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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/64308
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dc.creatorMateus de Souza Angelopt_BR
dc.creatorJoão Francisco Coelho dos Santos Juniorpt_BR
dc.creatorWagner José Corradi Barbosapt_BR
dc.creatorFrancisco Ferreira de Souza Maiapt_BR
dc.creatorAndrés Eduardo Piattipt_BR
dc.date.accessioned2024-02-20T13:15:15Z-
dc.date.available2024-02-20T13:15:15Z-
dc.date.issued2017-
dc.citation.volume17pt_BR
dc.citation.issue1pt_BR
dc.citation.spage4-1pt_BR
dc.citation.epage4-24pt_BR
dc.identifier.doihttps://doi.org/10.1088/1674-4527/17/1/4pt_BR
dc.identifier.issn1674-4527pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/64308-
dc.description.resumoGalactic open clusters (OCs) that survive the early gas-expulsion phase are gradually de- stroyed over time by the action of disruptive dynamical processes. Their final evolutionary stages are characterized by a poorly populated concentration of stars called an open cluster remnant (OCR). This study is devoted to assessing the real physical nature of the OCR candidate NGC 7193. GMOS/Gemini spectroscopy of 53 stars in the inner target region were obtained to derive radial velocities and at- mospheric parameters. We also employed photometric and proper motion data. The analysis method consists of the following steps: (i) analysis of the statistical resemblance between the cluster and a set of field samples with respect to the sequences defined in color-magnitude diagrams (CMDs); (ii) a 5-dimensional iterative exclusion routine was employed to identify outliers from kinematical and positional data; (iii) isochrone fitting to the Ks × (J − Ks) CMD of the remaining stars and the dispersion of spectral types along empirical sequences in the (J − H) × (H − Ks) diagram were checked. A group of stars was identified for which the mean heliocentric distance is compatible with that obtained via isochrone fitting and whose metallicities are compatible with each other. Fifteen of the member stars observed spectroscopically were identified together with another 19 probable members. Our results indicate that NGC 7193 is a genuine OCR, of a once very populous OC, for which the following parameters were derived: d = 501±46 pc, t = 2.5±1.2 Gyr, 〈[Fe/H]〉 = −0.17±0.23 and E(B−V ) = 0.05±0.05. Its luminosity and mass functions show depletion of low mass stars, confirming the OCR is in a dynamically evolved state.pt_BR
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológicopt_BR
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Geraispt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofResearch in Astronomy and Astrophysics-
dc.rightsAcesso Abertopt_BR
dc.subjectOpen cluster remnantspt_BR
dc.subjectGalactic open clusterspt_BR
dc.subject.otherAglomerados galáticospt_BR
dc.subject.otherEstrelaspt_BR
dc.titleInvestigation of galactic open cluster remnants: the case of NGC 7193pt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://iopscience.iop.org/article/10.1088/1674-4527/17/1/4pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-6138-0674pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5150-5282pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2569-4032pt_BR
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