Abstract
To determine the 3-dimensional distribution of matter that produces the observed morphologies in planetary nebulae (PNe) is essential in understanding the gas ejection mechanisms that form these objects, giving also important constraints for stellar evolution theories. Monteiro et al. (2000) showed that ellipsoidal geometry, usually adopted in the literature for the typical annular PN NGC 3132, is not able to consistently reproduce the density and velocity profiles. It was also shown that a Diabolo structure reproduced these aspects. However, in order to obtain a consistent model, more detailed observations are needed. We then performed spatially resolved observations in the 1.6-m telescope of the Laboratorio Nacional de Astrofisica (LNA, Brazil). Using these observations (images, total line intensities, etc.), a 3-dimensional photoionization code and the Diabolo structure, characteristic parameters for the gas and the central star were obtained.
