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  • 1.
    Abdalla, H.
    et al.
    North-West University, South Africa.
    Abramowski, A.
    University of Hamburg, Germany.
    Aharonian, F.
    Max Planck Institute for Nuclear Physics, Germany ; Dublin Institute for Advanced Studies, Ireland ; National Academy of Sciences of the Republic of Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Institute for Nuclear Physics, Germany.
    Akhperjanian, A. G.
    National Academy of Sciences of the Republic of Armenia, Armenia ; Yerevan Physics Institute, Armenia.
    Andersson, T.
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Angüner, E. O.
    Humboldt University of Berlin, Germany.
    Arrieta, M.
    Paris Diderot University, France.
    Aubert, P.
    University of Savoy, France.
    Backes, M.
    University of Namibia, Namibia.
    Balzer, A.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany.;Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL1098 XH Amsterdam, Netherlands.;Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Barnard, M.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    Berge, D.
    Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.;Univ Amsterdam, Inst High Energy Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Bernhard, S.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Bernlohr, K.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Blackwell, R.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Bottcher, M.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Boisson, C.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Bolmont, J.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Bordas, P.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Bregeon, J.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Brun, F.
    Univ Bordeaux, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignam, F-33175 Gradignan, France..
    Brun, P.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Bryan, M.
    Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL1098 XH Amsterdam, Netherlands..
    Bulik, T.
    Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL00478 Warsaw, Poland..
    Capasso, M.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Carr, J.
    Aix Marseille Univ, CNRS IN2P3, CPPM UMR 7346, F-13288 Marseille, France..
    Casanova, S.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Cerruti, M.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Chakraborty, N.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Chalme-Calvet, R.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Chaves, R. C. G.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Chen, A.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Chevalier, J.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Chretien, M.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Colafrancesco, S.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Cologna, G.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Condon, B.
    Univ Bordeaux, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignam, F-33175 Gradignan, France..
    Conrad, J.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden..
    Cui, Y.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Davids, I. D.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.;Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
    Decock, J.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Degrange, B.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Deil, C.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Devin, J.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    deWilt, P.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Dirson, L.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Djannati-Atai, A.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Domainko, W.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Donath, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Drury, L. O 'C.
    Dubus, G.
    Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France..
    Dutson, K.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
    Dyks, J.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Dyrda, M.
    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Edwards, T.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Egberts, K.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Eger, P.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Ernenwein, J. -P
    Eschbach, S.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Farnier, Christian
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering. Stockholm University.
    Fegan, S.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Fernandes, M. V.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Fiasson, A.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Fontaine, G.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Forster, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Funk, S.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Fussling, M.
    DESY, D-15738 Zeuthen, Germany..
    Gabici, S.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Gajdus, M.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Gallant, Y. A.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Garrigoux, T.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Giavitto, G.
    DESY, D-15738 Zeuthen, Germany..
    Giebels, B.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Glicenstein, J. F.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Gottschal, D.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Goya, A.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Grondin, M. -H
    Hadasch, D.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Hahn, J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Haupt, M.
    DESY, D-15738 Zeuthen, Germany..
    Hawkes, J.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Heinzelmann, G.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Henri, G.
    Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France..
    Hermann, G.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hervet, O.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Hinton, J. A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hofmann, W.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hoischen, C.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Holler, M.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Horns, D.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Ivascenko, A.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Jacholkowska, A.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Jamrozy, M.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Janiak, M.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Jankowsky, D.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Jankowsky, F.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Jingo, M.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Jogler, T.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Jouvin, L.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Jung-Richardt, I.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Kastendieck, M. A.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Katarzynski, K.
    Nicolaus Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland..
    Katz, U.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Kerszberg, D.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Khelifi, B.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Kieffer, M.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    King, J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Klepser, S.
    DESY, D-15738 Zeuthen, Germany..
    Klochkov, D.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Kluzniak, W.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Kolitzus, D.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Komin, Nu.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Kosack, K.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Krakau, S.
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    Kraus, M.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Krayzel, F.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Kruger, P. P.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Laffon, H.
    Univ Bordeaux, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignam, F-33175 Gradignan, France..
    Lamanna, G.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Lau, J.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Lees, J. -P
    Lefaucheur, J.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Lefranc, V.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Lemiere, A.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Lemoine-Goumard, M.
    Univ Bordeaux, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignam, F-33175 Gradignan, France..
    Lenain, J. - P.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Leser, E.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Lohse, T.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Lorentz, M.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Liu, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Lopez-Coto, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Lypova, I.
    DESY, D-15738 Zeuthen, Germany..
    Marandon, V.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Marcowith, A.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Mariaud, C.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Marx, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Maurin, G.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Maxted, N.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Mayer, M.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Meintjes, P. J.
    Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa..
    Meyer, M.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden..
    Mitchell, A. M. W.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Moderski, R.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Mohamed, M.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Mohrmann, L.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Mora, K.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden..
    Moulin, E.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Murach, T.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    de Naurois, M.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Niederwanger, F.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Niemiec, J.
    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Oakes, L.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    O'Brien, P.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
    Odaka, H.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Ottl, S.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Ohm, S.
    DESY, D-15738 Zeuthen, Germany..
    Ostrowski, M.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Oya, I.
    DESY, D-15738 Zeuthen, Germany..
    Padovani, M.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Panter, M.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Parsons, R. D.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Pekeur, N. W.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Pelletier, G.
    Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France..
    Perennes, C.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Petrucci, P. -O
    Peyaud, B.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Piel, Q.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Pita, S.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Poon, H.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Prokhorov, Dmitry
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Prokoph, Heike
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Puhlhofer, G.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Punch, Michael
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering. Univ Paris Diderot, France.
    Quirrenbach, A.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Raab, S.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Reimer, A.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Reimer, O.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Renaud, M.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    de los Reyes, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Rieger, F.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;ITA Univ Heidelberg, D-69117 Heidelberg, Germany..
    Romoli, C.
    Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland..
    Rosier-Lees, S.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Rowel, G.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Rudak, B.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Rulten, C. B.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Sahakian, V.
    Natl Acad Sci Republ Armenia, Marshall Baghramian Ave 24, Yerevan, Armenia.;Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan, Armenia..
    Salek, D.
    Univ Amsterdam, Inst High Energy Phys, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Sanchez, D. A.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Santangelo, A.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Sasaki, M.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Schlickeiser, R.
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    Schussler, F.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Schulz, A.
    DESY, D-15738 Zeuthen, Germany..
    Schwanke, U.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Schwemmer, S.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Settimo, M.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Seyffert, A. S.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Shafi, N.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Shilon, I.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Simoni, R.
    Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL1098 XH Amsterdam, Netherlands..
    Sol, H.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Spanier, F.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Spengler, G.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden..
    Spies, F.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Stawarz, L.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Steenkamp, R.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
    Stegmann, C.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany.;DESY, D-15738 Zeuthen, Germany..
    Stinzing, F.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Stycz, K.
    DESY, D-15738 Zeuthen, Germany..
    Sushch, I.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Tavernet, J. -P
    Tavernier, T.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Taylor, A. M.
    Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland..
    Terrier, R.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Tibaldo, L.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Tiziani, D.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Tluczykont, M.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Trichard, C.
    Aix Marseille Univ, CNRS IN2P3, CPPM UMR 7346, F-13288 Marseille, France..
    Tuffs, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Uchiyama, Y.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
    van der Walt, D. J.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Eldik, C.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    van Rensburg, C.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Soelen, B.
    Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa..
    Vasileiadis, G.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Veh, J.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Venter, C.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Viana, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vincent, P.
    Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, Sorbonne Paris Cite,CNRS,Lab Phys Nucl & Hautes E, 4 Pl Jussieu, F-75252 Paris 5, France..
    Vink, J.
    Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL1098 XH Amsterdam, Netherlands..
    Voisin, F.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Volk, H. J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vuillaume, T.
    Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules, CNRS IN2P3, F-74941 Annecy Le Vieux, France..
    Wadiasingh, Z.
    North Wes Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Wagner, S. J.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Wagner, P.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Wagner, R. M.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden..
    White, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Wierzcholska, A.
    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Willmann, P.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Wornlein, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Wouters, D.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Yang, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zabalza, V.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
    Zaborov, D.
    Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, F-91128 Palaiseau, France..
    Zacharias, M.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Zanin, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zdziarski, A. A.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Zech, A.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Zefi, F.
    Univ Paris Diderot, AstroParticule & Cosmol, Observ Paris,Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, 10 Rue Alice Dormon & Leonie Duquet, F-75205 Paris 13, France..
    Ziegler, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Zywucka, N.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    HESS discovery of very high energy gamma-ray emission from PKS 0625-3542018In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 476, no 3, p. 4187-4198Article in journal (Refereed)
    Abstract [en]

