SIMBAD references

We study the content in S-bearing molecules of protoplanetary disks around low-mass stars. We used the new IRAM 30-m receiver EMIR to perform simultaneous observations of the 1₁₀-1₀₁ line of H₂S at 168.8GHz and 2₂₃-1₁₂ line of SO at 99.3GHz. We compared the observational results with predictions coming from the astrochemical code NAUTILUS, which has been adapted to protoplanetary disks. The data were analyzed together with existing CS J=3-2 observations. We fail to detect the SO and H₂S lines, although CS is detected in LkCa15, DMTau, and GOTau but not in MWC480. However, our new upper limits are significantly better than previous ones and allow us to put some interesting constraints on the sulfur chemistry. Our best modeling of disks is obtained for a C/O ratio of 1.2, starting from initial cloud conditions of H density of 2x10⁵cm^–3 and age of 10⁶yr. The results agree with the CS data and are compatible with the SO upper limits, but fail to reproduce the H₂S upper limits. The predicted H₂S column densities are too high by at least one order of magnitude. H₂S may remain locked onto grain surfaces and react with other species, thereby preventing the desorption of H₂S.