Working Groups
WG1: Protostellar disks and multiple systems (A. Maury, L. Testi, Ph. André; R. Launhardt). This group will focus on the 1.3mm and 2.7mm continuum PdBI data to map the inner structure of dusty Class 0 envelopes, search for compact disks and secondary components on scales <100 AU, and clarify their nature thanks to the molecular line observations analysed by WG2,WG3.
WG2: Molecular jets and outflows (C. Codella, B. Lefloch, F. Gueth, S. Cabrit). This working group will focus on the 12CO and SiO data to trace the structure and kinematics of the molecular outflows and jets, respectively, and correlate them with envelope/disk properties to clarify the mechanisms responsible for protostellar ejection.
WG3: Envelope structure, kinematics, and chemistry (S. Maret, S. Bottinelli, A. Bacmann, A. Belloche). This working group will analyse and model line emission from C18O, N2H+, and CH3OH to unveil the 3D structure, kinematics, and angular momentum of protostellar envelopes from large to small scales, and to probe the heating process and the origin of hot corinos.
WG4: Numerical simulations and radiative transfer (P. Hennebelle, R. Klessen, C. Dullemond, B. Commercon). This working group will carry out a dedicated modeling program, using a chain of three state-of-the art, complementary codes to interpret the PdBI data. 3D MHD numerical simulations of collapsing cores will be carried out using the RAMSES code (eg. Hennebelle & Ciardi 2009) and then coupled to a chemical model (S. Maret) to post-process chemical abundances. The RADMC 3D radiative code (C. Dullemond) will then be used to compute the lines and dust continuum. Finally, these will be processed with the PdBI simulator to produce synthetic observations comparable to the observed maps. All models and reduced datacubes will be put on a public website at the end of the project.
