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C.R. Tam (McGill), M.S.E. Roberts, V.M. Kaspi (McGill/MIT), E.V. Gotthelf (Columbia), M. Lyutikov (McGill/MIT), G. Vasisht (JPL/Caltech), N. Kawai (RIKEN)
We present high-resolution X-ray and radio studies of the supernova remnant G11.2-0.3 and its associated pulsar wind nebula. A detailed comparison between Chandra and VLA images of the PWN region morphology and spectrum is made. Spectral tomography results in the radio band reveal spectral indices for the individual components of this remnant. We also present preliminary results on the expansion of G11.2-0.3, the probable remnant of the supernova of 386 AD. For these measurements we compare archival VLA data, taken during 1984-85, with recent VLA obseravations, currently still underway. If G11.2-0.3 is indeed associated with this historical event, then because of its young age we would expect to find an expansion of the order 1%. These expansion measurements in conjunction with detailed X-ray spectral results provide a basis on which we set new constraints on the age of the remnant.
This work was supported in part by SAO, NASA, NSERC, and the Quebec Merit Fellowship.