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We study the content in S-bearing molecules of protoplanetary disks aroundlow-mass stars. We used the new IRAM 30-m receiver EMIR to perform simultaneousobservations of the $1_{10}-1_{01}$ line of H$_2$S at 168.8 GHz and$2_{23}-1_{12}$ line of SO at 99.3 GHz. We compared the observational resultswith predictions coming from the astrochemical code NAUTILUS, which has beenadapted to protoplanetary disks. The data were analyzed together with existingCS J=3-2 observations. We fail to detect the SO and H$_2$S lines, although CSis detected in LkCa15, DM\,Tau, and GO\,Tau but not in MWC\,480. However, ournew upper limits are significantly better than previous ones and allow us toput some interesting constraints on the sulfur chemistry. Our best modeling ofdisks is obtained for a C/O ratio of 1.2, starting from initial cloudconditions of H density of $2\times 10^5$ cm$^{-3}$ and age of $10^6$ yr. Theresults agree with the CS data and are compatible with the SO upper limits, butfail to reproduce the H$_2$S upper limits. The predicted H$_2$S columndensities are too high by at least one order of magnitude. H$_2$S may remainlocked onto grain surfaces and react with other species, thereby preventing thedesorption of H$_2$S.

CID: Chemistry in disks VI.sulfur-bearing molecules in the protoplanetary disks surrounding LkCa15, MWC480, DM Tau, and GO Tau