Volume 494, Number 2, February I 2009
|Page(s)||591 - 610|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||04 December 2008|
Abundances in the Galactic bulge: results from planetary nebulae and giant stars
Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland e-mail: Cristina.Chiappini@unige.ch
2 Osservatorio Astronomico di Trieste – OAT/INAF, via G. B. Tiepolo 11, 34131 Trieste, TS, Italy e-mail: firstname.lastname@example.org
3 Copernicus Astronomical center, Rabiańska 8, 87-100 Toruń, Poland e-mail: email@example.com
4 LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, Place Jules Janssen, 92190 Meudon, France e-mail: firstname.lastname@example.org
5 Universidade de São Paulo, IAG, Rua do Matão 1226, Cidade Universitária, São Paulo 05508-900, Brazil e-mail: email@example.com
Accepted: 27 October 2008
Context. Our understanding of the chemical evolution (CE) of the Galactic bulge requires the determination of abundances in large samples of giant stars and planetary nebulae (PNe). Studies based on high resolution spectroscopy of giant stars in several fields of the Galactic bulge obtained with very large telescopes have allowed important progress.
Aims. We discuss PNe abundances in the Galactic bulge and compare these results with those presented in the literature for giant stars.
Methods. We present the largest, high-quality data-set available for PNe in the direction of the Galactic bulge (inner-disk/bulge). For comparison purposes, we also consider a sample of PNe in the Large Magellanic Cloud (LMC). We derive the element abundances in a consistent way for all the PNe studied. By comparing the abundances for the bulge, inner-disk, and LMC, we identify elements that have not been modified during the evolution of the PN progenitor and can be used to trace the bulge chemical enrichment history. We then compare the PN abundances with abundances of bulge field giant.
Results. At the metallicity of the bulge, we find that the abundances of O and Ne are close to the values for the interstellar medium at the time of the PN progenitor formation, and hence these elements can be used as tracers of the bulge CE, in the same way as S and Ar, which are not expected to be affected by nucleosynthetic processes during the evolution of the PN progenitors. The PN oxygen abundance distribution is shifted to lower values by 0.3 dex with respect to the distribution given by giants. A similar shift appears to occur for Ne and S. We discuss possible reasons for this PNe-giant discrepancy and conclude that this is probably due to systematic errors in the abundance derivations in either giants or PNe (or both). We issue an important warning concerning the use of absolute abundances in CE studies.
Key words: stars: abundances / ISM: planetary nebulae: general / Galaxy: bulge / Galaxy: abundances
© ESO, 2009
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