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Discovery of extended VHE gamma-ray emission from the asymmetric pulsar wind nebula in MSH 15-52 with HESS

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posted on 24.10.2012, 08:53 by F. Aharonian, A. G. Akhperjanian, K. M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus, K. Bernlohr, C. Boisson, O. Bolz, I. Braun, F. Breitling, A. M. Brown, J. B. Gordo, P. M. Chadwick, L. M. Chounet, R. Cornils, L. Costamante, B. Degrange, A. Djannati-Atai, L. O. Drury, G. Dubus, D. Emmanoulopoulos, P. Espigat, F. Feinstein, P. Fleury, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, J. F. Glicenstein, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, de Jager O. C., B. Khelifi, N. Komin, A. Konopelko, IJ. Latham, Le Gallou R., A. Lemiere, M. Lemoine-Goumard, N. Leroy, T. Lohse, O. Martineau-Huynh, A. Marcowith, C. Masterson, T. J. L. McComb, de Naurois M., S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Puhlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Sauge, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J. P. Tavernet, R. Terrier, C. G. Theoret, M. Tluczykont, G. Vasileiadis, C. Venter, P. Vincent, H. J. Volk, S. J. Wagner
The Supernova Remnant MSH 15-52 has been observed in very high energy (VHE) $\gamma$-rays using the HESS 4-telescope array located in Namibia. A $\gamma$-ray signal is detected at the 25 sigma level during an exposure of 22.1 h live time. The image reveals an elliptically shaped emission region around the pulsar PSR B1509-58, with semi-major axis ~6' in the NW-SE direction and semi-minor axis ~2'. This morphology coincides with the diffuse pulsar wind nebula as observed at X-ray energies by ROSAT. The overall energy spectrum from 280 GeV up to 40 TeV can be fitted by a power law with photon index $\Gamma=2.27\pm0.03_{\textrm {\scriptsize\,stat}}\pm 0.20_{\textrm{\scriptsize\,syst}}$. The detected emission can be plausibly explained by inverse Compton scattering of accelerated relativistic electrons with soft photons.



Astronomy & Astrophysics, 2005, 435 (1), pp. L17-L20


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