Variability over the over the eight observational epochs. We show the peak flux intensity and the integrated flux density in Stokes I (top) and Stokes V (middle), and the size of the deconvolved component of the emission in Stokes I, calculated by using the values and errors of the major and minor axes in Table 2. Vertical bars show 1σ errors. For the days without a Stokes V detection, we have provided 3σ upper limits for the peak flux.