G349.7+0.2 is the third brightest Galactic supernova remnant (SNR) at radio wavelengths, after Cas A and the Crab Nebula. It is a distant (22 kpc), small diameter (2.5 arcmin) shell-type SNR. The presence of OH(1720 MHz) masers and shocked molecular gas show that the SNR is interacting with ambient molecular clouds. Our ASCA observations are consistent with this interpretation, revealing a large mass of swept-up material. We have obtained high resolution Chandra observations of G349.7+0.2 to fully explore its X-ray morphology, and to search for possible spectral variations across the remnant. We find that the X-ray morphology agrees well with that observed in the radio, which contrasts with the centrally dominated X-ray morphology often associated with remnants associated with OH(1720 MHz) masers (e.g., W28, W44, IC 443). We review our results of spectral investigations with Chandra, which appear to indicate a multi-phase shock structure, and compare the spatial structure with available data at other frequencies. This work was supported in part from Chandra grant GO2-3080A.
|Title of host publication||American Astronomical Society, HEAD meeting 7|
|Publication status||Published - 1 Mar 2003|