Submillimeter arcsecond-resolution mapping of the highly collimated protostellar jet HH 211

We have mapped the protostellar jet HH 211 in 342 GHz continuum, SiO(J = 8-7), and CO(J = 3-2) emission at similar to 1 '' resolution with the Submillimeter Array. Thermal dust emission is seen in continuum at the center of the jet, tracing an envelope and a possible optically thick compact disk (with a size < 130 AU) around the protostar. A knotty jet is seen in CO and SiO as in H-2, but extending closer to the protostar. It consists of a chain of knots on each side of the protostar, with an interknot spacing of similar to 2 ''-3 '' or 600-900 AU and the innermost pair of knots at only similar to 1.7 '' or 535 AU from the protostar. These knots likely trace unresolved internal (bow) shocks (i.e., working surfaces) in the jet, with a velocity range up to similar to 25 km s(-1). The two-sided mass-loss rate of the jet is estimated to be similar to(0.7-2.8)x10(-6) M(circle dot)yr(-1). The jet is episodic, precessing, and bending. A velocity gradient is seen consistently across two bright SiO knots (BK3 and RK2) perpendicular to the jet axis, with similar to 1.5 +/- 0.8 km s(-1) at similar to 30 +/- 15AU, suggesting the presence of jet rotation. The launching radius of the jet, derived from the potential jet rotation, is similar to 0.15-0.06 AU in the inner disk.