Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2
Galaxy clusters are crucial to understanding the role of the environment in galaxy evolution. However, due to their rarity, only a limited number of clusters have been identified at z ≳ 2. In this paper, we report a discovery of seven cluster candidates with massive quiescent galaxies at z ∼ 2 in...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ada5f4 |
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| author | Tomokazu Kiyota Makoto Ando Masayuki Tanaka Alexis Finoguenov Sadman Shariar Ali Jean Coupon Guillaume Desprez Stephen Gwyn Marcin Sawicki Rhythm Shimakawa |
| author_facet | Tomokazu Kiyota Makoto Ando Masayuki Tanaka Alexis Finoguenov Sadman Shariar Ali Jean Coupon Guillaume Desprez Stephen Gwyn Marcin Sawicki Rhythm Shimakawa |
| author_sort | Tomokazu Kiyota |
| collection | DOAJ |
| description | Galaxy clusters are crucial to understanding the role of the environment in galaxy evolution. However, due to their rarity, only a limited number of clusters have been identified at z ≳ 2. In this paper, we report a discovery of seven cluster candidates with massive quiescent galaxies at z ∼ 2 in the 3.5 deg ^2 area of the XMM Large Scale Structure field, roughly doubling the known cluster sample at this frontier redshift if confirmed. We construct a photometric redshift catalog based on deep ( i ∼ 26, K _s ∼ 24) multiwavelength photometry from the u * band to the K band gathered from the Hyper Suprime-Cam Subaru Strategic Program and other collaborative/public surveys. We adopt a Gaussian kernel density estimate with two different spatial scales (10″ and 60″) to draw a density map of massive ( $\mathrm{log}({M}_{* }/{M}_{\odot })\gt 10.5$ ) and quiescent ( $\mathrm{log}(\mathrm{sSFR}\,[{\mathrm{yr}}^{-1}])\lt -10$ ) galaxies at z ∼ 2. Then, we identify seven prominent overdensities. These candidates show clear red sequences in color–magnitude diagrams ( z − H versus H ). Moreover, one of them shows an extended X-ray emission with L _X = (1.46 ± 0.35) × 10 ^44 erg s ^−1 , suggesting its virialized nature. There is no clear evidence of enhancement nor suppression of the star formation rate of the main-sequence galaxies in the clusters. We find that cluster galaxies have a higher fraction of transition population with $-10.5\lt \mathrm{log}(\mathrm{sSFR}\,[{\mathrm{yr}}^{-1}])\lt -10$ (12%) than the field (2%), which implies the ongoing star formation quenching. The quiescent fraction in the cluster candidates also exceeds that in the field. We confirm that the excess of a quiescent fraction is larger for higher-mass galaxies. This is the first statistical evidence for the mass-dependent environmental quenching at work in clusters even at z ∼ 2. |
| format | Article |
| id | doaj-art-f4db0db1d74f4b6cbe1878f2b131c0a3 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-f4db0db1d74f4b6cbe1878f2b131c0a32025-02-06T08:06:29ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980110410.3847/1538-4357/ada5f4Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2Tomokazu Kiyota0https://orcid.org/0009-0004-4332-9225Makoto Ando1https://orcid.org/0000-0002-4225-4477Masayuki Tanaka2https://orcid.org/0000-0002-5011-5178Alexis Finoguenov3https://orcid.org/0000-0002-4606-5403Sadman Shariar Ali4https://orcid.org/0000-0003-3883-6500Jean Coupon5Guillaume Desprez6https://orcid.org/0000-0001-8325-1742Stephen Gwyn7https://orcid.org/0000-0001-8221-8406Marcin Sawicki8https://orcid.org/0000-0002-7712-7857Rhythm Shimakawa9https://orcid.org/0000-0003-4442-2750Department of Astronomical Science, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan ; tomokazu.kiyota@grad.nao.ac.jp; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JapanDepartment of Astronomical Science, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan ; tomokazu.kiyota@grad.nao.ac.jp; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JapanDepartment