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We present a detailed spatially-resolved spectroscopic analysis of two X-rayobservations (with a total integration time of 73280 seconds) made of theluminous northwestern rim complex of the Galactic supernova remnant (SNR)G266.2-1.2 (RX J0852.0-4622) with the Chandra X-ray Observatory. G266.2-1.2 isa member of a class of Galactic SNRs which feature X-ray spectra dominated bynon-thermal emission: in the cases of these SNRs, the emission is believed tohave a synchrotron origin and studies of the X-ray spectra of these SNRs canlend insights into how SNRs accelerate cosmic-ray particles. The Chandraobservations have clearly revealed fine structure in this rim complex and thespectra of these features are dominated by non-thermal emission. We havemeasured the length scales of the upstream structures at eight positions alongthe rim and derive lengths of 0.02-0.08 pc (assuming a distance of 750 pc toG266.2-1.2). We have also extracted spectra from seven regions in the rimcomplex and fit these spectra with such models as a simple power law as well asthe synchrotron models SRCUT and SRESC. We have constrained our fits to thelatter two models using estimates for the flux densities of these filaments at1 GHz as determined from radio observations made with the Australia TelescopeCompact Array (ATCA). Statistically-acceptable fits to all seven regions arederived using each model: differences in the fit parameters (such as photonindex and cutoff frequency) are seen in the different regions, which mayindicate variations in shock conditions and the maximum energies of thecosmic-ray electrons accelerated at each region. Finally, we estimate themaximum energy of cosmic-ray electrons accelerated along this rim complex to beapproximately 40 TeV. We include a summary of estimated maximum energies forboth Galactic SNRs as well as SNRs located in the Large Magellanic Cloud.

Non-Thermal X-ray Emission from the Northwestern Rim of the Galactic Supernova Remnant G266.2-1.2 (RX J0852.0-4622)