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https://hdl.handle.net/2440/37496
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Type: | Journal article |
Title: | A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7 |
Other Titles: | A possible association of the new VHE gamma-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7 |
Author: | Aharonian, F. Akhperjanian, A. Bazer-Bachi, A. Beilicke, M. Benbow, W. Berge, D. Bernlohr, K. Boisson, C. Bolz, O. Borrel, V. Braun, I. Breitling, F. Brown, A. Chadwick, P. Chounet, L. Cornils, R. Costamante, L. Degrange, B. Dickinson, H. Djannati-Atai, A. et al. |
Citation: | Astronomy and Astrophysics: a European journal, 2005; 442(3):L25-L29 |
Publisher: | E D P Sciences |
Issue Date: | 2005 |
ISSN: | 0004-6361 1432-0746 |
Statement of Responsibility: | F. Aharonian...G. Rowell...et al. |
Abstract: | We report on a possible association of the recently discovered very high-energy γ-ray source HESS J1825-137 with the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the 2.1 x 10^4 year old Vela-like pulsar PSR B1823-13. HESS J1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the HESS instrument in 2004. The centroid position of HESS J1825-137 is offset by 11´ south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESS J1825-137 and G 18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of ~2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger than the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times with the pulsar wind nebula, resulting in the offset X-ray and TeV γ-ray morphology. |
Keywords: | ISM: plerions ISM: individual objects: PSR B1823-13, HESS J1825-137, G 18.0-0.7 gamma-rays: observations |
Rights: | © ESO 2005 |
DOI: | 10.1051/0004-6361:200500180 |
Published version: | http://dx.doi.org/10.1051/0004-6361:200500180 |
Appears in Collections: | Aurora harvest 6 Physics publications |
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hdl_37496.pdf | Published version | 326.12 kB | Adobe PDF | View/Open |
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