  We observed the oxygen-rich Large Magellanic Cloud (LMC) supernova remnant
N132D (SNR 0525-69.6), using all instruments onboard the Spitzer Space
Telescope, IRS, IRAC, and MIPS (Infrared Spectrograph, Infrared Array Camera,
Multiband Imaging Photometer for Spitzer). The 5-40 micron IRS spectra toward
the southeastern shell of the remnant show a steeply rising continuum with
[NeIII] and [OIV] 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 [NeIII] and [OIV] 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 micron image.
A 15-20 micron 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 11.3
micron PAH C-H bending feature, and find the integrated strength of the 15-20
micron hump about a factor of seven stronger than the 11.3 micron band in the
shell of the remnant. IRAC 3-9 micron 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.
