AAS 205th Meeting, 9-13 January 2005
Session 106 SNRs and Loops
Poster, Wednesday, January 12, 2005, 9:20am-6:30pm, Exhibit Hall

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[106.01] Spitzer Imaging of Kepler's Supernova Remnant

W.P. Blair, R. Sankrit, P. Ghavamian (JHU), K.S. Long (STScI), K. Borkowski, S.P. Reynolds (NCSU)

We have obtained Spitzer Space Telescope MIPS and IRAC infrared images of the remnant of SN 1604, also known as Kepler's supernova remnant. The images, taken within two months of the 400th anniversary of the sighting of the supernova, provide the most detailed information to date on the spatial distribution and character of the dust in this supernova remnant. The MIPS 24 micron image shows the overall structure to best effect. While this image is brightest in the northwest and north (as is the optical), the entire circumference is visible, as are patches of emission seen in projection toward the center of the remnant. These patches of IR emission surround optical knots which, based on their kinematics, arise from the front and back sides of the expanding shell. By association, the IR emission is also due to the shell rather than interior emission. The IRAC 8 micron image has the best spatial resolution, but only shows the brightest regions, almost exactly coincident with the brightest optically emitting material. Likewise, the 70 micron MIPS image shows only the brighter regions from the 24 micron image, although some variations in observed 70:24 micron ratio are seen. The shorter wavelength IRAC images are progressively dominated by stellar emission. Comparison to imaging data at optical, X-ray, and radio wavelengths makes it clear we are seeing dust emission primarily from regions that have encountered the primary blast wave as it strikes circumstellar and interstellar material. We will compare the observed IR fluxes and their ratios with theoretical calculations of IR emission from collisionally heated silicate dust in order to determine physical conditions within the hot plasma, infer its dust content, and study the possible destruction of dust by the expanding blast wave.

This work is supported by grant JPL-1264303 to the Johns Hopkins University.

If you would like more information about this abstract, please follow the link to http://fuse.pha.jhu.edu/~wpb/Kepler/kepler.html. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: wpb@pha.jhu.edu

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