Arcsecond-Scale Spectroscopy of Cas A and the Implications for Cosmic-Ray Acceleration

Details Arcsecond-Scale Spectroscopy of Cas A and the Implications for Cosmic-Ray Acceleration Arcsecond-Scale Spectroscopy of Cas A and the Implications for Cosmic-Ray Acceleration

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sgrb.confe...2a&link_type=abstract

Presented at the KITP Conference: Supernova and Gamma-Ray Burst Remnants, Feb 10, 2006, Kavli Institute for Theoretical Physics,

Physics

Scientific paper

G. E. Allen (MIT), M. D. Stage (UMass), J. C. Houck (MIT) and J. E. Davis(MIT)We present the results of spectroscopic analyses of 1.1 megaseconds ofChandra ACIS X-ray data for the supernova remnant Cas A. The analyses wereperformed by extracting spectra from 1 xuml 1\" to 7 xuml 7\" overlapping boxesat each point on a rectangular grid with 1\" spacing. Each set of spectraand spatially-dependent responses was fitted with a simple thermalmodel. The results of this analysis suggest that some, if not all, of theregions in which the X-ray synchrotron emission is produced can beidentified. These regions have relatively high fitted electron temperaturesand relatively low elemental abundances. The regions whose X-ray emissionis dominated by synchrotron radiation seem be distributed around theforward shock, except, perhaps, for portions of the southwestern face ofthe remnant. The data for these regions were subsequently fitted with asynchrotron emission model. The fitted critical frequencies associatedwith the highest-energy electrons vary from about 10^16-10^18 Hz. Thisvariation indicates that the cut-off energy of the electron spectrum variesby as much as one order of magnitude and/or the magnetic field strengthvaries by as much as two orders of magnitude. In the regions with thehighest critical frequencies, the electrons must be accelerated about asfast as possible (i.e. have diffusion coefficients comparable to the Bohmcoefficient).

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