  We present results from deep Chandra observations of the young Type Ia
supernova remnant (SNR) 0509-68.7, also known as N103B, located in the Large
Magellanic cloud (LMC). The remnant displays an asymmetry in brightness, with
the western hemisphere appearing significantly brighter than the eastern half.
Previous multi-wavelength observations have attributed the difference to a
density gradient and suggested circumstellar material origins, drawing
similarities to Kepler's SNR. We apply a clustering technique combined with
traditional imaging analysis to spatially locate various emission components
within the remnant. We find that O and Mg emission is strongest along the blast
wave, and coincides with Spitzer observations of dust emission and optical
emission from the non-radiative shocks. The abundances of O and Mg in these
regions are enhanced relative to the average LMC abundances and appear as a
distinct spatial distribution compared to the ejecta products, supporting the
circumstellar medium (CSM) interpretation. We also find that the spatial
distribution of Cr is identical to that of Fe in the interior of the remnant,
and does not coincide at all with the O and Mg emission.
