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Issue A&A
Volume 442, Number 3, November II 2005
Page(s) L25 - L29
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200500180



A&A 442, L25-L29 (2005)
DOI: 10.1051/0004-6361:200500180

Letter

A possible association of the new VHE $\gamma$-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7

F. A. Aharonian1, A. G. Akhperjanian2, A. R. Bazer-Bachi3, M. Beilicke4, W. Benbow1, D. Berge1, K. Bernlöhr1, 5, C. Boisson6, O. Bolz1, V. Borrel3, I. Braun1, F. Breitling5, A. M. Brown7, P. M. Chadwick7, L.-M. Chounet8, R. Cornils4, L. Costamante1, 9, B. Degrange8, H. J. Dickinson7, A. Djannati-Ataï10, L. O'C. Drury11, G. Dubus8, D. Emmanoulopoulos12, P. Espigat10, F. Feinstein13, G. Fontaine8, Y. Fuchs14, S. Funk1, Y. A. Gallant13, B. Giebels8, S. Gillessen1, J. F. Glicenstein15, P. Goret15, C. Hadjichristidis7, M. Hauser12, G. Heinzelmann4, G. Henri14, G. Hermann1, J. A. Hinton1, W. Hofmann1, M. Holleran16, D. Horns1, A. Jacholkowska13, O. C. de Jager16, B. Khélifi1, Nu. Komin5, A. Konopelko1, 5, I. J. Latham7, R. Le Gallou7, A. Lemière10, M. Lemoine-Goumard8, N. Leroy8, T. Lohse5, J. M. Martin6, O. Martineau-Huynh17, A. Marcowith3, C. Masterson1, 9, T. J. L. McComb7, M. de Naurois17, S. J. Nolan7, A. Noutsos7, K. J. Orford7, J. L. Osborne7, M. Ouchrif17, 9, M. Panter1, G. Pelletier14, S. Pita10, G. Pühlhofer1, 12, M. Punch10, B. C. Raubenheimer16, M. Raue4, J. Raux17, S. M. Rayner7, A. Reimer18, O. Reimer18, J. Ripken4, L. Rob19, L. Rolland17, G. Rowell1, V. Sahakian2, L. Saugé14, S. Schlenker5, R. Schlickeiser18, C. Schuster18, U. Schwanke5, M. Siewert18, H. Sol6, D. Spangler7, R. Steenkamp20, C. Stegmann5, J.-P. Tavernet17, R. Terrier10, C. G. Théoret10, M. Tluczykont8, 9, G. Vasileiadis13, C. Venter16, P. Vincent17, H. J. Völk1 and S. J. Wagner12

1  Max-Planck-Institut für Kernphysik, Heidelberg, Germany
2  Yerevan Physics Institute, Yerevan, Armenia
3  Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, Toulouse, France
4  Universität Hamburg, Institut für Experimentalphysik, Hamburg, Germany
5  Institut für Physik, Humboldt-Universität zu Berlin, Germany
6  LUTH, UMR 8102 du CNRS, Observatoire de Paris, Section de Meudon, France
7  University of Durham, Department of Physics, Durham DH1 3LE, UK
8  Laboratoire Leprince-Ringuet, IN2P3/CNRS, Ecole Polytechnique, Palaiseau, France
9  European Associated Laboratory for Gamma-Ray Astronomy, jointly supported by CNRS and MPG
10  APC, Paris Cedex 05, France
11  Dublin Institute for Advanced Studies, Dublin, Ireland
12  Landessternwarte, Königstuhl, Heidelberg, Germany
13  Laboratoire de Physique Théorique et Astroparticules, Université Montpellier II, France
14  Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, France
15  DAPNIA/DSM/CEA, CE Saclay, Gif-sur-Yvette, France
16  Unit for Space Physics, North-West University, Potchefstroom, South Africa,
    e-mail: fskocdj@puk.ac.za
17  Laboratoire de Physique Nucléaire et de Hautes Énergies, IN2P3/CNRS, Universités Paris VI & VII, France
18  Institut für Theoretische Physik, Lehrstuhl IV, Ruhr-Universität Bochum, Germany
19  Institute of Particle and Nuclear Physics, Charles University, Prague, Czech Republic
20  University of Namibia, Windhoek, Namibia

(Received 27 July 2005 / Accepted 3 September 2005)

Abstract
We report on a possible association of the recently discovered very high-energy $\gamma$-ray source HESS J1825-137 with the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the $2.1\times 10^{4}$ year old Vela-like pulsar PSR B1823-13. HESS J1825-137 was detected with a significance of 8.1$\sigma$ 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 $\gamma$-ray morphology.


Key words: ISM: plerions -- ISM: individual objects: PSR B1823-13, HESS J1825-137, G 18.0-0.7 -- gamma-rays: observations

SIMBAD Objects



© ESO 2005


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