JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe
We present the number densities and physical properties of the bright galaxies spectroscopically confirmed at z ∼ 7–14. Our sample is composed of 60 galaxies at z _spec ∼ 7–14, including recently confirmed galaxies at z _spec = 12.34–14.18 with JWST, as well as new confirmations at z _spec = 6.583–7...
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| author | Yuichi Harikane Akio K. Inoue Richard S. Ellis Masami Ouchi Yurina Nakazato Naoki Yoshida Yoshiaki Ono Fengwu Sun Riku A. Sato Giovanni Ferrami Seiji Fujimoto Nobunari Kashikawa Derek J. McLeod Pablo G. Pérez-González Marcin Sawicki Yuma Sugahara Yi Xu Satoshi Yamanaka Adam C. Carnall Fergus Cullen James S. Dunlop Eiichi Egami Norman Grogin Yuki Isobe Anton M. Koekemoer Nicolas Laporte Chien-Hsiu Lee Dan Magee Hiroshi Matsuo Yoshiki Matsuoka Ken Mawatari Kimihiko Nakajima Minami Nakane Yoichi Tamura Hiroya Umeda Hiroto Yanagisawa |
| author_facet | Yuichi Harikane Akio K. Inoue Richard S. Ellis Masami Ouchi Yurina Nakazato Naoki Yoshida Yoshiaki Ono Fengwu Sun Riku A. Sato Giovanni Ferrami Seiji Fujimoto Nobunari Kashikawa Derek J. McLeod Pablo G. Pérez-González Marcin Sawicki Yuma Sugahara Yi Xu Satoshi Yamanaka Adam C. Carnall Fergus Cullen James S. Dunlop Eiichi Egami Norman Grogin Yuki Isobe Anton M. Koekemoer Nicolas Laporte Chien-Hsiu Lee Dan Magee Hiroshi Matsuo Yoshiki Matsuoka Ken Mawatari Kimihiko Nakajima Minami Nakane Yoichi Tamura Hiroya Umeda Hiroto Yanagisawa |
| author_sort | Yuichi Harikane |
| collection | DOAJ |
| description | We present the number densities and physical properties of the bright galaxies spectroscopically confirmed at z ∼ 7–14. Our sample is composed of 60 galaxies at z _spec ∼ 7–14, including recently confirmed galaxies at z _spec = 12.34–14.18 with JWST, as well as new confirmations at z _spec = 6.583–7.643 with −24 < M _UV < −21 mag using ALMA and Keck. Our JWST/NIRSpec observations have also revealed that very bright galaxy candidates at z ∼ 10–13 identified from ground-based telescope images before JWST are passive galaxies at z ∼ 3–4, emphasizing the necessity of strict screening and spectroscopy in the selection of the brightest galaxies at z > 10. The UV luminosity functions derived from these spectroscopic results are consistent with a double power-law function, showing tensions with theoretical models at the bright end. To understand the origin of the overabundance of bright galaxies, we investigate their morphologies using JWST/NIRCam high-resolution images obtained in various surveys, including PRIMER and COSMOS-Web. We find that ∼70% of the bright galaxies at z ∼ 7 exhibit clumpy morphologies with multiple subcomponents, suggesting merger-induced starburst activity, which is consistent with SED fitting results showing bursty star formation histories. At z ≳ 10, bright galaxies are classified into two types of galaxies: extended ones with weak high-ionization emission lines, and compact ones with strong high-ionization lines including N iv] λ 1486, indicating that at least two different processes (e.g., merger-induced starburst and compact star formation/AGN) are shaping the physical properties of the brightest galaxies at z ≳ 10 and are responsible for their overabundance. |
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| spelling | doaj-art-4c0033a4544544a595ec7643596c4aa62025-02-08T15:21:03ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980113810.3847/1538-4357/ad9b2cJWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early UniverseYuichi Harikane0https://orcid.org/0000-0002-6047-430XAkio K. Inoue1https://orcid.org/0000-0002-7779-8677Richard S. Ellis2https://orcid.org/0000-0001-7782-7071Masami Ouchi3https://orcid.org/0000-0002-1049-6658Yurina Nakazato4https://orcid.org/0000-0002-0984-7713Naoki Yoshida5https://orcid.org/0000-0001-7925-238XYoshiaki Ono6https://orcid.org/0000-0001-9011-7605Fengwu Sun7https://orcid.org/0000-0002-4622-6617Riku A. Sato8Giovanni Ferrami9https://orcid.org/0000-0002-2012-4612Seiji Fujimoto10https://orcid.org/0000-0001-7201-5066Nobunari Kashikawa11https://orcid.org/0000-0003-3954-4219Derek J. McLeod12https://orcid.org/0000-0003-4368-3326Pablo G. Pérez-González13https://orcid.org/0000-0003-4528-5639Marcin Sawicki14https://orcid.org/0000-0002-7712-7857Yuma Sugahara15https://orcid.org/0000-0001-6958-7856Yi Xu16https://orcid.org/0000-0002-5768-8235Satoshi Yamanaka17https://orcid.org/0000-0002-7738-5290Adam C. Carnall18https://orcid.org/0000-0002-1482-5818Fergus Cullen19https://orcid.org/0000-0002-3736-476XJames S. Dunlop20https://orcid.org/0000-0002-1404-5950Eiichi Egami21https://orcid.org/0000-0003-1344-9475Norman Grogin22https://orcid.org/0000-0001-9440-8872Yuki Isobe23https://orcid.org/0000-0001-7730-8634Anton M. Koekemoer24https://orcid.org/0000-0002-6610-2048Nicolas Laporte25https://orcid.org/0000-0001-7459-6335Chien-Hsiu Lee26https://orcid.org/0000-0003-1700-5740Dan Magee27https://orcid.org/0000-0002-6668-2011Hiroshi Matsuo28https://orcid.org/0000-0002-4559-6157Yoshiki Matsuoka29https://orcid.org/0000-0001-5063-0340Ken Mawatari30https://orcid.org/0000-0003-4985-0201Kimihiko Nakajima31https://orcid.org/0000-0003-2965-5070Minami Nakane32https://orcid.org/0009-0000-1999-5472Yoichi Tamura33https://orcid.org/0000-0003-4807-8117Hiroya Umeda34https://orcid.org/0009-0008-0167-5129Hiroto Yanagisawa35https://orcid.org/0009-0006-6763-4245Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected] of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan; Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, JapanDepartment of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT, UKInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected]; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo , Kashiwa, Chiba 277-8583, JapanDepartment of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanDepartment