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The evolution of star-forming regions and their thermal balance are stronglyinfluenced by their chemical composition, that, in turn, is determined by thephysico-chemical processes that govern the transition between the gas phase andthe solid state, specifically icy dust grains (e.g., particles adsorption anddesorption). Gas-grain and grain-gas transitions as well as formation andsublimation of interstellar ices are thus essential elements of understandingastrophysical observations of cold environments (e.g., pre-stellar cores) whereunexpected amounts of a large variety of chemical species have been observed inthe gas phase. Adsorbed atoms and molecules also undergo chemical reactionswhich are not efficient in the gas phase. Therefore, the parameterization ofthe physical properties of atoms and molecules interacting with dust grainparticles is clearly a key aspect to interpret astronomical observations and tobuild realistic and predictive astrochemical models. In this consensusevaluation, we focus on parameters controlling the thermal desorption of icesand how these determine pathways towards molecular complexity and define thelocation of snowlines, which ultimately influence the planet formation process.We review different crucial aspects of desorption parameters both from atheoretical and experimental point of view. We critically assess the desorptionparameters commonly used in the astrochemical community for astrophysicalrelevant species and provide tables with recommended values. In addition, weshow that a non-trivial determination of the pre-exponential factor nu usingthe Transition State Theory can affect the binding energy value. Finally, weconclude this work by discussing the limitations of theoretical andexperimental approaches currently used to determine the desorption propertieswith suggestions for future improvements.

Thermal desorption of interstellar ices. A review on the controlling parameters and their implications fromsnowlines to chemical complexity