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A Protocluster of Massive Quiescent Galaxies at z = 4

dc.contributor.authorMasayuki Tanaka
dc.contributor.authorMasato Onodera
dc.contributor.authorRhythm Shimakawa
dc.contributor.authorKei Ito
dc.contributor.authorTakumi Kakimoto
dc.contributor.authorMariko Kubo
dc.contributor.authorTakahiro Morishita
dc.contributor.authorSune Toft
dc.contributor.authorFrancesco Valentino
dc.contributor.authorPo-Feng Wu
dc.contributor.otherNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan ; masayuki.tanaka@nao.ac.jp; Graduate Institute for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
dc.contributor.otherGraduate Institute for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Subaru Telescope, National Astronomical Observatory of Japan , 650 North Aohoku Place, Hilo, HI 96720, USA
dc.contributor.otherWaseda Institute for Advanced Study (WIAS), Waseda University , Nishi Waseda, Shinjuku, Tokyo 169-0051, Japan; Center for Data Science, Waseda University , 1-6-1, Nishi-Waseda, Shinjuku, Tokyo 169-0051, Japan
dc.contributor.otherDepartment of Astronomy, School of Science, The University of Tokyo , 7-3-1, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
dc.contributor.otherGraduate Institute for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
dc.contributor.otherAstronomical Institute, Tohoku University , 6-3, Aramaki, Aoba-ku, Sendai, Miyagi, 980-8578, Japan
dc.contributor.otherIPAC, California Institute of Technology , MC 314-6, 1200 East California Boulevard, Pasadena, CA 91125, USA
dc.contributor.otherCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen, Denmark
dc.contributor.otherCosmic Dawn Center (DAWN) , Denmark; European Southern Observatory , Karl-Schwarzschild-Straße 2, D-85748 Garching bei Munchen, Germany
dc.contributor.otherGraduate Institute of Astrophysics and Department of Physics, National Taiwan University , Number 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan; Department of Physics and Center for Theoretical Physics, National Taiwan University , Number 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan; Physics Division, National Center for Theoretical Sciences , Number 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan
dc.date.accessioned2024-07-17T06:04:48Z
dc.date.accessioned2025-10-08T09:20:06Z
dc.date.available2025-10-08T09:20:06Z
dc.date.issued01-01-2024
dc.identifier.urihttp://digilib.fisipol.ugm.ac.id/repo/handle/15717717/39972
dc.description.abstractWe report on discovery of a concentration of massive quiescent galaxies located at z = 4. The concentration is first identified using high-quality photometric redshifts based on deep, multiband data in Subaru/XMM-Newton Deep Field. Follow-up near-infrared spectroscopic observations with MOSFIRE on Keck confirm a massive (∼10 ^11 M _⊙ ) quiescent galaxy at z = 3.99. Our spectral energy distribution analyses reveal that the galaxy experienced an episode of starburst about 500 Myr prior to the observed epoch, followed by rapid quenching. Since its spectrum is sufficiently good to measure the stellar velocity dispersion, we infer its dynamical mass and find that it is consistent with its stellar mass. The galaxy is surrounded by four massive (>10 ^10 M _⊙ ) quiescent galaxies on a ∼1 physical Mpc scale, all of which are consistent with being located at the same redshift based on high-accuracy spectrophotometric redshifts. This is likely a (proto)cluster dominated by quiescent galaxies, the first of the kind reported at such a high redshift as z = 4. Interestingly, it is in a large-scale structure revealed by spectroscopic redshifts from VANDELS. Furthermore, it also exhibits a red sequence, adding further support to the physical concentration of the galaxies. We find no such concentration in the Illustris-TNG300 simulation; it may be that the cluster is such a rare system that the simulation box is not sufficiently large to reproduce it. The total halo mass of the quiescent galaxies is ∼10 ^13 M _⊙ , suggesting that they form a group-sized halo once they collapse together. We discuss the implications of our findings for the quenching physics and conclude with future prospects.
dc.language.isoEN
dc.publisherIOP Publishing
dc.subject.lccAstrophysics
dc.titleA Protocluster of Massive Quiescent Galaxies at z = 4
dc.typeArticle
dc.description.keywordsGalaxy evolution
dc.description.doi10.3847/1538-4357/ad5316
dc.title.journalThe Astrophysical Journal
dc.identifier.e-issn1538-4357
dc.identifier.oaioai:doaj.org/journal:243f327402dd4f998a514b146b4dbadd
dc.journal.infoVolume 970, Issue 1


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