Forbidden emission lines in protostellar outflows and jets with MUSE

Flores-Rivera, Lizxandra; Flock, Mario; Kurtovic, Nicolás T.; Husemann, Bernd; Banzatti, Andrea; Ringqvist, Simon C.; Kamann, Sebastian; Müller, André; Fendt, Christian; García Lopez, Rebeca; Marleau, Gabriel-Dominique; Henning, Thomas; Carrasco-González, Carlos; van Boekel, Roy; Keppler, Miriam; Launhardt, Ralf; Aoyama, Yuhiko (2023). Forbidden emission lines in protostellar outflows and jets with MUSE. Astronomy and astrophysics, 670, A126. EDP Sciences 10.1051/0004-6361/202141664

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Context. Forbidden emission lines in protoplanetary disks are a key diagnostic in studies of the evolution of the disk and the host
star. They signal potential disk accretion or wind, outflow, or jet ejection processes of the material that affects the angular momentum
transport of the disk as a result.
Aims. We report spatially resolved emission lines, namely, [O I] λλ6300, 6363, [N II] λλ6548, 6583, Hα, and [S II] λλ6716, 6730 that
are believed to be associated with jets and magnetically driven winds in the inner disks, due to the proximity to the star, as suggested
in previous works from the literature. With a resolution of 0.025 × 0.025 arcsec2, we aim to derive the position angle of the outflow/jet
(PAoutflow/jet) that is connected with the inner disk. We then compare it with the position angle of the dust (PAdust) obtained from pre-
vious constraints for the outer disk. We also carry out a simple analysis of the kinematics and width of the lines and we estimate the
mass-loss rate based on the [O I] λ6300 line for five T Tauri stars.
Methods. Observations were carried out with the optical integral field spectrograph of the Multi Unit Spectroscopic Explorer (MUSE),
at the Very Large Telescope (VLT). The instrument spatially resolves the forbidden lines, providing a unique capability to access the
spatial extension of the outflows/jets that make the estimate of the PAoutflow/jet possible from a geometrical point of view.
Results. The forbidden emission lines analyzed here have their origin at the inner parts of the protoplanetary disk. From the maxi-
mum intensity emission along the outflow/jet in DL Tau, CI Tau, DS Tau, IP Tau, and IM Lup, we were able to reliably measure the
PAoutflow/jet for most of the identified lines. We found that our estimates agree with PAdust for most of the disks. These estimates depend
on the signal-to-noise level and the collimation of the outflow (jet). The outflows/jets in CIDA 9, GO Tau, and GW Lup are too compact
for a PAoutflow/jet to be estimated. Based on our kinematics analysis, we confirm that DL Tau and CI Tau host a strong outflow/jet with
line-of-sight velocities much greater than 100 km s−1, whereas DS Tau, IP Tau, and IM Lup velocities are lower and their structures
encompass low-velocity components to be more associated with winds. Our estimates for the mass-loss rate, ˙Mloss, range between
(1.1–6.5) × 10−7–10−8 M⊙ yr−1 for the disk-outflow/jet systems analyzed here.
Conclusions. The outflow/jet systems analyzed here are aligned within around 1◦ between the inner and outer disk. Further
observations are needed to confirm a potential misalignment in IM Lup.

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