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Metal-rich end of galactic chemical evolution: oxygen abundances from [OI] 6300, OI 7771–5 and near-UV OH.

Published online by Cambridge University Press:  23 December 2005

A. Ecuvillon ,
G. Israelian ,
N.C. Santos ,
N.G. Shchukina ,
M. Mayor  and
R. Rebolo
A. Ecuvillon
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain email: aecuvill@iac.es
G. Israelian
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain email: aecuvill@iac.es
N.C. Santos
Affiliation:
Observatorio Astronomico de Lisboa, Tapada de Ajuda, 1349-018 Lisboa, Portugal Observatoire de Genève, 51 ch. des Maillettes, CH–1290 Sauverny, Switzerland
N.G. Shchukina
Affiliation:
Main Astronomical Observatory, National Academy of Sciences, 03680 Kyiv-127, Ukraine
M. Mayor
Affiliation:
Observatoire de Genève, 51 ch. des Maillettes, CH–1290 Sauverny, Switzerland
R. Rebolo
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain email: aecuvill@iac.es Consejo Superior de Investigaciones Científicas, Spain
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Abstract

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We present a detailed and uniform study of oxygen abundances in a large set of 155 metal-rich dwarfs. EW measurements were carried out for the [OI] 6300 Å line and the OI triplet, while spectral synthesis was performed for several OH lines. NLTE corrections were calculated and applied to the LTE abundance results derived from the triplet. Abundances from [OI], the OI triplet and near-UV OH were obtained in 103, 87 and 77 dwarfs, respectively. A good agreement between [O/H] ratios from forbidden and OH lines is found, while the NLTE triplet shows a systematically lower abundance. Nevertheless, the consistency with other indicators improves if we consider LTE triplet results. In any case, discrepancies between OH, [OI] and the OI triplet hardly exceed 0.2dex. All three indicators show that, on average, [O/Fe] decreases with [Fe/H] in the metallicity range −0.8<[Fe/H]<0.5.

Keywords

Stars: abundancesGalaxy: abundancesGalaxy: solar neighborhoodGalaxy: disk
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 253 - 254
Copyright
© 2005 International Astronomical Union