Precise effective temperatures of solar analog stars

We perform a study of 62 solar analog stars to compute their effective temperatures (T _eff) using the Balmer line wing fitting procedure and compare them with T _eff values obtained using other commonly employed methods. We use observed Hα spectral lines and a fine grid of theoretical LTE model spectra calculated with the best available atomic data and most recent quantum theory. Our spectroscopic data are of very high quality and have been carefully normalized to recover the proper shape of the Hα line profile. We obtain T _eff values with internal errors of about 25K. Comparison of our results with those from other methods shows reasonably good agreement. Then, combining T _eff values obtained from four independent techniques, we are able to determine final T _eff values with errors of about 10K.