Blue magellanic clusters : near-infrared spectral evolution
Autor(a) principal: | |
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Data de Publicação: | 1990 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/98028 |
Resumo: | We present new integrated spectra in the range 5600-10000 Å for 28 LMC and 3 SMC young star clusters. We measure the equivalent widths (W) of prominent features and the continuum distribution. The analysis, supplemented by 8 additional LMC clusters from our previous studies, indicates that the red supergiant phase is indeed very time-peaked, occuring from 7 to 12 Myr. In addition to the previous case of NGC 2004, we find that NGC 1805, NGC 1994, NGC 2002, NGC 2098 and NGC 2100 as well as NGC 2011 to a lesser extent, are undergoing this phase. The red supergiant phase is clearly denoted by strong TiO bands and Ca II triplet as well as a flat continuum or in extreme cases a continuum with positive slope for λ> 6000 Å. In the SMC clusters, the molecular bands are weak, owing to metal deficiency, but we can show nevertheless that NGC 299 clearly belongs to the red supergiant phase as demonstrated by its spectral slope and enhanced Ca II. We also find new evidence of another red phase at t ≈ 100 Myr, possibly produced by AGB stars, in which the clusters NGC 2031 and NGC 2134 exhibit strong molecular bands like NGC 1866, a previously known case. Clusters between 10 and 50 Myr have strong Hα emission arising from Be stars, a phenomenon which occurs also in Galactic open clusters. From the LMC data set, it has been possible to identify 8 stages in the cluster spectral evolution from 5 to 500 Myr. We derive the corresponding average spectra which shall be useful for population synthesis of galaxies in which recent bursts of star formation have occurred. |
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Bica, Eduardo Luiz DamianiAlloin, Danielle MarieSantos Junior, Joao Francisco Coelho dos2014-07-18T02:04:08Z19900004-6361http://hdl.handle.net/10183/98028000015261We present new integrated spectra in the range 5600-10000 Å for 28 LMC and 3 SMC young star clusters. We measure the equivalent widths (W) of prominent features and the continuum distribution. The analysis, supplemented by 8 additional LMC clusters from our previous studies, indicates that the red supergiant phase is indeed very time-peaked, occuring from 7 to 12 Myr. In addition to the previous case of NGC 2004, we find that NGC 1805, NGC 1994, NGC 2002, NGC 2098 and NGC 2100 as well as NGC 2011 to a lesser extent, are undergoing this phase. The red supergiant phase is clearly denoted by strong TiO bands and Ca II triplet as well as a flat continuum or in extreme cases a continuum with positive slope for λ> 6000 Å. In the SMC clusters, the molecular bands are weak, owing to metal deficiency, but we can show nevertheless that NGC 299 clearly belongs to the red supergiant phase as demonstrated by its spectral slope and enhanced Ca II. We also find new evidence of another red phase at t ≈ 100 Myr, possibly produced by AGB stars, in which the clusters NGC 2031 and NGC 2134 exhibit strong molecular bands like NGC 1866, a previously known case. Clusters between 10 and 50 Myr have strong Hα emission arising from Be stars, a phenomenon which occurs also in Galactic open clusters. From the LMC data set, it has been possible to identify 8 stages in the cluster spectral evolution from 5 to 500 Myr. We derive the corresponding average spectra which shall be useful for population synthesis of galaxies in which recent bursts of star formation have occurred.application/pdfengAstronomy and Astrophysics. Berlin. Vol. 235, no. 1/2 (Aug. 1990), p. 103-113Aglomerados estelares e associacoesNuvens de magalhaesEvolucao estelarAstrofísicaStar clustersMagellanic CloudsRed supergiantStellar evolutionSpectral evolutionBlue magellanic clusters : near-infrared spectral evolutionEstrangeiroinfo: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:UFRGSORIGINAL000015261.pdf000015261.pdfTexto completo (inglês)application/pdf382583http://www.lume.ufrgs.br/bitstream/10183/98028/1/000015261.pdf6bcaecf456b21d591127b59b42fdfbb4MD51TEXT000015261.pdf.txt000015261.pdf.txtExtracted Texttext/plain5699http://www.lume.ufrgs.br/bitstream/10183/98028/2/000015261.pdf.txt2c8743b8c1b0cc2966aa6a06293b56e6MD52THUMBNAIL000015261.pdf.jpg000015261.pdf.jpgGenerated Thumbnailimage/jpeg2179http://www.lume.ufrgs.br/bitstream/10183/98028/3/000015261.pdf.jpga22720f1910ac2d61e34811d2302f942MD5310183/980282024-04-14 06:46:08.879247oai:www.lume.ufrgs.br:10183/98028Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-14T09:46:08Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Blue magellanic clusters : near-infrared spectral evolution |
