surface brightness the total Gaussian flux density was adopted. This was mostly the case for small, unresolved PNe. If the PN was extended the intensities within the 2 or 3 $\sigma$ level contour were summed. This value was compared with the statistics over a larger region across the nebula to obtain an error estimate (Fomalont, 1989).

For JaSt 69 only a small 3 $\sigma$ blob at the right position indicated the presence of a PN. No flux or size values could be determined. In some cases several blobs indicated the presence of a PN at 3 cm and hence their flux is a lower limit. Some objects detected at 6 cm, but having low peak flux density per beam, could not be seen at 3 cm.

PNe are normally optically thin at 6 cm in which case its 3 cm flux density is about 95% of the 6 cm flux density. In our case this means that the flux densities are similar within the error-bars. However when a PN is already well resolved at 6 cm, more flux may have been missed at 3 cm where the beam is half the size, especially if the nebula is extended and of 