The mass accretion rate is a crucial parameter for the study of the evolution of accretion discs around young lowmass stellar and substellar objects (YSOs). We revisit the case of MY Lup, an object where VLT/X-Shooter data suggested a negligible mass accretion rate, and show it to be accreting on a level similar to other Class II YSOs in Lupus based on Hubble Space Telescope (HST) observations. In our HST-Cosmic Origins Spectrograph (HST-COS) and -Space Telescope Imaging Spectrograph (HST-STIS) spectra, we find many emission lines, as well as substantial far-ultraviolet (FUV) continuum excess emission, which can be ascribed to active accretion. The total luminosity of the C iv λ1549Å doublet is 4.1×10 −4 L . Using scalings between accretion luminosity, Lacc, and C iv luminosity from the literature, we derive Lacc∼2×10 −1 L , which is more than an order of magnitude higher than the upper limit estimated from the X-Shooter observations. We discuss possible reasons for the X-Shooter-HST discrepancy, the most plausible being that the low contrast between the continuum excess emission and the photospheric+chromospheric emission at optical wavelengths in MY Lup hampered detection of excess emission. The luminosity of the FUV continuum and C iv lines, strong H2 fluorescence, and a "1600 A Bump" place MY Lup in the class of accreting objects with gas-rich discs. So far, MY Lup is the only peculiar case in which a significant difference between the HST and X-ShooterṀacc estimates exists that is not ascribable to variability. The mass accretion rate inferred from the revisited Lacc estimate isṀacc ∼ 1( +1.5 −0.5 )×10 −8 M yr −1 . This value is consistent with the typical value derived for accreting YSOs of similar mass in Lupus and points to less clearing of the inner disc than indicated by near-and mid-infrared observations. This is confirmed by Atacama Large Millimeter Array (ALMA) data, which show that the gaps and rings seen in the sub-millimetre are relatively shallow.

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 12 CO, 13 CO, and C 18 O 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 • from the vertical) above the disk with a velocity of ≈ 3.1 km s −1 . 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.

Following a production error, many arcsecond signs ( ) were replaced with degree signs ( • ) in the original version of this paper. Here we republish the paper in its entirety, correcting the errors.Article published by EDP Sciences C1, page 1 of 1 A&A 620, L1 (2018) ABSTRACTAims. 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 Tauri 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 12 CO, 13 CO, and C 18 O to study the Keplerian disk of DG Tauri 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 • from the vertical) above the disk with a velocity of ≈3.1 km s −1 . 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.