ROTATION AND OUTFLOW MOTIONS IN THE VERY LOW-MASS CLASS 0 PROTOSTELLAR SYSTEM HH 211 AT SUBARCSECOND RESOLUTION

HH 211 is a nearby young protostellar system with a highly collimated jet. We have mapped it in 352 GHz continuum, SiO (J = 8 - 7), and HCO(+) (J = 4 - 3) emission at up to similar to 0 ''.2 resolution with the Submillimeter Array (SMA). The continuum source is now resolved into two sources, SMM1 and SMM2, with a separation of similar to 84 AU. SMM1 is seen at the center of the jet, probably tracing a (inner) dusty disk around the protostar driving the jet. SMM2 is seen to the southwest of SMM1 and may trace an envelope-disk around a small binary companion. A flattened envelope-disk is seen in HCO(+) around SMM1 with a radius of similar to 80 AU perpendicular to the jet axis. Its velocity structure is consistent with a rotation motion and can be fitted with a Keplerian law that yields a mass of similar to 50 +/- 15 M(Jup) (a mass of a brown dwarf) for the protostar. Thus, the protostar could be the lowest mass source known to have a collimated jet and a rotating flattened envelope-disk. A small-scale (similar to 200 AU) low-speed (similar to 2 km s(-1)) outflow is seen in HCO(+) around the jet axis extending from the envelope-disk. It seems to rotate in the same direction as the envelope-disk and may carry away part of the angular momentum from the envelope-disk. The jet is seen in SiO close to similar to 100 AU from SMM1. It is seen with a C-shaped bending. It has a transverse width of less than or similar to 40 AU and a velocity of similar to 170 +/- 60 km s(-1). A possible velocity gradient is seen consistently across its innermost pair of knots, similar to 0.5 km s(-1) at similar to 10 AU, consistent with the sense of rotation of the envelope-disk. If this gradient is an upper limit of the true rotational gradient of the jet, then the jet carries away a very small amount of angular momentum of less than or similar to 5 AU km s(-1) and thus must be launched from the very inner edge of the disk near the corotation radius.