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Context. The Galactic chemical evolution of sulphur is still under debate. Atlow metallicities some studies find no correlation between [S/Fe] and [Fe/H],others find [S/Fe] increasing towards lower metallicities, and still othersfind a combination of the two. Each scenario has different implications for theGalactic chemical evolution of sulphur.  Aims. To contribute to the discussion on the Galactic chemical evolution ofsulphur by deriving sulphur abundances from non-LTE insensitive spectraldiagnostics in Disk and Halo stars with homogeneously determined stellarparameters.  Methods. We derive Teff from photometric colours, logg from stellarisochrones and Bayesian estimation, and [Fe/H] and [S/Fe] from spectrumsynthesis. We derive [S/Fe] from the [S i] 1082 nm line in 39 mostly cool andmetal-poor giants, using 1D LTE MARCS model atmospheres to model ourhigh-resolution NIR spectra obtained with the VLT, NOT and Gemini Southtelescopes.  Results. We derive homogeneous stellar parameters for 29 stars. Our resultsargue for a chemical evolution of sulphur that is typical for alpha-elements,contrary to some previous studies. Our abundances are systematically higher byabout 0.1 dex in comparison to other studies that arrived at similarconclusions using other sulphur diagnostics.  Conclusions. We find the [S i] line to be a valuable diagnostic of sulphurabundances in cool giants down to [Fe/H] ~ -2.3. We argue that a homogeneousdetermination of stellar parameters is necessary, since the derived abundancesare sensitive to them. Our results ([S/Fe]) show reasonable agreement withpredictions of contemporary models of Galactic chemical evolution. In thesemodels sulphur is predominantly created in massive stars by oxygen burning, andejected in the ISM during Type II SNe explosions. Systematic differences withprevious studies likely fall within modelling uncertainties.

On the Galactic chemical evolution of sulphur. Sulphur abundances from the [S i] 1082 nm line in giants