HST FUV C iv observations of the hot DG Tauri jet

Protostellar jets are tightly connected to the accretion pr ocess and regulate the angular momentum balance of accreting star-disk systems. The DG Tau jet is one of the best-studied protostellar jets and contains plasma with temperatures ranging over three orders of magnitude within the innermost 50 AU of the jet. We present new Hubble Space Telescope (HST) far ultraviolet (FUV) long-slit spectra spatially resolving the Civ emission (T∼ 10 5 K) from the jet for the first time, and quasi-simultaneous HST observations of optical forbidden emission lines ([Oi], [Nii], [Sii] and [Oiii]) and fluorescent H2 lines. The Civ emission peaks at≈ 42 AU from the stellar position and has a FWHM of≈ 52 AU along the jet. Its deprojected velocity of around 200 km s −1 decreases monotonically away from the driving source. In addition, we compare our HST data with the X-ray emission from the DG Tau jet. We investigate the requirements to explain the data by an initially hot jet c ompared to local heating. Both scenarios indicate a mass loss by the T∼ 10 5 K jet of∼ 10 −9 M⊙ yr −1 , i.e., between the values for the lower temperature jet ( T≈ 10 4 K) and the hotter X-ray emitting part (T& 10 6 K). However, a simple initially hot wind requires a large launching region (∼ 1 AU), and we therefore favor local heating.