2006ApJ...653..267T

We observed the oxygen-rich Large Magellanic Cloud (LMC) supernova remnant N132D (SNR 0525-69.6), using all instruments on board the Spitzer Space Telescope, IRS, IRAC, and MIPS (Infrared Spectrograph, Infrared Array Camera, and Multiband Imaging Photometer for Spitzer). The 5-40 µm IRS spectra toward the southeastern shell of the remnant show a steeply rising continuum with [Ne III] and [O IV], as well as PAH emission. We also present the spectrum of a fast moving ejecta knot, previously detected at optical wavelengths, which is dominated by strong [Ne III] and [O IV] emission lines. We interpret the continuum as thermal emission from swept-up, shock-heated dust grains in the expanding shell of N132D, which is clearly visible in the MIPS 24 µm image. A 15-20 µm emission hump appears superposed on the dust continuum, and we attribute this to PAH CCC bending modes. We also detect the well-known 11.3 µm PAH CH bending feature, and find the integrated strength of the 15-20 µm hump about a factor of 7 stronger than the 11.3 µm band in the shell of the remnant. IRAC 3-9 µm images do not show clear evidence of large-scale, shell-like emission from the remnant, partly due to confusion with the ambient ISM material. However, we identified several knots of shocked interstellar gas based on their distinct infrared colors. We discuss the bright infrared continuum and the polycyclic aromatic hydrocarbon features with respect to dust processing in young supernova remnants.