PAH Detection In The Supernova Remnant N132D

Details PAH Detection In The Supernova Remnant N132D PAH Detection In The Supernova Remnant N132D

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.6305t&link_type=abstract

American Astronomical Society Meeting 208, #63.05; Bulletin of the American Astronomical Society, Vol. 38, p.143

Astronomy and Astrophysics

Astronomy

Scientific paper

We report the detection of polycyclic aromatic hydrocarbon (PAH) bands associated with the oxygen-rich supernova remnant N132D (SNR 0525-69.6) in the Large Magellanic Cloud. We observed N132D with 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 [NeIII] and [OIV] as well as PAH emission. We interpret the continuum as thermal emission from shocked, heated dust grains in its expanding shell, which is clearly visible in the MIPS 24μm image. Superposed on the dust continuum, we detect 15-20μm features, including the 16.4 and 17.4μm lines, which are considered to be 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 features about a factor of five stronger than the 11.3μm band. This ratio is higher than commonly observed in reflection/planetary nebulae or young stellar objects, and similar to HII-regions, suggesting that large and/or dehydrogenated/ionized PAHs dominate the material close to the blast wave of N132D. Smaller PAHs and very small grains may have been destroyed through thermal sputtering in the hot plasma. 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 also seen at optical wavelengths, based on their distinct infrared colors, which suggest the presence of continuum emission from heated silicate/graphite dust grains. We discuss the bright infrared continuum and the polycyclic aromatic hydrocarbon features with respect to dust processing in young supernova remnants.This work is based on observations made with the Spitzer Space Telescope. Support was provided by the NASA LTSA program.

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