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Metallicities of Young Populous Clusters in the Magellanic Clouds

Published online by Cambridge University Press:  04 August 2017

B. Nelles  and
T. Richtler
B. Nelles
Affiliation:
Observatorium Hoher List der Universitätssternwarte Bonn D-5568 Daun, Fed. Rep. Germany
T. Richtler
Affiliation:
Observatorium Hoher List der Universitätssternwarte Bonn D-5568 Daun, Fed. Rep. Germany

Extract

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We present metallicities for the young LMC clusters NGC 1818, 1866 2157, 2136 and 2214. This sample is increased by taking over additional values from literature, so for NGC 1850, 1994, 2004, 2100 from the list of Hodge (1981). The intention is to compare these values with metallicities found in a field population of comparable age. Such a population may be represented by bright Cepheids, for which metallicities based on Washington photometry (Harris 1983) are available. The only young SMC cluster, for which we could estimate a metallicity, is NGC 330. Therefore, a comparison with SMC Cepheids, whose metallicities are also quoted by Harris (1981), can lead to uncertain statements only, until further observations of young SMC clusters will have been made.

Type
Magellanic Cloud Clusters
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 33 - 34
Copyright
Copyright © Reidel 1984 

References

Canterna, R. et al.: 1982, Astrophys. J. 258, 612 Google Scholar
Harris, H.: 1981, Astron. J. 86, 1192 CrossRefGoogle Scholar
Harris, H.: 1983, Astron. J. 88, 507 Google Scholar
Hodge, P.: 1981, in “Astrophysical Parameters for Globular Clusters” IAU Coll.68, eds. Davis Philip, A.G. and Hayes, D.S., L. Davis Press Inc., Schenectady, p. 205 Google Scholar