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We present a comprehensive study of the X-ray emission from SNR 0453-68.5 inthe Large Magellanic Cloud (LMC) as seen from the \textit{Chandra} X-rayObservatory. This object is in a class of composite remnants that exhibit ashell of emission surrounding a central plerion, more commonly known as apulsar wind nebula (PWN). This is one of only five remnants in the LMC with anidentified PWN. We find that the shell of emission is not ejecta dominated, butrather due to shocked ISM that has been swept up by the supernova blast wave orlocated in a precursor cavity wall. This is supported by the morphology of thelocal molecular cloud as seen with the \textit{Spitzer} Space Telescope. Thespectral properties are consistent with a middle-aged remnant $>$17000 yearsold. A point source detected within the central knot is determined to be thepulsar powering the synchrotron emission of the PWN. Spectral fits show thenebula is well characterized by a power law with photon index $\Gamma=2.0$.This index is constant over a spatial scale of 0.4-1.2 pc, which isinconsistent with younger PWN containing remnants such as the Crab Nebula andSNR 0540-69.3. These fits also contain significant contributions from an ejectadominated thermal plasma which we interpret as evidence of mixing during anevolved interaction of the PWN with the reverse shock of the SNR. We observe noevidence that the central pulsar contains a significant velocity transverse tothe line of sight and argue that despite the asymmetric surface brightnessdistribution the SN explosion giving birth to this remnant may have been quitesymmetric.

SNR 0453-68.5: An Asymmetric Remnant and its Plerion in the Large Magellanic Cloud