A demonstration of the strong correlation between polarized and unpolarized emission. The polarized emission lags the unpolarized emission, indicating that the centroid of the polarized emission is angularly offset from the bulk of the unpolarized source emission. At this particular epoch, 26 February 2006, the delay was about 55 min and similar for both Stokes Q and U. A typical noise uncertainty after 30 s integration on the I, Q, and U data points is about 1.5 mJy. This is less than the width of the lightcurve for Stokes I. To create a flux density-scaled Stokes I lightcurve, overplotted on the Stokes Q and U lightcurves, we subtracted the 12 h averaged total flux density, multiplied the difference by a scale factor, typically 0.015–0.03, and added the average flux of the relevant Stokes parameter as presented in Fig. 6. The Stokes U signals have negative polarity on this epoch, hence we flipped the sign of the scaled and shifted Stokes I signals. In this plot the data were averaged to a timescale of 30 s.