Sect. \[results\]. The improved method for determining the distances, based on a relationship between radii and radio surface brightness (Van de Steene & Zijlstra [@VdSteene95]) is used in Sect. \[distances\] to determine the distances of the PNe and discuss their distribution in the galactic bulge. In Sect. \[extinction\] we determine the extinction values of these new bulge PNe.

Observations
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Radio continuum observations for 64 new PNe which had been confirmed spectroscopically at the ESO 1.52-m and CTIO 4-m telescopes were obtained with the Australia Telescope Compact Array. The array was in configuration $\#$ 6A. The shortest baseline was 337 m and the longest 5939 m. The bandwidth was 128 MHz centered at 4800 MHz and 8640 MHz, corresponding to 6 and 3 cm respectively. The synthesized beam for the 6 km array at 6 cm is $\sim$ 2 and $\sim$1 at 3 cm. According to the ACA manual, the largest well imaged structure in a 60 min observation is 30 at 6 cm and 15 at 3 cm. Consequently we expected all our sources to be well imaged at 6 cm and virtually all at 3 cm. Forty PNe were observed at 3 and 6 cm simultaneously for 12 