Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition
Autor(a) principal: | |
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Data de Publicação: | 1992 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/98350 |
Resumo: | The star clusters G 158 and G 177, located at projected distances smaller than 1.5 kpc from the semi-stellar nucleus of M 31, show spectra extreme in absorption-line strengths, comparable to those from the nuclei of giant ellipticals or from the M 31 nucleus itself. A synthesis has been performed of the integrated spectrum of the Galactic globular cluster 47 Tucanae ([Fe/H]= –0.7) with a solar neighbourhood stellar library: as expected, lines of elements like Mg and Fe are stronger in the solar metallicity model. In turn, 47 Tuc presents a blue-violet blanketing excess which, from a detailed study of the spectral residuais (47 Tuc-model) using laboratory molecular patterns, was found to arise from molecules containing C, N and O. In this Research Note we discuss, at a much higher metallicity level, a very similar blanketing excess observed in G 177 with respect to G 158. We suggest that G 177 is an inner bulge cluster, whereas G 158 is an inner disc one, in analogy with the difference found between the halo cluster 47 Tuc and the model which simulates an old cluster with disc stars. In this scenario the [O/Fe] overabundance, known to exist in metal poor Galactic halo stars as compared to the disc, would persist through the bulge and inner bulge. The inner disc stars might have in common with solar neighbourhood ones the solar CNO/Fe ratio. |
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Bica, Eduardo Luiz DamianiJablonka, PascaleSantos Junior, Joao Francisco Coelho dosAlloin, Danielle MarieDottori, Horacio Alberto2014-07-22T02:03:34Z19920004-6361http://hdl.handle.net/10183/98350000055979The star clusters G 158 and G 177, located at projected distances smaller than 1.5 kpc from the semi-stellar nucleus of M 31, show spectra extreme in absorption-line strengths, comparable to those from the nuclei of giant ellipticals or from the M 31 nucleus itself. A synthesis has been performed of the integrated spectrum of the Galactic globular cluster 47 Tucanae ([Fe/H]= –0.7) with a solar neighbourhood stellar library: as expected, lines of elements like Mg and Fe are stronger in the solar metallicity model. In turn, 47 Tuc presents a blue-violet blanketing excess which, from a detailed study of the spectral residuais (47 Tuc-model) using laboratory molecular patterns, was found to arise from molecules containing C, N and O. In this Research Note we discuss, at a much higher metallicity level, a very similar blanketing excess observed in G 177 with respect to G 158. We suggest that G 177 is an inner bulge cluster, whereas G 158 is an inner disc one, in analogy with the difference found between the halo cluster 47 Tuc and the model which simulates an old cluster with disc stars. In this scenario the [O/Fe] overabundance, known to exist in metal poor Galactic halo stars as compared to the disc, would persist through the bulge and inner bulge. The inner disc stars might have in common with solar neighbourhood ones the solar CNO/Fe ratio.application/pdfengAstronomy and Astrophysics. Berlin. Vol. 260, no. 1/2 (July 1992), p. 109-111AstrofísicaAstronomia e astrofisicaAglomerados de galaxiasAglomerados estelares e associacoesMetalicidadeHalosAbundanciaAglomerado globular 47 TucGalaxias elipticasGaláxiasGalaxies: individual M 31Clusters: globularGalaxy: bulgeGalaxy: discGalaxies: stellar content ofSpectroscopyStars: abundancesSuper metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transitionEstrangeiroinfo: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:UFRGSORIGINAL000055979.pdf000055979.pdfTexto completo (inglês)application/pdf348880http://www.lume.ufrgs.br/bitstream/10183/98350/1/000055979.pdff3513a1261600a949a525f22232a743dMD51TEXT000055979.pdf.txt000055979.pdf.txtExtracted Texttext/plain12033http://www.lume.ufrgs.br/bitstream/10183/98350/2/000055979.pdf.txtfbb01614a67d94851f065e154eea2450MD52THUMBNAIL000055979.pdf.jpg000055979.pdf.jpgGenerated Thumbnailimage/jpeg2104http://www.lume.ufrgs.br/bitstream/10183/98350/3/000055979.pdf.jpga8a5cbf8e8eac1c18645d30739cdbb50MD5310183/983502024-04-14 06:46:49.765594oai:www.lume.ufrgs.br:10183/98350Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-14T09:46:49Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
