Planetary Nebulae of the Large Magellanic Cloud I: A Multiwavelength Analysis

Planetary nebulae (PNe) have three main components: a central star (CS),ionised gas and dust in the nebula. Each of them contains critical chemicalfingerprints of their evolution, serving as tracers of the evolution,nucleosynthesis and dust production that occurred during the precedingasymptotic giant branch (AGB) phase. We aim to build a bridge to link the PNphase to the evolution of their progenitors, trying to better understand thedust production and mass-loss mechanism during the final AGB phase. Here, wepresent a comprehensive study of nine Large Magellanic Cloud (LMC) spherical orelliptical PNe whose observations from the ultraviolet (UV) through theinfrared (IR) are available in the literature. We characterize nebulae and CSs,finding information as the amount of gas that makes up the nebula and the dustthat surrounds the CS, necessary to reconstruct the evolutionary history ofmass-loss and dust production. We compare the observed energy distribution ofthe selected PNe to that obtained from photoionization modeling, taking intoaccount the presence of dust. The physical and chemical parameters of thecentral stars are then compared with the predictions from the evolutionarytracks. We characterized the source, assigning to each CS a progenitor,early-AGB mass. We estimated the mass of the nebula and the dust-to-gas ratio.For 5 objects, we find evidence for the presence of a near-IR bump, which wouldbe connected to the presence of hot dust.