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Infrared spectra of carbon-rich objects which have evolved off the asymptoticgiant branch reveal a range of dust properties, including fullerenes,polycyclic aromatic hydrocarbons (PAHs), aliphatic hydrocarbons, and severalunidentified features, including the 21 um emission feature. To test for thepresence of fullerenes, we used the position and width of the feature at18.7-18.9 um and examined other features at 17.4 and 6-9 um. This method addsthree new fullerene sources to the known sample, but it also calls intoquestion three previous identifications. We confirm that the strong 11 umfeatures seen in some sources arise primarily from SiC, which may exist as acoating around carbonaceous cores and result from photo-processing. Spectrashowing the 21 um feature usually show the newly defined Class D PAH profile at7-9 um. These spectra exhibit unusual PAH profiles at 11-14 um, with weakcontributions at 12.7 um, which we define as Class D1, or show features shiftedto ~11.4, 12.4, and 13.2 um, which we define as Class D2. Alkyne hydrocarbonsmatch the 15.8 um feature associated with 21 um emission. Sources showingfullerene emission but no PAHs have blue colors in the optical, suggesting aclear line of sight to the central source. Spectra with 21 um features andClass D2 PAH emission also show photometric evidence for a relatively clearline of sight to the central source. The multiple associations of the 21 umfeature to aliphatic hydrocarbons suggest that the carrier is related to thismaterial in some way.

Carbon-rich dust past the asymptotic giant branch: aliphatics, aromatics, and fullerenes in the Magellanic Clouds