    PKS 0625-354 (z = 0.055) was observed with the four High Energy Stereoscopic System (H.E.S.S.) telescopes in 2012 during 5.5 h. The source was detected above an energy threshold of 200 GeV at a significance level of 6.1 sigma. No significant variability is found in these observations. The source is well described with a power-law spectrum with photon index Gamma = 2.84 +/- 0.50(stat) +/- 0.10(syst) and normalization (at E-0 = 1.0 TeV) N-0(E-0)=(0.58 +/- 0.22(stat) +/- 0.12(syst)) x 10(-12) TeV-1 cm(-2) s(-1). Multiwavelength data collected with Fermi-LAT, Swift-XRT, Swift-UVOT, ATOM and WISE are also analysed. Significant variability is observed only in the Fermi-LAT gamma-ray and Swift-XRT X-ray energy bands. Having a good multiwavelength coverage from radio to very high energy, we performed a broad-band modelling from two types of emission scenarios. The results from a one zone lepto-hadronic and a multizone leptonic models are compared and discussed. On the grounds of energetics, our analysis favours a leptonic multizone model. Models associated to the X-ray variability constraint support previous results, suggesting a BL Lac nature of PKS 0625-354 with, however, a large-scale jet structure typical of a radio galaxy.

  • 2. Abdalla, H.
    et al.
    Aharonian, F.
    Benkhali, F. Ait
    Anguner, E. O.
    Arakawa, M.
    Arcaro, C.
    Armand, C.
    Arrieta, M.
    Backes, M.
    Barnard, M.
    Becherini, Y.
    Tjus, J. Becker
    Berge, D.
    Bernhard, S.
    Bernloehr, K.
    Blackwell, R.
    Bottcher, M.
    Boisson, C.
    Bolmont, J.
    Bonnefoy, S.
    Bordas, P.
    Bregeon, J.
    Brun, F.
    Brun, P.
    Bryan, M.
    Buechele, M.
    Bulik, T.
    Bylund, T.
    Capasso, M.
    Caroff, S.
    Carosi, A.
    Casanova, S.
    Cerruti, M.
    Chakraborty, N.
    Chandra, S.
    Chaves, R. C. G.
    Chen, A.
    Colafrancesco, S.
    Condon, B.
    Davids, I. D.
    Dei, C.
    Devin, J.
    deWilt, P.
    Dirson, L.
    Djannati-Atai, A.
    Dmytriiev, A.
    Donath, A.
    Drury, L. O. 'C.
    Dyks, J.
    Egberts, K.
    Emery, G.
    Ernenwein, J. -P.
    Eschbach, S.
    Fegan, S.
    Fiasson, A.
    Fontaine, G.
    Funk, S.
    Fuessling, M.
    Gabici, S.
    Gallant, Y. A.
    Garrigoux, T.
    Gate, F.
    Giavitto, G.
    Glawion, D.
    Glicenstein, J. F.
    Gottschall, D.
    Grondin, M. -H.
    Hahn, J.
    Haupt, M.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hinton, J. A.
    Hofmann, W.
    Hoischen, C.
    Holch, T. L.
    Holler, M.
    Horns, D.
    Huber, D.
    Iwasaki, H.
    Jacholkowska, A.
    Jamrozy, M.
    Jankowsky, D.
    Jankowsky, F.
    Jouvin, L.
    Jung-Richardt, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katsuragawa, M.
    Katz, U.
    Kerszberg, D.
    Khangulyan, D.
    Khelifi, B.
    King, J.
    Klepser, S.
    Kluzniak, W.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Kraus, M.
    Kruger, R. R.
    Lamanna, G.
    Lau, J.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P.
    Leser, E.
    Lohse, T.
    Lorentz, M.
    Lopez-Coto, R.
    Lypova, I.
    Malyshev, D.
    Marandon, V.
    Marcowith, A.
    Mariaud, C.
    Marti-Devesa, G.
    Marx, R.
    Maurin, G.
    Meintjes, P. J.
    Mitche, A. M. W.
    Moderski, R.
    Mohamed, M.
    Mohrmann, L.
    Moulin, E.
    Murach, T.
    Nakashima, S.
    de Naurois, M.
    Ndiyavala, H.
    Niederwanger, F.
    Niemiec, J.
    Oakes, L.
    O'Brien, P.
    Odaka, H.
    Ohm, S.
    Ostrowski, M.
    Oya, I.
    Padovani, M.
    Panter, M.
    Parsons, R. D.
    Perennes, C.
    Petrucci, P. -O.
    Peyaud, B.
    Piel, Q.
    Pita, S.
    Poireau, V.
    Noel, A. Priyana
    Prokhorov, D. A.
    Prokoph, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Rauth, R.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    Rieger, F.
    Rinchiuso, L.
    Romoli, C.
    Rowell, G.
    Rudak, B.
    Ruiz-Velasco, E.
    Sahakian, V.
    Saito, S.
    Sanchez, D. A.
    Santangelo, A.
    Sasaki, M.
    Schlickeiser, R.
    Schussler, F.
    Schulz, A.
    Schwanke, U.
    Schwemmer, S.
    Seglar-Arroyo, M.
    Senniappan, M.
    Seyffert, A. S.
    Shafi, N.
    Shilon, I.
    Shiningayamwe, K.
    Simoni, R.
    Sinha, A.
    Sol, H.
    Spanier, F.
    Specovius, A.
    Spir-Jacob, M.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Steppa, C.
    Sushch, I.
    Takahashi, T.
    Tavernet, J. -P.
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tibaldo, L.
    Tiziani, D.
    Tluczykont, M.
    Trichard, C.
    Tsirou, M.
    Tsuji, N.
    Tuffs, R.
    Uchiyama, Y.
    van der Walt, D. J.
    van Eldik, C.
    van Rensburg, C.
    van Soelen, B.
    Vasileiadis, G.
    Veh, J.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voisin, F.
    Voelk, H. J.
    Vuillaume, T.
    Wadiasingh, Z.
    Wagner, S. J.
    Wagner, P.
    Wagner, Robert M.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    White, R.
    Wierzcholska, A.
    Woernlein, A.
    Yang, R.
    Zaborov, D.
    Zacharias, M.
    Zanin, R.
    Zdziarski, A. A.
    Zech, A.
    Zefi, F.
    Ziegler, A.
    Zorn, J.
    Zywucka, N.
    VHE gamma-ray discovery and multiwavelength study of the blazar 1ES 2322-4092019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 482, no 3, p. 3011-3022Article in journal (Refereed)
    Abstract [en]

