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HH 211 is a highly collimated jet originating from a nearby young Class 0protostar. Here is a follow-up study of the jet with our previous observationsat unprecedented resolution up to ~ 0.3" in SiO (J=8-7), CO (J=3-2), and SO(N_J=8_9-7_8). SiO, CO, and SO can all be a good tracer of the HH 211 jet,tracing the internal shocks in the jet. Although the emissions of thesemolecules show roughly the same morphology of the jet, there are detaileddifferences. In particular, the CO emission traces the jet closer to the sourcethan the SiO and SO emissions. In addition, in the better resolved internalshocks, both the CO and SO emission are seen slightly ahead of the SiOemission. The jet is clearly seen on both sides of the source with more thanone cycle of wiggle. The wiggle is reflection-symmetric about the source andcan be reasonably fitted by an orbiting source jet model. The best-fitparameters suggest that the source itself could be a very low-mass protobinarywith a total mass of ~ 60 M_Jup and a binary separation of ~ 4.6 AU. Theabundances of SiO and SO in the gas phase are found to be highly enhanced inthe jet as compared to the quiescent molecular clouds, even close to within 300AU from the source where the dynamical time scale is <10 yrs. The abundanceenhancements of these molecules are closely related to the internal shocks. Thedetected SiO is either the consequence of the release of Si-bearing materialfrom dust grains or of its formation via gas chemistry in the shocks. The SO,on the other hand, seems to form via gas chemistry in the shocks.

The reflection-symmetric wiggle of the young protostellar jet HH 211