Comparison between the 15 Κ and 25 Κ models. In the panels, we show the initial ice and gas-phase components of the H₂S, OCS, SO, SO₂, and H₂S₃ species in the inner core before the collapse, and we compare them with the final abundance of these species in the gas-phase after the collapse. There is a significant fall of H₂S, OCS, SO and SO₂ in the ices after the 25 Κ pre-phase, compared with the 15 Κ pre-stellar phase. On the contrary, H₂S₃ is formed in the ices during the warmer pre-phase, something that did not happen in the cooler one. After the collapse of the 25 Κ model, the final H₂S, SO and SO₂ drops in ~1 order of magnitude with respect to the 15 Κ simulation. This is not true for OCS, whose abundance falls more than 2 orders of magnitude. H₂S₃ final gas-phase abundance is greater in the warmer model, reaching an abundance of ~5×l0^–6.