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Observations of Cepheid Variables in Two LMC Clusters Using EROS 2 Data

Published online by Cambridge University Press:  25 May 2016

V. Ripepi ,
F. Bauer  and
J. P. Beaulieu
V. Ripepi
Affiliation:
Osservatorio Astronomico di Capodimonte (Napoli), Italy
F. Bauer
Affiliation:
College de France, Paris, France
J. P. Beaulieu
Affiliation:
Institut d'Astrophysique de Paris, France

Extract

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It is well known that Cepheid variables are very important distance indicators because of their PL and PLC relations. The distances derived through the quoted relations are affected by well known systematic effects, since, in general, we have a poor knowledge of both reddening and metallicity of the Cepheid sample. Good estimates of the quoted parameters can be achieved if the observed Cepheids are cluster members since, by comparison between cluster CMD and theoretical isochrones we can estimate the cluster reddening, metallicity and age, i.e., the evolving masses for each evolutionary phase. The ideal objects to be searched for Cepheid membership are Magellanic Cloud clusters since they are well populated in the relevant evolutionary phases.

Type
Part 8. Cepheids and Distances
Information
Symposium - International Astronomical Union , Volume 190: New Views of the Magellanic Clouds , 1999 , pp. 559 - 560
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Bauer, , et al. (the EROS collaboration) 1999, A&A, 348, 175 Google Scholar
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Degl'Innocenti, S, Marconi, M. 1998 (private communication) Google Scholar