PoS - Proceedings of Science
Volume 395 - 37th International Cosmic Ray Conference (ICRC2021) - GAI - Gamma Ray Indirect
Modelling Spatial and Temporal Emission Properties of the Young Pulsar Wind Nebula Kes 75
C. Venter*, C.V. Rensburg and A. Kundu
Full text: pdf
Pre-published on: July 27, 2021
Published on: March 18, 2022
The H.E.S.S. Collaboration has firmly detected gamma-ray emission from HESS J1846-029, which is spatially coincident with Kes 75 (G29.7-0.3), one of the youngest composite supernova remnants in the Galaxy. This remnant contains the nebula of PSR J1846-0258, a glitching young pulsar with a particularly high spin-down luminosity, that has manifested magnetar-like bursts in 2006. However, H.E.S.S. was not able to distinguish between shell and nebular emission. This source may also plausibly be associated with the HAWC-detected source 2HWC J1844-032. Recent Chandra observations revealed a relatively rapid expansion of the embedded pulsar wind nebula over the past two decades and an X-ray flux decrease of 10% in 7 years. We apply a multi-zone
spatio-temporal pulsar wind nebula model to the morphological and spectral data over several epochs, and find reasonable fits to the broadband radiation spectrum, X-ray surface brightness
profile, photon spectral index in the X-ray energy range and expansion rate. Such spectral and morphological fitting constrains the model parameters and may aid in clarifying the nature of the gamma-ray emission.
DOI: https://doi.org/10.22323/1.395.0928
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