title |
Blue magellanic clusters : near-infrared spectral evolution |
spellingShingle |
Blue magellanic clusters : near-infrared spectral evolution Bica, Eduardo Luiz Damiani Aglomerados estelares e associacoes Nuvens de magalhaes Evolucao estelar Astrofísica Star clusters Magellanic Clouds Red supergiant Stellar evolution Spectral evolution |
title_short |
Blue magellanic clusters : near-infrared spectral evolution |
title_full |
Blue magellanic clusters : near-infrared spectral evolution |
title_fullStr |
Blue magellanic clusters : near-infrared spectral evolution |
title_full_unstemmed |
Blue magellanic clusters : near-infrared spectral evolution |
title_sort |
Blue magellanic clusters : near-infrared spectral evolution |
author |
Bica, Eduardo Luiz Damiani |
author_facet |
Bica, Eduardo Luiz Damiani Alloin, Danielle Marie Santos Junior, Joao Francisco Coelho dos |
author_role |
author |
author2 |
Alloin, Danielle Marie Santos Junior, Joao Francisco Coelho dos |
author2_role |
author author |
dc.contributor.author.fl_str_mv |
Bica, Eduardo Luiz Damiani Alloin, Danielle Marie Santos Junior, Joao Francisco Coelho dos |
dc.subject.por.fl_str_mv |
Aglomerados estelares e associacoes Nuvens de magalhaes Evolucao estelar Astrofísica |
topic |
Aglomerados estelares e associacoes Nuvens de magalhaes Evolucao estelar Astrofísica Star clusters Magellanic Clouds Red supergiant Stellar evolution Spectral evolution |
dc.subject.eng.fl_str_mv |
Star clusters Magellanic Clouds Red supergiant Stellar evolution Spectral evolution |
description |
We present new integrated spectra in the range 5600-10000 Å for 28 LMC and 3 SMC young star clusters. We measure the equivalent widths (W) of prominent features and the continuum distribution. The analysis, supplemented by 8 additional LMC clusters from our previous studies, indicates that the red supergiant phase is indeed very time-peaked, occuring from 7 to 12 Myr. In addition to the previous case of NGC 2004, we find that NGC 1805, NGC 1994, NGC 2002, NGC 2098 and NGC 2100 as well as NGC 2011 to a lesser extent, are undergoing this phase. The red supergiant phase is clearly denoted by strong TiO bands and Ca II triplet as well as a flat continuum or in extreme cases a continuum with positive slope for λ> 6000 Å. In the SMC clusters, the molecular bands are weak, owing to metal deficiency, but we can show nevertheless that NGC 299 clearly belongs to the red supergiant phase as demonstrated by its spectral slope and enhanced Ca II. We also find new evidence of another red phase at t ≈ 100 Myr, possibly produced by AGB stars, in which the clusters NGC 2031 and NGC 2134 exhibit strong molecular bands like NGC 1866, a previously known case. Clusters between 10 and 50 Myr have strong Hα emission arising from Be stars, a phenomenon which occurs also in Galactic open clusters. From the LMC data set, it has been possible to identify 8 stages in the cluster spectral evolution from 5 to 500 Myr. We derive the corresponding average spectra which shall be useful for population synthesis of galaxies in which recent bursts of star formation have occurred. |
publishDate |
1990 |
dc.date.issued.fl_str_mv |
1990 |
dc.date.accessioned.fl_str_mv |
2014-07-18T02:04:08Z |
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 |
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publishedVersion |
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http://hdl.handle.net/10183/98028 |
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0004-6361 |
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000015261 |
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url |
http://hdl.handle.net/10183/98028 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and Astrophysics. Berlin. Vol. 235, no. 1/2 (Aug. 1990), p. 103-113 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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application/pdf |
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