Chemistry in disks

V. Sulfur-bearing molecules in the protoplanetary disks surrounding LkCa15, MWC480, DM Tauri, and GO Tauri^⋆

¹ Université de Bordeaux, Observatoire Aquitain des Sciences de l’Univers (OASU), 2 rue de l’Observatoire, BP 89, 33271 Floirac Cedex, France
e-mail: dutrey@obs.u-bordeaux1.fr
² CNRS - UMR5804, Laboratoire d’Astrophysique de Bordeaux (LAB), 2 rue de l’Observatoire, BP 89, 33271 Floirac Cedex, France
³ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
⁴ MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany
⁵ IRAM, 300 rue de la piscine, 38406 Saint Martin d’Hères, France
⁶ Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, 07745 Jena, Germany

Received: 21 March 2011
Accepted: 29 July 2011

Abstract

Aims. We study the content in S-bearing molecules of protoplanetary disks around low-mass stars.

Methods. We used the new IRAM 30-m receiver EMIR to perform simultaneous observations of the 1₁₀−1₀₁ line of H₂S at 168.8 GHz and 2₂₃−1₁₂ line of SO at 99.3 GHz. 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.

Results. We fail to detect the SO and H₂S lines, although CS is detected in LkCa15, DM Tau, and GO Tau but not in MWC 480. However, our new upper limits are significantly better than previous ones and allow us to put some interesting constraints on the sulfur chemistry.

Conclusions. Our best modeling of disks is obtained for a C/O ratio of 1.2, starting from initial cloud conditions of H density of 2 × 10⁵ cm^-3 and age of 10⁶ yr. 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.