EDP Sciences
Free access
Volume 411, Number 3, December I 2003
Page(s) 559 - 564
Section Formation and evolution of planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20031378

A&A 411, 559-564 (2003)
DOI: 10.1051/0004-6361:20031378

High precision effective temperatures for 181 F-K dwarfs from line-depth ratios

V. V. Kovtyukh1, C. Soubiran2, S. I. Belik1 and N. I. Gorlova3

1  Astronomical Observatory of Odessa National University and Isaac Newton Institute of Chile, Shevchenko Park, 65014 Odessa, Ukraine
2  Observatoire de Bordeaux, CNRS UMR 5804, BP 89, 33270 Floirac, France
3  Steward Observatory, The University of Arizona, Tucson, AZ 85721, USA

(Received 6 May 2003 / Accepted 19 August 2003)

Line depth ratios measured on high resolution ( $R=42\,000$), high  S/N echelle spectra are used for the determination of precise effective temperatures of 181 F, G, K Main Sequence stars with about solar metallicity ( $-0.5 < [{\rm Fe/H]}
< +0.5$ ). A set of 105 relations is obtained which rely  $T_{\rm
eff}$ on ratios of the strengths of lines with high and low excitation potentials, calibrated against previously published precise (one per cent) temperature estimates. The application range of the calibrations is 4000-6150 K (F8V-K7V). The internal error of a single calibration is less than 100 K, while the combination of all calibrations for a spectrum of  S/N=100 reduces uncertainty to only 5-10 K, and for S/N=200 or higher - to better than 5 K. The zero point of the temperature scale is directly defined from reflection spectra of the Sun with an uncertainty about 1 K. The application of this method to investigation of the planet host stars properties is discussed.

Key words: stars: fundamental parameters -- stars: planetary systems

Offprint request: V. V. Kovtyukh, val@deneb.odessa.ua

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