  A number of planetary nebulae show binary central stars and significant
abundance discrepancies between values estimated from colisionally excited
lines when compared to the same abundances estimated from recombination lines.
One approach to investigate this yet unsolved problem is using spatially
resolved images of emission lines in an attempt to detect a possibly distinct
metal rich component in the nebula. In this work we present results of
spatially resolved bundance analysis of NGC 6778 based on data gathered from
VLT VIMOS-IFU. We discuss the spatial variations found as well as possible
limitations of the method in answering questions about abundance variations.
