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The LMC Globular Cluster Hodge 11 (=SL 868)

Published online by Cambridge University Press:  04 August 2017

L. L. Stryker
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics
J. M. Nemec
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics
J. E. Hesser
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics
R.D. McClure
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics

Extract

The age of the star cluster H11 has been controversial for a number of years. The color-magnitude diagram (CMD) of Walker (1979) to V=21.5 was interpreted as an “…evolved main-sequence, whose termination point corresponds to an age of about 0.6 Gyr, but with a giant branch which is displaced blueward by about Δ (B-V)o=0.4 from the positions of the giant branches of open clusters of similar age in our Galaxy.” On the other hand, the integrated colors are similar to those of metal-poor globular clusters in the Galaxy (Freeman and Gascoigne 1977, and references therein), and “…incompatible with an age of say 0.3 Gyr.” Searle, Wilkinson and Bagnuolo (1980) classify it as Group VII, the oldest group. The system has no RR Lyrae stars (Graham and Nemec 1984).

Type
Magellanic Cloud Clusters
Copyright
Copyright © Reidel 1984 

References

Freeman, K.C. & Gascoigne, S.C.B.: 1977, Proc. Astron. Soc. Aust. 3, p. 136.CrossRefGoogle Scholar
Graham, J.A. & Nemec, J.M.: 1984, this volume, p. 37.Google Scholar
Searle, L., Wilkinson, A. & Bagnuolo, W.: 1980, Ap. J. 239, p. 803.CrossRefGoogle Scholar
Tody, D.: 1980, in SPIE Symp. “Applications of Digital Image Processing to Astronomy”, ed. Elliott, D.A., p. 121.Google Scholar
Walker, M.F.: 1979, Mon. Not. Roy. Ast. Soc. 186, p. 767.CrossRefGoogle Scholar

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