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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.1; Ferrarese,Laura1; C?té,Patrick1; MacArthur,Lauren A.1,2; Sánchez-Janssen,Rúben1; Blakeslee,John P.1; Peng,Eric W.3,4; Liu,Chengze5; Munoz,Roberto6; Cuillandre,Jean-Charles7; Gwyn,Stephen1; Mei,Simona8,9,10; Boissier,Samuel11; Boselli,Alessandro11; Cantiello,Michele12,13; Courteau,Stéphane14; Duc,Pierre-Alain7; Lan?on,Ariane15; Mihos,J. Christopher16; Puzia,Thomas H.6; Taylor,James E.17; Durrell,Patrick R.18; Toloba,Elisa19,20; Guhathakurta,Puragra19; Zhang,Hongxin6,21
2017-02-13
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume836Issue:1
AbstractAbstract 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.
Keywordgalaxies: clusters: individual (Virgo) galaxies: dwarf galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: stellar content
DOI10.3847/1538-4357/836/1/120
Language英语
WOS IDIOP:0004-637X-836-1-120
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/36113
Collection中国科学院国家天文台
Affiliation1.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
2.Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
3.Department of Astronomy, Peking University, Beijing 100871, China
4.Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
5.Center for Astronomy and Astrophysics, Department of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai 200240, China
6.Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicu?a Mackenna 4860, 7820436 Macul, Santiago, Chile
7.AIM Paris Saclay, CNRS/INSU, CEA/Irfu, Université Paris Diderot, Orme des Merisiers, F-91191 Gif sur Yvette Cedex, France
8.LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, F-75014 Paris, France
9.Université Paris Denis Diderot, Université Paris Sorbonne Cité, 75205 Paris Cedex 13, France
10.Jet Propulsion Laboratory, Cahill Center for Astronomy & Astrophysics, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
11.Aix Marseille Université, CNRS, Laboratoire d’Astrophysique de Marseille UMR 7326, F-13388, Marseille, France
12.INAF Osservatorio Astr. di Teramo, via Maggini, I-64100, Teramo, Italy
13.INAF Osservatorio Astr. di Capodimonte, Salita Moiariello, 16, I-80131 Napoli, Italy
14.Department of Physics, Engineering Physics and Astronomy, Queen’s University, Kingston, ON, Canada
15.Observatoire Astronomique, Université de Strasbourg & CNRS UMR 7550, 11 rue de l’Université, F-67000 Strasbourg, France
16.Department of Astronomy, Case Western Reserve University, Cleveland, OH 41106, USA
17.Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada
18.Department of Physics and Astronomy, Youngstown State University, Youngstown, OH 44555, USA
19.UCO/Lick Observatory, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA
20.Department of Physics, Texas Tech University, Box 41051, Lubbock, TX 79409, USA
21.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Recommended Citation
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).
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