A rotating fast bipolar wind and disk system around the B[e]-type star MWC 922.

We present interferometric observations with the Atacama Large Millimeter Array (ALMA) of the free-free continuum and recombination line emission at 1 and 3 mm of the "Red Square Nebula" surrounding the B[e]-type star MWC922. The unknown distance to the source is usually taken to be =1.7-3 kpc. The unprecedented angular resolution and exquisite sensitivity of these data unveil, for the first time, the structure and kinematics of the emerging, compact ionized region at its center. We imaged the line emission of H30 and H39, previously detected with single-dish observations, as well as of H51, H55, and H63, detected for the first time in this work. The line emission is seen over a full velocity range of ~180 km s arising in a region of diameter (less than a few hundred au) in the maser line H30, which is the most intense transition reported here. We resolve the spatio-kinematic structure of a nearly edge-on disk rotating around a central mass of ~10 (=1.7 kpc) or ~18 (=3 kpc), assuming Keplerian rotation. Our data also unveil a fast (~100 km s) bipolar ejection (a jet?) orthogonal to the disk. In addition, a slow (<15 km s) wind may be lifting off the disk. Both, the slow and the fast winds are found to be rotating in a similar manner to the ionized layers of the disk. ~ ). The launching radius of the fast wind is found to be <30-51 au i.e., smaller than the inner rim of the ionized disk probed by our observations. We believe that the fast wind is actively being launched, probably by a disk-mediated mechanism in a (accretion?) disk around a possible compact companion. We have modelled our observations using the radiative transfer code MORELI. This has enabled us to describe with unparalleled detail the physical conditions and kinematics in the inner layers of MWC 922, which has revealed itself as an ideal laboratory for studying the interplay of disk rotation and jet-launching. Although the nature of MWC 922 remains unclear, we believe it could be a ~15 post-main sequence star in a mass-exchanging binary system. If this is the case, a more realistic value of the distance may be ~3 kpc.