Ages and metallicities of lmc and smc red clusters through hb and g band photometry

Detalhes bibliográficos
Autor(a) principal: Bica, Eduardo Luiz Damiani
Data de Publicação: 1986
Outros Autores: Dottori, Horacio Alberto, Pastoriza, Miriani Griselda
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UFRGS
Texto Completo: http://hdl.handle.net/10183/98359
Resumo: We present narrow band integrated photometry of the Hβ and G band absorption features for 41 LMC and 10 SMC red star clusters. An age-metallicity calibration is provided for the color-color diagram. We derive SWB types between IV and VII for 23 unclassified clusters and discuss their distribution in the age vs metallicity plane. We study the chemical evolution of the Magellanic Clouds (MC): the LMC presents a steeper chemical enrichment slope. An intrinsic metallicity dispersion is found in the LMC chemical evolution, indicating that the gas has been inhomogeneous at any time, prevailing a local enrichment over a global one. One zone models describe the evolution of both Clouds, being the efficiency of star cluster formation larger in the LMC. The LMC presents a burst of star cluster formation at t = 4.5 10⁹ yr. We also present new B – V data for fainter SMC clusters, providing an essentially complete color histogram for clusters with globular cluster appearance.
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spelling Bica, Eduardo Luiz DamianiDottori, Horacio AlbertoPastoriza, Miriani Griselda2014-07-22T02:03:37Z19860004-6361http://hdl.handle.net/10183/98359000112963We present narrow band integrated photometry of the Hβ and G band absorption features for 41 LMC and 10 SMC red star clusters. An age-metallicity calibration is provided for the color-color diagram. We derive SWB types between IV and VII for 23 unclassified clusters and discuss their distribution in the age vs metallicity plane. We study the chemical evolution of the Magellanic Clouds (MC): the LMC presents a steeper chemical enrichment slope. An intrinsic metallicity dispersion is found in the LMC chemical evolution, indicating that the gas has been inhomogeneous at any time, prevailing a local enrichment over a global one. One zone models describe the evolution of both Clouds, being the efficiency of star cluster formation larger in the LMC. The LMC presents a burst of star cluster formation at t = 4.5 10⁹ yr. We also present new B – V data for fainter SMC clusters, providing an essentially complete color histogram for clusters with globular cluster appearance.application/pdfengAstronomy and Astrophysics. Berlin. Vol. 156, no. 1/2 (Feb. 1986), p. 261-267MetalicidadeAstrofisica extragalaticaNuvens de magalhaesFotometriaMagellanic cloudsRed star clustersAge-metallicity relationshipAges and metallicities of lmc and smc red clusters through hb and g band photometryEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL000112963.pdf000112963.pdfTexto completo (inglês)application/pdf669033http://www.lume.ufrgs.br/bitstream/10183/98359/1/000112963.pdfacb5bef078dbe288d78312de0bbefc7bMD51TEXT000112963.pdf.txt000112963.pdf.txtExtracted Texttext/plain26496http://www.lume.ufrgs.br/bitstream/10183/98359/2/000112963.pdf.txt07057e4920777432837b5364160bbeb4MD52THUMBNAIL000112963.pdf.jpg000112963.pdf.jpgGenerated Thumbnailimage/jpeg2132http://www.lume.ufrgs.br/bitstream/10183/98359/3/000112963.pdf.jpg05abc57e0034bcbaf926bc55cf915830MD5310183/983592024-04-11 06:25:50.826577oai:www.lume.ufrgs.br:10183/98359Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-11T09:25:50Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false
dc.title.pt_BR.fl_str_mv Ages and metallicities of lmc and smc red clusters through hb and g band photometry
title Ages and metallicities of lmc and smc red clusters through hb and g band photometry
spellingShingle Ages and metallicities of lmc and smc red clusters through hb and g band photometry
Bica, Eduardo Luiz Damiani
Metalicidade
Astrofisica extragalatica
Nuvens de magalhaes
Fotometria
Magellanic clouds
Red star clusters
Age-metallicity relationship
title_short Ages and metallicities of lmc and smc red clusters through hb and g band photometry
title_full Ages and metallicities of lmc and smc red clusters through hb and g band photometry
title_fullStr Ages and metallicities of lmc and smc red clusters through hb and g band photometry
title_full_unstemmed Ages and metallicities of lmc and smc red clusters through hb and g band photometry
title_sort Ages and metallicities of lmc and smc red clusters through hb and g band photometry
author Bica, Eduardo Luiz Damiani
author_facet Bica, Eduardo Luiz Damiani
Dottori, Horacio Alberto
Pastoriza, Miriani Griselda
author_role author
author2 Dottori, Horacio Alberto
Pastoriza, Miriani Griselda
author2_role author
author
dc.contributor.author.fl_str_mv Bica, Eduardo Luiz Damiani
Dottori, Horacio Alberto
Pastoriza, Miriani Griselda
dc.subject.por.fl_str_mv Metalicidade
Astrofisica extragalatica
Nuvens de magalhaes
Fotometria
topic Metalicidade
Astrofisica extragalatica
Nuvens de magalhaes
Fotometria
Magellanic clouds
Red star clusters
Age-metallicity relationship
dc.subject.eng.fl_str_mv Magellanic clouds
Red star clusters
Age-metallicity relationship
description We present narrow band integrated photometry of the Hβ and G band absorption features for 41 LMC and 10 SMC red star clusters. An age-metallicity calibration is provided for the color-color diagram. We derive SWB types between IV and VII for 23 unclassified clusters and discuss their distribution in the age vs metallicity plane. We study the chemical evolution of the Magellanic Clouds (MC): the LMC presents a steeper chemical enrichment slope. An intrinsic metallicity dispersion is found in the LMC chemical evolution, indicating that the gas has been inhomogeneous at any time, prevailing a local enrichment over a global one. One zone models describe the evolution of both Clouds, being the efficiency of star cluster formation larger in the LMC. The LMC presents a burst of star cluster formation at t = 4.5 10⁹ yr. We also present new B – V data for fainter SMC clusters, providing an essentially complete color histogram for clusters with globular cluster appearance.
publishDate 1986
dc.date.issued.fl_str_mv 1986
dc.date.accessioned.fl_str_mv 2014-07-22T02:03:37Z
dc.type.driver.fl_str_mv Estrangeiro
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dc.type.status.fl_str_mv info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.uri.fl_str_mv http://hdl.handle.net/10183/98359
dc.identifier.issn.pt_BR.fl_str_mv 0004-6361
dc.identifier.nrb.pt_BR.fl_str_mv 000112963
identifier_str_mv 0004-6361
000112963
url http://hdl.handle.net/10183/98359
dc.language.iso.fl_str_mv eng
language eng
dc.relation.ispartof.pt_BR.fl_str_mv Astronomy and Astrophysics. Berlin. Vol. 156, no. 1/2 (Feb. 1986), p. 261-267
dc.rights.driver.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
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instacron:UFRGS
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institution UFRGS
reponame_str Repositório Institucional da UFRGS
collection Repositório Institucional da UFRGS
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