Spitzer Observations of Supernova Remnant N49 in the LMC

Details Spitzer Observations of Supernova Remnant N49 in the LMC Spitzer Observations of Supernova Remnant N49 in the LMC

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20915613t&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #156.13; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

N49 (SNR 0525-66.1) is the brightest optical supernova remnant (SNR) in the Large Magellanic Cloud, located at the edge of a massive, dense molecular cloud. The environment surrounding the N49 remnant is ideal to study the interaction of the supernova ejecta with the interstellar medium and to ascertain whether this SNe has triggered star formation processes within the adjacent molecular cloud. We present Spitzer Space Telescope infrared imaging and spectroscopy of N49 obtained with the Infrared Array Camera (IRAC) at 3.6, 4.5, 5.8, and 8.0 microns, the Multiband Imaging Photometer (MIPS) at 24 and 70 microns, and three modules of the Infrared Spectrograph (IRS) covering the wavelengths between 5 and 38 microns. The IRAC morphology resembles that evident at visible and x-ray wavelengths. The peak IRAC surface brightness of the SNR is along the southeastern edge, where it encounters the molecular cloud. While the MIPS images exhibit the same enhancement in the southeast, a complete shell structure is detected in the 24 micron image. The IRS spectra show strong ionic emission lines of [Si II], [Fe II], [O IV], [S III], [Ne II], and [Ne III], molecular hydrogen line emission, and no apparent dust features at the selected slit position.
Support for this work is in part provided by NASA through contracts 1256406 and 1215746 issued by JPL/Caltech to the University of Minnesota.

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