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Pointed observations of Galactic supernova remnants (SNRs) as conducted at multiple wavelengths and with leading observatories (such as the Chandra X-ray Observatory and the Spitzer Space Telescope) have revealed many new insights into both SNRs themselves and the interstellar medium (ISM) with which these sources are interacting. We are currently investigating the multi-wavelength (chiefly X-ray and radio) properties of poorly studied SNRs that have been readily detected in the infrared to help improve understanding of how SNRs and their surrounding ISM interplay. to demonstrate this, we present an analysis of an archival pointed observation of the Galactic SNR G340.6+0.3 with the Chandra X-ray Observatory. The high angular resolution image reveals shell-like morphology that similarly matches the radio morphology of the SNR. In addition, spatially-resolved spectroscopy of the SNR using standard thermal plasma models reveals an asymmetry in the spectral properties of the rim. While enhanced (relative to solar) abundances of elements such as silicon are indicated from fits to the spectrum of the X-ray luminous northeastern rim (indicating that X-ray emitting plasma at this site is ejecta-dominated), the measured elemental abundances at other locations of the SNR are consistent with solar, indicating that those sites' plasma is dominated by swept-up ISM. From spectral fits and our adopted distance to this SNR of 15 kiloparsecs, we estimate a median electron number density for X-ray-emitting plasma to be 0.20 per cubic centimeter and the swept-up Xray emitting mass of the plasma to be approximately 50 solar masses.

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An Analysis Of Galactic Supernova Remnant G340.6+0.3



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