Astronomy Colloquium

Molecules are unique tracers of the dynamical and chemical evolution of star and planet forming regions. Thus, astrochemistry is crucial to test theories and shed light on our origins. Stars and planetary systems in our Galaxy form within dense (n(H2) ~ 100,000 cm-3) and cold (T ~ 10 K) fragments of interstellar molecular clouds, called pre-stellar cores. Important chemical processes take place at this early stage, such as isotope fractionation, production of complex organic molecules and growth of thick icy mantles onto dust grains, where water and organics are stored, and which boost dust coagulation. These processes can affect later phases of star and planet formation, which can now be traced with powerful interferometers such as ALMA and NOEMA. In this talk I shall review the chemical and physical structure of pre-stellar and protostellar cores, as well as theoretical work on prototostellar disk formation and early evolution. Links to protoplanetary disks and our Solar System will be made.