Eleven mineral fractions from the Allende C3 chondrite were analyzed for He, Ne, Ar, Kr, and Xe by mass spectrometry. As was shown previously (Lewis et al., 1975), most of the heavy noble gases, of unexceptional isotopic composition, are contained in an ill-defined HNO3-soluble mineral fraction ('Q') comprising 0.04% of the meteorite. The remaining noble gases, of decidedly nonsolar isotopic composition, are contained in chromite (0.2%) and amorphous carbon (0.2%). They have virtually identical concentrations and isotopic compositions in the two minerals: 20Ne/22Ne=8.7 and 36Ar/38Ar=4.82. Xenon is enriched up to twofold in both heavy and light isotopes, while Kr is enriched only in heavy isotopes. The enrichment of the heavy isotopes is presumably due to fission, but the fission spectra derived depend critically on the assumed composition of the trapped component. The enrichment patterns of the light xenon isotopes diffr slightly for chromite and carbon. Partial destruction of the minerals by chemical treatments gave no evidence for other gas-rich phases or other gas components and only marginal evidence for heterogeneities within the known gas-rich phases. Spinel has ≪0.1 the gas content of other phases. The chromite-carbon fractions contain 30--60% more spallogenic 21Ne than does the bulk meteorite, although they are deficient in target elements for the production of 21Ne. A possible explanation is recoil of 21Ne from adjacent Mg-rich phases. All of the available isotopic and chemical data suggest that chromite, carbon, and Q, and hence their associated gas components, are of local rather than extra-solar system origin. The excess heavy Kr and Xe isotopes may have been produced by fission of a superheavy element, while the remaining isotopic anomalies may be due to mass fractionation during trapping. The virtual identity of the noble gas components of chromite and carbon suggests that both minerals formed simultaneously, perhaps by a reaction such as Fe+2Cr+4CO→FeCr2O4+4C.