low surface brightness. It is clear that due to these factors the flux density at 3 cm is generally less well-determined than at 6 cm, except for the bright and compact PNe. When a PN is optically thick at 6 cm, its 3 cm flux density is expected to be three times the flux density at 6 cm. There are some PNe like JaSt 65 and JaSt 79 for which the 3 cm flux density is clearly higher than the 6 cm flux density and which are point sources. In this case the PNe may not yet be completely optically thin at 6 cm and should be quite young.

In Fig. \[fluxhist\] we plotted the histogram of the radio flux of the known and new galactic bulge PNe. We selected a sample of known galactic bulge PNe for which radio flux densities and angular diameters are available, as in Van de Steene & Zijlstra ([@VdSteene95]). The new bulge PNe are within 2 degrees of the galactic center. None has a radio flux larger than 100 mJy and their angular sizes are smaller than 20. Hence they fulfill the same selection criteria as these previously known bulge PNe.

There is a 