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We wish to test the origins proposed for the extended hot H2 at 2000K aroundthe atomic jet from the T Tauri star DGTau, in order to constrain thewide-angle wind structure and the possible presence of an MHD disk wind. Wepresent flux calibrated IFS observations in H2 1-0 S(1) obtained withSINFONI/VLT. Thanks to spatial deconvolution by the PSF and to accuratecorrection for uneven slit illumination, we performed a thorough analysis andmodeled the morphology, kinematics, and surface brightness. We also comparedour results with studies in [FeII], [OI], and FUV-pumped H2. Thelimb-brightened H2 emission in the blue lobe is strikingly similar toFUV-pumped H2 imaged 6yr later, confirming that they trace the same hot gas andsetting an upper limit of 12km/s on any expansion proper motion. The wide-angleH2 rims are at lower blueshifts than probed by narrow long-slit spectra. Weconfirm that they extend to larger angle and to lower speed the onion-likevelocity structure observed in optical atomic lines. The latter is shown to besteady over more/equal than 4yr but undetected in [FeII] by SINFONI, probablydue to strong iron depletion. The H2 rim thickness less/equal than 14AU rulesout excitation by C-shocks, and J-shock speeds are constrained to 10km/s. Wefind that explaining the H2 wide-angle emission with a shocked layer requireseither a recent outburst (15yr) into a pre-existing ambient outflow or anexcessive wind mass flux. A slow photoevaporative wind from the denseirradiated disk surface and an MHD disk wind heated by ambipolar diffusion seemto be more promising and need to be modeled in more detail.

Origin of the wide-angle hot H2 in DG Tauri: New insight from SINFONI spectro-imaging