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Stellar Velocity Dispersion of a Massive Quenching Galaxy at z = 4.01

Tanaka, Masayuki and Valentino, Francesco and Toft, Sune and Onodera, Masato and Shimakawa, Rhythm and Ceverino, Daniel and Faisst, Andreas L. and Gallazzi, Anna and Gómez-Guijarro, Carlos and Kubo, Mariko and Magdis, Georgios E. and Steinhardt, Charles L. and Stockmann, Mikkel and Yabe, Kiyoto and Zabl, Johannes (2019) Stellar Velocity Dispersion of a Massive Quenching Galaxy at z = 4.01. Astrophysical Journal Letters, 885 (2). Art. No. L34. ISSN 2041-8213. https://resolver.caltech.edu/CaltechAUTHORS:20191002-104646904

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Abstract

We present the first stellar velocity dispersion measurement of a massive quenching galaxy at z = 4. The galaxy is first identified as a massive z ≥ 4 galaxy with suppressed star formation from photometric redshifts based on deep multiband data. A follow-up spectroscopic observation with MOSFIRE on Keck revealed strong multiple absorption features, which are identified as Balmer lines, giving a secure redshift of z = 4.01. This is the most distant quiescent galaxy known to date. Thanks to the high S/N of the spectrum, we are able to estimate the stellar velocity dispersion, σ=268±59 km s⁻¹, making a significant leap from the previous highest redshift measurement at z = 2.8. Interestingly, we find that the velocity dispersion is consistent with that of massive galaxies today, implying no significant evolution in velocity dispersion over the last 12 Gyr. Based on a stringent upper limit on its physical size from deep optical images (r_(eff) < 1.3 kpc), we find that its dynamical mass is consistent with the stellar mass inferred from photometry. Furthermore, the galaxy is located on the mass fundamental plane extrapolated from lower redshift galaxies. The observed no strong evolution in σ suggests that the mass in the core of massive galaxies does not evolve significantly, while most of the mass growth occurs in the outskirts of the galaxies, which also increases the size. This picture is consistent with a two-phase formation scenario in which mass and size growth is due to accretion in the outskirts of galaxies via mergers. Our results imply that the first phase may be completed as early as z ~ 4.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/ab4ff3DOIArticle
https://doi.org/10.3847/2041-8213/ab8b5aDOIErratum
https://arxiv.org/abs/1909.10721arXivDiscussion Paper
ORCID:
AuthorORCID
Tanaka, Masayuki0000-0002-5011-5178
Toft, Sune0000-0003-3631-7176
Ceverino, Daniel0000-0002-8680-248X
Faisst, Andreas L.0000-0002-9382-9832
Gómez-Guijarro, Carlos0000-0002-4085-9165
Magdis, Georgios E.0000-0002-4872-2294
Steinhardt, Charles L.0000-0003-3780-6801
Stockmann, Mikkel0000-0001-5983-6273
Additional Information:© 2019 The American Astronomical Society. Received 2019 September 23; revised 2019 October 15; accepted 2019 October 22; published 2019 November 6. This work is supported by JSPS KAKENHI grant Nos. JP23740144 and JP15K17617. F.V. and G.E.M. acknowledge the Villum Fonden research grant 13160 "Gas to stars, stars to dust: tracing star formation across cosmic time." F.V. acnknowledges the Carlsberg Fonden research grant CF18-0388 "Galaxies: Rise And Death." The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. S.T. and G.E.M. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). M.O. acknowledges support by KAKENHI JP17K14257. K.Y. acknowledges support by JSPS KAKENHI grant No. JP18K13578. We thank the anonymous referee for a useful report, which helped improve the paper. The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by NAOJ, Kavli IPMU, the University of Tokyo, KEK, ASIAA, and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology, the Japan Society for the Promotion of Science, Japan Science and Technology Agency, the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for LSST. We thank the LSST Project for making their code available as free software at http://dm.lsst.org. This paper is based in part on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and ADC at NAOJ. Data analysis was in part carried out with the cooperation of CfCA and NAOJ. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. Facility: Keck(MOSFIRE). -
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)JP23740144
Japan Society for the Promotion of Science (JSPS)JP15K17617
VILLUM FONDEN13160
Carlsberg FoundationCF18-0388
Danish National Research Foundation140
European Research Council (ERC)648179
Japan Society for the Promotion of Science (JSPS)JP17K14257
Japan Society for the Promotion of Science (JSPS)JP18K13578
Japanese Cabinet OfficeUNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Japan Science and Technology AgencyUNSPECIFIED
Toray Science FoundationUNSPECIFIED
National Astronomical Observatory of JapanUNSPECIFIED
Kavli Institute for the Physics and Mathematics of the UniverseUNSPECIFIED
High Energy Accelerator Research Organization (KEK)UNSPECIFIED
Academia Sinica Institute of Astronomy and AstrophysicsUNSPECIFIED
Princeton UniversityUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Participating InstitutionsUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
NASAUNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Subject Keywords:Galaxy formation; Galaxy evolution; Elliptical galaxies; Galaxy dynamics; High-redshift galaxies
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Galaxy formation (595); Galaxy evolution (594); Elliptical galaxies (456); Galaxy dynamics (591); High-redshift galaxies (734)
Record Number:CaltechAUTHORS:20191002-104646904
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20191002-104646904
Official Citation:Masayuki Tanaka et al 2019 ApJL 885 L34
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:99017
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:02 Oct 2019 18:06
Last Modified:05 May 2020 16:55

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