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We wish to constrain the possible contribution of a magnetohydrodynamic diskwind (DW) to the HH212 molecular jet. We mapped the flow base with ALMA Cycle 4at 0.13"$\sim$ 60 au resolution and compared these observations with syntheticDW predictions. We identified, in SO/SO$_2$, a rotating flow that is wider andslower than the axial SiO jet. The broad outflow cavity seen in C$^{34}$S isnot carved by a fast wide-angle wind but by this slower agent. Rotationsignatures may be fitted by a DW of a moderate lever arm launched out to $\sim$40 au with SiO tracing dust-free streamlines from 0.05-0.3 au. Such a DW couldlimit the core-to-star efficiency to $\leq$50%.

ALMA discovery of a rotating SO/SO$_2$ flow in HH212. A possible MHD disk wind?