The ALMA REBELS Survey: the first infrared luminosity function measurement at z  ∼ 7

Author:

Barrufet L1ORCID,Oesch P A12ORCID,Bouwens R3,Inami H4ORCID,Sommovigo L5ORCID,Algera H46ORCID,da Cunha E7,Aravena M8,Dayal P9ORCID,Ferrara A5,Fudamoto Y610,Gonzalez V1112,Graziani L1314ORCID,Hygate A P S3ORCID,de Looze I1516,Nanayakkara T17,Pallottini A5ORCID,Schneider R1314ORCID,Stefanon M1819,Topping M20ORCID,van der Werf P3

Affiliation:

1. Department of Astronomy, University of Geneva , Chemin Pegasi 51, CH-1290 Versoix, Switzerland

2. Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 København N, Denmark

3. Leiden Observatory, Leiden University , PO Box 9500, NL-2300 RA Leiden, the Netherlands

4. Hiroshima Astrophysical Science Center, Hiroshima University , 1-3-1 Kagamiyama-Higashi, Hiroshima 739-8526, Japan

5. Scuola Normale Superiore , Piazza dei Cavalieri 7, I-56126 Pisa, Italy

6. National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, 169-8555, Tokyo, Japan

7. International Centre for Radio Astronomy Research, University of Western Australia , Stirling Hwy, Crawley 26, WA 6009, Australia

8. Nucleo de Astronomia Facultad de Ingenieria y Ciencias, Universidad Diego Portales , Av Ejercito 441, Santiago, Chile

9. Kapteyn Astronomical Institute, University of Groningen , PO Box 800, NL-9700 AV Groningen, the Netherlands

10. Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan

11. Departmento de Astronomia, Universidad de Chile , Casilla 36-D, Santiago 7591245, Chile

12. Centro de Astrofisica y Tecnologias Afines (CATA), Camino del Observatorio 1515 , Las Condes, Santiago 7591245, Chile

13. Dipartimento di Fisica, Sapienza, Universita di Roma , Piazzale Aldo Moro 5, I-00185 Roma, Italy

14. INAF/Osservatorio Astronomico di Roma , via Frascati 33, I-00078 Monte Porzio Catone, Roma, Italy

15. Sterrenkundig Observatorium, Ghent University , Krijgslaan 281-59, B-9000 Gent, Belgium

16. Department of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT, UK

17. Centre for Astrophysics and Supercomputing, Swinburne University of Technology , PO Box 218, Hawthorn, VIC 3112, Australia

18. Departament d’Astronomia i Astrofisica, Universitat de Valencia , C. Dr Moliner 50, E-46100 Burjassot, Valencia, Spain

19. Unidad Asociada CSIC ‘Grupo de Astrofisica Extragalactica y Cosmologia’ (Instituto de Fisica de Cantabria – Universitat de Valencia) , 46980, Valencia, Spain

20. Steward Observatory, University of Arizona , 933 N Cherry Ave, Tucson, AZ 85721, USA

Abstract

ABSTRACT We present the first observational infrared luminosity function (IRLF) measurement in the Epoch of Reionization (EoR) based on a ultraviolet (UV)-selected galaxy sample with the Atacama Large Millimeter Array (ALMA) spectroscopic observations. Our analysis is based on the ALMA large program Reionization Era Bright Emission Line Survey (REBELS), which targets 42 galaxies at z  = 6.4–7.7 with [C ii] 158 $\rm{\mu m}$ line scans. 16 sources exhibit dust detection, 15 of which are also spectroscopically confirmed through the [C ii] line. The infrared (IR) luminosities of the sample range from log LIR/L⊙ = 11.4 to 12.2. Using the UV luminosity function as a proxy to derive the effective volume for each of our target sources, we derive IRLF estimates, both for detections and for the full sample including IR luminosity upper limits. The resulting IRLFs are well reproduced by a Schechter function with the characteristic luminosity of $\log L_{*}/\mathrm{ L}_\odot =11.6^{+0.2}_{-0.1}$ . Our observational results are in broad agreement with the average of predicted IRLFs from simulations at z ∼ 7. Conversely, our IRLFs lie significantly below lower redshift estimates, suggesting a rapid evolution from z ∼ 4 to z ∼ 7, into the reionization epoch. The IR obscured contribution to the cosmic star formation rate density at z ∼ 7 amounts to $\mathrm{log(SFRD/{\rm M}_{\odot }\,yr^{-1}\,Mpc^{-3}) = -2.66^{+0.17}_{-0.14} }$ that is at least ∼10 per cent of UV-based estimates. We conclude that the presence of dust is already abundant in the EoR and discuss the possibility of unveiling larger samples of dusty galaxies with future ALMA and JWST observations.

Funder

Swiss National Science Foundation

Danish National Research Foundation

European Research Council

NWO

European Commission

University of Groningen

ERC

NAOJ

ANID

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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