2008A&A...477..249M

We communicate the detection of soft (20-200keV) γ-rays from the pulsar and pulsar wind nebula of PSR J1846-0258 and aim to identify the component of the system which is responsible for the γ-ray emission. We combine spectral information from the INTEGRAL γ-ray mission with archival data from the Chandra X-ray Observatory to pinpoint the source of soft γ-ray emission. Our analysis shows that the soft γ-rays detected from PSR J1846-0258 include emission from both the pulsar and the pulsar wind nebula, but the measured spectral shape is dominated by the pulsar wind nebula. We discuss PSR J1846-0258 in the context of rotation-powered pulsars with high magnetic field strengths and review the anomalously high fraction of spin-down luminosity converted into X- and γ-ray emission in light of a possible overestimate of the distance to this pulsar.