so that it increases outward from the remnant center. Note that the profiles of the filament in 2005 (solid lines) are slightly shifted outward from those in 2003 (dashed lines). We fit the profiles along the cuts A and B with a Gaussian and obtain shifts of $0.''063\pm 0.''032$ and $0.''095\pm 0.''064$ in their central positions, respectively. For comparison, the profiles of nearby stars, e.g., the strong peak at $24''$ in Fig. 7 (left), do not show any appreciable shift. The mean shift in stellar positions from the same 1-dimensional Gaussian analysis of nearby seven stars is found to be $-0.''0067 \pm 0.''0029$. Therefore, the mean proper motion of the SE filament with respect to the nearby stars during 2.2 years amounts to $0.''076 \pm 0.''029$, which corresponds to a rate of $0.''035\pm 0.''013$ yr$^{-1}$.

212 emission: Photometry and Spectroscopy
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Fig. 8 is a star-subtracted and median-filtered 212 image. The image has been made in the same way as Fig. 2. Two small ($\sim 30''$) filaments, one at the southern SNR radio boundary and another fainter one outside the NE boundary are now clearly seen. The one in the southeast (-SE filament) is bright and elongated along the radio 