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T.G. Pannuti (SSC/JPL/Caltech), G.E. Allen (MIT CSR)
We present the results of a 74 kilosecond X-ray observation with Chandra of the northwestern rim complex of the Galactic supernova remnant G266.2-1.2. This SNR is a member of the small but growing class of sources known to feature X-ray spectra dominated by non-thermal emission: a detailed analysis of this emission is crucial in gaining new insights on the phenomenon of cosmic-ray acceleration by SNRs. Our high angular resolution X-ray image of this rim complex reveals new fine structure including a remarkably well-defined leading shock structure. We have also extracted spectra from seven discrete regions in the complex and fit this spectra with several different models, including a power law as well as the synchrotron models SRCUT and SRESC. Clear variations are seen in the derived fit parameters for the different regions, indicating differences in the cosmic-ray acceleration conditions in this complex. A summary and discussion of these results will be presented. We acknowledge support for this work from the Chandra General Observer Grant GO3-4072Z.
The author(s) of this abstract have provided an email address for comments about the abstract: tpannuti@ipac.caltech.edu
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Bulletin of the American Astronomical Society, 37 #2
© 2005. The American Astronomical Soceity.