  Planetary nebulae (PNe) have three main components: a central star (CS),
ionised gas and dust in the nebula. Each of them contains critical chemical
fingerprints of their evolution, serving as tracers of the evolution,
nucleosynthesis and dust production that occurred during the preceding
asymptotic giant branch (AGB) phase. We aim to build a bridge to link the PN
phase to the evolution of their progenitors, trying to better understand the
dust production and mass-loss mechanism during the final AGB phase. Here, we
present a comprehensive study of nine Large Magellanic Cloud (LMC) spherical or
elliptical PNe whose observations from the ultraviolet (UV) through the
infrared (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 dust
that surrounds the CS, necessary to reconstruct the evolutionary history of
mass-loss and dust production. We compare the observed energy distribution of
the selected PNe to that obtained from photoionization modeling, taking into
account the presence of dust. The physical and chemical parameters of the
central stars are then compared with the predictions from the evolutionary
tracks. 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 would
be connected to the presence of hot dust.
