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We present 11.3$\mu$m, presumably SiC, and 12.8$\mu$m, [NeII] images of the young PN IC 418 obtained with the Berkeley/IGPP/LEA mid-IR camera on the UKIRT. Comparison of these images with each other and other ionized lines reveal that the 11.3$\mu$m emission is spatially coincident with the ionized region of the nebula on the large scale. However, the 11.3$\mu$m emission is anticorrelated with the radio continuum on the smaller scale which we interpret as inhomogeneities in the dust temperature. We successfully model the large scale spatial distribution of 11.3\m~ dust emission and [NeII] line emission in IC418 using a detailed radiative transfer code which assumes that the 11.3$\mu$m emission arises from thermal emission from large SiC dust grains (a$> 0.01\mu$m).
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