HH 211 is a highly collimated jet originating from a nearby young Class 0 protostar .
Here is a follow-up study of the jet with our previous observations at unprecedented resolution up to \sim 0 ^ { \prime \prime } _ { { } ^ { \textrm { . } } } 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 these molecules show roughly the same morphology of the jet , there are detailed differences .
In particular , the CO emission traces the jet closer to the source than the SiO and SO emissions .
In addition , in the better resolved internal shocks , both the CO and SO emission are seen slightly ahead of the SiO emission .
The jet is clearly seen on both sides of the source with more than one cycle of wiggle .
The wiggle is reflection-symmetric about the source and can be reasonably fitted by an orbiting source jet model .
The best-fit parameters suggest that the source itself could be a very low-mass protobinary with a total mass of \sim 60 M _ { \textrm { \scriptsize Jup } } and a binary separation of \sim 4.6 AU .
The abundances of SiO and SO in the gas phase are found to be highly enhanced in the jet as compared to the quiescent molecular clouds , even close to within 300 AU from the source where the dynamical time scale is < 10 yrs .
The abundance enhancements of these molecules are closely related to the internal shocks .
The detected SiO is either the consequence of the release of Si-bearing material from 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 .