  In this Letter, we present a series of seven observations of the compact,
non-thermal radio source associated with T Tauri South made with the Very Long
Baseline Array over the course of one year. The emission is found to be
composed of a compact structure most certainly originating from the
magnetosphere of an underlying pre-main sequence star, and a low-brightness
extension which may result from reconnection flares at the star-disk interface.
The accuracy of the absolute astrometry offered by the VLBA allows very precise
determinations of the trigonometric parallax and proper motion of T Tau South.
The proper motion derived from our VLBA observations agrees with that measured
with the VLA over a similar period to better than 2 mas yr$^{-1}$, and is fully
consistent with the infrared proper motion of T Tau Sb, the pre-main sequence M
star with which the radio source has traditionally been associated. The
parallax, $\pi$ = 7.07 $\pm$ 0.14 mas, corresponds to a distance of
141.5$^{+2.8}_{-2.7}$ pc.
