2004A&A...413..609W

We report observations of the expected main S-bearing species (SO, SO₂ and H₂S) in the low-mass star forming region L1689N. We obtained large scale (∼300''x200'') maps of several transitions from these molecules with the goal to study the sulphur chemistry, i.e. how the relative abundances change in the different physical conditions found in L1689N. We identified eight interesting regions, where we carried out a quantitative comparative study: the molecular cloud (as reference position), five shocked regions caused by the interaction of the molecular outflows with the cloud, and the two protostars IRAS 16293-2422 and 16293E. In the cloud we carefully computed the gas temperature and density by means of a non-LTE LVG code, while in other regions we used previous results. We hence derived the column density of SO, SO₂ and H₂S, together with SiO and H₂CO - which were observed previously - and their relevant abundance ratios. We find that SiO is the molecule that shows the largest abundance variations in the shocked regions, whereas S-bearing molecules show more moderate variations. Remarkably, the region of the brightest SiO emission in L1689N is undetected in SO₂, H₂S and H₂CO and only marginally detected in SO. In the other weaker SiO shocks, SO₂ is enhanced with respect to SO. We propose a schema in which the different molecular ratios correspond to different ages of the shocks. Finally, we find that SO, SO₂ and H₂S have significant abundance jumps in the inner hot core of IRAS 16293-2422 and discuss the implications of the measured abundances.