摘要：Context. The sulfur abundance is poorly known in most environments. Yet, deriving the sulfur abundance is key to understanding theevolution of the chemistry from molecular clouds to planetary atmospheres. We present observations of H2S 110−101 at 168.763 GHztoward the Herbig Ae star AB Aur.Aims. We aim to study the abundance of sulfuretted species toward AB Aur and to constrain how different species and phases con?tribute to the sulfur budget.Methods. We present new NOrthern Extended Millimeter Array (NOEMA) interferometric observations of the continuum and H2S110−101 line at 168.763 GHz toward AB Aur. We derived radial and azimuthal profiles and used them to compare the geometrical distri?bution of different species in the disk. Assuming local thermodynamical equilibrium (LTE), we derived column density and abundancemaps for H2S, and we further used Nautilus to produce a more detailed model of the chemical abundances at different heights overthe mid-plane at a distance of r = 200 au.Results. We have resolved H2S emission in the AB Aur protoplanetary disk. The emission comes from a ring extending from 0.6700(∼109 au) to 1.6900 (∼275 au). Assuming T = 30 K, nH = 109cm−3, and an ortho-to-para ratio of three, we derived a column density of(2.3 ± 0.5) × 1013 cm−2. Under simple assumptions, we derived an abundance of (3.1 ± 0.8) × 10−10 with respect to H nuclei, whichwe compare with Nautilus models to deepen our understanding of the sulfur chemistry in protoplanetary disks. Chemical modelsindicate that H2S is an important sulfur carrier in the solid and gas phase. We also find an important transition at a height of ∼12 au,where the sulfur budget moves from being dominated by ice species to being dominated by gas species.Conclusions. We confirm that present-day models still struggle to simultaneously reproduce the observed column densities of the dif?ferent sulfuretted species, and the observed abundances are still orders of magnitude away from the cosmic sulfur abundance. Studyingsulfuretted species in detail in the different phases of the interstellar medium is key to solving the issue.
