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Supernova remnants (SNRs) are the primary candidate of Galactic cosmic-rayaccelerators. It is still an open issue when and how young SNRs, whichtypically exhibit strong synchrotron X-rays and GeV and TeV gamma-rays, undergothe state transition to middle-aged SNRs dominated by thermal X-rays and GeVgamma-rays. The SNR N132D in the Large Magellanic Cloud is an ideal target tostudy such a transition, exhibiting bright X-rays and gamma-rays, and with theexpected age of ~2500 yrs. In this paper we present results of NuSTAR andSuzaku spectroscopy. We reveal that N132D has a nearly equilibrium plasma witha temperature of > 5 keV or a recombining plasma with a lower temperature (~1.5keV) and a recombining timescale (net) of 8.8 (7.0--10.0)e12 cm^-3s. Togetherwith the center filled morphology observed in the iron K line image, ourresults suggest that N132D is now at transition stage from a young SNR tomiddle-aged. We have constrained the tight upper-limit of nonthermal X-rays.Bright gamma-rays compared to faint nonthermal X-rays suggest that thegamma-rays are hadronic in origin. The spectral energy distribution from radioto gamma-rays shows a proton cut-off energy of ~30 TeV. These facts confirmthat N132D is in the transition from young to middle-aged SNR. The largethermal energy of > 10^51 erg and accelerated proton energy of ~ 10^50 ergsuggest the supernova explosion might have been very energetic.

The Transition from Young to Middle-aged Supernova Remnants: Thermal and Nonthermal Aspects of SNR N132D