Complex organics in embedded protostellar regions

The results from physicochemical simulations will be shown, which model the spatial distribution within protostellar envelopes of solid and gaseous complex organic molecules. For the case of high-mass protostars, the physical model of protostellar core evolution based on the Turbulent Core Model, is adopted and combined with a large gas-grain chemical network. For the case of low-mass protostars, a dynamic semi-analytic collapse model is used in conjunction with the same chemical set up. Hereby, high-mass star-forming regions are contrasted with the low-mass regime.