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N132D is the brightest gamma-ray supernova remnant (SNR) in the LargeMagellanic Cloud (LMC). We carried out $^{12}$CO($J$ = 1-0, 3-2) observationstoward the SNR using the Atacama Large Millimeter/submillimeter Array (ALMA)and Atacama Submillimeter Telescope Experiment. We find diffuse CO emission notonly at the southern edge of the SNR as previously known, but also inside theX-ray shell. We spatially resolved nine molecular clouds using ALMA with anangular resolution of $5''$, corresponding to a spatial resolution of $\sim$1pc at the distance of the LMC. Typical cloud sizes and masses are $\sim$2.0 pcand $\sim$100 $M_\odot$, respectively. High-intensity ratios of CO $J$ = 3-2 /1-0 $> 1.5$ are seen toward the molecular clouds, indicating that shock-heatinghas occurred. Spatially resolved X-ray spectroscopy reveals that thermal X-raysin the center of N132D are produced not only behind a molecular cloud, but alsoin front of it. Considering the absence of a thermal component associated withthe forward shock towards one molecular cloud located along the line of sightto the center of the remnant, this suggests that this particular cloud isengulfed by shock waves and is positioned on the near side of remnant. If thehadronic process is the dominant contributor to the gamma-ray emission, theshock-engulfed clouds play a role as targets for cosmic-rays. We estimate thetotal energy of cosmic-ray protons accelerated in N132D to be $\sim$0.5-$3.8\times 10^{49}$ erg as a conservative lower limit, which is similar to thatobserved in Galactic gamma-ray SNRs.

astrophysical journal/the astrophysical journal

ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large  Magellanic Cloud: Possible Evidence for Shocked Molecular Clouds Illuminated  by Cosmic-Ray Protons