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HH 211-mms is one of the youngest Class 0 protostellar systems in Perseus at~ 235 pc away. We have mapped its central region at up to ~ 7 AU (0.03")resolution. A dusty disk is seen deeply embedded in a flattened envelope, withan intensity jump in dust continuum at ~ 350 GHz. It is nearly edge-on and isalmost exactly perpendicular to the jet axis. It has a size of ~ 30 au alongthe major axis. It is geometrically thick, indicating that the (sub)millimeterlight emitting grains have yet to settle to the midplane. Its inner part isexpected to have transformed into a Keplerian rotating disk with a radius of ~10 au. A rotating disk atmosphere and a compact rotating bipolar outflow aredetected in SO. The outflow fans out from the inner disk surfaces and isrotating in the same direction as the flattened envelope, and hence could tracea disk wind carrying away angular momentum from the inner disk. From therotation of the disk atmosphere, the protostellar mass is estimated to be <~ 50M_Jup. Together with results from the literature, our result favors a modelwhere the disk radius grows linearly with the protostellar mass, as predictedby models of pre-stellar dense core evolution that asymptotes to an $r^{-1}$radial profile for both the column density and angular velocity.

ALMA observations of the very young Class 0 protostellar system HH 211-mms: a 30-au dusty disk with a disk-wind traced by SO?