Abstract
This project continues the same research lines the members of the team have been working on during the last few years, aiming to describe the abundances and model the chemical evolution of galaxies, in particular the Milky Way, through the investigation of their distinct substructures. This will be done by deriving chemical abundances of photoionized nebulae and stars that can be seen as probes capable to describe the chemical evolution in distinct regions.We intend to investigate the distribution of chemical abundances of planetary nebulae in substructures of the Milky Way such as the bulge, the bulge-disk connection and the external edge of the disk. The derived results will be used as constraints to model the entire stellar system. Observational results analogous to those obtained for the Milky Way can be derived for other galaxies, deriving parameters that will be used as constraints to formulate generalized models to describe their evolution, as well as for specific models of galaxy bulges and disks. The derivation of ages of central stars of planetary nebulae and AGB stars will also contribute to the understanding of galactic chemical evolution, in particular the time evolution of the radial abundance gradient.Using modern observational resources such as optical interferometry, high angular resolution imaging and integral field spectroscopy, we intend to investigate the physical processes associated to the morphology of stellar envelopes and to the structure of spatially resolved planetary nebulae, describing more precisely the characteristics and evolution of these objects. (AU)
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