while the influence of variable stars was considerably abated. This new H$\alpha$ map led directly to the discovery of a significant new population of LMC emission sources, including the many new PNe that comprise the Reid-Parker catalog of LMC PNe.

Candidate emission sources were identified using an adaptation of a technique available within the KARMA collaboration [@Gooch96] which is fully described by [@RP06a]. The stacked SR and H$\alpha$ images were each assigned a specific color: red for SR and blue for H$\alpha$. The colored images were then merged, resulting in a pink color for continuum sources, whereas compact or point source emitters develop a blue aura around a pink core whose relative size depends on the intensity of the emission. Extended nebulae, including regions, supernova remnants, super-bubbles and resolved, faint PNe can appear solely blue on an otherwise dark background. Many of the PNe are only visible as blue features in the false-color image. Most PNe central stars however are too faint, and the resolution too poor in the ground based UKST images, to be detected. A variety of telescopes and instruments were employed for spectroscopic follow-up including FLAMES on the Very Large Telescope (VLT) UT2, the 1.9-m telescope at 