Context : Elemental abundances are of prime importance to help us reconstruct the origin and evolution of stars and galaxies in our Universe .
Sulfur abundances have not been as heavily studied as other elements , so some details regarding its behaviour are still unclear .

Aims : We aim to investigate [ \mathrm { S / Fe } ] ratios in stars of the solar neighbourhood in order to analyse the chemical evolution of sulfur and probe for possible differences in abundances of planet host and non-planet host stars .

Methods : We use the code MOOG to perform spectral synthesis and derive v sin i values and [ \mathrm { S / Fe } ] ratios for 719 FGK stars with high-resolution ( R \sim 115000 ) and high-quality spectra from the HARPS-GTO program .
We find the best fit and corresponding parameter values by performing \chi ^ { 2 } minimisation of the deviation between synthetic profiles and observational spectra .

Results : Our results reveal that sulfur behaves as a typical \alpha -element , with low abundances in young thin disk stars and high abundances in old thick disk stars , following what was expected from our understanding of the Galactic chemical evolution ( GCE ) .
Nevertheless , further studies into the abundances of sulfur in very metal-poor stars are required as our sample only derived sulfur abundances to stars with metallicity as low as [ \mathrm { Fe / H } ] = -1.13 dex .
High- \alpha metal rich stars are more enhanced in sulfur compared to their thin disk counterparts at the same metallicity .
We compare our results to GCE models from other authors in the [ \mathrm { S / Fe } ] vs . [ \mathrm { Fe / H } ] plane .
The [ \mathrm { S / Fe } ] -age relationship is a good proxy for time , just like it is the case with other \alpha -elements .
We report no differences in the abundances of sulfur between stars with and without planetary companions in the metallicity range [ \mathrm { Fe / H } ] \geqslant - 0.3 dex .

Conclusions :