Shock Processing of Interstellar Dust and Polycyclic Aromatic Hydrocarbons in the Supernova Remnant N132d

We observed the oxygen-rich Large Magellanic Cloud (LMC) supernova remnant N132D (SNR0525– 69.6), using all instruments onboard the Spitzer Space Telescope, IRS, IRAC, and MIPS (Infrared Spectrograph, Infrared Array Camera, Multiband Imaging Photometer for Spitzer). The 5–40μm 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 24μm image. A 15–20μm emission hump appears superposed on the dust continuum, and we attribute this to PAH C-C-C bending modes. We also detect the well-known 11.3μm PAH C-H bending feature, and find the integrated strength of the 15–20μm hump about a factor of seven stronger than the 11.3μm band in the shell of the remnant. IRAC 3–9μm 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. Subject headings: infrared: ISM — supernova remnants — supernovae: individual (N132D)