4 Comments on individual sources

- 0800+472: the source has an overall extent of $\sim$1 arcsec in the VLA 8.4 GHz image (see Paper I). About 40% of the flux density is missing in our VLBA image. Since $\sim$90% of the 8.4 GHz flux density originates within a region of $\sim$120 mas, it is likely that most of the missing flux density is on angular scales of this order. The VLBA source structure is strongly bent and the bending probably continues to match the arcsec structure. It is possible that we are in presence of an asymmetric core-jet, with a weak core, as in Stanghellini et al. (2001).

- 0809+404: at arcsec scale the source appears as a very asymmetric double, with 1.2 $^{\prime\prime}$ separation and a flux density ratio $\sim$100:1 at 4.9 GHz (see Paper I). The structure we see here corresponds to the brighter component and is rather amorphous, with the PA of the major axis misaligned by $\sim$40$^\circ$ with respect to the orientation of the outer weak component. About 45% of the total flux density is missing in our VLBA observations.

- 1007+422: about 15% of total flux density is missing in our VLBA observations.

- 1044+454: on the arcsec scale the source appears as a very asymmetric double, with flux density ratio $\sim$20:1 at 4.9 GHz (see Paper I). On the VLBA scale the structure of the northernmost brighter component is again double and asymmetric, along the same PA but on a $\sim$six times smaller scale. The source could be either a core-jet with a weak core or a very asymmetric MSO. About 12% of the total flux density is missing in our VLBA observations.

- 1049+384: About 12% of the total flux density is missing in our VLBA observations.

- 1136+420: on the arcsec scale the source appears as a very asymmetric double, with flux density ratio $\sim$20:1 at 4.9 GHz (see Paper I), roughly oriented in the East-West direction. At VLBA resolution only the brighter component is visible and displays a very amorphous structure. About 30% of the total flux density is missing in our VLBA observations.

- 1314+453: about 15% of the total flux density is missing in the VLBA image.

- 1343+386: a weak feature, accounting for $\sim$9 mJy is present to the North of the major components.

Figure 4: Plot of the correlated flux density versus projected baseline for the source B3 1314+453. The horizontal arrows indicate the integrated flux density in the VLBA image and total flux density from the VLA as given in Table 1.

- 1432+428: a weak feature, accounting for $\sim$10 mJy is present to the South of the major components. About 13% of the total flux density is missing in our VLBA observations.

- 2348+450: about 20% of total flux density is missing in the VLBA image.