  Spectro-astrometry is used to investigate the low velocity component (LVC) of
the optical forbidden emission from the T Tauri stars RU Lupi and AS 205 N.
Both stars also have high velocity forbidden emission (HVC) which is tracing a
jet. For AS 205 N, analysis reveals a complicated outflow system. For RU Lupi,
the [O I] 6300 and [S II] 6716, 6731 LV narrow component (NC) is offset along
the same position angle (PA) as the HVC but with a different velocity gradient
than the jet, in that displacement from the stellar position along the rotation
axis is decreasing with increasing velocity. From the LVC NC PA and velocity
gradient, it is inferred that the NC is tracing a wide angled MHD disk wind. A
photoevaporative wind is ruled out. This is supported by a comparison with a
previous spectro-astrometric study of the CO fundamental line. The decrease in
offset with increasing velocity is interpreted as tracing an increase in the
height of the wind with increasing disk radius. This is one of the first
measurements of the spatial extent of the forbidden emission line LVC NC (~ 40
au, 8 au for RU~Lupi in the [S II] 6731 and [O I] 6300 lines) and the first
direct confirmation that the LVC narrow component can trace an MHD disk wind.
