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Volatile elements play a crucial role in the formation of planetary systems.Their abundance and distribution in protoplanetary disks provide vital insightsinto the connection between formation processes and the atmospheric compositionof individual planets. Sulfur, being one of the most abundant elements inplanet-forming environments, is of great significance, and now observable inexoplanets with JWST. However, planetary formation models currently lack vitalknowledge regarding sulfur chemistry in protoplanetary disks. Developing adeeper understanding of the major volatile sulfur carriers in disks isessential to building models that can meaningfully predict planetaryatmospheric composition, and reconstruct planetary formation pathways. In thiswork, we combine archival observations with new data from ALMA and APEX,covering a range of sulfur-bearing species/isotopologs. We interpret this datausing the DALI thermo-chemical code, for which our model is highly refined anddisk-specific. We find that volatile sulfur is heavily depleted from the cosmicvalue by a factor of 1000, with a disk-averaged abundance of S/H = 1e-8. Weshow that the gas-phase sulfur abundance varies radially by 3 orders ofmagnitude, with the highest abundances inside the inner dust ring andcoincident with the outer dust ring at 150 to 230 au. Extracting chemicalabundances from our models, we find OCS, H2CS, and CS to be the dominantmolecular carriers in the gas phase. We also infer the presence of asubstantial OCS ice reservoir. We relate our results to the potentialatmospheric composition of planets in HD 100546, and the wider exoplanetpopulation

Spatially resolving the volatile sulfur abundance in the HD 100546 protoplanetary disk