From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
The assembly of galaxies over cosmic time is tightly connected to the assembly of their host dark matter halos. We investigate the stellar mass growth history and the chemical enrichment history of central galaxies in the Sloan Digital Sky Survey Mapping Nearby Galaxies at Apache Point Observatory....
| Main Authors: | , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad036b |
| _version_ | 1797448980318126080 |
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| author | Cheqiu Lyu Yingjie Peng Yipeng Jing Xiaohu Yang Luis C. Ho Alvio Renzini Bitao Wang Kai Wang Bingxiao Xu Dingyi Zhao Jing Dou Qiusheng Gu Roberto Maiolino Filippo Mannucci Feng Yuan |
| author_facet | Cheqiu Lyu Yingjie Peng Yipeng Jing Xiaohu Yang Luis C. Ho Alvio Renzini Bitao Wang Kai Wang Bingxiao Xu Dingyi Zhao Jing Dou Qiusheng Gu Roberto Maiolino Filippo Mannucci Feng Yuan |
| author_sort | Cheqiu Lyu |
| collection | DOAJ |
| description | The assembly of galaxies over cosmic time is tightly connected to the assembly of their host dark matter halos. We investigate the stellar mass growth history and the chemical enrichment history of central galaxies in the Sloan Digital Sky Survey Mapping Nearby Galaxies at Apache Point Observatory. We find that the derived stellar metallicity of passive central galaxies is always higher than that of the star-forming ones. This stellar metallicity enhancement becomes progressively larger toward low-mass galaxies (at a given epoch) and earlier epochs (at a given stellar mass), which suggests strangulation as the primary mechanism for star formation quenching in central galaxies not only in the local Universe but also very likely at higher redshifts up to z ∼ 3. We show that at the same present-day stellar mass, passive central galaxies assembled half of their final stellar mass ∼2 Gyr earlier than star-forming central galaxies, which agrees well with the semi-analytic model. Exploring the semi-analytic model, we find that this is because passive central galaxies reside in, on average, more massive halos with a higher halo mass increase rate across cosmic time. As a consequence, passive central galaxies are assembled faster and also quenched earlier than their star-forming counterparts. While at the same present-day halo mass, different halo assembly history also produces a very different final stellar mass of the central galaxy within, and halos assembled earlier host more massive centrals with a higher quenched fraction, in particular around the “golden halo mass” at 10 ^12 M _⊙ . Our results call attention back to the dark matter halo as a key driver of galaxy evolution. |
| first_indexed | 2024-03-09T14:18:17Z |
| format | Article |
| id | doaj.art-08cb3375081a4a14bf1209c6f127b7e5 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-09T14:18:17Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-08cb3375081a4a14bf1209c6f127b7e52023-11-28T18:24:23ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-019591510.3847/1538-4357/ad036bFrom Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central GalaxiesCheqiu Lyu0https://orcid.org/0009-0000-7307-6362Yingjie Peng1Yipeng Jing2https://orcid.org/0000-0002-4534-3125Xiaohu Yang3https://orcid.org/0000-0003-3997-4606Luis C. Ho4https://orcid.org/0000-0001-6947-5846Alvio Renzini5https://orcid.org/0000-0002-7093-7355Bitao Wang6https://orcid.org/0000-0002-6137-6007Kai Wang7https://orcid.org/0000-0002-3775-0484Bingxiao Xu8Dingyi Zhao9Jing Dou10https://orcid.org/0000-0002-6961-6378Qiusheng Gu11https://orcid.org/0000-0002-3890-3729Roberto Maiolino12https://orcid.org/0000-0002-4985-3819Filippo Mannucci13https://orcid.org/0000-0002-4803-2381Feng Yuan14https://orcid.org/0000-0003-3564-6437Department of Astronomy, School of Physics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of China ; yjpeng@pku.edu.cn; Kavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaDepartment of Astronomy, School of Physics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of China ; yjpeng@pku.edu.cn; Kavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaDepartment of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University , Shanghai 200240, People's Republic of China; Tsung-Dao Lee Institute, and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao Tong University , Shanghai 200240, People's Republic of ChinaDepartment of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University , Shanghai 200240, People's Republic of China; Tsung-Dao Lee Institute, and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao Tong University , Shanghai 200240, People's Republic of ChinaDepartment of Astronomy, School of Physics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of China ; yjpeng@pku.edu.cn; Kavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaINAF–Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyKavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaDepartment of Astronomy, School of Physics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of China ; yjpeng@pku.edu.cn; Kavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Beijing 100871, People's Republic of ChinaSchool of Astronomy and Space Science, Nanjing University , Nanjing 210093, People's Republic of ChinaSchool of Astronomy and Space Science, Nanjing University , Nanjing 210093, People's Republic of ChinaCavendish Laboratory, University of Cambridge , 19 J.J. Thomson Avenue, Cambridge, CB3 0HE, UK; Kavli Institute for Cosmology, University of Cambridge , Madingley Road, Cambridge, CB3 0HA, UK; Department of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT, UKINAF–Osservatorio Astrofisico di Arcetri , Largo Enrico Fermi 5, I-50125 Firenze, ItalyKey Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People's Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People's Republic of ChinaThe assembly of galaxies over cosmic time is tightly connected to the assembly of their host dark matter halos. We investigate the stellar mass growth history and the chemical enrichment history of central galaxies in the Sloan Digital Sky Survey Mapping Nearby Galaxies at Apache Point Observatory. We find that the derived stellar metallicity of passive central galaxies is always higher than that of the star-forming ones. This stellar metallicity enhancement becomes progressively larger toward low-mass galaxies (at a given epoch) and earlier epochs (at a given stellar mass), which suggests strangulation as the primary mechanism for star formation quenching in central galaxies not only in the local Universe but also very likely at higher redshifts up to z ∼ 3. We show that at the same present-day stellar mass, passive central galaxies assembled half of their final stellar mass ∼2 Gyr earlier than star-forming central galaxies, which agrees well with the semi-analytic model. Exploring the semi-analytic model, we find that this is because passive central galaxies reside in, on average, more massive halos with a higher halo mass increase rate across cosmic time. As a consequence, passive central galaxies are assembled faster and also quenched earlier than their star-forming counterparts. While at the same present-day halo mass, different halo assembly history also produces a very different final stellar mass of the central galaxy within, and halos assembled earlier host more massive centrals with a higher quenched fraction, in particular around the “golden halo mass” at 10 ^12 M _⊙ . Our results call attention back to the dark matter halo as a key driver of galaxy evolution.https://doi.org/10.3847/1538-4357/ad036bGalaxy evolutionGalaxy dark matter halosStar formation |
| spellingShingle | Cheqiu Lyu Yingjie Peng Yipeng Jing Xiaohu Yang Luis C. Ho Alvio Renzini Bitao Wang Kai Wang Bingxiao Xu Dingyi Zhao Jing Dou Qiusheng Gu Roberto Maiolino Filippo Mannucci Feng Yuan From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies The Astrophysical Journal Galaxy evolution Galaxy dark matter halos Star formation |
| title | From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies |
| title_full | From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies |
| title_fullStr | From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies |
| title_full_unstemmed | From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies |
| title_short | From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies |
| title_sort | from halos to galaxies vii the connections between stellar mass growth history quenching history and halo assembly history for central galaxies |
| topic | Galaxy evolution Galaxy dark matter halos Star formation |
| url | https://doi.org/10.3847/1538-4357/ad036b |
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