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We present the first compelling evidence of shock-heated molecular cloudsassociated with the supernova remnant (SNR) N49 in the Large Magellanic Cloud(LMC). Using $^{12}$CO($J$ = 2-1, 3-2) and $^{13}$CO($J$ = 2-1) line emissiondata taken with the Atacama Large Millimeter/Submillimeter Array, we derivedthe H$_2$ number density and kinetic temperature of eight $^{13}$CO-detectedclouds using the large velocity gradient approximation at a resolution of3.5$''$ (~0.8 pc at the LMC distance). The physical properties of the cloudsare divided into two categories: three of them near the shock front show thehighest temperatures of ~50 K with densities of ~500-700 cm$^{-3}$, while otherclouds slightly distant from the SNR have moderate temperatures of ~20 K withdensities of ~800-1300 cm$^{-3}$. The former clouds were heated by supernovashocks, but the latter were dominantly affected by the cosmic-ray heating.These findings are consistent with the efficient production of X-rayrecombining plasma in N49 due to thermal conduction between the cold clouds andhot plasma. We also find that the gas pressure is roughly constant except forthe three shock-engulfed clouds inside or on the SNR shell, suggesting thatalmost no clouds have evaporated within the short SNR age of ~4800 yr. Thisresult is compatible with the shock-interaction model with dense and clumpyclouds inside a low-density wind bubble.

ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds