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dc.contributor.authorOrtolani, Sergiopt_BR
dc.contributor.authorBica, Eduardo Luiz Damianipt_BR
dc.contributor.authorBarbuy, Beatrizpt_BR
dc.date.accessioned2014-12-11T02:15:42Zpt_BR
dc.date.issued2003pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/108029pt_BR
dc.description.abstractColour-Magnitude Diagrams are presented for the globular clusters NGC 6325 and NGC 6355. These clusters are embedded in crowded bulge fields. Both clusters are concentrated and have blue Horizontal Branches, and NGC 6325 shows a blue tail. We derive a reddening E(B−V) 0:95 and a distance from the Sun d 6:9 kpc for NGC 6325, and E(B−V) 0:78 and d 8:8 kpc for NGC 6355. They are both at 1 kpc from the Galactic center, above the plane. The metallicity has been estimated based on red giant branch morphology, being consistent with an intermediate metallicity of [Fe=H] −1:3 for both clusters, at the lower end of the metallicity distribution of bulge field stars. They add to the list of blue Horizontal Branch clusters with intermediate metallicities within the bulge volume.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and astrophysics. Berlin. Vol. 402, no. 2 (May 2003), p. 565-569pt_BR
dc.rightsOpen Accessen
dc.subjectAstronomiapt_BR
dc.subjectgalaxy: clusters: individual: NGC 6325, NGC 6355en
dc.subjectStars: Hertzsprung-Russell (HR) and C-M diagramsen
dc.titleB, V and I photometry of the intermediate metallicity bulge globular clusters NGC 6325 and NGC 6355pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000383590pt_BR
dc.type.originEstrangeiropt_BR


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