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Title:
The Globular Cluster NGC 5286. I. A New CCD BV Color-Magnitude Diagram
Authors:
Zorotovic, M.; Catelan, M.; Zoccali, M.; Pritzl, B. J.; Smith, H. A.; Stephens, A. W.; Contreras, R.; Escobar, M. E.
Affiliation:
AA(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile ), AB(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile ), AC(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile ), AD(Department of Physics and Astronomy, University of Wisconsin Oshkosh, Oshkosh, WI 54901, USA ), AE(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA ), AF(Gemini Observatory, 670 N. Aóhoku Place, Hilo, HI 96720, USA ), AG(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile ; INAF, Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy; ), AH(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile )
Publication:
The Astronomical Journal, Volume 137, Issue 1, pp. 257-265 (2009). (AJ Homepage)
Publication Date:
01/2009
Origin:
IOP
AJ Keywords:
galaxies: dwarf, galaxies: star clusters, globular clusters: individual: NGC 5286 NGC 5272, Hertzsprung-Russell diagram, stars: variables: other
DOI:
10.1088/0004-6256/137/1/257
Bibliographic Code:
2009AJ....137..257Z

Abstract

We present BV photometry of the Galactic globular cluster NGC 5286, based on 128 V frames and 133 B frames, and covering the entire face of the cluster. Our photometry reaches almost two magnitudes below the turn-off level, and is accordingly suitable for age analysis. Field stars were removed statistically from the cluster's color-magnitude diagram (CMD), and a differential reddening correction applied, thus allowing a precise ridgeline to be calculated. Using the latter, a metallicity of [Fe/H] = -1.70 ± 0.05 in the Zinn & West scale, and [Fe/H] = -1.47 ± 0.02 in the Carretta & Gratton scale, was derived on the basis of several parameters measured from the red giant branch, in good agreement with the value provided in the Harris catalog. Comparing the NGC 5286 CMD with the latest photometry for M3 by P. B. Stetson, and using VandenBerg isochrones for a suitable chemical composition, we find evidence that NGC 5286 is around 1.7 ± 0.9 Gyr older than M3. This goes in the right sense to help account for the blue horizontal branch of NGC 5286, for which we provide a measurement of several morphological indicators. If NGC 5286 is a bona fide member of the Canis Major dwarf spheroidal galaxy, as previously suggested, our results imply that the latter's oldest components may be at least as old as the oldest Milky Way globular clusters.

Based on observations obtained with the 1.3 m Warsaw telescope at the Las Campanas Observatory, Chile.

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