Pathways to chemical complexity during star- and planet-formation

Complex organic molecules (>6 atoms) have been detected toward low- and high-mass protostars, galactic center clouds, protostellar outflows and comets, demonstrating the existence of efficient astrophysical pathways to chemical complexity. Exploring these pathways are key both to constrain the prebiotic evolution during star formation and to develop new tracers of otherwise inaccessible physical phenomena. The detected complex molecules all reside in the gas. Yet they probably form on interstellar grains, in ices that evolve with their environment and finally evaporate as the grains are heated by new-born stars or by shocks.  This ice evolution is observed directly through infrared observations and indirectly through millimeter observations of evaporated ices. In this talk such observational results are combined with laboratory studies on different ice processes, especially UV photodesorption and UV induced organic chemistry, to map out the chemical evolution of ices during the pre- and proto-stellar stages of star formation. The protostellar stage is followed by the formation of a protoplanetary disk, with unique physical properties that may result in the activation new chemical pathways. I will end with showing exciting new observational results on the chemistry in protoplanetary disks, acquired within the ongoing SMA legacy program DISCS, and also some thoughts on future observational and laboratory programs to expand our knowledge of the chemical evolution during planet formation.