High-temperature evaporation processes under high-vacuum conditions have played a crucial role in the early evolution of planetary bodies, impact events, and volcanic degassing on airless bodies such as Jupiter's moon Io, Earth's Moon, and Mercury. These processes significantly influence the distribution and loss of volatile and moderately volatile elements from planetary objects. However, the exact conditions and mechanisms remain poorly constrained. For instance, NASA's MESSENGER mission to Mercury identified surface features known as hollows—irregular depressions up to 80 m deep and several kilometers in diameter. Bright halos surrounding these hollows, and the morphology of these depressions suggest an ongoing formation process linked to volatile loss. Additionally, MESSENGER detected bright spots, or faculae, interpreted as pyroclastic volcanic deposits, similar to the Moon's dark mantle deposits. The pyroclastic eruptions on Mercury must have been driven by a gas phase that remains poorly understood. Understanding the volatile species and release processes, involved in both hollow formation and pyroclastic eruptions, is key to deciphering Mercury's volatile inventory. To address these questions, we have established a new experimental facility capable of in-situ measurement of volatile species under high-vacuum conditions and at temperatures up to 2000 °C. Here, we present the experimental setup and initial results.