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Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

  • F. Aharonian
  • , A. G. Akhperjanian
  • , G. Anton
  • , U. De Barres Almeida
  • , A. R. Bazer-Bachi
  • , Y. Becherini
  • , B. Behera
  • , W. Benbow
  • , K. Bernlöhr
  • , C. Boisson
  • , A. Bochow
  • , V. Borrel
  • , I. Braun
  • , E. Brion
  • , J. Brucker
  • , P. Brun
  • , R. Bühler
  • , T. Bulik
  • , I. Büsching
  • , T. Boutelier
  • S. Carrigan, P. M. Chadwick, A. Charbonnier, R. C.G. Chaves, A. Cheesebrough, L. M. Chounet, A. C. Clapson, G. Coignet, M. Dalton, M. K. Daniel, B. Degrange, C. Deil, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O'C Drury, F. Dubois, G. Dubus, J. Dyks, M. Dyrda, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, S. Gabici, Y. A. Gallant, L. Gérard, B. Giebels, J. F. Glicenstein, B. Glück, P. Goret, D. Hauser, M. Hauser, S. Heinz, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. De Jager, I. Jung, K. Katarzyński, U. Katz, S. Kaufmann, E. Kendziorra, M. Kerschhagg, D. Khangulyan, B. Khélifi, D. Keogh, Nu Komin, K. Kosack, G. Lamanna, J. P. Lenain, T. Lohse, V. Marandon, J. M. Martin, O. Martineau-Huynh, A. Marcowith, D. Maurin, T. J.L. McComb, M. C. Medina, R. Moderski, E. Moulin, M. Naumann-Godo, M. De Naurois, D. Nedbal, D. Nekrassov, J. Niemiec, S. J. Nolan, S. Ohm, J. F. Olive, E. De Oña Wilhelmi, K. J. Orford, M. Ostrowski, M. Panter, M. Paz Arribas, G. Pedaletti, G. Pelletier, P. O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, O. Reimer, F. Rieger, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, J. L. Skilton, H. Sol, D. Spangler, Stawarz, R. Steenkamp, C. Stegmann, G. Superina, P. H. Tam, J. P. Tavernet, R. Terrier, O. Tibolla, C. Van Eldik, G. Vasileiadis, C. Venter, L. Venter, J. P. Vialle, P. Vincent, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, A. Zech
  • Max-Planck-Institut für Kernphysik
  • Dublin Institute for Advanced Studies
  • Yerevan Physics Institute
  • Friedrich-Alexander University (FAU) Erlangen-Nürnberg and Universitätsklinikum Erlangen
  • Durham University
  • Centre national de la recherche scientifique
  • Astroparticule and Cosmol APC
  • CEA/UVSQ/CNRS
  • Landessternwarte Heidelberg
  • Humboldt-Universität zu Berlin
  • LUTH - Laboratoire de l'Univers et de ses Theories
  • Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
  • North-West University
  • Universités Paris VI and VII
  • Ip Paris
  • Université Paris-Sud
  • Institute for Nuclear Physics
  • Laboratoire Univers et Particules de Montpellier
  • Universität Hamburg
  • University of Leeds
  • University of Tübingen
  • Nicolaus Copernicus University
  • Charles University
  • CNRS and MPG
  • Jagiellonian University
  • Kavli Institute for Particle Astrophysics and Cosmology
  • University of Adelaide
  • Ruhr-University Bochum
  • University of Namibia

Research output: Contribution to journalArticlepeer-review

Abstract

Aims. Detection of a γ-ray source above 300 GeV is reported, confirming the unidentified source MGRO J1908+06, discovered by the Milagro collaboration at a median energy of 20 TeV. Methods. The source was observed during 27 h as part of the extension of the HESS Galactic plane survey to longitudes >30°. Results. HESS J108+063 is detected at a significance level of 10.9σ with an integral flux above 1 TeV of (3.76 ± 0.29 stat Plusmn: 0.75 sys ) × 10-12 ph cm-2 s-1, and a spectral photon index Γ = 2.10 ± 0.07 stat ± 0.2sys. The positions and fluxes of HESS J1908+063 and MGRO J1908+06 are in good agreement. Possible counterparts at other wavelengths and the origin of the γ-ray emission are discussed. The nearby unidentified GeV source, GRO J1908+0556 (GeV) which also remains unidentified and the new Fermi pulsar 0FGL J1907.5+0617, may be connected to the TeV source.

Original languageEnglish
Pages (from-to)723-728
Number of pages6
JournalAstronomy and Astrophysics
Volume499
Issue number3
DOIs
Publication statusPublished - 1 Jan 2009
Externally publishedYes

Keywords

  • Gamma rays
  • Observations

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