    A hotspot at a position compatible with the BL. Lac object 1ES 2322-409 was serendipitously detected with H.E.S.S. during observations performed in 2004 and 2006 on the blazar PKS 2316-423. Additional data on 1ES 2322-409 were taken in 2011 and 2012, leading to a total live-time of 22.3 h. Point-like very-high-energy (VHE; E > 100 GeV) gamma-ray emission is detected from a source centred on the IFS 2322-409 position, with an excess of 116.7 events at a significance of 6.0 sigma. The average VHE gamma-ray spectrum is well described with a power law with a photon index Gamma = 3.40 +/- 0.66(stat) +/- 0.20(sys) and an integral flux Phi(E > 200 GeV) = (3.11 +/- 0.71(stat) 0.62(sys)) x 10(-2)cm(-2)s(-1), which corresponds to 1.1 per cent of the Crab nebula flux above 200 GeV. Multiwavelength data obtained with Fermi LAT, Swift XRT and UVOT, RXTE PCA, ATOM, and additional data from WISE, GROND, and Catalina are also used to characterize the broad-band non-thermal emission of lES 2322-409. The multiwavelength behaviour indicates day-scale variability. Swift UVOT and XRT data show strong variability at longer scales. A spectral energy distribution (SED) is built from contemporaneous observations obtained around a high state identified in Swift data. A modelling of the SED is performed with a stationary homogeneous one-zone synchrotronself-Compton leptonic model. The redshift of the source being unknown, two plausible values were tested for the modelling. A systematic scan of the model parameters space is performed, resulting in a well-constrained combination of values providing a good description of the broad-band behaviour of 1ES 2322-409.

  • 3. Abdalla, H.
    et al.
    Aharonian, F.
    Benkhali, F. Ait
    Anguner, E. O.
    Arakawa, M.
    Arcaro, C.
    Armand, C.
    Arrieta, M.
    Backes, M.
    Barnard, M.
    Becherini, Y.
    Tjus, J. Becker
    Berge, D.
    Bernloehr, K.
    Blackwell, R.
    Bottcher, M.
    Boisson, C.
    Bolmont, J.
    Bonnefoy, S.
    Bordas, P.
    Bregeon, J.
    Brun, F.
    Brun, P.
    Bryan, M.
    Buchele, M.
    Bulik, T.
    Bylund, T.
    Capasso, M.
    Caroff, S.
    Carosi, A.
    Casanova, S.
    Cerruti, M.
    Chakraborty, N.
    Chand, T.
    Chandra, S.
    Chaves, R. C. G.
    Chen, A.
    Colafrancesco, S.
    Condon, B.
    Davids, I. D.
    Deil, C.
    Devin, J.
    deWilt, P.
    Dirson, L.
    Djannati-Atai, A.
    Dmytriiev, A.
    Donath, A.
    Doroshenko, V.
    Drury, L. O'C.
    Dyks, J.
    Egberts, K.
    Emery, G.
    Ernenwein, J. -P.
    Eschbach, S.
    Fegan, S.
    Fiasson, A.
    Fontaine, G.
    Funk, S.
    Fuessling, M.
    Gabici, S.
    Gallant, Y. A.
    Gate, F.
    Giavitto, G.
    Glawion, D.
    Glicenstein, J. F.
    Gottschall, D.
    Grondin, M. -H.
    Hahn, J.
    Haupt, M.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hinton, J. A.
    Hofmann, W.
    Hoischen, C.
    Holch, T. L.
    Holler, M.
    Horns, D.
    Huber, D.
    Iwasaki, H.
    Jacholkowska, A.
    Jamrozy, M.
    Jankowsky, D.
    Jankowsky, F.
    Jouvin, L.
    Jung-Richardt, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katsuragawa, M.
    Katz, U.
    Khangulyan, D.
    Khelifi, B.
    King, J.
    Klepser, S.
    Kluzniak, W.
    Komin, Nu.
    Kosack, K.
    Kraus, M.
    Lamanna, G.
    Lau, J.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P.
    Leser, E.
    Lohse, T.
    Lopez-Coto, R.
    Lorentz, M.
    Lypova, I.
    Malyshev, D.
    Marandon, V.
    Marcowith, A.
    Mariaud, C.
    Marti-Devesa, G.
    Marx, R.
    Maurin, G.
    Meintjes, P. J.
    Mitchell, A. M. W.
    Moderski, R.
    Mohamed, M.
    Mohrmann, L.
    Moore, C.
    Moulin, E.
    Murach, T.
    Nakashima, S.
    de Naurois, M.
    Ndiyavala, H.
    Niederwanger, F.
    Niemiec, J.
    Oakes, L.
    O'Brien, P.
    Odaka, H.
    Ohm, S.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Perennes, C.
    Petrucci, P. -O.
    Peyaud, B.
    Piel, Q.
    Pita, S.
    Poireau, V.
    Noel, A. Priyana
    Prokhorov, D. A.
    Prokoph, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Rauth, R.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    Rieger, F.
    Rinchiuso, L.
    Romoli, C.
    Rowell, G.
    Rudak, B.
    Ruiz-Velasco, E.
    Sahakian, V.
    Saito, S.
    Sanchez, D. A.
    Santangelo, A.
    Sasaki, M.
    Schlickeiser, R.
    Schussler, F.
    Schulz, A.
    Schutte, H.
    Schwanke, U.
    Schwemmer, S.
    Seglar-Arroyo, M.
    Senniappan, M.
    Seyffert, A. S.
    Shafi, N.
    Shilon, I.
    Shiningayamwe, K.
    Simoni, R.
    Sinha, A.
    Sol, H.
    Specovius, A.
    Spir-Jacob, M.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Steppa, C.
    Takahashi, T.
    Tavernet, J. -P.
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tiziani, D.
    Tluczykont, M.
    Trichard, C.
    Tsirou, M.
    Tsuji, N.
    Tuffs, R.
    Uchiyama, Y.
    van der Walt, D. J.
    van Eldik, C.
    van Rensburg, C.
    van Soelen, B.
    Vasileiadis, G.
    Veh, J.
    Venter, C.
    Vincent, P.
    Vink, J.
    Voisin, F.
    Voelk, H. J.
    Vuillaume, T.
    Wadiasingh, Z.
    Wagner, S. J.
    Wagner, Robert M.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    White, R.
    Wierzcholska, A.
    Yang, R.
    Yoneda, H.
    Zaborov, D.
    Zacharias, M.
    Zanin, R.
    Zdziarski, A. A.
    Zech, A.
    Ziegler, A.
    Zorn, J.
    Zywucka, N.
    HESS observations of the flaring gravitationally lensed galaxy PKS 1830-2112019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 486, no 3, p. 3886-3891Article in journal (Refereed)
    Abstract [en]

