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HH 212 is a Class 0 protostellar system found to host a "hamburger"-shapeddusty disk with a rotating disk atmosphere and a collimated SiO jet at adistance of ~ 400 pc. Recently, a compact rotating outflow has been detected inSO and SO2 toward the center along the jet axis at ~ 52 au (0.13") resolution.Here we resolve the compact outflow into a small-scale wide-opening rotatingoutflow shell and a collimated jet, with the observations in the same S-bearingmolecules at ~ 16 au (0.04") resolution. The collimated jet is aligned with theSiO jet, tracing the shock interactions in the jet. The wide-opening outflowshell is seen extending out from the inner disk around the SiO jet and has awidth of ~ 100 au. It is not only expanding away from the center, but alsorotating around the jet axis. The specific angular momentum of the outflowshell is ~ 40 au km/s. Simple modeling of the observed kinematics suggests thatthe rotating outflow shell can trace either a disk wind or disk material pushedaway by an unseen wind from the inner disk or protostar. We also resolve thedisk atmosphere in the same S-bearing molecules, confirming the Keplerianrotation there.

A 100 au-Wide Bipolar Rotating Shell Emanating From The HH 212Protostellar Disk: A Disk Wind?