most of the extended emission is resolved out (Figures \[fig:vlbimap\]-d to \[fig:vlbimap\]-g) and only a few compact knots remain visible. Figure \[fig:vlbimap\]-e at 4.8 GHz highlights the core-jet structure within 150 pc ($\sim$30 mas); the ridge line appears to oscillate from side to side. At the resolution of this image the core A is resolved into two sub-components, which we denote A1 and A2. Figure \[fig:vlbimap\]-g at 8.3 GHz focuses on the nuclear region within 50 pc ($\sim$10 mas) and clearly shows two well-separated components. Beyond this distance the brightness of the inner jet is below the detection threshold. This is consistent with what was seen in the 8.4- and 15.4-GHz images from the 1996 VLBA observations [@Wor04].

Figure \[fig:core\] focuses on the core A and inner jet out to the hot spot B. Figure \[fig:core\]-a shows the 1.5-GHz image from 2004. Unlike the image already shown in Figure \[fig:vlbimap\]-b, this image was produced with a super-uniform weighting of the $uv$ plane (see the caption of Figure \[fig:core\] for details). The high-resolution 1.5-GHz image reveals a quasi-oscillatory jet extending to a distance of $\sim$40 mas ($\sim$200 pc) to the north of the core A. Interestingly, Figure \[fig:core\]-b shows similar oscillatory 