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dc.contributor.authorBruzual A., G.pt_BR
dc.contributor.authorBarbuy, Beatrizpt_BR
dc.contributor.authorOrtolani, Sergiopt_BR
dc.contributor.authorBica, Eduardo Luiz Damianipt_BR
dc.contributor.authorCuisinier, Francoispt_BR
dc.contributor.authorLejeune, Tribaultpt_BR
dc.contributor.authorSchiavon, Ricardo P.pt_BR
dc.date.accessioned2014-12-04T02:13:44Zpt_BR
dc.date.issued1997pt_BR
dc.identifier.issn0004-6256pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/107733pt_BR
dc.description.abstractWe compare observed color-magnitude diagrams (CMDs) of the three metal-rich bulge globular clusters NGC 6553, NGC 6528, and Terzan 5, and integrated spectral energy distributions (SEDs) of NGC 6528, and 47 Tuc, to theoretical isochrones and model SEDs computed with the code of Bruzual & Charlot (1997, ApJ, in preparation, hereafter BC97). The BC97 models provide the evolution in time of the spectrophotometric properties of simple stellar populations (SSPs) for a wide range of stellar metallicity. These models allow us to compare predictions based on different sets of evolutionary tracks and various choices of the stellar spectral libraries with observational data. We conclude that: (a) At least for solar metallicity models, the serni-empirical flux corrections applied by Lejeune et al. (1997, A&A, in press; 1997, A&A, in preparation) to available grids of synthetic stellar spectra improve the agreement between population model predictions and observations. (b) The adopted reddening and distance moduli for the three clusters seem well deterrnined, since the theoretical isochrones fit quite well the observed CMDs. (c) The overall metallicity of these clusters is close to solar. (d) Based on our CMD and SED models we estimate that the ages of NGC 6553 and NGC 6528 must be ≈ 12±2 Gyr. These are the only two clusters in our sample with main sequence photometry. From the UV-optical SED of 47 Tuc we estimate an age of ≈ 14±2 Gyr. © 1997 American Astronomical Society. [S0004-6256(97)02509-0]en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe Astronomical journal. New York. Vol. 114, no. 4 (Oct. 1997), p. 1531-1538pt_BR
dc.rightsOpen Accessen
dc.subjectEspectros estelarespt_BR
dc.subjectEvolucao estelarpt_BR
dc.subjectComposicao estelarpt_BR
dc.subjectGalaxiapt_BR
dc.subjectAglomerados estelares globularespt_BR
dc.titleMatching stellar population models to bulge globular clusterspt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000152371pt_BR
dc.type.originEstrangeiropt_BR


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