The abundance of nitrogen in starburst nucleus galaxies
| dc.creator | Coziol, R. | |
| dc.creator | Reyes, R. E. Carlos | |
| dc.creator | Considere, S. | |
| dc.creator | Davoust, E. | |
| dc.creator | Contini, T. | |
| dc.date | 1999-03-18 | |
| dc.date.accessioned | 2026-07-07T02:30:54Z | |
| dc.date.available | 2026-07-07T02:30:54Z | |
| dc.description | We show that the excess of nitrogen emission observed in a large sample of Starburst Nucleus Galaxies (SBNGs) can only be explained at a given metallicity by an overabundance of nitrogen with respect to normal HII regions in the disks of late-type spirals. The N/O ratios in the SBNGs are comparable to the values found in the bulges of normal early-type spirals, which suggests that what we observe could be the main production of nitrogen in the bulges of these galaxies. The variation of the N/O ratio as a function of metallicity in SBNGs follows a primary + secondary relation, but the increase of nitrogen does not appear as a continuous process. In SBNGs, nitrogen is probably produced by different populations of intermediate-mass stars, which were formed during past sequences of bursts of star formation. This assumption pushes the origin of the main bursts 2-3 Gyrs back in the past. On a cosmological scale, this time interval corresponds to redshifts z = 0.2-0.3, where a significant increase of star formation activity occurred. The origin of the SBNG phenomenon would thus have cosmological implications, it would be related to a more active phase of star formation in the Universe sometime in its recent past. | |
| dc.description | 16 pages, Astronomy & Astrophysics, in press | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9903279 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9903279 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/13976 | |
| dc.subject | Astrophysics | |
| dc.title | The abundance of nitrogen in starburst nucleus galaxies | |
| dc.type | text |