EDP Sciences
Free access
Volume 432, Number 1, March II 2005
Page(s) L9 - L12
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200500008

A&A 432, L9-L12 (2005)
DOI: 10.1051/0004-6361:200500008


Search for TeV emission from the region around PSR B1706-44 with the HESS experiment

F. Aharonian1, A. G. Akhperjanian2, K.-M. Aye3, A. R. Bazer-Bachi4, M. Beilicke5, W. Benbow1, D. Berge1, P. Berghaus6, K. Bernlöhr1, 7, C. Boisson8, O. Bolz1, C. Borgmeier7, I. Braun1, F. Breitling7, A. M. Brown3, J. Bussons Gordo9, P. M. Chadwick3, L.-M. Chounet10, R. Cornils5, L. Costamante1, 11, B. Degrange10, A. Djannati-Ataï6, L. O'C. Drury12, G. Dubus10, T. Ergin7, P. Espigat6, F. Feinstein9, P. Fleury10, G. Fontaine10, Y. Fuchs13, S. Funk1, Y. A. Gallant9, B. Giebels10, S. Gillessen1, P. Goret14, C. Hadjichristidis3, M. Hauser15, G. Heinzelmann5, G. Henri13, G. Hermann1, J. A. Hinton1, W. Hofmann1, M. Holleran16, D. Horns1, O. C. de Jager16, I. Jung1, 15, B. Khélifi1, Nu. Komin7, A. Konopelko1, 7, I. J. Latham3, R. Le Gallou3, A. Lemière6, M. Lemoine10, N. Leroy10, T. Lohse7, A. Marcowith4, C. Masterson1, 11, T. J. L. McComb3, M. de Naurois17, S. J. Nolan3, A. Noutsos3, K. J. Orford3, J. L. Osborne3, M. Ouchrif17, 11, M. Panter1, G. Pelletier13, S. Pita6, G. Pühlhofer1, 15, M. Punch6, B. C. Raubenheimer16, M. Raue5, J. Raux17, S. M. Rayner3, I. Redondo10, 11, A. Reimer18, O. Reimer18, J. Ripken5, L. Rob19, L. Rolland17, G. Rowell1, V. Sahakian2, L. Saugé13, S. Schlenker7, R. Schlickeiser18, C. Schuster18, U. Schwanke7, M. Siewert18, H. Sol8, R. Steenkamp20, C. Stegmann7, J.-P. Tavernet17, R. Terrier6, C. G. Théoret6, M. Tluczykont10, 11, G. Vasileiadis9, C. Venter16, P. Vincent17, B. Visser16, H. J. Völk1 and S. J. Wagner15

1  Max-Planck-Institut für Kernphysik, PO Box 103980, 69029 Heidelberg, Germany
    e-mail: Bruno.Khelifi@mpi-hd.mpg.de
2  Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia
3  University of Durham, Department of Physics, South Road, Durham DH1 3LE, UK
4  Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, 9 Av. du Colonel Roche, BP 4346, 31029 Toulouse Cedex 4, France
5  Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, 22761 Hamburg, Germany
6  Physique Corpusculaire et Cosmologie, IN2P3/CNRS, Collège de France, 11 place Marcelin Berthelot, 75231 Paris Cedex 05, France
7  Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, 12489 Berlin, Germany
8  LUTH, UMR 8102 du CNRS, Observatoire de Paris, Section de Meudon, 92195 Meudon Cedex, France
9  Groupe d'Astroparticules de Montpellier, IN2P3/CNRS, Université Montpellier II, CC85, Place Eugène Bataillon, 34095 Montpellier Cedex 5, France
10  Laboratoire Leprince-Ringuet, IN2P3/CNRS, Ecole Polytechnique, 91128 Palaiseau, France
11  European Associated Laboratory for Gamma-Ray Astronomy, jointly supported by CNRS and MPG
12  Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland
13  Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France
14  Service d'Astrophysique, DAPNIA/DSM/CEA, CE Saclay, 91191 Gif-sur-Yvette, France
15  Landessternwarte, Königstuhl, 69117 Heidelberg, Germany
16  Unit for Space Physics, North-West University, Potchefstroom 2520, South Africa
17  Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Universités Paris VI & VII, 4 place Jussieu, 75231 Paris Cedex 05, France
18  Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, 44780 Bochum, Germany
19  Institute of Particle and Nuclear Physics, Charles University, V Holesovickach 2, 180 00 Prague 8, Czech Republic
20  University of Namibia, Private Bag 13301, Windhoek, Namibia

(Received 22 December 2004 / Accepted 20 January 2005 )

The region around PSR B1706-44 has been observed with the HESS imaging atmospheric Cherenkov telescopes in 2003. No evidence for $\gamma$-ray emission in the TeV range was found at the pulsar position or at the radio arc which corresponds to the supernova remnant G 343.1-2.3. The 99% confidence level flux upper limit at the pulsar position is $F_{{\rm ul}}$( $E>350~{\rm GeV}) = 1.4 \times 10^{-12}~ {\rm s}^{-1}\,{\rm cm}^{-2}$ assuming a power law ( ${\rm d}N/{\rm d}E \propto E^{-\Gamma}$) with photon index of $\Gamma = 2.5$ and $F_{{\rm ul}}$( $E > 500\,{\rm GeV}) = 1.3 \times 10^{-12} ~ {\rm s}^{-1}\, {\rm cm}^{-2}$ without an assumption on the spectral shape. The reported upper limits correspond to 8% of the flux from an earlier detection by the CANGAROO experiment.

Key words: gamma rays: observations -- ISM: individual objects: PSR B1706-44 -- ISM: supernova remnants -- ISM: individual objects: G 343.1-2.3

SIMBAD Objects

© ESO 2005

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