    PKS 1830-211 is a known macrolensed quasar located at a redshift of z = 2.5. Its highenergy gamma-ray emission has been detected with the Fermi-Large Area Telescope (LAT) instrument and evidence for lensing was obtained by several authors from its high-energy data. Observations of PKS 1830-211 were taken with the High Energy Stereoscopic System (H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014 August, following a flare alert by the Fermi-LAT Collaboration. The H.E.S.S observations were aimed at detecting a gamma-ray flare delayed by 20-27 d from the alert flare, as expected from observations at other wavelengths. More than 12 h of good-quality data were taken with an analysis threshold of similar to 67 GeV. The significance of a potential signal is computed as a function of the date and the average significance over the whole period. Data are compared to simultaneous observations by Fermi-LAT. No photon excess or significant signal is detected. An upper limit on PKS 1830-211 flux above 67 GeV is computed and compared to the extrapolation of the Fermi-LAT flare spectrum.

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    DESY, D-15738 Zeuthen, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Paris Diderot, LUTH, Observ Paris, PSL Res Univ,CNRS, 5 Pl Jules Janssen, E-92190 Meudon, France..
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    Univ Paris Diderot, Sorbonne Univ, Sorbonne Paris Cite, CNRS,IN2P3,Lab Phys Theor & Hautes Energies, 4 Pl Jussieu, F-75252 Paris, France..
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    DESY, D-15738 Zeuthen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Univ Amsterdam, GRAPPA, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland..
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    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
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    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS, F-74000 Annecy, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
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    Univ Paris Diderot, Sorbonne Univ, Sorbonne Paris Cite, CNRS,IN2P3,Lab Phys Theor & Hautes Energies, 4 Pl Jussieu, F-75252 Paris, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
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    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
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    Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France..
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    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
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    Univ Paris Diderot, AstroParticule & Cosmol, Sorbonne Paris Cite, Observ Paris,APC,CNRS,IN2P3,CEA Irfu, 10 Rue Alice Damon & Leonie Duquet, F-75205 Paris 13, France..
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    Univ Paris Diderot, LUTH, Observ Paris, PSL Res Univ,CNRS, 5 Pl Jules Janssen, E-92190 Meudon, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland..
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    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
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    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Golm, Germany..
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    Univ Paris Diderot, Sorbonne Univ, Sorbonne Paris Cite, CNRS,IN2P3,Lab Phys Theor & Hautes Energies, 4 Pl Jussieu, F-75252 Paris, France..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    DESY, D-15738 Zeuthen, Germany..
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    Univ Paris Diderot, AstroParticule & Cosmol, Sorbonne Paris Cite, Observ Paris,APC,CNRS,IN2P3,CEA Irfu, 10 Rue Alice Damon & Leonie Duquet, F-75205 Paris 13, France..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS, F-74000 Annecy, France..
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    DESY, D-15738 Zeuthen, Germany..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Golm, Germany..
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    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Univ Paris Diderot, Sorbonne Univ, Sorbonne Paris Cite, CNRS,IN2P3,Lab Phys Theor & Hautes Energies, 4 Pl Jussieu, F-75252 Paris, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
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    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan..
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    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
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    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
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    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
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    Uniwersytet Jagiellonski, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland..
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    DESY, D-15738 Zeuthen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS, F-74000 Annecy, France..
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    Uniwersytet Jagiellonski, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland..
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    DESY, D-15738 Zeuthen, Germany..
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    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
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    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering. Univ Paris Diderot, France.
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Thilchenphys, A-6020 Innsbruck, Austria..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;ITA Univ Heidelberg, D-69117 Heidelberg, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Natl Acad Sci Republ Armenia, Marshall Baglzramian Ave, Yerevan 240019, Armenia.;Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia..
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    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS, F-74000 Annecy, France..
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    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    DESY, D-15738 Zeuthen, Germany..
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    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Senniappan, Mohanraj
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Shafi, N.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Shilon, I.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Shiningayamwe, K.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
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    Univ Amsterdam, GRAPPA, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Sinha, A.
    Univ Paris Diderot, AstroParticule & Cosmol, Sorbonne Paris Cite, Observ Paris,APC,CNRS,IN2P3,CEA Irfu, 10 Rue Alice Damon & Leonie Duquet, F-75205 Paris 13, France..
    Sol, H.
    Univ Paris Diderot, LUTH, Observ Paris, PSL Res Univ,CNRS, 5 Pl Jules Janssen, E-92190 Meudon, France..
    Spanier, F.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Specovius, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Spir-Jacob, M.
    Univ Paris Diderot, AstroParticule & Cosmol, Sorbonne Paris Cite, Observ Paris,APC,CNRS,IN2P3,CEA Irfu, 10 Rue Alice Damon & Leonie Duquet, F-75205 Paris 13, France..
    Stawarz, L.
    Uniwersytet Jagiellonski, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland..
    Steenkamp, R.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
    Stegmann, C.
    DESY, D-15738 Zeuthen, Germany.;Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Golm, Germany..
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    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Golm, Germany..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Takahashi, T.
    Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan..
    Tavernet, J. -P
    Tavernier, T.
    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Taylor, A. M.
    DESY, D-15738 Zeuthen, Germany..
    Terrier, R.
    Univ Paris Diderot, AstroParticule & Cosmol, Sorbonne Paris Cite, Observ Paris,APC,CNRS,IN2P3,CEA Irfu, 10 Rue Alice Damon & Leonie Duquet, F-75205 Paris 13, France..
    Tibaldo, L.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Tiziani, D.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Tluczykont, M.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Trichard, C.
    Aix Marseille Univ, CNRS, IN2P3, CPPM, F-13288 Marseille 09, France..
    Tsirou, M.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Tsuji, N.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
    Tuffs, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Uchiyama, Y.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
    van der Walt, D. J.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Eldik, C.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    van Rensburg, C.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Soelen, B.
    Univ Free State, Dept Phys, POB 339, ZA-9100 Bloemfontein, South Africa..
    Vasileiadis, G.
    Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Veh, J.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Venter, C.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Viana, A.
    Univ Sao Paulo, Inst Fis Sao Carlos, Ave Trabalhador Sao Carlense 400, BR-13566590 Sao Carlos, SP, Brazil.;Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vincent, P.
    Univ Paris Diderot, Sorbonne Univ, Sorbonne Paris Cite, CNRS,IN2P3,Lab Phys Theor & Hautes Energies, 4 Pl Jussieu, F-75252 Paris, France..
    Vink, J.
    Univ Amsterdam, GRAPPA, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Voisin, F.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Voelk, H. J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vuillaume, T.
    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS, F-74000 Annecy, France..
    Wadiasingh, Z.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Wagner, P.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Wagner, R. M.
    Stockholm Univ, Oskar Klein Ctr, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden..
    White, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Wierzcholska, A.
    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Woernlein, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Yang, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zaborov, D.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Zacharias, M.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Zanin, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zdziarski, A. A.
    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Zech, A.
    Univ Paris Diderot, LUTH, Observ Paris, PSL Res Univ,CNRS, 5 Pl Jules Janssen, E-92190 Meudon, France..
    Zefi, F.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Ziegler, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Zorn, J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zywucka, N.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    VHE gamma-ray discovery and multiwavelength study of the blazar 1ES 2322-4092019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 482, no 3, p. 3011-3022Article in journal (Refereed)
    Abstract [en]

