adjusted the flux scale of the first epoch by this relative gain factor. Figure 1 shows the corrected ratio of the flux densities of all the sources. The reduced $\chi^2$ of the estimate of the gain constant is 0.76, which suggests that the flux density errors may be slightly overestimated by about 15 percent. Since the $\chi^2$ is close to unity we conclude that there is no evidence for variability among the 11 sources, whereas the changes in flux densities of S-1 and the jet are highly significant. Figure 2 shows contour images of the emission observed at 8.46 GHz in the two epochs, as well as the difference image (2006.42 - 2003.74). The positions, flux densities, and deconvolved angular sizes of the sources identified in Fig. 2 are given in Table 1. The observed parameters for each component were determined from a linearized least-squares fit to a Gaussian ellipsoid function using the task JMFIT of AIPS. In Table 2 we summarize the parameters of the proper motions of all sources in the field, derived from differences of the positions in the two epochs. Note that the position of the jet changes slightly between the epochs by about 6 mas 