of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected] Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721, USA; Center for Astrophysics ∣ Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USADepartment of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, JapanSchool of Physics, University of Melbourne , Parkville, VIC 3010, Australia; ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaDepartment of Astronomy, The University of Texas at Austin , Austin, TX, USADepartment of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan; Research Center for the Early Universe, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanSUPA, Institute for Astronomy, University of Edinburgh , Royal Observatory, Edinburgh EH9 3HJ, UKCentro de Astrobiología (CAB/CSIC-INTA) , Carretera de Ajalvir km 4, Torrejón de Ardoz, E-28850, Madrid, SpainDepartment of Astronomy and Physics and the Institute for Computational Astrophysics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaDepartment of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan; Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected]; Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanGeneral Education Department, National Institute of Technology, Toba College , 1-1, Ikegami-cho, Toba, Mie 517-8501, JapanSUPA, Institute for Astronomy, University of Edinburgh , Royal Observatory, Edinburgh EH9 3HJ, UKSUPA, Institute for Astronomy, University of Edinburgh , Royal Observatory, Edinburgh EH9 3HJ, UKSUPA, Institute for Astronomy, University of Edinburgh , Royal Observatory, Edinburgh EH9 3HJ, UKSteward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721, USASpace Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USAWaseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, JapanSpace Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USAAix-Marseille Université , CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, 13388 Marseille, FranceHobby-Eberly Telescope , McDonald Observatory, 32 Mount Fowlkes, Fort Davis, TX 79734, USADepartment of Astronomy and Astrophysics, UCO/Lick Observatory, University of California , Santa Cruz, CA 95064, USANational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanResearch Center for Space and Cosmic Evolution, Ehime University , Matsuyama, Ehime 790-8577, JapanWaseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected]; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanDivision of Particle and Astrophysical Science, Graduate School of Science, Nagoya University , Nagoya 464-8602, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected]; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; [email protected]; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanWe present the number densities and physical properties of the bright galaxies spectroscopically confirmed at z ∼ 7–14. Our sample is composed of 60 galaxies at z _spec ∼ 7–14, including recently confirmed galaxies at z _spec = 12.34–14.18 with JWST, as well as new confirmations at z _spec = 6.583–7.643 with −24 < M _UV < −21 mag using ALMA and Keck. Our JWST/NIRSpec observations have also revealed that very bright galaxy candidates at z ∼ 10–13 identified from ground-based telescope images before JWST are passive galaxies at z ∼ 3–4, emphasizing the necessity of strict screening and spectroscopy in the selection of the brightest galaxies at z > 10. The UV luminosity functions derived from these spectroscopic results are consistent with a double power-law function, showing tensions with theoretical models at the bright end. To understand the origin of the overabundance of bright galaxies, we investigate their morphologies using JWST/NIRCam high-resolution images obtained in various surveys, including PRIMER and COSMOS-Web. We find that ∼70% of the bright galaxies at z ∼ 7 exhibit clumpy morphologies with multiple subcomponents, suggesting merger-induced starburst activity, which is consistent with SED fitting results showing bursty star formation histories. At z ≳ 10, bright galaxies are classified into two types of galaxies: extended ones with weak high-ionization emission lines, and compact ones with strong high-ionization lines including N iv] λ 1486, indicating that at least two different processes (e.g., merger-induced starburst and compact star formation/AGN) are shaping the physical properties of the brightest galaxies at z ≳ 10 and are responsible for their overabundance.https://doi.org/10.3847/1538-4357/ad9b2cGalaxy formationGalaxy evolutionHigh-redshift galaxies |
| spellingShingle | Yuichi Harikane Akio K. Inoue Richard S. Ellis Masami Ouchi Yurina Nakazato Naoki Yoshida Yoshiaki Ono Fengwu Sun Riku A. Sato Giovanni Ferrami Seiji Fujimoto Nobunari Kashikawa Derek J. McLeod Pablo G. Pérez-González Marcin Sawicki Yuma Sugahara Yi Xu Satoshi Yamanaka Adam C. Carnall Fergus Cullen James S. Dunlop Eiichi Egami Norman Grogin Yuki Isobe Anton M. Koekemoer Nicolas Laporte Chien-Hsiu Lee Dan Magee Hiroshi Matsuo Yoshiki Matsuoka Ken Mawatari Kimihiko Nakajima Minami Nakane Yoichi Tamura Hiroya Umeda Hiroto Yanagisawa JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe The Astrophysical Journal Galaxy formation Galaxy evolution High-redshift galaxies |
| title | JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe |
| title_full | JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe |
| title_fullStr | JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe |
| title_full_unstemmed | JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe |
| title_short | JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at z ∼ 7–14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe |
| title_sort | jwst alma and keck spectroscopic constraints on the uv luminosity functions at z ∼ 7 14 clumpiness and compactness of the brightest galaxies in the early universe |
| topic | Galaxy formation Galaxy evolution High-redshift galaxies |
| url | https://doi.org/10.3847/1538-4357/ad9b2c |
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