Contribution Contributed Talk
Astrochemistry at work in pristine protostellar jet-disk systems
What are the basic chemical mechanisms that led atoms to molecules in star forming regions? What is the role of the pre-solar chemistry in the present chemical composition of the Solar System bodies, planets, comets, and asteroids? The molecular complexity builds up at each step of the process leading to star formation, starting from simple molecules and ending up in Complex Organic Molecules (COMs). The detection of COMs is thus key to understanding the formation of pre-biotic molecules in the interstellar medium and their subsequent delivery onto planetary systems. However, observations of COMs are still instrumental in making progress; it is of paramount importance to have reliable information on the spatial distribution of COMs in order to investigate whether the regions precursor of planetary systems are already rich in COMs and pre-biotic molecules. This requires spatial resolutions less than 100 AU.
We present here ALMA and NOEMA observations at mm and sub-mm wavelengths of Class 0 protostars (such as L1157 and HH212): thanks to the unprecedented combination of high-sensitivities and high-angular resolutions provided by these new interferometers, it is now possible to image in details the earliest stages of a Sun-like star formation. In particular, we show (i) how to disentangle the COMs emission due to different ingredients of the star formation recipe: warm envelopes and cavities opened by hot and fast jets, accretion disks and shocks, and (ii) how to use protostellar shocks as laboratory to investigate the relative importance of the gas phase processes as compared to a direct formation of COMs on the dust grain surfaces.