an error in the intensity of H$_2$ (2–1) S(3) line at 2.0735 $\mu$m. According to [@han96], the error is about $2$% when the air masses differ by 0.3, so that it would be $\simlt 5$% for our H$_2$ (2–1) S(3) line. Again, this is less than the ($1\sigma$) statistical error. We therefore consider that the uncertainty due to the calibration errors is less than the statistical errors quoted in this paper (Table 2). For the wavelength solutions of the spectra, we used the OH sky lines [@rou00].

Results
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Fig. 1 (right) is our three-color image representing the near-IR 164 (B), 212 (G), and 2.166 $\mu$m (R) emission of the SNR 11p2. We also show an 1.4 GHz VLA image for comparison which was obtained by [@gre88] in 1984–85 with $3''$ resolution. Note that the expansion rate of 11p2 at 1.4 GHz is $0.''057\pm 0.''012$ yr$^{-1}$ [@tam03] which amounts to $\sim 1''$ over the last 20 years (see also §3.3). The near-IR emission features in Fig. 1 can be summarized as follows: (1) an extended ($\sim 2.'5$), bright (blue) filament along the SE radio shell; (2) some faint, knotty emission features along the NW radio shell as well as in 