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The soft gamma-ray repeater (SGR) 0526-66 is the first-identified magnetar,and is projected within the supernova remnant N49 in the Large MagellanicCloud. Based on our ~50 ks NuSTAR observation, we detect the quiescent-state0526-66 for the first time in the 10-40 keV band. Based on the joint analysisof our NuSTAR and the archival Chandra ACIS data, we firmly establish thepresence of the nonthermal component in the X-ray spectrum of 0526-66 inaddition to the thermal emission. In the best-fit blackbody (BB) plus power law(PL) model, the slope of the PL component (photon index Gamma = 2.1) is steeperthan those (Gamma > ~1.5) for other magnetars. The soft part of the X-rayspectrum can be described with a BB component with the temperature of kT = 0.43keV. The best-fit radius (R = 6.5 km) of the X-ray-emitting area is smallerthan the canonical size of a neutron star. If we assume an underlying cool BBcomponent with the canonical radius of R = 10 km for the neutron star inaddition to the hot BB component (2BB + PL model), a lower BB temperature of kT= 0.24 keV is obtained for the passively cooling neutron star'ssurface, whilethe hot spot emission with kT = 0.46 keV dominates the thermal spectrum (~85%of the thermal luminosity in the 0.5-5 keV band). The nonthermal component(Gamma ~ 1.8) is still required.

NuSTAR Detection of Quiescent Hard X-Ray Emission from SGR 0526-66 in the Large Magellanic Cloud