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W UMa-type systems in globular clusters

Published online by Cambridge University Press:  18 January 2010

Lifang Li ,
Fenghui Zhang  and
Zhanwen Han
Lifang Li
Affiliation:
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan Province, 650011, P. R. China email: llf@ynao.ac.cn
Fenghui Zhang
Affiliation:
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan Province, 650011, P. R. China email: llf@ynao.ac.cn
Zhanwen Han
Affiliation:
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan Province, 650011, P. R. China email: llf@ynao.ac.cn
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Abstract

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W UMa systems can be found everywhere in the Galaxy. They can be used as a distance tracer. Therefore, W UMa systems are very important to investigate the structure of the Galaxy. The distance to W UMa systems in globular clusters (GCs) is determined using a period–color–luminosity relation. It is found that the mean distance (ra) of W UMa systems is consistent with their host cluster distances (rGC) deduced from their intrinsic distance moduli if rGC ≤ 10 kpc. There is a significant difference between ra and rGC for rGC ≥ 10 kpc. We discuss the reasons causing this deviation.

Keywords

binaries: eclipsingglobular clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 451 - 453
Copyright
Copyright © International Astronomical Union 2010

References

Kaluzny, J., Olech, A., & Stanek, K. Z. 2001, AJ, 121, 1533CrossRefGoogle Scholar
Kaluzny, J. & Thompson, I. B. 2003, AJ, 125, 2534CrossRefGoogle Scholar
Kaluzny, J., Thompson, I. B., Krzeminski, W., & Schwarzenberg–Czerny, A. 2006, MNRAS, 365, 548CrossRefGoogle Scholar
Layden, A. C. & Sarajedini, A. 2003, AJ, 125, 208CrossRefGoogle Scholar
Mazur, B., Krzeminski, W., & Thompson, I. B. 2003, MNRAS, 340, 1205CrossRefGoogle Scholar
Park, N. K. & Nemec, J. M. 2000, AJ, 119, 1803CrossRefGoogle Scholar
Pritzl, B. J., Smith, H. A., Catelan, M., & Sweigart, A. V. 2001, AJ, 122, 2600CrossRefGoogle Scholar
Pritzl, B. J., Smith, H.A., Catelan, M., & Sweigart, A. V. 2002, AJ, 124, 949CrossRefGoogle Scholar
Rucinski, S. M. 1998, AJ, 116, 2998CrossRefGoogle Scholar
Rucinski, S. M. 2000, AJ, 120, 319CrossRefGoogle Scholar
Rucinski, S. M. 2004, NewAR, 48, 703CrossRefGoogle Scholar
von Braun, K. & Mateo, M. 2001, AJ, 121, 1522CrossRefGoogle Scholar
von Braun, K. & Mateo, M. 2002, AJ, 123, 279CrossRefGoogle Scholar
von Braun, K., Mateo, M., Chiboucas, K., Athey, A., & Hurley–Keller, D. 2002, AJ, 124, 2067CrossRefGoogle Scholar