Molecular environment of the thermal composite supernova remnant G352.7$-$0.1

Galactic supernova remnants (SNRs) play an important role in our understanding of supernovae and their feedback on the interstellar environment. SNR G352.7$-$0.1 is special for its thermal composite morphology and double-ring structure. We have performed spectroscopic mapping in ${}^{12}$CO and ${}^{13}$CO $J=2$-1 lines toward G352.7$-$0.1 with the Atacama Pathfinder Experiment telescope. Broad ${}^{12}$CO lines are found in the northeastern ring at a local-standard-of-rest velocity range of $\sim -50$-$-30$ km s${}^{-1}$, suggesting that the remnant is interacting with molecular clouds (MCs) at $\sim -51$ km s${}^{-1}$. Thus, we adopt a distance of $\sim 10.5$ kpc for this SNR. The momentum and kinetic energy of the shocked gas along the line of sight are estimated to be $\sim {10}^2{\mathrm{M}}_{\mathrm{s}\mathrm{u}\mathrm{n}}$ km s${}^{-1}$ and $\sim {10}^{46}$ erg, respectively. We also find an expanding structure around the remnant, which is possibly related to the wind-blown bubble of the progenitor star. From the Fermi-LAT data in an energy range of 0.1-500 GeV, we find no gamma-ray counterparts of G352.7$-$0.1.