Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/37496
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dc.contributor.author | Aharonian, F. | - |
dc.contributor.author | Akhperjanian, A. | - |
dc.contributor.author | Bazer-Bachi, A. | - |
dc.contributor.author | Beilicke, M. | - |
dc.contributor.author | Benbow, W. | - |
dc.contributor.author | Berge, D. | - |
dc.contributor.author | Bernlohr, K. | - |
dc.contributor.author | Boisson, C. | - |
dc.contributor.author | Bolz, O. | - |
dc.contributor.author | Borrel, V. | - |
dc.contributor.author | Braun, I. | - |
dc.contributor.author | Breitling, F. | - |
dc.contributor.author | Brown, A. | - |
dc.contributor.author | Chadwick, P. | - |
dc.contributor.author | Chounet, L. | - |
dc.contributor.author | Cornils, R. | - |
dc.contributor.author | Costamante, L. | - |
dc.contributor.author | Degrange, B. | - |
dc.contributor.author | Dickinson, H. | - |
dc.contributor.author | Djannati-Atai, A. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2005 | - |
dc.identifier.citation | Astronomy and Astrophysics: a European journal, 2005; 442(3):L25-L29 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.issn | 1432-0746 | - |
dc.identifier.uri | http://hdl.handle.net/2440/37496 | - |
dc.description.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. | - |
dc.description.statementofresponsibility | F. Aharonian...G. Rowell...et al. | - |
dc.language.iso | en | - |
dc.publisher | E D P Sciences | - |
dc.rights | © ESO 2005 | - |
dc.source.uri | http://dx.doi.org/10.1051/0004-6361:200500180 | - |
dc.subject | ISM: plerions | - |
dc.subject | ISM: individual objects: PSR B1823-13, HESS J1825-137, G 18.0-0.7 | - |
dc.subject | gamma-rays: observations | - |
dc.title | A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7 | - |
dc.title.alternative | A possible association of the new VHE gamma-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7 | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1051/0004-6361:200500180 | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | - |
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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