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We performed a spatially resolved spectral X-ray study of the pulsar windnebula (PWN) in the supernova remnant G0.9+0.1. Furthermore we modeled itsnonthermal emission in the X-ray and very high energy (VHE, E > 100 GeV)gamma-ray regime. Using Chandra ACIS-S3 data, we investigated the east-westdependence of the spectral properties of G0.9+0.1 by calculating hardnessratios. We analyzed the EPIC-MOS and EPIC-pn data of two on-axis observationsof the XMM-Newton telescope and extracted spectra of four annulus-shapedregions, centered on the region of brightest emission of the source. A radiallysymmetric leptonic model was applied in order to reproduce the observed X-rayemission of the inner part of the PWN. Using the optimized model parametervalues obtained from the X-ray analysis, we then compared the modeled inverseCompton (IC) radiation with the published H.E.S.S. gamma-ray data. The spectralindex within the four annuli increases with growing distance to the pulsar,whereas the surface brightness drops. With the adopted model we are able toreproduce the characteristics of the X-ray spectra. The model results for theVHE gamma radiation, however, strongly deviate from the H.E.S.S. data.

Spatially resolved X-ray spectroscopy and modeling of the nonthermal emission of the PWN in G0.9+0.1