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XMM-Newton observations of HESS J1813-178 reveal a composite Supernova remnant

By S. Funk, J. Hinton, Y. Moriguchi, F. Aharonian, Y. Fukui, W. Hofmann, D. Horns, G. Puhlhofer, O. Reimer, G. Rowell, R. Terrier, J. Vink and S. Wagner

Abstract

Submitted to Cornell University’s online archive www.arXiv.org in 2006 by Stefan Funk.Aims.We present X-ray and 12CO(J=1-0) observations of the very-high-energy (VHE) -ray source HESS J1813-178 with the aim of understanding the origin of the -ray emission. Methods. High-angular resolution X-ray studies of the VHE -ray emission region are performed using 18.6 ks of XMM-Newton data, taken on HESS J1813-178 in October 2005. Using this data set we are able to undertake spectral and morphological studies of the X-ray emission from this object with greater precision than previous studies. NANTEN 12CO(J=1-0) data are used to search for correlations of the -ray emission with molecular clouds which could act as target material for -ray production in a hadronic scenario. Results.The NANTEN 12CO(J=1-0) observations show a giant molecular cloud of mass at a distance of 4 kpc in the vicinity of HESS J1813-178. Even though there is no direct positional coincidence, this giant cloud may have influenced the evolution of the -ray source and its surroundings. The X-ray data show a highly absorbed ( cm-2) non-thermal X-ray emitting object coincident with the previously known ASCA source AX J1813-178 exhibiting a compact core and an extended tail towards the north-east, located in the centre of the radio shell-type Supernova remnant (SNR) G12.82-0.02 . This central object shows morphological and spectral resemblance to a Pulsar Wind Nebula (PWN) and we therefore consider that this object is very likely to be a composite SNR. We discuss the scenario in which the -rays originate in the shell of the SNR, and that in which they originate in the central object, in terms of a time-dependent one-zone leptonic model. We demonstrate, that in order to connect the core X-ray emission to the VHE -ray emission electrons have to be accelerated to energies of at least 1 PeV.S. Funk, J. A. Hinton, Y. Moriguchi, F. A. Aharonian, Y. Fukui, W. Hofmann, D. Horns, G. Pühlhofer, O. Reimer, G. Rowell, R. Terrier, J. Vink and S. J. Wagne

Publisher: E D P Sciences
Year: 2007
DOI identifier: 10.1051/0004-6361:20066779
OAI identifier: oai:digital.library.adelaide.edu.au:2440/43376
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