On the Transition of the Galaxy Quenching Mode at 0.5 < z < 1 in CANDELS
文献类型:期刊论文
作者 | Liu, F. S.4,5,6; Jia, Meng4; Yesuf, Hassen M.5,6; Faber, S. M.5,6; Koo, David C.5,6; Guo, Yicheng7; Bell, Eric F.1; Jiang, Dongfei4; Wang, Weichen2; Koekemoer, Anton M.3 |
刊名 | ASTROPHYSICAL JOURNAL |
出版日期 | 2018-06-10 |
卷号 | 860期号:1页码:16 |
ISSN号 | 0004-637X |
关键词 | galaxies: high-redshift galaxies: photometry galaxies: star formation |
DOI | 10.3847/1538-4357/aac20d |
英文摘要 | We investigate the galaxy quenching process at intermediate redshift using a sample of similar to 4400 galaxies with M-* >10(9) M-circle dot between redshift 0.5 and 1.0 in all five CANDELS fields. We divide this sample, using the integrated specific star formation rate (sSFR), into four subgroups: star-forming galaxies (SFGs) above and below the ridge of the star-forming main sequence (SFMS), transition galaxies and quiescent galaxies. We study their UVI (U -V versus V-I) color gradients to infer their sSFR gradients out to twice effective radii. We show that on average both star-forming and transition galaxies at all masses are not fully quenched at any radii, whereas quiescent galaxies are fully quenched at all radii. We find that at low masses (M-* = 10(9) - 10(10) M-circle dot) SFGs both above and below the SFMS ridge generally have flat sSFR profiles, whereas the transition galaxies at the same masses generally have sSFRs that are more suppressed in their outskirts. In contrast, at high masses (M-* > 10(10.5) M-circle dot), SFGs above and below the SFMS ridge and transition galaxies generally have varying degrees of more centrally suppressed sSFRs relative to their outskirts. These findings indicate that at z similar to 0.5-1.0 the main galaxy quenching mode depends on its already formed stellar mass, exhibiting a transition from "the outside-in" at M*<= 10(10) M-circle dot to "the inside-out" at M-* > 10(10.5) M-circle dot. In other words, our findings support that internal processes dominate the quenching of massive galaxies, whereas external processes dominate the quenching of low-mass galaxies. |
WOS关键词 | STAR-FORMING GALAXIES ; CATALOGS SOURCE IDENTIFICATION ; QUIESCENT GALAXIES ; MAIN-SEQUENCE ; MASS FUNCTION ; EVOLUTION ; STELLAR ; PHOTOMETRY ; ENVIRONMENT ; COMPACTION |
资助项目 | NSF grants of China[11573017] ; NSF grants of China[11733006] ; NASA through a grant from the STScI[HST-GO-12060] ; NASA[NAS5-26555] ; 3D-HST Treasury Program[GO 12177] ; 3D-HST Treasury Program[12328] ; US NSF[AST-16-15730] ; Spanish Government MINECO[AYA2015-70815-ERC] ; Spanish Government MINECO[AYA2015-63650-P] |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000435102000010 |
资助机构 | NSF grants of China ; NSF grants of China ; NASA through a grant from the STScI ; NASA through a grant from the STScI ; NASA ; NASA ; 3D-HST Treasury Program ; 3D-HST Treasury Program ; US NSF ; US NSF ; Spanish Government MINECO ; Spanish Government MINECO ; NSF grants of China ; NSF grants of China ; NASA through a grant from the STScI ; NASA through a grant from the STScI ; NASA ; NASA ; 3D-HST Treasury Program ; 3D-HST Treasury Program ; US NSF ; US NSF ; Spanish Government MINECO ; Spanish Government MINECO ; NSF grants of China ; NSF grants of China ; NASA through a grant from the STScI ; NASA through a grant from the STScI ; NASA ; NASA ; 3D-HST Treasury Program ; 3D-HST Treasury Program ; US NSF ; US NSF ; Spanish Government MINECO ; Spanish Government MINECO ; NSF grants of China ; NSF grants of China ; NASA through a grant from the STScI ; NASA through a grant from the STScI ; NASA ; NASA ; 3D-HST Treasury Program ; 3D-HST Treasury Program ; US NSF ; US NSF ; Spanish Government MINECO ; Spanish Government MINECO |
源URL | [http://ir.bao.ac.cn/handle/114a11/21800] |
专题 | 中国科学院国家天文台 |
通讯作者 | Liu, F. S. |
作者单位 | 1.Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA 2.Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA 3.Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA 4.Shenyang Normal Univ, Coll Phys Sci & Technol, Shenyang 110034, Liaoning, Peoples R China 5.Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA 6.Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA 7.Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA 8.Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia 9.Univ Paris Diderot, Univ PSL, Observ Paris, Sorbonne Univ,CNRS,LERMA, Paris, France 10.Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China |
推荐引用方式 GB/T 7714 | Liu, F. S.,Jia, Meng,Yesuf, Hassen M.,et al. On the Transition of the Galaxy Quenching Mode at 0.5 < z < 1 in CANDELS[J]. ASTROPHYSICAL JOURNAL,2018,860(1):16. |
APA | Liu, F. S..,Jia, Meng.,Yesuf, Hassen M..,Faber, S. M..,Koo, David C..,...&Liu, Lu.(2018).On the Transition of the Galaxy Quenching Mode at 0.5 < z < 1 in CANDELS.ASTROPHYSICAL JOURNAL,860(1),16. |
MLA | Liu, F. S.,et al."On the Transition of the Galaxy Quenching Mode at 0.5 < z < 1 in CANDELS".ASTROPHYSICAL JOURNAL 860.1(2018):16. |
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来源:国家天文台
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