%0 Journal Article
%T H.E.S.S. observations of the Carina nebula and its enigmatic colliding wind binary Eta Carinae
%+ Institut für Experimentalphysik [Hamburg]
%+ Laboratoire Univers et Particules de Montpellier (LUPM)
%+ Max-Planck-Institut für Kernphysik (MPIK)
%+ Yerevan Physics Institute
%+ Friedrich-Alexander Universität Erlangen-Nürnberg = University of Erlangen-Nuremberg (FAU)
%+ Nicolaus Copernicus University [Toruń]
%+ CEA- Saclay (CEA)
%+ Laboratoire Leprince-Ringuet (LLR)
%+ AstroParticule et Cosmologie (APC (UMR_7164))
%+ Institut für Theoretische Physik IV [Bochum] (ITP4)
%+ Humboldt-Universität zu Berlin = Humboldt University of Berlin = Université Humboldt de Berlin  (HU Berlin)
%+ Laboratoire Univers et Théories (LUTH (UMR_8102))
%+ Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE)
%+ Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen
%+ Physikalisches Institut [Erlangen]
%+ Astronomical Observatory [Warsaw]
%+ Dublin Institute for Advanced Studies (DIAS)
%+ Laboratoire d'Annecy de Physique des Particules (LAPP)
%+ Institut für Theoretische Physik [Berlin]
%+ Institut für Astronomie und Astrophysik [Tübingen] (IAAT)
%+ Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU)
%+ National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA)
%A Abramowski, A.
%A Acero, Fabio
%A Aharonian, F.
%A Akhperjanian, A. G.
%A Anton, G.
%A Balzer, Agnès
%A Barnacka, A.
%A Becherini, Y.
%A Becker, J.
%A Bernlöhr, K.
%A Birsin, E.
%A Biteau, J.
%A Bochow, A.
%A Boisson, C.
%A Bolmont, J.
%A Bordas, P.
%A Brucker, J.
%A Brun, F.
%A Brun, P.
%A Bulik, T.
%A Büsching, I.
%A Carrigan, S.
%A Casanova, S.
%A Cerruti, M.
%A Chadwick, P. M.
%A Charbonnier, A.
%A Chaves, R. C. G.
%A Cheesebrough, A.
%A Cologna, G.
%A Conrad, J.
%A Dalton, M.
%A Daniel, M. K.
%A Davids, I. D.
%A Degrange, B.
%A Deil, C.
%A Dickinson, H. J.
%A Djannati-Ataï, A.
%A Domainko, W.
%A Drury, L. O'C.
%A Dubus, G.
%A Dutson, K.
%A Dyks, J.
%A Dyrda, M.
%A Egberts, K.
%A Eger, P.
%A Espigat, P.
%A Fallon, L.
%A Fegan, S.
%A Feinstein, F.
%A Fernandes, M. V.
%A Fiasson, A.
%A Fontaine, G.
%A Förster, A.
%A Füssling, M.
%A Gallant, Y. A.
%A Garrigoux, T.
%A Gast, H.
%A Gérard, L.
%A Giebels, B.
%A Glicenstein, J. F.
%A Glück, B.
%A Göring, D.
%A Grondin, M.-H.
%A Häffner, S.
%A Hague, J. D.
%A Hahn, J.
%A Hampf, D.
%A Harris, J.
%A Hauser, M.
%A Heinz, S.
%A Heinzelmann, G.
%A Henri, G.
%A Hermann, G.
%A Hillert, A.
%A Hinton, J. A.
%A Hofmann, W.
%A Hofverberg, P.
%A Holler, M.
%A Horns, D.
%A Jacholkowska, A.
%A Jahn, C.
%A Jamrozy, M.
%A Jung, I.
%A Kastendieck, M. A.
%A Katarzyński, K.
%A Katz, U.
%A Kaufmann, S.
%A Khélifi, B.
%A Klochkov, D.
%A Kluźniak, W.
%A Kneiske, T.
%A Komin, Nu.
%A Kosack, K.
%A Kossakowski, R.
%A Krayzel, F.
%A Laffon, H.
%A Lamanna, G.
%A Lenain, J.-P.
%A Lennarz, D.
%A Lohse, T.
%A Lopatin, A.
%A Lu, C.-C.
%A Marandon, V.
%A Marcowith, Alexandre
%A Masbou, Julien
%A Maurin, G.
%A Maxted, N.
%A Mayer, M.
%A Mccomb, T. J. L.
%A Medina, M. C.
%A Méhault, J.
%A Moderski, R.
%A Mohamed, M.
%A Moulin, Emmanuel
%A Naumann, C. L.
%A Naumann-Godo, M.
