Oxygen abundances in planet-harbouring stars. Comparison of different abundance indicators

TL;DR

This study compares different oxygen abundance indicators in 155 solar-type stars, including planet hosts and non-hosts, revealing consistent results among indicators and no significant abundance anomalies related to planet presence.

Contribution

It provides the first detailed comparison of [O I], O I triplet, and OH lines in a large sample of solar-type stars, including planet hosts and non-hosts.

Findings

Good agreement between [O/H] from forbidden and OH lines.

NLTE triplet shows systematically lower abundance.

No significant abundance anomalies linked to planets.

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 \AA 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 \AA\ 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 -0.8<[Fe/H]<0.5. The planet host stars present an average oxygen overabundance of 0.1-0.2dex with respect to the comparison sample.