Spectroscopic Gradients in Elliptical Galaxies
| dc.creator | Gonzalez, J. Jesus | |
| dc.creator | Gorgas, Javier | |
| dc.date | 1995-07-12 | |
| dc.date.accessioned | 2026-07-07T02:19:54Z | |
| dc.date.available | 2026-07-07T02:19:54Z | |
| dc.description | Preliminary results based on a large compilation of line-strength profiles are presented and discussed. Elliptical galaxies (Es) with strong central Mg$_2$ show steeper line-strength gradients. These galaxies are more massive and have higher velocity dispersions, note nevertheless, that the Mg$_2$ gradient correlates better with central Mg$_2$ than with any other global or structural parameter. This correlation, and the fact that Mg$_2$ measures $Z/Z_\odot$ together with the [Mg/Fe] abundances among Es, are of extreme importance for the use of the central Mg$_2-σ$ relation as a reflection of a mass-metallicity relation. Spectroscopic gradients arise mainly from a radial decrease in mean stellar metallicity. However, the Mg$_2$ and $<{\rm Fe}>$ gradients do not correlate within measuring errors, indicating that something else, besides metallicity, is also varying within a galaxy. H$β$ gradients indicate that the centers of Es tend to look spectroscopically ``younger'' than their stellar populations further out. | |
| dc.description | 10 pages, compressed uuencoded PostScript including figures. To appear on "Fresh Views on Elliptical Galaxies", ASP Conf. Ser., eds Buzzoni, A., and Renzini, A | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9507042 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9507042 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/10049 | |
| dc.subject | Astrophysics | |
| dc.title | Spectroscopic Gradients in Elliptical Galaxies | |
| dc.type | text |