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
Corresponding author: V. V. Kovtyukh, email@example.com
Accepted: 19 August 2003
Line depth ratios measured on high resolution (), high echelle spectra are used for the determination of precise effective temperatures of 181 F, G, K Main Sequence stars with about solar metallicity (). A set of 105 relations is obtained which rely 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 reduces uncertainty to only 5–10 K, and for 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
© ESO, 2003