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We present infrared (IR) and submillimeter observations of the Crab-likesupernova remnant (SNR) G54.1+0.3 including 350 micron (SHARC-II), 870 micron(LABOCA), 70, 100, 160, 250, 350, 500 micron (Herschel) and 3-40 micron(Spitzer). We detect dust features at 9, 11 and 21 micron and a long wavelengthcontinuum dust component. The 21 micron dust coincides with [Ar II] ejectaemission, and the feature is remarkably similar to that in Cas A. The IRAC 8micron image including Ar ejecta is distributed in a shell-like morphologywhich is coincident with dust features, suggesting that dust has formed in theejecta. We create a cold dust map that shows excess emission in thenorthwestern shell. We fit the spectral energy distribution of the SNR usingthe continuous distributions of ellipsoidal (CDE) grain model of pre-solargrain SiO2 that reproduces the 21 and 9 micron dust features and discuss grainsof SiC and PAH that may be responsible for the 10-13 micron dust features. Toreproduce the long-wavelength continuum, we explore models consisting ofdifferent grains including Mg2SiO4, MgSiO3, Al2O3, FeS, carbon, and Fe3O4. Wetested a model with a temperature-dependent silicate absorption coefficient. Wedetect cold dust (27-44 K) in the remnant, making this the fourth such SNR withfreshly-formed dust. The total dust mass in the SNR ranges from 0.08-0.9 Msundepending on the grain composition, which is comparable to predicted massesfrom theoretical models. Our estimated dust masses are consistent with the ideathat SNe are a significant source of dust in the early Universe.

A Dust Twin of Cas A: Cool Dust and 21-micron Silicate Dust Feature in the Supernova Remnant G54.1+0.3