HAL : in2p3-00024345, version 1

arXiv : astro-ph/0505380

DOI : 10.1051/0004-6361:200500130

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Astronomy and Astrophysics 437 (2005) L7-L10

Detection of TeV $\gamma$-ray Emission from the Shell-Type Supernova Remnant RX J0852.0-4622 with H.E.S.S

F. Aharonian, A. G. Akhperjanian, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, K. Bernlöhr, C. Boisson, O. Bolz, V. Borrel, I. Braun, F. Breitling, A. M. Brown, P. M. Chadwick, L.-M. Chounet1, R. Cornils, L. Costamante, B. Degrange1, H. J. Dickinson, A. Djannati-Ataï2, Drury L. O'C., G. Dubus1, D. Emmanoulopoulos, P. Espigat2, F. Feinstein3, G. Fontaine1, Y. Fuchs, S. Funk, Y. A. Gallant3, B. Giebels1, 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, A. Jacholkowska3, Jager O. C. De, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, Gallou R. Le, A. Lemière2, M. Lemoine-Goumard1, N. Leroy1, T. Lohse, J. M. Martin, O. Martineau-Huynh4, A. Marcowith, C. Masterson, T. J. L. Mccomb, M. Naurois De4, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif4, M. Panter, G. Pelletier, S. Pita2, G. Pühlhofer, M. Punch2, B. C. Raubenheimer, M. Raue, J. Raux4, S. M. Rayner, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland4, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, D. Spangler, R. Steenkamp, C. Stegmann, J.-P. Tavernet4, R. Terrier2, C.G. Théoret2, M. Tluczykont1, G. Vasileiadis3, C. Venter, P. Vincent4, H. J. Völk, S. J. Wagner

HESS Collaboration(s)

(2005)

We report the detection of TeV $\gamma$-rays from the shell-type supernova remnant RX J0852.0-4622 with data of 3.2 h of live time recorded with H.E.S.S. in February 2004. An excess of (700 $\pm$ 60) events from the whole remnant with a significance of 12 $\sigma$ was found. The observed emission region is clearly extended with a radius of the order of 1 degree and the spatial distribution of the signal correlates with X-ray observations. The spectrum in the energy range between 500 GeV and 15 TeV is well described by a power law with a photon index of $\Gamma=2.1 \pm 0.1_{stat} \pm 0.2_{syst}$ and a differential flux at 1 TeV of $\varphi$ 1TEV= (2.1 $\pm 0.2_{stat} \pm 0.6_{syst}) \times 10^{-11} cm^{-2} s^{-1} TeV^{-1}$. The integral flux above 1 TeV was measured to be $\Phi$ (E > 1 TeV) = (1.9 $\pm 0.3_{stat} \pm 0.6_{syst}) \times 10^{-11} cm^{-2} s^{-1}$, which is at the level of the flux of the Crab nebula at these energies. More data are needed to draw firm conclusions on the magnetic field in the remnant and the type of the particle population creating the TeV $\gamma$-rays.

1 :	LLR - Laboratoire Leprince-Ringuet
2 :	APC - AstroParticule et Cosmologie
3 :	LPTA - Laboratoire de Physique Théorique et Astroparticules
4 :	LPNHE - Laboratoire de Physique Nucléaire et de Hautes Énergies

Thème(s)

:

Planète et Univers/Astrophysique Physique/Astrophysique/Cosmologie et astrophysique extra-galactique

Mot(s)-clé(s) : gamma rays: observations – supernovae: individual: RX J0852.0-4622 (G266.2-1.2)

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Soumis le : Lundi 30 Octobre 2006, 15:53:19

Dernière modification le : Lundi 30 Octobre 2006, 20:02:55