The stellar population of the decoupled nucleus in M 31
| dc.creator | Sil'chenko, O. K. | |
| dc.creator | Burenkov, A. N. | |
| dc.creator | Vlasyuk, V. V. | |
| dc.date | 1998-05-26 | |
| dc.date.accessioned | 2026-07-07T02:27:02Z | |
| dc.date.available | 2026-07-07T02:27:02Z | |
| dc.description | The results of a spectroscopic and photometric investigation of the central region of M 31 are presented. An analysis of absorption-index radial profiles involving magnesium, calcium, and iron lines has shown that the unresolved nucleus of M 31 is distinct by its increased metallicity; unexpectedly, among two nuclei of M 31, it is the faintest one located exactly in the dynamical center of the galaxy (and dynamically decoupled) which is chemically distinct. The Balmer absorption line H-beta has been included into the analysis to disentangle metallicity and age effects; an age difference by a factor 3 is detected between stellar populations of the nucleus and of the bulge, the nucleus being younger. The morphological analysis of CCD images has revealed the presence of a nuclear stellar-gaseous disk with a radius of some 100 pc, the gas component of which looks non-stationary, well inside the bulge of M 31. | |
| dc.description | 8 pages LATEX and 7 postscript figures, accepted to Astronomy and Astrophysics | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9805318 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9805318 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/12521 | |
| dc.subject | Astrophysics | |
| dc.title | The stellar population of the decoupled nucleus in M 31 | |
| dc.type | text |