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B. Koralesky (U. Minnesota), E.V. Gotthelf (Columbia U.), S.S. Holt (NASA/GSFC), U. Hwang (NASA/GSFC & University of Maryland), T.W. Jones (U. Minnesota), R. Petre (NASA/GSFC), L. Rudnick (U. Minnesota)
Through comparisons among Chandra silicon line and high energy continuum images and VLA radio observations we see clear signatures for multiple plasmas in the Cassiopeia A supernova remnant. On large scales (>15") we find that the radio and X-ray emissions are linearly correlated, but with different slopes interior and exterior to the bright ring, as opposed to previous analyses. We discuss the implications for differing particle acceleration and magnetic field amplification processes behind the apparent outer and reverse shocks.
The small scale (<5") X-ray brightness is uncorrelated with the local radio brightness. Ignoring the actual brightness, we find no global correlation between X-ray and radio features, only a partial overlap. This provides a limit to the contribution from synchrotron emission at several keV and argues that magnetic field amplification regions can be separated from the shocked thermal plasma on scales of 0.1 pc.
In addition, only half of the silicon line and high energy emission overlap on small scales, which further demonstrates that multiple components are present. Spectral information on these components are discussed on an accompanying poster.
SNR research at the University of Minnesota is supported by the NASA Graduate Student Research Program and the National Science Foundation under grant AST 96-19438. E.V.G. is supported by NASA LTSA grant NAG5-7935. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
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