ALMA detects a radial disk wind in DG Tau

C. Eibensteiner (U. Vienna); Ch. Rab (U. Groningen); Ch. Schneider (U. Hamburg); E. Vorobyov (U. Vienna); J. Forbrich (U. Hertfordshire); M. Audard (U. Geneva); M. Guedel (U. Vienna); O. Dionatos (U. Vienna); S. Kraus (U. Exeter); S. Skinner (U. Colorado)

ALMA detects a radial disk wind in DG Tau

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arxiv 1810.12251 v1 pith:SLEAJHQ6 submitted 2018-10-29 astro-ph.SR astro-ph.GA

M. Guedel (U. Vienna) , C. Eibensteiner (U. Vienna) , O. Dionatos (U. Vienna) , M. Audard (U. Geneva) , J. Forbrich (U. Hertfordshire) , S. Kraus (U. Exeter) , Ch. Rab (U. Groningen) , Ch. Schneider (U. Hamburg)

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S. Skinner (U. Colorado) E. Vorobyov (U. Vienna)

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Aims: We aim to use the high spatial resolution of the Atacama Large Millimeter/submillimeter Array (ALMA) to map the flow pattern of molecular gas near DG Tau and its disk, a young stellar object driving a jet and a molecular outflow. Methods: We use observations from ALMA in the J = 2 - 1 transition of 12CO, 13CO, and C18O to study the Keplerian disk of DG Tau and outflows that may be related to the disk and the jet. Results: We find a new wind component flowing radially at a steep angle (~25 deg from the vertical) above the disk with a velocity of ~ 3.1 km/s. It continues the trend of decreasing velocity for increasing distance from the jet axis ("onion-like velocity structure"). Conclusions: The new component is located close to the protostellar disk surface and may be related to photoevaporative winds.

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Synthetic SKA-Mid observations of simulated MHD and photoevaporative disk winds show that free-free emission is detectable in hours and stacked hydrogen recombination lines are spectrally resolvable in ~10 hours.

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