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We present photometric observations from the {\it Stratospheric Observatoryfor Infrared Astronomy (SOFIA)} at 11.1 $\mu$m of the Type IIn supernova (SNIIn) 2010jl. The SN is undetected by {\it SOFIA}, but the upper limitsobtained, combined with new and archival detections from {\it Spitzer} at 3.6\& 4.5 $\mu$m allow us to characterize the composition of the dust present.Dust in other Type IIn SNe has been shown in previous works to reside in acircumstellar shell of material ejected by the progenitor system in the fewmillenia prior to explosion. Our model fits show that the dust in the systemshows no evidence for the strong, ubiquitous 9.7 $\mu$m feature from silicatedust, suggesting the presence of carbonaceous grains. The observations are bestfit with 0.01-0.05 $\msun$ of carbonaceous dust radiating at a temperature of$\sim 550-620$ K. The dust composition may reveal clues concerning the natureof the progenitor system, which remains ambiguous for this subclass. Most ofthe single star progenitor systems proposed for SNe IIn, such as luminous bluevariables, red supergiants, yellow hypergiants, and B[e] stars, all clearlyshow silicate dust in their pre-SN outflows. However, this post-SN result isconsistent with the small sample of SNe IIn with mid-IR observations, none ofwhich show signs of emission from silicate dust in their IR spectra.

SOFIA Observations of SN 2010jl: Another Non-Detection of the 9.7 $\mu$m Silicate Dust Feature