Abstract
A fast rotating neutron star, or a pulsar, left behind by a core collapse supernova produces a Pulsar Wind Nebula (PWN) as a result of interactions between a relativistic outflow from the neutron star and the surrounding material. The pulsars and their nebulae offer a unique opportunity for studying the physics of relativistic plasma. Here we report on observations of gamma-ray emission from PWN N 157B in the Large Magellanic Cloud, powered by the most powerful pulsar known to date. The detected emission component allows two competing interpretations: (i) either it can be produced by particles forming a Maxwellian-type distribution through the inverse Compton scattering; or (ii) as synchrotron emission of particles accelerated by some extremely efficient process. The latter possibility is supported by the possible variability of the GeV emission. Detailed observations in the hard X-rays with NuSTAR or the GeV band with large dish Cherenkov detectors may shed light on the nature of this component.
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