Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285
Autor(a) principal: | |
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Data de Publicação: | 1995 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/98495 |
Resumo: | We present evidence for a young stellar population component in the early-type member of the E+S galaxy pair AM 0327-285. This young population is consistent with the occurrence of cross-fueling in this interacting system. We used spectroscopy, optical imaging, IRAS data, and stellar population synthesis to study the stellar content in the early-type galaxy. We also attempted to date episodes of star formation in its nuclear region, from population synthesis and basic dynamical considerations. The dominant population is old and metal-rich ([Z/Z]Θ=0.3) while ~ 10% of the flux at 5870 Å arises from a superimposed young stellar population with age <_ 5 x 10⁸ yr. This age is close to several estimates of the characteristic timescale of the interaction, suggesting that the mass influx associated with this star formation occurred as a result of an earlier phase of the interaction and not as a result of the present geometry of the pair. |
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Mello, D.F. deKell, W.C.Sulentic, J.W.Rampazzo, R.Bica, Eduardo Luiz DamianiWhite, R.E.2014-07-24T02:04:18Z19950004-6361http://hdl.handle.net/10183/98495000190601We present evidence for a young stellar population component in the early-type member of the E+S galaxy pair AM 0327-285. This young population is consistent with the occurrence of cross-fueling in this interacting system. We used spectroscopy, optical imaging, IRAS data, and stellar population synthesis to study the stellar content in the early-type galaxy. We also attempted to date episodes of star formation in its nuclear region, from population synthesis and basic dynamical considerations. The dominant population is old and metal-rich ([Z/Z]Θ=0.3) while ~ 10% of the flux at 5870 Å arises from a superimposed young stellar population with age <_ 5 x 10⁸ yr. This age is close to several estimates of the characteristic timescale of the interaction, suggesting that the mass influx associated with this star formation occurred as a result of an earlier phase of the interaction and not as a result of the present geometry of the pair.application/pdfengAstronomy and Astrophysics. Berlin. Vol. 297, no. 2 (May 1995), p. 331-337Astrofisica extragalaticaGalaxias elipticasPopulacoes estelaresFormacao de estrelasGalaxies: ellipticalGalaxies: stellar contentGalaxies: interactionsGalaxies: AM 0327-285Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285Estrangeiroinfo: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:UFRGSORIGINAL000190601.pdf000190601.pdfTexto completo (inglês)application/pdf4111473http://www.lume.ufrgs.br/bitstream/10183/98495/1/000190601.pdfd1128dca11bf220042e4b1114ffa5b33MD51TEXT000190601.pdf.txt000190601.pdf.txtExtracted Texttext/plain30231http://www.lume.ufrgs.br/bitstream/10183/98495/2/000190601.pdf.txtf983f5f02e5fc3961c47e003faf9dc62MD52THUMBNAIL000190601.pdf.jpg000190601.pdf.jpgGenerated Thumbnailimage/jpeg2168http://www.lume.ufrgs.br/bitstream/10183/98495/3/000190601.pdf.jpgc3d8d8c7be7bb0aabb45d312a7d5669dMD5310183/984952024-04-14 06:46:19.021088oai:www.lume.ufrgs.br:10183/98495Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-14T09:46:19Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
title |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
spellingShingle |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 Mello, D.F. de Astrofisica extragalatica Galaxias elipticas Populacoes estelares Formacao de estrelas Galaxies: elliptical Galaxies: stellar content Galaxies: interactions Galaxies: AM 0327-285 |
title_short |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
title_full |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
title_fullStr |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
title_full_unstemmed |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
title_sort |
Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285 |
author |
Mello, D.F. de |
author_facet |
Mello, D.F. de Kell, W.C. Sulentic, J.W. Rampazzo, R. Bica, Eduardo Luiz Damiani White, R.E. |
author_role |
author |
author2 |
Kell, W.C. Sulentic, J.W. Rampazzo, R. Bica, Eduardo Luiz Damiani White, R.E. |
author2_role |
author author author author author |
dc.contributor.author.fl_str_mv |
Mello, D.F. de Kell, W.C. Sulentic, J.W. Rampazzo, R. Bica, Eduardo Luiz Damiani White, R.E. |
dc.subject.por.fl_str_mv |
Astrofisica extragalatica Galaxias elipticas Populacoes estelares Formacao de estrelas |
topic |
Astrofisica extragalatica Galaxias elipticas Populacoes estelares Formacao de estrelas Galaxies: elliptical Galaxies: stellar content Galaxies: interactions Galaxies: AM 0327-285 |
dc.subject.eng.fl_str_mv |
Galaxies: elliptical Galaxies: stellar content Galaxies: interactions Galaxies: AM 0327-285 |
description |
We present evidence for a young stellar population component in the early-type member of the E+S galaxy pair AM 0327-285. This young population is consistent with the occurrence of cross-fueling in this interacting system. We used spectroscopy, optical imaging, IRAS data, and stellar population synthesis to study the stellar content in the early-type galaxy. We also attempted to date episodes of star formation in its nuclear region, from population synthesis and basic dynamical considerations. The dominant population is old and metal-rich ([Z/Z]Θ=0.3) while ~ 10% of the flux at 5870 Å arises from a superimposed young stellar population with age <_ 5 x 10⁸ yr. This age is close to several estimates of the characteristic timescale of the interaction, suggesting that the mass influx associated with this star formation occurred as a result of an earlier phase of the interaction and not as a result of the present geometry of the pair. |
publishDate |
1995 |
dc.date.issued.fl_str_mv |
1995 |
dc.date.accessioned.fl_str_mv |
2014-07-24T02:04:18Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
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info:eu-repo/semantics/publishedVersion |
format |
article |
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publishedVersion |
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http://hdl.handle.net/10183/98495 |
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0004-6361 |
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000190601 |
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0004-6361 000190601 |
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http://hdl.handle.net/10183/98495 |
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eng |
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eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and Astrophysics. Berlin. Vol. 297, no. 2 (May 1995), p. 331-337 |
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openAccess |
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