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RX J0046.5$-$7308 is a shell-type supernova remnant (SNR) in the SmallMagellanic Cloud (SMC). We carried out new $^{12}$CO($J$ = 1-0, 3-2)observations toward the SNR using Mopra and the Atacama Submillimeter TelescopeExperiment. We found eight molecular clouds (A-H) along the X-ray shell of theSNR. The typical cloud size and mass are $\sim$10-15 pc and $\sim$1000-3000$M_{\odot}$, respectively. The X-ray shell is slightly deformed and has thebrightest peak in the southwestern shell where two molecular clouds A and B arelocated. The four molecular clouds A, B, F, and G have high intensity ratios of$^{12}$CO($J$ = 3-2) / $^{12}$CO($J$ = 1-0) $> 1.2$, which are not attributableto any identified internal infrared sources or high-mass stars. The HI cavityand its expanding motion are found toward the SNR, which are likely created bystrong stellar winds from a massive progenitor. We suggest that the molecularclouds A-D, F, and G and HI clouds within the wind-blown cavity at$V_\mathrm{LSR} = 117.1$-122.5 km s$^{-1}$ are to be associated with the SNR.The X-ray spectroscopy reveals the dynamical age of $26000^{+1000}_{-2000}$ yrand the progenitor mass of $\gtrsim 30$ $M_{\odot}$, which is also consistentwith the proposed scenario. We determine physical conditions of the giantmolecular cloud LIRS 36A using the large velocity gradient analysis witharchival datasets of the Atacama Large Millimeter/submillimeter Array; thekinematic temperature is $72^{+50}_{-37}$ K and the number density of molecularhydrogen is $1500^{+600}_{-300}$ cm$^{-3}$. The next generation of $\gamma$-rayobservations will allow us to study the pion-decay $\gamma$-rays from themolecular clouds in the SMC SNR.

Discovery of Shocked Molecular Clouds Associated with the Shell-Type Supernova Remnant RX J0046.5$-$7308 in the Small Magellanic Cloud