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We report on Green Bank Telescope 23.87 GHz NH$_3$(3,3), emissionobservations in five supernova remnants interacting with molecular clouds(G1.4$-$0.1, IC443, W44, W51C, and G5.7$-$0.0). The observations show a clumpygas density distribution, and in most cases the narrow line widths of$\sim3-4$\,km\,s$^{-1}$ are suggestive of maser emission. Very Large Arrayobservations reveal 36~GHz and/or 44~GHz CH$_3$OH, maser emission in a majority(72\%) of the NH$_3$, peak positions towards three of these SNRs. This goodpositional correlation is in agreement with the high densities required for theexcitation of each line. Through these observations we have shown thatCH$_3$OH, and NH$_3$, maser emission can be used as indicators of high densityclumps of gas shocked by supernova remnants, and provide density estimatesthereof. Modeling of the optical depth of the NH$_3$(3,3) emission is comparedto that of CH$_3$OH, constraining the densities of the clumps to a typicaldensity of the order of $10^5$~cm$^{-3}$ for cospatial masers. Regions of gaswith this density are found to exist in the post-shocked gas quite close to theSNR shock front, and may be associated with sites where cosmic rays producegamma-ray emission via neutral pion decay.

NH$_3$(3,3) and CH$_3$OH near Supernova Remnants: GBT and VLA Observations