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The supernova remnant LMC N132D is a remarkably luminous gamma-ray emitter at$\sim$50 kpc with an age of $\sim$2500 years. It belongs to the small group ofoxygen-rich SNRs, which includes Cassiopeia A (Cas A) and Puppis A. N132D isinteracting with a nearby molecular cloud. By adding 102 hours of newobservations with the High Energy Stereoscopic System (H.E.S.S.) to thepreviously published data with exposure time of 150 hours, we achieve thesignificant detection of N132D at a 5.7$\sigma$ level in the very high energy(VHE) domain. The gamma-ray spectrum is compatible with a single power lawextending above 10 TeV. We set a lower limit on an exponential cutoff energy at8 TeV with 95% CL. The multi-wavelength study supports a hadronic origin of VHEgamma-ray emission indicating the presence of sub-PeV cosmic-ray protons. Thedetection of N132D is remarkable since the TeV luminosity is higher than thatof Cas A by more than an order of magnitude. Its luminosity is comparable to,or even exceeding the luminosity of RX J1713.7-3946 or HESS J1640-465.Moreover, the extended power-law tail in the VHE spectrum of N132D issurprising given both the exponential cutoff at 3.5 TeV in the spectrum of its340-year-old sibling, Cassiopeia A, and the lack of TeV emission from a Fermi-LAT 2FHL source (E > 50 GeV) associated with Puppis A. We discuss a physicalscenario leading to the enhancement of TeV emission via the interaction betweenN132D and a near molecular cloud.

LMC N132D: a mature supernova remnant with a youthful gamma-ray spectrum