high, the lines from heated molecular gas could show ‘thermal’ line ratios [@gre95]. The line intensities from such clump depend on details, and no model calculations that may be directly applicable to our case are available [cf. @dra90; @dra91; @mal96]. In the following, we instead simply consider the energy budget. If the 212 line is emitted by reprocessing the X-ray photons from the SNR falling onto the molecular clump, its luminosity may be written as $L_{2.122} \sim \epsilon L_X (\Omega_{\rm cl}/4\pi)$ where $\epsilon$ is an efficiency of converting the incident X-ray energy flux into 212 line emission, $L_X$ is the X-ray luminosity of the remnant, and $\Omega_{\rm cl}$ is the solid angle of the clump seen from the SNR center. The above formula is accurate if the clump is small and if the X-ray source is spherically symmetric. Although 11p2 is not a spherically symmetric source in X-rays, we may use the formula to make a rough estimate of the expected 212 line luminosity. The conversion efficiency for SNRs embedded in molecular clouds was calculated to be $\simlt 1 \times 10^{-3}$ [@lep83; @dra90; @dra91]. The efficiency is a function of X-ray energy absorbed per H-nucleon and the above inequality might 