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Temperature, surface gravity, and metallicitity are basic stellar atmosphericparameters necessary to characterize a star. We aim to improve the descriptionof the spectroscopic temperatures especially for the cooler stars where thedifferences with the Infrared Flux Method are higher, as presented in previouswork. Our spectroscopic analysis is based on the iron excitation and ionizationbalance, assuming Kurucz model atmospheres in LTE. The abundance analysis isdetermined using the code MOOG. We optimize the line list using a cool starwith high resolution and high signal-to-noise spectrum, as a reference in orderto check for weak, isolated lines. We test the quality of the new line list byre-deriving stellar parameters for 451 stars with high resolution andsignal-to-noise HARPS spectra, that were analyzed in a previous work with alarger line list. The comparison in temperatures between this work and thelatest IRFM shows that the differences for the cooler stars are significantlysmaller and more homogeneously distributed than in previous studies for starswith temperatures below 5000 K. We use the new line list to re-deriveparameters for some of the cooler stars that host planets. Finally, we presentthe impact of the new temperatures on the [Cr I/Cr II] and [Ti I/Ti II]abundance ratios that previously showed systematic trends with temperature.

Deriving precise parameters for cool solar-type stars. Optimizing the iron line list