detected several lines toward the peak position of the -SE filament (-pk1). Table 2 summarizes the detected lines and their relative strengths, and Fig. 6 shows the spectra. 1.257 $\mu$m and 164 lines originate from the same upper level, so that their unreddened flux ratio is fixed by relative Einstein $A$ coefficients which is 1.04 according to [@qui96]. Toward -pk1, the ratio is 0.31, which implies $A_V=13$ mag ($A_{1.644\mu {\rm m}}=2.43$ mag) or H-nuclei column density of $2.49\pm 0.07 \times 10^{22}$ cm$^{-2}$ using the extinction cross section of the carbonaceous-silicate model for interstellar dust with $R_V=3.1$ of [@dra03][^3]. This is a little larger than the column density to the remnant derived from X-ray observations $(1.7-2.4)\times 10^{22}$ cm$^{-2}$ [@rob03]. We note that the numerical values of the Einstein $A$ coefficients for near-IR lines in the literature differ as much as 50%: using the values of [@nus88], the expected 1.257 $\mu$m to 164 line-intensity ratio is 1.36, while [@smi06] empirically derived 1.49 from their spectroscopy of P Cyg. If the intrinsic ratio is 1.36 or 1.49, we obtain a little (20–30%) higher column density. We adopt the $A$-values of [@qui96] in this paper which yield a column density closer to the X-ray 