    A hotspot at a position compatible with the BL. Lac object 1ES 2322-409 was serendipitously detected with H.E.S.S. during observations performed in 2004 and 2006 on the blazar PKS 2316-423. Additional data on 1ES 2322-409 were taken in 2011 and 2012, leading to a total live-time of 22.3 h. Point-like very-high-energy (VHE; E > 100 GeV) gamma-ray emission is detected from a source centred on the IFS 2322-409 position, with an excess of 116.7 events at a significance of 6.0 sigma. The average VHE gamma-ray spectrum is well described with a power law with a photon index Gamma = 3.40 +/- 0.66(stat) +/- 0.20(sys) and an integral flux Phi(E > 200 GeV) = (3.11 +/- 0.71(stat) 0.62(sys)) x 10(-2)cm(-2)s(-1), which corresponds to 1.1 per cent of the Crab nebula flux above 200 GeV. Multiwavelength data obtained with Fermi LAT, Swift XRT and UVOT, RXTE PCA, ATOM, and additional data from WISE, GROND, and Catalina are also used to characterize the broad-band non-thermal emission of lES 2322-409. The multiwavelength behaviour indicates day-scale variability. Swift UVOT and XRT data show strong variability at longer scales. A spectral energy distribution (SED) is built from contemporaneous observations obtained around a high state identified in Swift data. A modelling of the SED is performed with a stationary homogeneous one-zone synchrotronself-Compton leptonic model. The redshift of the source being unknown, two plausible values were tested for the modelling. A systematic scan of the model parameters space is performed, resulting in a well-constrained combination of values providing a good description of the broad-band behaviour of 1ES 2322-409.

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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland.;Natl Acad Sci Republ Armenia, 24 Marshall Baghramian Ave, Yerevan 0019, Armenia..
    Benkhali, F. Ait
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Aix Marseille Univ, CNRS, IN2P3, CPPM, F-13009 Marseille, France..
    Arakawa, M.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
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    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.;Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
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    Ruhr Univ Bochum, Lehrstuhl Weltraum & Astrophys 4, Inst Theoret Phys, D-44780 Bochum, Germany..
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    DESY, D-15738 Zeuthen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
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    Univ Paris Diderot, Sorbonne Univ, LPNHE, CNRS,IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France..
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    DESY, D-15738 Zeuthen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland..
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    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
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    Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICC UB, Marti Franques 1, E-08028 Barcelona, Spain.;Univ Paris Diderot, Sorbonne Univ, LPNHE, CNRS,IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
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    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
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    Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France..
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    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
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    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
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    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Drury, L. O 'C.
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    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
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    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
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    Univ Paris Diderot, Sorbonne Univ, LPNHE, CNRS,IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    DESY, D-15738 Zeuthen, Germany..
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    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
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    DESY, D-15738 Zeuthen, Germany..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    DESY, D-15738 Zeuthen, Germany..
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    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
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    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.;Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
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    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
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    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
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    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
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    Univ Paris Diderot, Sorbonne Univ, LPNHE, CNRS,IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France..
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    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
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    Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Ctr Astron, Grudziadzka 5, PL-87100 Torun, Poland..
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    Univ Tokyo, UTIAS, Kavli Inst Phys & Math Universe Kavli IPMU, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
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    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    DESY, D-15738 Zeuthen, Germany..
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    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
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    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Kraus, M.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Lamanna, G.
    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
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    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
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    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
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    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
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    Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France..
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    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
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    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    DESY, D-15738 Zeuthen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
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    Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa..
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    Univ Zurich, Inst Phys, Winterthurerstr 190, CH-8057 Zurich, Switzerland.;Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
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    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
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    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
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    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    DESY, D-15738 Zeuthen, Germany..
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    RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan..
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    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
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    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
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    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
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    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
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    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
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    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
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    Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan..
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    DESY, D-15738 Zeuthen, Germany..
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    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
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    DESY, D-15738 Zeuthen, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
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    Univ Paris Diderot, Sorbonne Univ, LPNHE, CNRS,IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France..
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    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
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    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
    Pita, S.
    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Poireau, V.
    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
    Noel, A. Priyana
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Prokhorov, D. A.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Prokoph, H.
    DESY, D-15738 Zeuthen, Germany..
    Puehlhofer, G.
    Punch, Michael
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering. Univ Paris Diderot, France.
    Quirrenbach, A.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Raab, S.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Rauth, R.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Reimer, A.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Reimer, O.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Renaud, M.
    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Rieger, F.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Rinchiuso, L.
    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Romoli, C.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Rowell, G.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Rudak, B.
    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Ruiz-Velasco, E.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Sahakian, V.
    Natl Acad Sci Republ Armenia, 24 Marshall Baghramian Ave, Yerevan 0019, Armenia.;Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia..
    Saito, S.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
    Sanchez, D. A.
    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
    Santangelo, A.
    Sasaki, M.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Schlickeiser, R.
    Ruhr Univ Bochum, Lehrstuhl Weltraum & Astrophys 4, Inst Theoret Phys, D-44780 Bochum, Germany..
    Schussler, F.
    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Schulz, A.
    DESY, D-15738 Zeuthen, Germany..
    Schutte, H.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Schwanke, U.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Schwemmer, S.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Seglar-Arroyo, M.
    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Senniappan, Mohanraj
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Seyffert, A. S.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Shafi, N.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Shilon, I.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Shiningayamwe, K.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
    Simoni, R.
    Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Sinha, A.
    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Sol, H.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Specovius, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Spir-Jacob, M.
    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Stawarz, L.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Steenkamp, R.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
    Stegmann, C.
    DESY, D-15738 Zeuthen, Germany.;Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Steppa, C.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Takahashi, T.
    Univ Tokyo, UTIAS, Kavli Inst Phys & Math Universe Kavli IPMU, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan..
    Tavernet, J. -P
    Tavernier, T.
    Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France..
    Taylor, A. M.
    DESY, D-15738 Zeuthen, Germany..
    Terrier, R.
    Univ Paris Diderot, APC AstroParticule & Cosmol, Observ Paris, CNRS,IN2P3,CEA Irfu,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Tiziani, D.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Tluczykont, M.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Trichard, C.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Tsirou, M.
    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Tsuji, N.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
    Tuffs, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Uchiyama, Y.
    Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan..
    van der Walt, D. J.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Eldik, C.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    van Rensburg, C.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Soelen, B.
    Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa..
    Vasileiadis, G.
    Univ Montpellier, Lab Univers & Particules Montpellier, CC 72, CNRS,IN2P3, Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Veh, J.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Venter, C.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Vincent, P.
    Univ Paris Diderot, Sorbonne Univ, LPNHE, CNRS,IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France..
    Vink, J.
    Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Voisin, F.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia..
    Voelk, H. J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vuillaume, T.
    Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France..
    Wadiasingh, Z.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Wagner, S. J.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Wagner, R. M.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden..
    White, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Wierzcholska, A.
    Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Yang, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Yoneda, H.
    Univ Tokyo, UTIAS, Kavli Inst Phys & Math Universe Kavli IPMU, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan..
    Zaborov, D.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Zacharias, M.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Zanin, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zdziarski, A. A.
    Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Zech, A.
    Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Ziegler, A.
    Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Zorn, J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zywucka, N.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    HESS observations of the flaring gravitationally lensed galaxy PKS 1830-2112019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 486, no 3, p. 3886-3891Article in journal (Refereed)
    Abstract [en]

