Lee, Chin-FeiChin-FeiLeeLi, Zhi-YunZhi-YunLiCODELLA, CLAUDIOCLAUDIOCODELLA0000-0003-1514-3074Ho, Paul T. P.Paul T. P.HoPODIO, LINDALINDAPODIO0000-0003-2733-5372Hirano, NaomiNaomiHiranoShang, HsienHsienShangTurner, Neal J.Neal J.TurnerZhang, QizhouQizhouZhang2020-11-162020-11-1620180004-637Xhttp://hdl.handle.net/20.500.12386/28362HH 212 is a Class 0 protostellar system found to host a “hamburger”-shaped dusty disk with a rotating disk atmosphere and a collimated SiO jet at a distance of ∼400 pc. Recently, a compact rotating outflow has been detected in SO and SO<SUB>2</SUB> 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 rotating outflow shell and a collimated jet, with the observations in the same S-bearing molecules at ∼16 au (0.″04) resolution. The collimated jet is aligned with the SiO jet, tracing the shock interactions in the jet. The wide-opening outflow shell is seen extending out from the inner disk around the SiO jet and has a width of ∼100 au. It is not only expanding away from the center, but also rotating around the jet axis. The specific angular momentum of the outflow shell is ∼40 au km s<SUP>-1</SUP>. Simple modeling of the observed kinematics suggests that the rotating outflow shell can trace either a disk wind or disk material pushed away by an unseen wind from the inner disk or protostar. We also resolve the disk atmosphere in the same S-bearing molecules, confirming the Keplerian rotation there.STAMPAenArticle10.3847/1538-4357/aaae6d2-s2.0-85044782717000428051200013https://iopscience.iop.org/article/10.3847/1538-4357/aaae6d2018ApJ...856...14LFIS/05 - ASTRONOMIA E ASTROFISICA