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This paper presents late-time near-infrared and {\it Spitzer} mid-infraredphotometric and spectroscopic observations of warm dust in the Type IIn SN2005ip in NGC 2906. The spectra show evidence for two dust components withdifferent temperatures. Spanning the peak of the thermal emission, theseobservations provide strong constraints on the dust mass, temperature, andluminosity, which serve as critical diagnostics for disentangling the originand heating mechanism of each component. The results suggest the warmer dusthas a mass of $\sim 5 \times 10^{-4}~$\msolar, originates from newly formeddust in the ejecta, or possibly the cool, dense shell, and is continuouslyheated by the circumstellar interaction. By contrast, the cooler componentlikely originates from a circumstellar shock echo that forms from the heatingof a large, pre-existing dust shell $\sim 0.01 - 0.05$~\msolar~by the late-timecircumstellar interaction. The progenitor wind velocity derived from the blueedge of the He 1 1.083 \micron~P Cygni profile indicates a progenitor eruptionlikely formed this dust shell $\sim$100 years prior to the supernova explosion,which is consistent with a Luminous Blue Variable (LBV) progenitor star.

Disentangling the Origin and Heating Mechanism of Supernova Dust: Late-Time Spitzer Spectroscopy of the Type IIn SN 2005ip