hide
Free keywords:
pulsars: individual: PSR J1813-1749 – gamma rays: general – gamma rays: ISM
MPINP:
HESS - Abteilung Hinton
Abstract:
HESS, Context. J. is very-high-energy γ-ray source spatially coincident with the young, a. energetic pulsar PSR, J. and thought to be associated with its pulsar wind nebula Recently, (PWN). evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) This motivates revisiting the HESS, data. J. region taking advantage of improved analysis methods and an extended Using data taken by the High Energy Stereoscopic System experiment and the Fermi-LAT, dataset.
Aims. (H.E.S.S.) we aim to describe the γ-ray emission in the region with consistent model, a. to provide insights into its We performed likelihood-based analysis on, origin.
Methods. a. hours of data and, H.E.S.S. yr of Fermi-LAT data and we fitted spectro-morphological model to the combined These results allowed us to develop physical model for the origin of the observed γ-ray emission in the In addition to the compact very-high-energy γ-ray emission centred on the pulsar, a. datasets. a. region.
Results. we find significant yet previously undetected component along the Galactic With Fermi-LAT data, a. plane. we confirm extended high-energy emission consistent with the position and elongation of the extended emission observed with These results establish consistent description of the emission in the region from GeV energies to several tens of This study suggests that HESS, H.E.S.S. a. TeV.
Conclusions. J. is associated with γ-ray PWN powered by PSR, a. J. possible origin of the extended emission component is inverse Compton emission from electrons and positrons that have escaped the confines of the pulsar and form halo around the PWN.