    PKS 1830-211 is a known macrolensed quasar located at a redshift of z = 2.5. Its highenergy gamma-ray emission has been detected with the Fermi-Large Area Telescope (LAT) instrument and evidence for lensing was obtained by several authors from its high-energy data. Observations of PKS 1830-211 were taken with the High Energy Stereoscopic System (H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014 August, following a flare alert by the Fermi-LAT Collaboration. The H.E.S.S observations were aimed at detecting a gamma-ray flare delayed by 20-27 d from the alert flare, as expected from observations at other wavelengths. More than 12 h of good-quality data were taken with an analysis threshold of similar to 67 GeV. The significance of a potential signal is computed as a function of the date and the average significance over the whole period. Data are compared to simultaneous observations by Fermi-LAT. No photon excess or significant signal is detected. An upper limit on PKS 1830-211 flux above 67 GeV is computed and compared to the extrapolation of the Fermi-LAT flare spectrum.

  • 6. Abolmasov, Pavel
    et al.
    Poutanen, Juri
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Gamma-ray opacity of the anisotropic stratified broad-line regions in blazars2017In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 464, no 1, p. 152-169Article in journal (Refereed)
    Abstract [en]

    The GeV-range spectra of blazars are shaped not only by non-thermal emission processes internal to the relativistic jet but also by external pair-production absorption on the thermal emission of the accretion disc and the broad-line region (BLR). For the first time, we compute here the pair-production opacities in the GeV range produced by a realistic BLR accounting for the radial stratification and radiation anisotropy. Using photoionization modelling with the CLOUDY code, we calculate a series of BLR models of different sizes, geometries, cloud densities, column densities and metallicities. The strongest emission features in the model BLR are Ly alpha and He II Ly alpha. Contribution of recombination continua is smaller, especially for hydrogen, because Ly continuum is efficiently trapped inside the large optical depth BLR clouds and converted to Lyman emission lines and higher order recombination continua. The largest effects on the gamma-ray opacity are produced by the BLR geometry and localization of the gamma-ray source. We show that when the gamma-ray source moves further from the central source, all the absorption details move to higher energies and the overall level of absorption drops because of decreasing incidence angles between the gamma-rays and BLR photons. The observed positions of the spectral breaks can be used to measure the geometry and the location of the gamma-ray emitting region relative to the BLR. Strong dependence on geometry means that the soft photons dominating the pair-production opacity may be actually produced by a different population of BLR clouds than the bulk of the observed broad line emission.

  • 7. Abolmasov, Pavel
    et al.
    Poutanen, Juri
    Stockholm University, Nordic Institute for Theoretical Physics (Nordita). University of Turku, Finland.
    Gamma-ray opacity of the anisotropic stratified broad-line regions in blazars2017In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 464, no 1, p. 152-169Article in journal (Refereed)
    Abstract [en]

    The GeV-range spectra of blazars are shaped not only by non-thermal emission processes internal to the relativistic jet but also by external pair-production absorption on the thermal emission of the accretion disc and the broad-line region (BLR). For the first time, we compute here the pair-production opacities in the GeV range produced by a realistic BLR accounting for the radial stratification and radiation anisotropy. Using photoionization modelling with the CLOUDY code, we calculate a series of BLR models of different sizes, geometries, cloud densities, column densities and metallicities. The strongest emission features in the model BLR are Ly alpha and He II Ly alpha. Contribution of recombination continua is smaller, especially for hydrogen, because Ly continuum is efficiently trapped inside the large optical depth BLR clouds and converted to Lyman emission lines and higher order recombination continua. The largest effects on the gamma-ray opacity are produced by the BLR geometry and localization of the gamma-ray source. We show that when the gamma-ray source moves further from the central source, all the absorption details move to higher energies and the overall level of absorption drops because of decreasing incidence angles between the gamma-rays and BLR photons. The observed positions of the spectral breaks can be used to measure the geometry and the location of the gamma-ray emitting region relative to the BLR. Strong dependence on geometry means that the soft photons dominating the pair-production opacity may be actually produced by a different population of BLR clouds than the bulk of the observed broad line emission.

