calibrate the data. From the visibilities images were made using the multi-frequency synthesis technique and robust weighting with a robustness parameter of 0.5, which gives nearly the same sensitivity as natural weighting but with a significantly better beam. First a low resolution image of the primary beam was made to identify confusing sources. Next a high resolution image was made including all sources. These maps were [CLEAN]{}ed. Because we had offsetted the PNe from the field center, we applied the primary beam correction which amounted to about 1% at 6 cm and 2% at 3 cm. Self-calibration was not applied because the flux values of the PNe are too low. Contour plots of the detected PNe are presented in the Appendix.

Analysis and Results {#results}
====================

Positions
---------

In Table \[tabpos\] we list the position of the peak flux density per beam of the PN at 6 cm together with the optical positions as determined from the H$\alpha$ or \[S III\]$\lambda$9532 images (Jacoby & Van de Steene, 2001, in preparation). The peak of the radio emission is adopted as the PN position. If the PN is extended in the radio, the radio position may be off center. The radio position 