of Physics, University of Helsinki , P.O. Box 64, FI-00014 Helsinki, FinlandSubaru Telescope, National Astronomical Observatory of Japan , 650 North Aohoku Place, Hilo, HI 96720, USADepartment of Astronomy, University of Geneva , ch. d’Écogia 16, CH-1290 Versoix, SwitzerlandDepartment of Astronomy and Astrophysics and Institute for Computational Astrophysics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaNRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Road, Victoria, BC V9E 2E7, CanadaDepartment of Astronomy and Astrophysics and Institute for Computational Astrophysics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaWaseda Institute for Advanced Study (WIAS), Waseda University , 1-21-1 Nishi-Waseda, Shinjuku, Tokyo, 169-0051, Japan; Center for Data Science, Waseda University , 1-6-1 Nishi-Waseda, Shinjuku, Tokyo, 169-0051, JapanGalaxy clusters are crucial to understanding the role of the environment in galaxy evolution. However, due to their rarity, only a limited number of clusters have been identified at z ≳ 2. In this paper, we report a discovery of seven cluster candidates with massive quiescent galaxies at z ∼ 2 in the 3.5 deg ^2 area of the XMM Large Scale Structure field, roughly doubling the known cluster sample at this frontier redshift if confirmed. We construct a photometric redshift catalog based on deep ( i ∼ 26, K _s ∼ 24) multiwavelength photometry from the u * band to the K band gathered from the Hyper Suprime-Cam Subaru Strategic Program and other collaborative/public surveys. We adopt a Gaussian kernel density estimate with two different spatial scales (10″ and 60″) to draw a density map of massive ( $\mathrm{log}({M}_{* }/{M}_{\odot })\gt 10.5$ ) and quiescent ( $\mathrm{log}(\mathrm{sSFR}\,[{\mathrm{yr}}^{-1}])\lt -10$ ) galaxies at z ∼ 2. Then, we identify seven prominent overdensities. These candidates show clear red sequences in color–magnitude diagrams ( z − H versus H ). Moreover, one of them shows an extended X-ray emission with L _X = (1.46 ± 0.35) × 10 ^44 erg s ^−1 , suggesting its virialized nature. There is no clear evidence of enhancement nor suppression of the star formation rate of the main-sequence galaxies in the clusters. We find that cluster galaxies have a higher fraction of transition population with $-10.5\lt \mathrm{log}(\mathrm{sSFR}\,[{\mathrm{yr}}^{-1}])\lt -10$ (12%) than the field (2%), which implies the ongoing star formation quenching. The quiescent fraction in the cluster candidates also exceeds that in the field. We confirm that the excess of a quiescent fraction is larger for higher-mass galaxies. This is the first statistical evidence for the mass-dependent environmental quenching at work in clusters even at z ∼ 2.https://doi.org/10.3847/1538-4357/ada5f4Galaxy clustersGalaxy evolutionGalaxy formationHigh-redshift galaxiesQuenched galaxies |
| spellingShingle | Tomokazu Kiyota Makoto Ando Masayuki Tanaka Alexis Finoguenov Sadman Shariar Ali Jean Coupon Guillaume Desprez Stephen Gwyn Marcin Sawicki Rhythm Shimakawa Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 The Astrophysical Journal Galaxy clusters Galaxy evolution Galaxy formation High-redshift galaxies Quenched galaxies |
| title | Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 |
| title_full | Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 |
| title_fullStr | Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 |
| title_full_unstemmed | Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 |
| title_short | Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 |
| title_sort | cluster candidates with massive quiescent galaxies at z ∼ 2 |
| topic | Galaxy clusters Galaxy evolution Galaxy formation High-redshift galaxies Quenched galaxies |
| url | https://doi.org/10.3847/1538-4357/ada5f4 |
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