The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ～106 L⊙ and Comparisons with Galaxy Formation Models

doi:10.3847/1538-4357/836/1/120

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	The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ～106 L⊙ and Comparisons with Galaxy Formation Models
	Roediger,Joel C.7; Ferrarese,Laura 7; C?té,Patrick 7; MacArthur,Lauren A.7,8; Sánchez-Janssen,Rúben 7; Blakeslee,John P.7; Peng,Eric W.9,10; Liu,Chengze 11; Munoz,Roberto 12; Cuillandre,Jean-Charles 13
刊名	The Astrophysical Journal
	2017-02-13
卷号	836 期号:1
关键词	galaxies: clusters: individual (Virgo) galaxies: dwarf galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: stellar content
ISSN号	0004-637X
DOI	10.3847/1538-4357/836/1/120
英文摘要	Abstract We use deep optical photometry from the Next Generation Virgo Cluster Survey (NGVS) to investigate the color–magnitude diagram for the galaxies inhabiting the core of this cluster. The sensitivity of the NGVS imaging allows us to continuously probe galaxy colors over a factor of ～2?×?105 in luminosity, from brightest cluster galaxies to scales overlapping classical satellites of the Milky Way ( M g ′ ?～??9; M?～?106 M⊙), within a single environment. Remarkably, we find the first evidence that the red sequence (RS) flattens in all colors at the faint-magnitude end (starting between ?14?≤? M g ′ ?≤??13, around M?～?4?×?107 M⊙), with the slope decreasing to ～60% or less of its value at brighter magnitudes. This could indicate that the stellar populations of faint dwarfs in Virgo’s core share similar characteristics (e.g., constant mean age) over ～3 mag in luminosity, suggesting that these galaxies were quenched coevally, likely via pre-processing in smaller hosts. We also compare our results to galaxy formation models, finding that the RS in model clusters have slopes at intermediate magnitudes that are too shallow, and in the case of semianalytic models, do not reproduce the flattening seen at both extremes (bright/faint) of the Virgo RS. Deficiencies in the chemical evolution of model galaxies likely contribute to the model-data discrepancies at all masses, while overly efficient quenching may also be a factor at dwarf scales. Deep UV and near-IR photometry are required to unambiguously diagnose the cause of the faint-end flattening.
语种	英语
出版者	The American Astronomical Society
WOS记录号	IOP:0004-637X-836-1-120
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/36112]
专题	中国科学院国家天文台
作者单位	1.Observatoire Astronomique, Université de Strasbourg & CNRS UMR 7550, 11 rue de l’Université, F-67000 Strasbourg, France 2.UCO/Lick Observatory, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA 3.Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada 4.Department of Astronomy, Case Western Reserve University, Cleveland, OH 41106, USA 5.Department of Physics and Astronomy, Youngstown State University, Youngstown, OH 44555, USA 6.Department of Physics, Texas Tech University, Box 41051, Lubbock, TX 79409, USA 7.National Research Council of Canada, Herzberg Astronomy and Astrophysics Program, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada; Joel.Roediger@nrc-cnrc.gc.ca 8.Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 9.Department of Astronomy, Peking University, Beijing 100871, China 10.Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
推荐引用方式 GB/T 7714	Roediger,Joel C.,Ferrarese,Laura,C?té,Patrick,等. The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ～106 L⊙ and Comparisons with Galaxy Formation Models[J]. The Astrophysical Journal,2017,836(1).
APA	Roediger,Joel C..,Ferrarese,Laura.,C?té,Patrick.,MacArthur,Lauren A..,Sánchez-Janssen,Rúben.,...&Zhang,Hongxin.(2017).The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ～106 L⊙ and Comparisons with Galaxy Formation Models.The Astrophysical Journal,836(1).
MLA	Roediger,Joel C.,et al."The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ～106 L⊙ and Comparisons with Galaxy Formation Models".The Astrophysical Journal 836.1(2017).