Mass transfer and star formation in the early-type galaxy of a mixed pair, am 0327-285
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 synt...
| Autores: | , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 1995 |
| País: | Brasil |
| Institución: | Universidade Federal do Rio Grande do Sul (UFRGS) |
| Repositorio: | Repositório Institucional da UFRGS |
| Idioma: | inglés |
| OAI Identifier: | oai:www.lume.ufrgs.br:10183/98495 |
| Acceso en línea: | http://hdl.handle.net/10183/98495 |
| Access Level: | acceso abierto |
| Palabra clave: | Astrofisica extragalatica Galaxias elipticas Populacoes estelares Formacao de estrelas Galaxies: elliptical Galaxies: stellar content Galaxies: interactions Galaxies: AM 0327-285 |
| Sumario: | 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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