| Issue |
A&A
Volume 530, June 2011
|
|
|---|---|---|
| Article Number | A98 | |
| Number of page(s) | 10 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/201016191 | |
| Published online | 18 May 2011 | |
Abundance ratios in the hot ISM of elliptical galaxies
1
Dipartimento di AstronomiaUniversità di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy
e-mail: pipino@oats.inaf.it; pipinoa@phys.ethz.ch
2
Institut fur Astronomie, ETH Zurich, 8093 Zurich, Switzerland
3
INAF Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy
Received: 23 November 2010
Accepted: 8 March 2011
Aims. We constrain possible explanations of the theoretical Fe discrepancy in the hot interstellar medium of elliptical galaxies and simultaneously explain the [α/Fe] ratios.
Methods. We use the latest theoretical nucleosynthetic yields, incorporate dust, and explore different SNIa progenitor scenarios by means of a self-consistent chemical evolution model that reproduces the stellar populations properties of elliptical galaxies.
Results. Models with Fe-only dust and/or a lower effective SNIa rate achieve a closer agreement with the observed Fe abundance. However, a suitable modification of the SNIa yields relative to the standard W7 model is needed to fully describe the abundance ratio pattern. The 2D explosion model C-DDT by Maeda and collaborator may be capable of reproducing the [Fe/H] and the [α/Fe] ratios.
Key words: ISM: abundances / galaxies: abundances / galaxies: elliptical and lenticular, CD / X-rays: ISM / galaxies: evolution
© ESO, 2011
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