English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  First detection of a VHE gamma-ray spectral maximum from a Cosmic source: H.E.S.S. discovery of the Vela X nebula

Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., Beilicke, M., Benbow, W., Berge, D., et al. (2006). First detection of a VHE gamma-ray spectral maximum from a Cosmic source: H.E.S.S. discovery of the Vela X nebula. Astronomy and Astrophysics, 448(2), L43-L47. Retrieved from http://xxx.lanl.gov/abs/astro-ph/0601575.

Item is

Files

show Files

Locators

show

Creators

show
hide
 Creators:
Aharonian, F.1, Author           
Akhperjanian, A. G.1, Author           
Bazer-Bachi, A. R.2, Author
Beilicke, M.1, Author           
Benbow, W.1, Author           
Berge, D.1, Author           
Borrel, V.2, Author
Bernlöhr, K.1, Author           
Bolz, O.1, Author           
Boisson, C:2, Author
Glicenstein, J.F.1, Author           
Breitling, F.2, Author
Brown, A. M.2, Author
Dickinson, H.J.2, Author
Chadwick, P. M.2, Author
Braun, I.1, Author           
Chounet, L.-M.2, Author
Cornils, R.1, Author           
Costamante, L.1, Author           
Degrange, B.2, Author
Djannati-Atai, A.1, Author           Drury, L.O'C.2, AuthorEmmanoulopoulos, D.2, AuthorEspigat, P.2, AuthorFeinstein, F.1, Author           Jacholkowska, A.2, AuthorFontaine, G.2, AuthorFunk, S.1, Author           Gallant, Y. A.1, Author           Giebels, B.2, AuthorGillessen, S.1, Author           Goret, P.2, AuthorDubus, G.1, Author           Hadjichristidis, C.2, AuthorHauser, M.2, AuthorHeinzelmann, G.2, AuthorHenri, G.2, AuthorHermann, G.1, Author           Hinton, J. A.1, Author           Hofmann, W.1, Author           Holleran, M.2, AuthorHorns, D.1, Author           de Jager, O. C.2, AuthorKhélifi, B.1, Author           Komin, N.2, AuthorKonopelko, A.3, Author           Latham, I. J.2, AuthorLe Gallou, R.2, AuthorLemoine-Goumard, M.2, AuthorLemière, A.2, AuthorLeroy, N.2, AuthorLohse, T.2, AuthorMarcowith, A.2, AuthorMasterson, C.1, Author           McComb, T. J. L.2, Authorde Naurois, M.1, Author           Nolan, S. J.2, AuthorNoutsos, A.2, AuthorOrford, K. J.1, Author           Osborne, J. L.1, Author           Ouchrif, M.2, AuthorPanter, M.1, Author           Pelletier, G.2, AuthorPita, S.2, AuthorFuchs, Y.2, AuthorPühlhofer, G.1, Author           Punch, M.2, AuthorRaubenheimer, B. C.2, AuthorRaue, M.1, Author           Raux, J.2, AuthorRayner, S. M.2, AuthorMartin, J.M.2, AuthorReimer, A.2, AuthorReimer, O.2, AuthorRipken, J.2, AuthorTerrier, R.2, AuthorRob, L.2, AuthorRolland, L.2, AuthorRowell, G.1, Author           Sahakian, V.2, AuthorSaugé, L.1, Author           Schlenker, S.2, AuthorSchlickeiser, R.2, AuthorSchuster, C.2, AuthorSchwanke, U.2, AuthorSiewert, M.2, AuthorSol, H.2, AuthorSteenkamp, R.2, AuthorStegmann, C.2, AuthorTavernet, J.-P-2, AuthorThéoret, C. G.2, AuthorTluczykont, M.2, AuthorVenter, C.2, AuthorVasileiadis, G.1, Author           Vincent, P.2, AuthorVölk, H. J.3, Author           Wagner, S. J.2, AuthorMartineau-Huynh, O.2, AuthorSpangler, D.2, Author more..
Affiliations:
1Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society, ou_904550              
2Yerevan Physics Institute, 2 Alikhanian Brothers Street, 375036 Yerevan, Armenia. Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK. Centre d'Etude Spatiale des Rayonnements, CNRS/UPS, 9 av. du Colonel Roche, BP 4346, F-31029 Toulouse Cedex 4, France. Institut für Experimentalphysik, Universität Hamburg, Luruper Chaussee 149, D-22761 Hamburg, Germany. APC, UMR 7164 du CNRS, 11 Place Marcelin Berthelot, F-75231 Paris Cedex 05, France. Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D-12489 Berlin, Germany. Laboratoire Univers et Théories (LUTH), UMR 8102 du CNRS, Observatoire de Paris, Section de Meudon, F-92195 Meudon Cedex, France. Laboratoire de Physique Théorique et Astroparticules, IN2P3/CNRS, Université Montpellier II, CC 70, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France. Laboratoire Leprince-Ringuet, IN2P3/CNRS, Ecole Polytechnique, F-91128 Palaiseau, France. Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland. Landessternwarte, Königstuhl, D-69117 Heidelberg, Germany. Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, BP 53, F-38041 Grenoble Cedex 9, France. DAPNIA/DSM/CEA, CE Saclay, F-91191 Gif-sur-Yvette, France. Unit for Space Physics, North-West University, Potchefstroom 2520, South Africa. Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Universités Paris VI & VII, 4 Place Jussieu, F-75252 Paris Cedex 05, France. Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D-44780 Bochum, Germany. Institute of Particle and Nuclear Physics (IPNP), Charles University, V Holesovickach 2, 180 00 Prague 8, Czech Republic. University of Namibia, Private Bag 13301, Windhoek, Namibia., ou_persistent22              
3Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society, ou_907548              

Content

show
hide
Free keywords: Gamma rays: observations H.E.S.S.
 Abstract: The Vela supernova remnant (SNR) is a complex region containing a number of sources of non-thermal radiation. The inner section of this SNR, within 2 degrees of the pulsar PSR B0833-45, has been observed by the H.E.S.S. gamma-ray atmospheric Cherenkov detector in 2004 and 2005. A strong signal is seen from an extended region to the south of the pulsar, within an integration region of radius 0.8 deg. around the position (RA = 08h 35m 00s, dec = -45 deg. 36' J2000.0). The excess coincides with a region of hard X-ray emission seen by the ROSAT and ASCA satellites. The observed energy spectrum of the source between 550 GeV and 65 TeV is well fit by a power law function with photon index = 1.45 +/- 0.09(stat) +/- 0.2(sys) and an exponential cutoff at an energy of 13.8 +/- 2.3(stat) +/- 4.1(sys) TeV. The integral flux above 1 TeV is (1.28 +/- 0.17 (stat) +/- 0.38(sys)) x 10^{-11} cm^{-2} s^{-1}. This result is the first clear measurement of a peak in the spectral energy distribution from a VHE gamma-ray source, likely related to inverse Compton emission. A fit of an Inverse Compton model to the H.E.S.S. spectral energy distribution gives a total energy in non-thermal electrons of ~2 x 10^{45} erg between 5 TeV and 100 TeV, assuming a distance of 290 parsec to the pulsar. The best fit electron power law index is 2.0, with a spectral break at 67 TeV.

Details

show
hide
Language(s): eng - English
 Dates: 2006-03
 Publication Status: Issued
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: eDoc: 276606
URI: http://xxx.lanl.gov/abs/astro-ph/0601575
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Astronomy and Astrophysics
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 448 (2) Sequence Number: - Start / End Page: L43 - L47 Identifier: -