Sublimation front locations for the H₂S-H₂S and H₂S-H₂O binding energies estimated for a representative T-Tauri disk midplane. Most of the H₂S will remain entrapped in the ice past its sublimation front radii and will only be released to the gas phase close to the water snowline. The CO₂ snowline location is also shown for comparison. It was estimated based on the mean binding energy derived by Noble et al. (2012) for (sub)monolayer CO₂ ice on a nonporous ASW surface and their adopted pre-exponential factor of 10¹² s⁻¹, while assuming ice abundances N(CO₂)/N(H₂O) 0.28 (median value observed in low-mass young stellar objects; Boogert et al. 2015).