Infrared spectroscopy of molecular supernova remnants

3C 391, where blast waves are impacting molecular clouds. The complete wavelength range from 42 to 188 mum was observed with the Long Wavelength Spectrometer, as well as narrow ranges centered on 4.695, 9.665, 25.98, and 34.82 mum with the Short Wavelength Spectrometer. Atomic fine-structure lines were detected from (in order of atomic number): C+, N+, N-++,N- O-0, O++, O+++, Si+, P+, and Fe+ The two lines of H-2 that we observed, S(3) and S(9), were detected for all three remnants. The observations require both shocks into gas with moderate (similar to 10(2) cm(-3)) and high (similar to 10(4) cm(-3)) preshock densities, with the moderate-density shocks producing the ionic lines and the high-density shock producing the molecular lines. No single shock model can account for all of the observed lines, even at the order of magnitude level. We find that the principal coolants of radiative supernova shocks in moderate-density gas are the far-infrared continuum from dust grains surviving the shock, followed by collisionally excited [O I] 63.2 mum and [Si II] 34.8 mum lines. The principal coolant of the high-density shocks is collisionally excited F-1, rotational and re-vibrational line emission. We systematically examine the ground-state fine structure of all cosmically abundant elements to explain the presence or lack of all atomic fine lines in our spectra in terms of the atomic structure, interstellar abundances, and a moderate-density, partially ionized plasma. The [P II] line at 60.6 mum is the first known astronomical detection, but its brightness can be explained using the solar abundance of P. There is only one, bright unidentified line in our spectra, at 74.26 mum; as there is no plausible atomic fine-structure line at this wavelength, we suggest this line is molecular. The presence of bright [Si II] and [Fe II] lines requires partial destruction of the dust. The required gas-phase abundance of Fe suggests 15%-30% of the Fe-bearing grains were destroyed. Adding the Si and Fe gas mass, and correcting for the mass of other elements normally found in dust, we find similar to0.5 M-circle dot of dust vapors from the shocked clump 3C 391:BML. The infrared continuum brightness requires similar to1 M-circle dot of dust survives the shock, suggesting about 1/3 of the dust mass was destroyed, in agreement with the depletion estimate and with theoretical models for dust destruction.