Tabone, B.B.TaboneCabrit, S.S.CabritBianchi, E.E.BianchiFerreira, J.J.FerreiraPineau des Forêts, G.G.Pineau des ForêtsCODELLA, CLAUDIOCLAUDIOCODELLAGusdorf, A.A.GusdorfGueth, F.F.GuethPODIO, LINDALINDAPODIOChapillon, E.E.Chapillon2020-09-142020-09-1420170004-6361http://hdl.handle.net/20.500.12386/27366We wish to constrain the possible contribution of a magnetohydrodynamic disk wind (DW) to the HH212 molecular jet. We mapped the flow base with ALMA Cycle 4 at 0.̋13 60 au resolution and compared these observations with synthetic DW predictions. We identified, in SO/SO<SUB>2</SUB>, a rotating flow that is wider and slower than the axial SiO jet. The broad outflow cavity seen in C<SUP>34</SUP>S is not carved by a fast wide-angle wind but by this slower agent. Rotation signatures may be fitted by a DW of a moderate lever arm launched out to 40 au with SiO tracing dust-free streamlines from 0.05-0.3 au. Such a DW could limit the core-to-star efficiency to ≤50%.STAMPAenArticle10.1051/0004-6361/2017316912-s2.0-85034420902000415265300001https://www.aanda.org/articles/aa/abs/2017/11/aa31691-17/aa31691-17.html2017A&A...607L...6TFIS/05 - ASTRONOMIA E ASTROFISICA