This dataset will appear as a supplement to the book chapter: Renggli C.J., Steenstra E.S., Saal A. Sulfur in the Moon and Mercury. Eds.: Daniel Harlov & Gleb Pokrovski, Springer (in review). Introduction: 50 years after the return of Apollo 17, the analysis of returned lunar samples has become a priority for planetary scientists across the world. The advances in analytical technology have made an important contribution to this development. As we expect a significant increase of available lunar materials through upcoming missions including ARTEMIS, it is worth taking a look at the published record. Here, we present a compilation of all published S concentration and S-isotope data from bulk mare basalts, soil samples, as well as impact and regolith breccias from the Apollo and two Luna landing sites. We also include more recent in-situ measurements of S-concentrations and isotopic compositions from pyroclastic glass beads. Recent studies reported rare data on S-concentrations in Mg-suite samples and anorthosites. Finally, we include data on the S concentration and isotopic composition in the basalt lava flow sampled by Chang’e-5. Discussion: In our review we gathered a total of 163 mare basalt, 165 soil, 57 breccia, 12 anorthosite, 6 Mg-suite, and 142 pyroclastic glass S-concentration measurements, presented in Figure 1 as a function of the TiO2 concentration. Sulfur concentrations in the impact breccias and soils broadly reflect those of the target basalts, highland rocks, and pyroclastic glasses of the landing sites. However, their heavy δ34S isotopic signatures contrast with the light δ34S compositions of the volcanic glasses. The former most likely originates from solar-wind sputtering, proton stripping, micro-meteorite impact vaporization and later condensation, or a combination of these processes, whereas the latter probably formed during degassing at low fO2 conditions. The S systematics of magmatic lunar rocks are controlled by the composition of the rocks (e.g. TiO2 content), degree of degassing, impact gardening of soils (resulting in high δ34S), mantle source compositions and the early history of the Moon. However, the behavior of S during many of these lunar processes remains poorly constrained. This is of particular importance in the light of constraints on the volatile element budget and evolution of the Moon.