High Angular Resolution X-ray Observations of the Galactic Supernova Remnant G266.2-1.2 (RX J0852.0-4622)

Details High Angular Resolution X-ray Observations of the Galactic Supernova Remnant G266.2-1.2 (RX J0852.0-4622) High Angular Resolution X-ray Observations of the Galactic Supernova Remnant G266.2-1.2 (RX J0852.0-4622)

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005xrrc.proce4.14p&link_type=abstract

"X-Ray and Radio Connections (eds. L.O. Sjouwerman and K.K Dyer) Published electronically by NRAO, http://www.aoc.nrao.edu/event

Physics

1

X-Ray, Radio, Supernova Remnants

Scientific paper

G266.2-1.2 (RX J0852.0-4622) is a member of the emerging class of Galactic supernova remnants (SNRs) which feature X-ray spectra dominated by non-thermal emission. This X-ray emission is believed to be synchrotron radiation produced by cosmic-ray electrons accelerated to TeV energies along the expanding shock fronts of SNRs. To explore this phenomenon of high energy X-ray emission from SNRs in more detail, we are conducting a broadband X-ray study of these sources using both new and archived observations. To illustrate this work, we present the results of our two observations made with Chandra (with a total effective exposure time of 73972 seconds) of the luminous northwestern rim of G266.2-1.2: this observation has revealed for the first time fine X-ray structure in this rim. A satisfactory fit to the spectrum of a sharply defined leading shock is derived using a power law model with a photon index γ = 2.41±0.06. Alternatively, this spectrum can be fit with the SRCUT model which leads to an estimate of ≈40 TeV for the maximum energy of cosmic-ray electrons accelerated along this rim: however, additional radio observations of this rim are required to test more stringently the application of this model. Finally, we find that the spectra of regions located on and just interior to the rim may also be fit with a power law: a radial gradient in the values for the photon index may be explained as a localization of the acceleration of cosmic-ray particles to the shock region.

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