The pulsar wind nebula (PWN) HESS J1825-137, known to exhibit strong energy dependent morphology, was discovered by HESS in 2005 [1, 2]. Powered by the pulsar PSR B1823-13, the TeV gamma-ray emitting nebula is significantly offset from the pulsar. The asymmetric shape and 21 kyr characteristic age of the pulsar suggest that HESS J1825-137 is in an evolved state, having possibly already undergone reverse shock interactions from the progenitor supernova. Given its large angular extent, despite its 4 kpc distance, it may have the largest intrinsic size of any TeV PWN so far detected. A rich dataset is currently available with H.E.S.S., including H.E.S.S. II data with a low energy threshold, enabling detailed studies of the source properties and environment. We present new views of the changing nature of the PWN with energy, including maps of the region and spectral studies.
6th International Symposium on High Energy Gamma-Ray Astronomy
- Pub Date:
- January 2017
- Astrophysics - High Energy Astrophysical Phenomena
- 6 pages, 5 figures. In Proceedings of the 6th International Symposium on High Energy Gamma-Ray Astronomy (Gamma16), Heidelberg, Germany