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Mono-deuterated methanol is thought to form during the prestellar core stageof star formation. Observed variations in the CH2DOH/CH3OD ratio suggest thatits formation is strongly dependent on the surrounding cloud conditions. Thus,it is a potential tracer of the physical conditions before the onset of starformation. A single-point physical model representative of a typical prestellarcore is coupled to chemical models to investigate potential formation pathwaystowards deuterated methanol at the prestellar stage. Simple addition reactionsof H and D are not able to reproduce observed abundances. The implementation ofan experimentally verified abstraction scheme leads to the efficient formationof methyl-deuterated methanol, but lacks sufficient formation ofhydroxy-deuterated methanol. CH3OD is most likely formed at a laterevolutionarymstage, potentially from H-D exchange reactions in warm icesbetween HDO (and D2O) and CH3OH. The CH2DOH/CH3OD ratio is not an appropriatetracer of the physical conditions during the prestellar stage, but might bebetter suited as a tracer of ice heating.

Fevering Interstellar Ices Have More CH3OD