Abstract
We present an 8–13 μm spectrum of the planetary nebula IC 2165. In addition to a bright [S IV] emission line, we identify weak emission from the [A III] and [Cl IV] fine structure lines and the H7–6 hydrogen recombination line. These lines are used to derive ionic abundances which are in agreement with those expected from the known excitation of the nebula. The rather weak continuum is attributed to free–free emission near 8 μm, but with increasing contributions from dust emission with increasing wavelength. From the presence of emission from silicon carbide dust, we infer that the emitting dust grains were formed in a carbon-rich environment, in accord with abundance determinations from optical and ultraviolet line emission.
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