Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1509r&link_type=abstract
American Astronomical Society Meeting 210, #15.09; Bulletin of the American Astronomical Society, Vol. 39, p.114
Other
Scientific paper
We present an investigation of Kepler's blast wave emission from our 741 ks Chandra observation, focusing on the nonthermal component. We report the discovery of a network of nonthermally-dominated regions and filaments that surround most of Kepler's periphery. Images in 4.5 -- 6.2 keV continuum are strikingly different from the integrated image or the Fe K alpha image; the platelet-smoothed continuum image shows linear features and knots that do not correlate well with total X-ray brightness. While most such structures are at the periphery, some run across the face of the remnant and are probably linear structures rather than sheets seen edge-on. We analyze the spectra of regions dominated by this hard continuum. The emission is dominated by Si and Fe-rich ejecta over much of the periphery, but the SW quadrant shows primarily lineless spectra well described by synchrotron radiation models. There is least nonthermal emission across the N rim, where nonradiative, Balmer-dominated shocks are seen, evidently encountering partially neutral gas. This anticorrelation of nonthermal emission and partially neutral material is also seen in SN 1006. While some synchrotron emission originates in very thin filaments as seen in Tycho and SN 1006, some appears in more diffuse structures, and a few small knots are also synchrotron-dominated. A hard spectral component is required for spectra in most regions; we identify this component as synchrotron radiation as well. The synchrotron-dominated portion of the remnant periphery is the faintest overall; we estimate the required thermal-gas density contrast and discuss constraints on the efficiency of electron acceleration. Characteristic rolloff frequencies of the synchrotron emission are (1 -- 4) x 10^17 Hz, indicating that the spectrum of shock-accelerated electrons begins to steepen at an energy of about 50 -- 100 (B/10 microGauss)^{-1/2} TeV, similar to values found for the other historical shell remnants.
Badenes Carles
Blondin John M.
Borkowski Kazimierz J.
Hughes John Patrick
Hwang Una
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