Thermal desorption of interstellar ices. A review on the controlling
  parameters and their implications fromsnowlines to chemical complexity
  The evolution of star-forming regions and their thermal balance are strongly
influenced by their chemical composition, that, in turn, is determined by the
physico-chemical processes that govern the transition between the gas phase and
the solid state, specifically icy dust grains (e.g., particles adsorption and
desorption). Gas-grain and grain-gas transitions as well as formation and
sublimation of interstellar ices are thus essential elements of understanding
astrophysical observations of cold environments (e.g., pre-stellar cores) where
unexpected amounts of a large variety of chemical species have been observed in
the gas phase. Adsorbed atoms and molecules also undergo chemical reactions
which are not efficient in the gas phase. Therefore, the parameterization of
the physical properties of atoms and molecules interacting with dust grain
particles is clearly a key aspect to interpret astronomical observations and to
build realistic and predictive astrochemical models. In this consensus
evaluation, we focus on parameters controlling the thermal desorption of ices
and how these determine pathways towards molecular complexity and define the
location of snowlines, which ultimately influence the planet formation process.
We review different crucial aspects of desorption parameters both from a
theoretical and experimental point of view. We critically assess the desorption
parameters commonly used in the astrochemical community for astrophysical
relevant species and provide tables with recommended values. In addition, we
show that a non-trivial determination of the pre-exponential factor nu using
the Transition State Theory can affect the binding energy value. Finally, we
conclude this work by discussing the limitations of theoretical and
experimental approaches currently used to determine the desorption properties
with suggestions for future improvements.