  • 8. Abramowski, A.
    et al.
    Acero, F.
    Aharonian, F.
    Akhperjanian, A. G.
    Anguener, E.
    Anton, G.
    Balenderan, S.
    Balzer, A.
    Barnacka, A.
    Becherini, Y.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Couturier, C.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, Hugh J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, Christian
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Gast, H.
    Giebels, B.
    Glicenstein, J. F.
    Goering, D.
    Grondin, M-H
    Grudzinska, M.
    Haeffner, S.
    Hague, J. D.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemoine-Goumard, M.
    Lenain, J-P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C-C
    Marandon, V.
    Marcowith, A.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Medina, M. C.
    Mehault, J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Nedbal, D.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P-O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spiess, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J-P
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H-S
    Perkins, J. S.
    Ojha, R.
    Stevens, J.
    Edwards, P. G.
    Kadler, M.
    HESS and Fermi-LAT discovery of gamma-rays from the blazar 1ES 1312-4232013In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 434, no 3, p. 1889-1901Article in journal (Refereed)
    Abstract [en]

    A deep observation campaign carried out by the High Energy Stereoscopic System (HESS) on Centaurus A enabled the discovery of gamma-rays from the blazar 1ES 1312-423, 2 degrees away from the radio galaxy. With a differential flux at 1 TeV of phi(1 TeV) = (1.9 +/- 0.6(stat) +/- 0.4(sys)) x 10(-13) cm(-2) s(-1) TeV-1 corresponding to 0.5 per cent of the Crab nebula differential flux and a spectral index Gamma = 2.9 +/- 0.5(stat) +/- 0.2(sys), 1ES 1312-423 is one of the faintest sources ever detected in the very high energy (E > 100 GeV) extragalactic sky. A careful analysis using three and a half years of Fermi Large Area Telescope (Fermi-LAT) data allows the discovery at high energies (E > 100 MeV) of a hard spectrum (Gamma = 1.4 +/- 0.4(stat) +/- 0.2(sys)) source coincident with 1ES 1312-423. Radio, optical, UV and X-ray observations complete the spectral energy distribution of this blazar, now covering 16 decades in energy. The emission is successfully fitted with a synchrotron self-Compton model for the non-thermal component, combined with a blackbody spectrum for the optical emission from the host galaxy.

  • 9. Abramowski, A.
    et al.
    Acero, F.
    Aharonian, F.
    Akhperjanian, A. G.
    Anguener, E.
    Anton, G.
    Balenderan, S.
    Balzer, A.
    Barnacka, A.
    Becherini, Yvonne
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Gast, H.
    Giebels, B.
    Glicenstein, J. F.
    Goering, D.
    Grondin, M-H
    Grudzinska, M.
    Haeffner, S.
    Hague, J. D.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemoine-Goumard, M.
    Lenain, J-P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C-C
    Marandon, V.
    Marcowith, A.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Medina, M. C.
    Mehault, J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Nedbal, D.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P-O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spiess, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J-P
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H-S
    Perkins, J. S.
    Ojha, R.
    Stevens, J.
    Edwards, P. G.
    Kadler, M.
    HESS and Fermi-LAT discovery of gamma-rays from the blazar 1ES 1312-4232013In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 434, no 3, p. 1889-1901Article in journal (Refereed)
    Abstract [en]

    A deep observation campaign carried out by the High Energy Stereoscopic System (HESS) on Centaurus A enabled the discovery of gamma-rays from the blazar 1ES 1312-423, 2 degrees away from the radio galaxy. With a differential flux at 1 TeV of phi(1 TeV) = (1.9 +/- 0.6(stat) +/- 0.4(sys)) x 10(-13) cm(-2) s(-1) TeV-1 corresponding to 0.5 per cent of the Crab nebula differential flux and a spectral index Gamma = 2.9 +/- 0.5(stat) +/- 0.2(sys), 1ES 1312-423 is one of the faintest sources ever detected in the very high energy (E > 100 GeV) extragalactic sky. A careful analysis using three and a half years of Fermi Large Area Telescope (Fermi-LAT) data allows the discovery at high energies (E > 100 MeV) of a hard spectrum (Gamma = 1.4 +/- 0.4(stat) +/- 0.2(sys)) source coincident with 1ES 1312-423. Radio, optical, UV and X-ray observations complete the spectral energy distribution of this blazar, now covering 16 decades in energy. The emission is successfully fitted with a synchrotron self-Compton model for the non-thermal component, combined with a blackbody spectrum for the optical emission from the host galaxy.

  • 10. Abramowski, A.
    et al.
    Acero, F.
    Aharonian, F.
    Akhperjanian, A. G.
    Anton, G.
    Balzer, A.
    Barnacka, A.
    Becherini, Y.
    Becker, J.
    Bernloehr, K.
    Birsin, E.
    Biteau, J.
    Bochow, A.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Buesching, I.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Charbonnier, A.
    Chaves, R. C. G.
    Cheesebrough, A.
    Cologna, G.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    Dickinson, Hugh J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Fallon, L.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gallant, Y. A.
    Garrigoux, T.
    Gast, H.
    Gerard, L.
    Giebels, B.
    Glicenstein, J. F.
    Glueck, B.
    Goering, D.
    Grondin, M. -H
    Haeffner, S.
    Hague, J. D.
    Hahn, J.
    Hampf, D.
    Harris, J.
    Hauser, M.
    Heinz, S.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Komin, Nu.
    Kosack, K.
    Kossakowski, R.
    Krayzel, F.
    Laffon, H.
    Lamanna, G.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Masbou, J.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Medina, M. C.
    Mehault, J.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Naumann, C. L.
    Naumann-Godo, M.
    de Naurois, M.
    Nedbal, D.
    Nekrassov, D.
    Nguyen, N.
    Nicholas, B.
    Niemiec, J.
    Nolan, S. J.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Ripken, Joachim
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Rob, L.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sheidaei, F.
    Skilton, J. L.
    Sol, H.
    Spengler, G.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Terrier, R.
    Tluczykont, M.
    Valerius, K.
    van Eldik, C.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorobiov, S.
    Vorster, M.
    Wagner, S. J.
    Ward, M.
    White, R.
    Wierzcholska, A.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Montmerle, T.
    HESS observations of the Carina nebula and its enigmatic colliding wind binary Eta Carinae2012In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 424, no 1, p. 128-135Article in journal (Refereed)
    Abstract [en]

    The massive binary system Eta Carinae and the surrounding H ii complex, the Carina nebula, are potential particle acceleration sites from which very high energy (VHE; E= 100 GeV) ?-ray emission could be expected. This paper presents data collected during VHE ?-ray observations with the HESS telescope array from 2004 to 2010, which cover a full orbit of Eta Carinae. In the 33.1-h data set no hint of significant ?-ray emission from Eta Carinae has been found and an upper limit on the ?-ray flux of (99 per cent confidence level) is derived above the energy threshold of 470 GeV. Together with the detection of high energy (HE; 0.1 =E= 100 GeV) ?-ray emission by the Fermi Large Area Telescope 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 ?-ray spectrum between the HE and VHE ?-ray range. This could be caused either by a cut-off in the accelerated particle distribution or by severe ?? absorption losses in the wind collision region. Furthermore, the search for extended ?-ray emission from the Carina nebula resulted in an upper limit on the ?-ray flux of (99 per cent 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 W28.

