joining B and A1 remains faint, but the shorter segment joining A1 and A2 can now be seen very clearly. A very small, faint extension also appears to emanate from image C, toward its North, similar to that seen in EVN VLBI observations (Patnaik & Porcas 1996; henceforth PP96).

We fitted elliptical isophotes to the brightness distribution of G in $I$, where it is most clearly defined in our combined images. We adjusted the pixel coordinates of the centers of the isophotes, as well as their ellipticities $e_i = 1 - b_i/a_i$, where $a_i$ and $b_i$ are the major and minor semi-axes of the $i^{th}$ isophote, respectively, and the position angles of the $a_i$. The coordinate offsets of the center of brightness of G from C are listed in Tables 1 and 2. The standard errors in these quantities are $\sim 0\farcs05$, as estimated from the isophote fitting. The mean ellipticity of the fitted isophotes is $e_G = 0.20 \pm 0.02$, and their mean position angle (E of N) on the sky is $\Phi_G = 71^\circ \pm 5^\circ$. The main contributor to the standard errors for these elliptical isophotes is the faintness of the outer regions of G. The residuals 