Recent high-resolution, high-sensitivity observations of protostellar jets have shown many to possess an underlying `wiggle' structure. HH 211 is one such example where recent sub-mm observations revealed a clear re ection-symmetric wiggle. An explanation for this is that the HH211 jet source is moving as part of a protobinary system. Here we test this assumption by simulating HH211 through 3D hydrodynamic simulations using the pluto code with a molecular chemistry and cooling module, and initial conditions based on an analytical model derived from SMA observations. Molecular chemistry allows us to accurately plot synthetic molecular emission maps and position-velocity diagrams for direct comparison to observa- tions, enabling us to test the observational assumptions and put constraints on the physical parameters of HH211. Our preliminary results show that the re ection-symmetric wiggle can be recreated through the assumption of a jet source being part of a binary system.

We present observational results characterizing molecular out ows from very low-mass objects in ρ Ophiuchi and Taurus. Our results provide us with important implications that clarify the formation process of very low-mass objects.