corrected on the assumption of a spectral index of $-0.7$.

The total-intensity images derived from the 1.5-GHz VLBA and 1.65-GHz EVN data are shown in Figures \[fig:vlbimap\]-a to \[fig:vlbimap\]-c. The jet morphology we see is consistent with other published high-resolution images [@Wil90; @Wil91; @Nan91; @Wor04; @Feng05]. The jet extends $\sim$0.5 arcsec in the north-south direction, and consists of a diffuse plume in which a number of bright compact knots are embedded. We label these knots in the image using nomenclature consistent with the previous VLBI observations [@Wil91; @Wor04] (we introduce the labels B3 and D2 for faint features in the B and D regions revealed by our new observations). The active nucleus is thought to be located at the southern end of the jet, i.e., close to the position of component A [@Sim90; @Wil91]. The bright knots, other than the nuclear component A, are thought to be associated with shocks that are created when the jet flow passes through the dense interstellar medium in the host galaxy [@Wil91; @Wor04; @Feng05]. Figure \[fig:vlbimap\]-b enlarges the inner jet region of the 3C 48, showing the structure between A and B2. At $\sim$0.05 arcsec north away from the core A, the jet brightens 