title |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
spellingShingle |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition Bica, Eduardo Luiz Damiani Astrofísica Astronomia e astrofisica Aglomerados de galaxias Aglomerados estelares e associacoes Metalicidade Halos Abundancia Aglomerado globular 47 Tuc Galaxias elipticas Galáxias Galaxies: individual M 31 Clusters: globular Galaxy: bulge Galaxy: disc Galaxies: stellar content of Spectroscopy Stars: abundances |
title_short |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
title_full |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
title_fullStr |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
title_full_unstemmed |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
title_sort |
Super metal-rich clusters g158 and g177 in m31 : clues on the inner bulge/disc transition |
author |
Bica, Eduardo Luiz Damiani |
author_facet |
Bica, Eduardo Luiz Damiani Jablonka, Pascale Santos Junior, Joao Francisco Coelho dos Alloin, Danielle Marie Dottori, Horacio Alberto |
author_role |
author |
author2 |
Jablonka, Pascale Santos Junior, Joao Francisco Coelho dos Alloin, Danielle Marie Dottori, Horacio Alberto |
author2_role |
author author author author |
dc.contributor.author.fl_str_mv |
Bica, Eduardo Luiz Damiani Jablonka, Pascale Santos Junior, Joao Francisco Coelho dos Alloin, Danielle Marie Dottori, Horacio Alberto |
dc.subject.por.fl_str_mv |
Astrofísica Astronomia e astrofisica Aglomerados de galaxias Aglomerados estelares e associacoes Metalicidade Halos Abundancia Aglomerado globular 47 Tuc Galaxias elipticas Galáxias |
topic |
Astrofísica Astronomia e astrofisica Aglomerados de galaxias Aglomerados estelares e associacoes Metalicidade Halos Abundancia Aglomerado globular 47 Tuc Galaxias elipticas Galáxias Galaxies: individual M 31 Clusters: globular Galaxy: bulge Galaxy: disc Galaxies: stellar content of Spectroscopy Stars: abundances |
dc.subject.eng.fl_str_mv |
Galaxies: individual M 31 Clusters: globular Galaxy: bulge Galaxy: disc Galaxies: stellar content of Spectroscopy Stars: abundances |
description |
The star clusters G 158 and G 177, located at projected distances smaller than 1.5 kpc from the semi-stellar nucleus of M 31, show spectra extreme in absorption-line strengths, comparable to those from the nuclei of giant ellipticals or from the M 31 nucleus itself. A synthesis has been performed of the integrated spectrum of the Galactic globular cluster 47 Tucanae ([Fe/H]= –0.7) with a solar neighbourhood stellar library: as expected, lines of elements like Mg and Fe are stronger in the solar metallicity model. In turn, 47 Tuc presents a blue-violet blanketing excess which, from a detailed study of the spectral residuais (47 Tuc-model) using laboratory molecular patterns, was found to arise from molecules containing C, N and O. In this Research Note we discuss, at a much higher metallicity level, a very similar blanketing excess observed in G 177 with respect to G 158. We suggest that G 177 is an inner bulge cluster, whereas G 158 is an inner disc one, in analogy with the difference found between the halo cluster 47 Tuc and the model which simulates an old cluster with disc stars. In this scenario the [O/Fe] overabundance, known to exist in metal poor Galactic halo stars as compared to the disc, would persist through the bulge and inner bulge. The inner disc stars might have in common with solar neighbourhood ones the solar CNO/Fe ratio. |
publishDate |
1992 |
dc.date.issued.fl_str_mv |
1992 |
dc.date.accessioned.fl_str_mv |
2014-07-22T02:03:34Z |
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/10183/98350 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-6361 |
dc.identifier.nrb.pt_BR.fl_str_mv |
000055979 |
identifier_str_mv |
0004-6361 000055979 |
url |
http://hdl.handle.net/10183/98350 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and Astrophysics. Berlin. Vol. 260, no. 1/2 (July 1992), p. 109-111 |
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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