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We present results of the second phase of our near-ultraviolet investigationinto protostellar jet rotation using HST/STIS. We obtain long-slit spectra atthe base of five T Tauri jets to determine if there is a difference in radialvelocity between the jet borders which may be interpreted as a rotationsignature. These observations are extremely challenging and push the limits ofcurrent instrumentation, but have the potential to provide long-awaitedobservational support for the magneto-centrifugal mechanism of jet launching inwhich jets remove angular momentum from protostellar systems. We successfullydetect all five jet targets (from RW Aur, HN Tau, DP Tau and CW Tau) in severalnear-ultraviolet emission lines, including the strong Mg II doublet. However,only RW Aur's bipolar jet presents sufficient signal-to-noise for analysis. Theapproaching jet lobe shows a difference of 10 km/s in a direction which agreeswith the disk rotation sense, but is opposite to previously published opticalmeasurements for the receding jet. The near-ultraviolet difference is not foundsix months later, nor is it found in the fainter receding jet. Overall, in thecase of RW Aur, differences are not consistent with a simple jet rotationinterpretation. Indeed, given the renowned complexity and variability of thissystem, it now seems likely that any rotation signature is confused by otherinfluences, with the inevitable conclusion that RW Aur is not suited to a jetrotation study.

Jet rotation investigated in the near-ultraviolet with HST/STIS