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We present a determination of photospheric parameters and C abundances for asample of 172 G and K dwarfs, subgiants, and giants with and without detectedplanets in the solar neighbourhood. The analysis was based on high S/N and highresolution spectra observed with the ELODIE spectrograph, and for which theobservational data was publicly available. We intend to contribute precise andhomogeneous C abundances in studies that compare the behaviour of lightelements in stars, hosting planets or not. This will bring new arguments to thediscussion of possible anomalies that have been suggested and will contributeto a better understanding of different planetary formation process. Thephotospheric parameters were computed through the excitation potential,equivalent widths, and ionisation equilibrium of Fe lines selected in thespectra. C abundances were derived from spectral synthesis applied to prominentmolecular head bands of C_2 Swan (5128 and 5165) and to a C atomic line(5380.3). The distribution of [C/Fe] vs. [Fe/H] shows no difference in thebehaviour of planet-host stars in comparison with stars for which no planet wasdetected, for both dwarf and giant subsamples. This result is in agreement withthe hypothesis of primordial origin for the chemical abundances presentlyobserved instead of self-enrichment during the planetary system formation andevolution. Additionally, giants are clearly depleted in [C/Fe] (~0.14 dex) whencompared with dwarfs, which is probably related to evolution-induced mixing ofH-burning products in the envelope of evolved stars. Subgiants, although insmall number, seems to follow the same C abundance distribution as dwarfs. Wealso analysed the kinematics of the sample stars that, in majority, are membersof the Galaxy's thin disc. Finally, comparisons with other analogue studieswere performed and, within the uncertainties, showed good agreement.

Homogeneous photospheric parameters and C abundances in G and K nearby stars with and without planets