Integrated spectral properties of star clusters in the near-ultraviolet
Autor(a) principal: | |
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Data de Publicação: | 1994 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/97462 |
Resumo: | We study integrated spectra of 37 star clusters in the range 3100-4200 Å. The sample includes Galactic globular and open clusters, as well as Magellanic Cloud clusters. Feature equivalent widths (W) and continuum distribution are analyzed as a function of age and metallicity. In particular we discuss the behaviour of the Balmer Jump and of the 4000 Å Break, which are measured by the same continuum ratio C3660 Å / C4020 Å. For ages t < 500 Myr the Balmer Jump is dominant over the 4000 Å Break and for t < 50 Myr it is an excellent age discriminator. The effects of blue Horizontal Branch morphology on globular cluster spectra are also discussed: they increase the Balmer line W, but do not dilute substantially the Near UV metallic features. The present data will provide a means to connect optical to UV integrated star cluster spectra, with im portant applications in stellar population analyses, in particular for distant galaxies at redshift up to 1. |
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Bica, Eduardo Luiz DamianiAlloin, Danielle MarieSchmitt, Henrique Roberto2014-07-11T02:05:16Z19940004-6361http://hdl.handle.net/10183/97462000220136We study integrated spectra of 37 star clusters in the range 3100-4200 Å. The sample includes Galactic globular and open clusters, as well as Magellanic Cloud clusters. Feature equivalent widths (W) and continuum distribution are analyzed as a function of age and metallicity. In particular we discuss the behaviour of the Balmer Jump and of the 4000 Å Break, which are measured by the same continuum ratio C3660 Å / C4020 Å. For ages t < 500 Myr the Balmer Jump is dominant over the 4000 Å Break and for t < 50 Myr it is an excellent age discriminator. The effects of blue Horizontal Branch morphology on globular cluster spectra are also discussed: they increase the Balmer line W, but do not dilute substantially the Near UV metallic features. The present data will provide a means to connect optical to UV integrated star cluster spectra, with im portant applications in stellar population analyses, in particular for distant galaxies at redshift up to 1.application/pdfengAstronomy and astrophysics. Vol. 283, no. 3 (Mar. 1994), p. 805-812Astrofisica extragalaticaAstronomiaAstrofísicaAglomerados estelares e associacoesGlobular clusters - open clustersGalaxies: star clustersMagellanic clouds-ultraviolet: starsGalaxies: evolutionIntegrated spectral properties of star clusters in the near-ultravioletEstrangeiroinfo: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:UFRGSORIGINAL000220136.pdf000220136.pdfTexto completo (inglês)application/pdf234503http://www.lume.ufrgs.br/bitstream/10183/97462/1/000220136.pdfc96e80531535e92104aaf1e71d78bf40MD51TEXT000220136.pdf.txt000220136.pdf.txtExtracted Texttext/plain176http://www.lume.ufrgs.br/bitstream/10183/97462/2/000220136.pdf.txtb2745261fcba4589cafd765f68d6e2ddMD52THUMBNAIL000220136.pdf.jpg000220136.pdf.jpgGenerated Thumbnailimage/jpeg2111http://www.lume.ufrgs.br/bitstream/10183/97462/3/000220136.pdf.jpg15a66b5f51a323e505ac325dd133a007MD5310183/974622024-04-14 06:46:31.175596oai:www.lume.ufrgs.br:10183/97462Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-14T09:46:31Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Integrated spectral properties of star clusters in the near-ultraviolet |
title |
Integrated spectral properties of star clusters in the near-ultraviolet |
spellingShingle |
Integrated spectral properties of star clusters in the near-ultraviolet Bica, Eduardo Luiz Damiani Astrofisica extragalatica Astronomia Astrofísica Aglomerados estelares e associacoes Globular clusters - open clusters Galaxies: star clusters Magellanic clouds-ultraviolet: stars Galaxies: evolution |
title_short |
Integrated spectral properties of star clusters in the near-ultraviolet |
title_full |
Integrated spectral properties of star clusters in the near-ultraviolet |
title_fullStr |
Integrated spectral properties of star clusters in the near-ultraviolet |
title_full_unstemmed |
Integrated spectral properties of star clusters in the near-ultraviolet |
title_sort |
Integrated spectral properties of star clusters in the near-ultraviolet |
author |
Bica, Eduardo Luiz Damiani |
author_facet |
Bica, Eduardo Luiz Damiani Alloin, Danielle Marie Schmitt, Henrique Roberto |
author_role |
author |
author2 |
Alloin, Danielle Marie Schmitt, Henrique Roberto |
author2_role |
author author |
dc.contributor.author.fl_str_mv |
Bica, Eduardo Luiz Damiani Alloin, Danielle Marie Schmitt, Henrique Roberto |
dc.subject.por.fl_str_mv |
Astrofisica extragalatica Astronomia Astrofísica Aglomerados estelares e associacoes |
topic |
Astrofisica extragalatica Astronomia Astrofísica Aglomerados estelares e associacoes Globular clusters - open clusters Galaxies: star clusters Magellanic clouds-ultraviolet: stars Galaxies: evolution |
dc.subject.eng.fl_str_mv |
Globular clusters - open clusters Galaxies: star clusters Magellanic clouds-ultraviolet: stars Galaxies: evolution |
description |
We study integrated spectra of 37 star clusters in the range 3100-4200 Å. The sample includes Galactic globular and open clusters, as well as Magellanic Cloud clusters. Feature equivalent widths (W) and continuum distribution are analyzed as a function of age and metallicity. In particular we discuss the behaviour of the Balmer Jump and of the 4000 Å Break, which are measured by the same continuum ratio C3660 Å / C4020 Å. For ages t < 500 Myr the Balmer Jump is dominant over the 4000 Å Break and for t < 50 Myr it is an excellent age discriminator. The effects of blue Horizontal Branch morphology on globular cluster spectra are also discussed: they increase the Balmer line W, but do not dilute substantially the Near UV metallic features. The present data will provide a means to connect optical to UV integrated star cluster spectra, with im portant applications in stellar population analyses, in particular for distant galaxies at redshift up to 1. |
publishDate |
1994 |
dc.date.issued.fl_str_mv |
1994 |
dc.date.accessioned.fl_str_mv |
2014-07-11T02:05:16Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
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/10183/97462 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-6361 |
dc.identifier.nrb.pt_BR.fl_str_mv |
000220136 |
identifier_str_mv |
0004-6361 000220136 |
url |
http://hdl.handle.net/10183/97462 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and astrophysics. Vol. 283, no. 3 (Mar. 1994), p. 805-812 |
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info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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application/pdf |
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