%A de Naurois, M.
%A Nedbal, D.
%A Nekrassov, D.
%A Nguyen, N.
%A Nicholas, B.
%A Niemiec, J.
%A Nolan, S. J.
%A Ohm, S.
%A Wilhelmi, E. de Oña
%A Opitz, B.
%A Ostrowski, M.
%A Oya, I.
%A Panter, M.
%A Arribas, M. Paz
%A Pekeur, N. W.
%A Pelletier, G.
%A Perez, J.
%A Petrucci, P. -O.
%A Peyaud, B.
%A Pita, S.
%A Pühlhofer, G.
%A Punch, M.
%A Quirrenbach, A.
%A Raue, M.
%A Reimer, A.
%A Reimer, O.
%A Renaud, Matthieu
%A Reyes, R. de Los
%A Rieger, F.
%A Ripken, J.
%A Rob, L.
%A Rosier-Lees, S.
%A Rowell, G.
%A Rudak, B.
%A Rulten, C. B.
%A Sahakian, V.
%A Sanchez, D. A.
%A Santangelo, A.
%A Schlickeiser, R.
%A Schulz, A.
%A Schwanke, U.
%A Schwarzburg, S.
%A Schwemmer, S.
%A Sheidaei, F.
%A Skilton, J. L.
%A Sol, H.
%A Spengler, G.
%A Stawarz, Ł.
%A Steenkamp, R.
%A Stegmann, C.
%A Stinzing, F.
%A Stycz, K.
%A Sushch, I.
%A Szostek, A.
%A Tavernet, J. -P.
%A Terrier, R.
%A Tluczykont, M.
%A Valerius, K.
%A van Eldik, C.
%A Vasileiadis, George
%A Venter, C.
%A Viana, A.
%A Vincent, P.
%A Völk, H. J.
%A Volpe, F.
%A Vorobiov, S.
%A Vorster, M.
%A Wagner, S. J.
%A Ward, M.
%A White, R.
%A Wierzcholska, A.
%A Zacharias, M.
%A Zajczyk, A.
%A Zdziarski, A. A.
%A Zech, A.
%A Zechlin, H. -S.
%A Montmerle, T.
%Z 8 pages, 3 figures
%< avec comité de lecture
%@ 0035-8711
%J Monthly Notices of the Royal Astronomical Society
%I Oxford University Press (OUP): Policy P - Oxford Open Option A
%V 424
%P 128-135
%8 2012-06
%D 2012
%Z 1204.5690
%Z 2012MNRAS.424..128H
%R 10.1111/j.1365-2966.2012.21180.x
%K Galaxy: open clusters and association
%K ISM: individual: Eta Carina
%K ISM: individual: Carina Nebula
%K Amma-rays: observations
%K X-rays: binaries
%Z Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
%Z Physics [physics]
%Z Physics [physics]/Astrophysics [astro-ph]Journal articles
%X The massive binary system Eta Carinae and the surrounding HII complex, the Carina Nebula, are potential particle acceleration sites from which very-high-energy (VHE; E > 100 GeV) \gamma-ray emission could be expected. This paper presents data collected during VHE \gamma-ray observations with the H.E.S.S. telescope array from 2004 to 2010, which cover a full orbit of Eta Carinae. In the 33.1-hour data set no hint of significant \gamma-ray emission from Eta Carinae has been found and an upper limit on the \gamma-ray flux of 7.7 x 10-13 ph cm-2 s-1 (99% confidence level) is derived above the energy threshold of 470 GeV. Together with the detection of high-energy (HE; 0.1 GeV > E > 100 GeV) \gamma-ray emission by the Fermi-LAT up to 100 GeV, and assuming a continuation of the average HE spectral index into the VHE domain, these results imply a cut-off in the \gamma-ray spectrum between the HE and VHE \gamma-ray range. This could be caused either by a cut-off in the accelerated particle distribution or by severe \gamma-\gamma\ absorption losses in the wind collision region. Furthermore, the search for extended \gamma-ray emission from the Carina Nebula resulted in an upper limit on the \gamma-ray flux of 4.2 x 10-12 ph cm-2 s-1 (99% confidence level). The derived upper limit of ~23 on the cosmic-ray enhancement factor is compared with results found for the old-age mixed-morphology supernova remnant W 28.
%G English
%Z HESS
%2 https://hal.in2p3.fr/in2p3-00697570/document
%2 https://hal.in2p3.fr/in2p3-00697570/file/1204.5690.pdf
%L in2p3-00697570
%U https://hal.in2p3.fr/in2p3-00697570
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%~ INSU
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%~ UPMC
%~ UGA
%~ LAPP
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