathi, N. P.0000-0001-6145-5090
Lemaux, B. C.0000-0002-1428-7036
Jones, G. C.0000-0002-0267-9024
Koekemoer, A. M.0000-0002-6610-2048
Oesch, P. A.0000-0001-5851-6649
Talia, M.0000-0003-4352-2063
Pozzi, F.0000-0002-7412-647X
Riechers, D. A.0000-0001-9585-1462
Toft, S.0000-0003-3631-7176
Vallini, L.0000-0002-3258-3672
Zamorani, G.0000-0002-2318-301X
Zucca, E.0000-0002-5845-8132
Additional Information:We thank Liu, Daizhong from Max-Planck- Institut für Astronomie for sending us their results in electronic form. 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. GL acknowledges support from the European Research Council (ERC) under the European Unions 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 dAvenir programme. AC, CG, FL, FP and MT acknowledge the support from grant PRIN MIUR 2017 - 20173ML3WW 001. ST acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant number: 648179). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. Our research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013; Price-Whelan et al. 2018). LV acknowledges funding from the European Unions Horizon 2020 research and innovation program under the Marie Sklodowska- Curie Grant agreement No. 746119. G.C.J. acknowledges ERC Advanced Grant 695671 “QUENCH" and support by the Science and Technology Facilities Council (STFC).
Funders:
Funding AgencyGrant Number
European Research Council (ERC)788212
Aix-Marseille UniversityUNSPECIFIED
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)20173ML3WW 001
European Research Council (ERC)648179
Danish National Research Foundation140
Marie Curie Fellowship746119
European Research Council (ERC)695671
Science and Technology Facilities Council (STFC)UNSPECIFIED
Record Number:CaltechAUTHORS:20200824-123559194
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200824-123559194
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105074
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:24 Aug 2020 20:11
Last Modified:24 Aug 2020 20:11

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