Oxygen abundances in planet-harbouring stars

Comparison of different abundance indicators

¹ Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain e-mail: aecuvill@ll.iac.es
² Centro de Astronomia e Astrofisica de Universidade de Lisboa, Observatorio Astronomico de Lisboa, Tapada de Ajuda, 1349-018 Lisboa, Portugal
³ Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
⁴ Main Astronomical Observatory, National Academy of Sciences, 27 Zabolotnogo Street, 03680 Kyiv-127, Ukraine
⁵ Consejo Superior de Investigaciones Científicas, Spain

Received: 18 May 2005
Accepted: 16 August 2005

Abstract

We present a detailed and uniform study of oxygen abundances in 155 solar type stars, 96 of which are planet hosts and 59 of which form part of a volume–limited comparison sample with no known planets. EW measurements were carried out for the [O I] 6300 Å line and the O I triplet, and spectral synthesis was performed for several OH lines. NLTE corrections were calculated and applied to the LTE abundance results derived from the O I 7771–5 Å triplet. Abundances from [O I], the O I triplet and near-UV OH were obtained in 103, 87 and 77 dwarfs, respectively. We present the first detailed and uniform comparison of these three oxygen indicators in a large sample of solar-type stars. There is good agreement between the [O/H] ratios from forbidden and OH lines, while the NLTE triplet shows a systematically lower abundance. We found that discrepancies between OH, [O I] and the O I triplet do not exceed 0.2 dex in most cases. We have studied abundance trends in planet host and comparison sample stars, and no obvious anomalies related to the presence of planets have been detected. All three indicators show that, on average, [O/Fe] decreases with [Fe/H] in the metallicity range Fe/H. The planet host stars present an average oxygen overabundance of 0.1–0.2 dex with respect to the comparison sample.