Tracing grain growth from clouds to cores and disks Leonardo Testi ESO, Muenchen, DE
Solids in protoplanetary disks are very different from those of the interstellar medium. Tracing the growth of grains and of their icy mantles is essential to understand a broad range of issues: the evolution of the gas to dust ratio, the extinction laws, and the importance of ice chemistry (and the release of processed molecules in the gas phase) from the diffuse medium to the cores and disks. Tracing the various steps of grain evolution is also critical to test models from grain growth and the assembly of large bodies (from pebbles to rocky cores of planets). I will discuss the results of our programme of observationally trace dust evolution combining measurements of infrared extinction and infrared through submillimetre emission. Combining our own and other groups measurements of dust properties we trace the evolution of dust from interstellar medium bare sub-micron size particles, through the formation of ice mantles and larger particles in molecular clumps, cores and protostars, all the way to pebbles covered by thick ice mantles in protoplanetary disks.
Collaborators: D. Johnstone, JCMT/NRC A. Miotello, MPE L. Ricci, Caltech	Suggested Session: Cores to Disks