Physical parameters of RR Lyrae stars in the globular cluster NGC 5466: The Oosterhoff dichotomy

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5717

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DC Field	Value	Language
dc.contributor.author	Rojas Lopez, V	-
dc.contributor.author	Arellano Ferro, A	-
dc.contributor.author	Giridhar, S	-
dc.contributor.author	Bramich, D. M	-
dc.date.accessioned	2012-03-01T10:47:39Z	-
dc.date.available	2012-03-01T10:47:39Z	-
dc.date.issued	2006-06	-
dc.identifier.citation	Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias) Vol. 26, pp. 49-49	en
dc.identifier.uri	http://hdl.handle.net/2248/5717	-
dc.description.abstract	The highlights of CCD photometry of RR Lyrae stars in NGC 5466 are presented. The image subtraction method (Bramich et al. 2005) was used. The Fourier light curve decomposition, lead to an average [Fe/H]=-1.88+/-0.3 and a distance of 14.8+/-0.4 kpc for the cluster and to other physical parameters of astrophysical relevance for individual RR Lyrae stars. When a comparison of the mean physical parameters in globular clusters, analysed by the same technique, is performed, clear insights of the stellar evolution on the Horizontal Branch are obtained. The origin of the Oosterhoff dichotomy is clearly of evolutionary nature, being age the determining factor.	en
dc.language.iso	en	en
dc.publisher	Instituto de Astronomía	en
dc.rights	© Instituto de Astronomía	en
dc.title	Physical parameters of RR Lyrae stars in the globular cluster NGC 5466: The Oosterhoff dichotomy	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

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