GBT20B-152

Probing the dust and gas evolution in starless cores

Abstract

Dust grains carry the budget of the cooling radiation and the knowledge of the grain properties is important to better understand the processes leading to star formation. In addition, grain surface chemistry plays an important role in the formation and freeze-out of molecules that are key to the chemical network. However, the expected evolution of dust properties such as grain sizes from the diffuse interstellar medium to dense cores is still an open issue. In this proposal, we ask for MUSTANG-2.0 observations towards 6 starless cores selected from the GEMS sample (30m IRAM Large Program) with the aim of studying the evolution of grain properties and their dependence on the environment. Eventually, we plan to delineate a comprehensive evolutionary trend by combining the dust properties derived from MUSTANG-2.0 observations with the gas chemical composition as determined with GEMS data and performing a detailed comparison with state-of-the-art hydrodynamical models.

Investigators

Name	Institution
David Navarro Almaida	Instituto Geográfico Nacional
Charles Romero	Pennsylvania, University of; Virginia, University of; Center for Astrophysics | Harvard & Smithsonian
Tony Mroczkowski	European Southern Observatory; Institut de Ciències de l'Espai
Simon Dicker	Pennsylvania, University of
Brian Mason	National Radio Astronomy Observatory
Asuncin Fuente *	Instituto Geográfico Nacional
Ana Chacon-Tanarro	Max-Planck-Institut für extraterrestrische Physik; Instituto Geográfico Nacional
Marina Rodriguez-Baras	Instituto Geográfico Nacional
Craig Sarazin	Virginia, University of
Thomas Devlin	Pennsylvania, University of; Rutgers, The State University of New Jersey
Mara Jos Maureira	Yale University; Max-Planck-Institut für extraterrestrische Physik
Jonathan Sievers	Toronto, University of; McGill University; Princeton University; KwaZulu-Natal, University of
Paola Caselli	Max-Planck-Institut für extraterrestrische Physik; Leeds, University of
Carsten Kramer	Instituto de RadioAstronomia Milimetrica

* indicates the PI