  HH 212 is a nearby (460 pc) protostellar jet discovered in H$_2$ powered by a
Class 0 source, IRAS 05413-0104, in the L1630 cloud of Orion. It is highly
collimated and symmetric with matched pairs of bow shocks on either side of the
source. We have mapped it in 850 $\mu$m continuum, SiO ($J=8-7$), CO ($J=3-2$),
SO ($N_J=8_9-7_8$), HCO$^+$ ($J = 4-3$), and H$^{13}$CO$^+$ ($J = 4-3$)
emission simultaneously at $\sim$ 1$''$ resolution with the Submillimeter Array
(SMA). Thermal dust emission is seen in continuum around the source, mainly
arising from an inner envelope (i.e., the inner part of a previously seen
flattened envelope) and a possible disk. The inner envelope is also seen with
rotation in CO, HCO$^+$, and probably SO. Like H$_2$ emission, CO and SiO
emission are seen along the jet axis but extending closer to the source,
tracing the bow shocks with a broad range of velocities and the continuous
structures in between. SO emission is seen only around the source, forming a
jetlike structure extending along the jet axis from the source, likely tracing
the jet near the launching region. The jet is episodic and bending. It may also
be slightly precessing as the jetlike SO structure shows a slight S-shaped
symmetry about the source. A hint of jet rotation is also seen across the jet
axis. Internal outflow shells are seen in CO and HCO$^+$, associated with the
bow shocks in the inner part of the jet. The bases of the HCO$^+$ shells are
seen with a hint of rotation similar to that seen in the inner envelope,
probably consisted mainly of the material extended from the inner envelope and
even the possible disk.
