All Tables

• Table 1: Source positions. All positions have been proper motion corrected to the observation epoch, as described in the text, but no attempt has been made to correct for orbital motion. The uncertainty in the last digit is given in parentheses. References: (a) Hipparcos position proper motion corrected to observation epoch with Hipparcos proper motion. (b) Offset from T Tau N given by Duchêne et al. (2002). (c) Offset from T Tau Sa given by Köhler et al. (2000). (d) Johnston et al. (2003).
• Table 2: Comparison of fluxes (in mJy) between VLA and VLBI maps. The peak and integrated flux values for each object in each time segment (0-6 h, 6-10 h, 10-11 h) are listed for the VLA maps. The VLBI fluxes are measured from the visibility plots shown in Fig. 4. All values are in mJy, with uncertainties in parentheses. The difference between the VLA integrated flux density and the VLA peak flux indicates the resolved flux in the VLA map (5th column). The difference between VLA peak and VLBI fluxes indicates the amount of flux which is compact at the VLA but resolved out by the VLBI (6th column).
• Table 3: Upper limits on source sizes at various times for different polarizations. The size is given as the half width half maximum of the fitted Gaussian, H, the corresponding HWHM on the sky in milliarcseconds and the physical source size for a distance of 140 pc (Elias 1978) in solar radii.
• Table 4: Brightness temperature lower limits for T Tau Sb. The fourth column contains brightness temperatures for the source size constraint listed in Col. 2. The fifth column shows values calculated for an assumed constant source size upper limit of 0.48 mas.