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We have analysed the full ISO spectrum of the planetary nebula NGC 6302 inorder to derive the mineralogical composition of the dust in the nebula. We usean optically thin dust model in combination with laboratory measurements ofcosmic dust analogues. We find two main temperature components at about 100 and50 K respectively, with distinctly different dust compositions. The warmcomponent contains an important contribution from dust without strong infraredresonances. In particular the presence of small warm amorphous silicate grainscan be excluded. The detection of weak PAH bands also points to a peculiarchemical composition of the dust in this oxygen-rich nebula. The cool dustcomponent contains the bulk of the mass and shows strong emission fromcrystalline silicates, which contain about 10 percent of the mass. In addition,we identify the 92 micron band with the mineral calcite, and argue that the 60micron band contains a contribution from the carbonate dolomite. We present themass absorption coefficients of six different carbonate minerals. The geometryof the dust shell around NGC 6302 is studied with mid-infrared images obtainedwith TIMMI2. We argue that the cool dust component is present in acircumstellar dust torus, while the diffuse emission from the warm componentoriginates from the lobes.

The mineral composition and spatial distribution of the dust ejecta of NGC 6302