The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10{sup 6}L{sub ⊙} and Comparisons with Galaxy Formation Models
- National Research Council of Canada, Herzberg Astronomy and Astrophysics Program, 5071 West Saanich Road, Victoria, BC, V9E 2E7 (Canada)
- Department of Astronomy, Peking University, Beijing 100871 (China)
- Center for Astronomy and Astrophysics, Department of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai 200240 (China)
- Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago (Chile)
- AIM Paris Saclay, CNRS/INSU, CEA/Irfu, Université Paris Diderot, Orme des Merisiers, F-91191 Gif sur Yvette Cedex (France)
- LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, F-75014 Paris (France)
- Aix Marseille Université, CNRS, Laboratoire d’Astrophysique de Marseille UMR 7326, F-13388, Marseille (France)
- INAF Osservatorio Astr. di Teramo, via Maggini, I-64100, Teramo (Italy)
- Department of Physics, Engineering Physics and Astronomy, Queen’s University, Kingston, ON (Canada)
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 × 10{sup 5} in luminosity, from brightest cluster galaxies to scales overlapping classical satellites of the Milky Way (M{sub g{sup ′}} ∼ −9; M {sub *} ∼ 10{sup 6} M {sub ⊙}), 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{sub g{sup ′}} ≤ −13, around M {sub *} ∼ 4 × 10{sup 7} M {sub ⊙}), 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.
- OSTI ID:
- 22869357
- Journal Information:
- Astrophysical Journal, Vol. 836, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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