Left panels: absolute abundances of selected sulfuretted species as a function of time predicted by the GRAINOBLE astrochemical model in the gas phase (solid curves) and in interstellar ices (dashed curves) at 10 K (top) and 20 K (bottom) and for n_H = 2× 10⁴ cm⁻³, ζ = 10⁻¹⁷ s⁻¹, and A_V = 20 mag. Middle and right panels: gaseous absolute abundances of selected sulfuretted species (coloured curves) and physical conditions (black curves) profiles in 1D C-type shocks predicted by the Paris-Durham shock code for a pre-shock density of 6 × 10⁴ cm⁻³ (centre panels) and 3 × 10⁵ cm⁻³ (right panels). Solid and dashed coloured curves show the abundances with and without the OCS formation/destruction reactions introduced by Loison et al. (2012), respectively (see text for more details). For the shocks considered here, the entire icy material formed in dark clouds is sputtered in the shock front, final ice abundances in the left panels are therefore similar to the gas phase obtained at the shock front in the middle and right panels, with the exception of H₂ S that is efficiently formed through hot gas phase chemistry.