---
author:
- 'G.C. Van de Steene'
- 'G.H. Jacoby [^1]'
date: 'received / accepted'
title: Radio observations of new galactic bulge planetary nebulae
---

Introduction
============

Planetary Nebulae (PNe) are bright emission line objects, observable throughout the Galaxy. They are excellent probes of abundance gradients, the chemical enrichment history of the interstellar medium, the effects of metallicity on stellar evolution, and kinematics.

Most small PNe ($\sim$90$\%$) within 10 of the galactic center are physically close to it (Pottasch & Acker 1989). Since they can be assumed to be at the same known distance of $\sim$7.8 kpc, their distance-dependent parameters, such as luminosity and size, can be determined. These parameters are needed to define the underlying population. The chemical composition and the central star parameters are computed via self-consistent photo-ionization modelling of the nebula. Because luminosity correlates with the central star mass, which correlates with the progenitor mass, which, in turn, correlates with stellar age, the relationship between age and composition can be deduced (Dopita et al. [@Dopita97], Walsh et al. [@Walsh00]). The chemical enrichment history of the Bulge could be tracked using PNe.

We surveyed a 4 x 4 degree field centered on the galactic center in \[S[iii]{}\]$\lambda$9532 and 