  • 11. Abramowski, A.
    et al.
    Acero, F.
    Aharonian, F.
    Akhperjanian, A. G.
    Anton, G.
    Balzer, A.
    Barnacka, A.
    Becherini, Yvonne
    Becker, J.
    Bernloehr, K.
    Birsin, E.
    Biteau, J.
    Bochow, A.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Buesching, I.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Charbonnier, A.
    Chaves, R. C. G.
    Cheesebrough, A.
    Cologna, G.
    Conrad, J.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Fallon, L.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gallant, Y. A.
    Garrigoux, T.
    Gast, H.
    Gerard, L.
    Giebels, B.
    Glicenstein, J. F.
    Glueck, B.
    Goering, D.
    Grondin, M. -H
    Haeffner, S.
    Hague, J. D.
    Hahn, J.
    Hampf, D.
    Harris, J.
    Hauser, M.
    Heinz, S.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Komin, Nu.
    Kosack, K.
    Kossakowski, R.
    Krayzel, F.
    Laffon, H.
    Lamanna, G.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Masbou, J.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Medina, M. C.
    Mehault, J.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Naumann, C. L.
    Naumann-Godo, M.
    de Naurois, M.
    Nedbal, D.
    Nekrassov, D.
    Nguyen, N.
    Nicholas, B.
    Niemiec, J.
    Nolan, S. J.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Ripken, J.
    Rob, L.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sheidaei, F.
    Skilton, J. L.
    Sol, H.
    Spengler, G.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Terrier, R.
    Tluczykont, M.
    Valerius, K.
    van Eldik, C.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorobiov, S.
    Vorster, M.
    Wagner, S. J.
    Ward, M.
    White, R.
    Wierzcholska, A.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Montmerle, T.
    HESS observations of the Carina nebula and its enigmatic colliding wind binary Eta Carinae2012In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 424, no 1, p. 128-135Article in journal (Refereed)
    Abstract [en]

    The massive binary system Eta Carinae and the surrounding H ii complex, the Carina nebula, are potential particle acceleration sites from which very high energy (VHE; E= 100 GeV) ?-ray emission could be expected. This paper presents data collected during VHE ?-ray observations with the HESS telescope array from 2004 to 2010, which cover a full orbit of Eta Carinae. In the 33.1-h data set no hint of significant ?-ray emission from Eta Carinae has been found and an upper limit on the ?-ray flux of (99 per cent confidence level) is derived above the energy threshold of 470 GeV. Together with the detection of high energy (HE; 0.1 =E= 100 GeV) ?-ray emission by the Fermi Large Area Telescope 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 ?-ray spectrum between the HE and VHE ?-ray range. This could be caused either by a cut-off in the accelerated particle distribution or by severe ?? absorption losses in the wind collision region. Furthermore, the search for extended ?-ray emission from the Carina nebula resulted in an upper limit on the ?-ray flux of (99 per cent 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 W28.

  • 12. Abramowski, A.
    et al.
    Acero, F.
    Aharonian, F.
    Benkhali, F. Ait
    Akhperjanian, A. G.
    Anguner, E.
    Anton, G.
    Balenderan, S.
    Balzer, A.
    Barnacka, A.
    Becherini, Y.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Clapson, A. -C
    Colafrancesco, S.
    Cologna, G.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, Christian
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, Manuel
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.22015In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 446, no 2, p. 1163-1169Article in journal (Refereed)
    Abstract [en]

    The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the HESS Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position RA = 18(h)32(m)50(s) +/- 3(stat)(s) +/- 2(syst)(s), Dec = -9 degrees 22'36 '' +/- 32(stat)'' +/- 20(syst)'' (J2000), spatially coincident with a part of the radio shell of the neighbouring remnant G22.7-0.2. The photon spectrum is well described by a power law of index Gamma = 2.6 +/- 0.3(stat) +/- 0.1(syst) and a normalization at 1 TeV of Phi(0) = (4.8 +/- 0.8(stat) +/- 1.0(syst)) x 10(-13) cm(-2) s(-1) TeV-1. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multiwavelength observations will help to shed new light on this intriguing VHE source.

  • 13.
    Abramowski, A.
    et al.
    Univ Hamburg, Germany.
    Acero, F.
    Univ Paris Diderot, France.
    Aharonian, F.
    Max Planck Inst Kernphys, Germany ; Dublin Inst Adv Studies, Ireland ; Natl Acad Sci Republ Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Inst Kernphys, Germany.
    Akhperjanian, A. G.
    Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia.
    Anguner, E.
    Humboldt Univ, Germany.
    Anton, G.
    Univ Erlangen Nurnberg, Germany.
    Balenderan, S.
    Univ Durham, UK.
    Balzer, A.
    DESY, Germany ; Univ Potsdam, Germany.
    Barnacka, A.
    Nicolaus Copernicus Astron Ctr, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Clapson, A. -C
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.22015In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 446, no 2, p. 1163-1169Article in journal (Refereed)
    Abstract [en]

    The region around the supernova remnant (SNR) W41 contains several TeV sources and has prompted the HESS Collaboration to perform deep observations of this field of view. This resulted in the discovery of the new very high energy (VHE) source HESS J1832-093, at the position RA = 18(h)32(m)50(s) +/- 3(stat)(s) +/- 2(syst)(s), Dec = -9 degrees 22'36 '' +/- 32(stat)'' +/- 20(syst)'' (J2000), spatially coincident with a part of the radio shell of the neighbouring remnant G22.7-0.2. The photon spectrum is well described by a power law of index Gamma = 2.6 +/- 0.3(stat) +/- 0.1(syst) and a normalization at 1 TeV of Phi(0) = (4.8 +/- 0.8(stat) +/- 1.0(syst)) x 10(-13) cm(-2) s(-1) TeV-1. The location of the gamma-ray emission on the edge of the SNR rim first suggested a signature of escaping cosmic rays illuminating a nearby molecular cloud. Then a dedicated XMM-Newton observation led to the discovery of a new X-ray point source spatially coincident with the TeV excess. Two other scenarios were hence proposed to identify the nature of HESS J1832-093. Gamma-rays from inverse Compton radiation in the framework of a pulsar wind nebula scenario or the possibility of gamma-ray production within a binary system are therefore also considered. Deeper multiwavelength observations will help to shed new light on this intriguing VHE source.

  • 14. Abramowski, A.
    et al.
    Aharonian, F.
    Benkhali, F. Ait
    Akhperjanian, A. G.
    Anguener, E.
    Anton, G.
    Balenderan, S.
    Balzer, A.
    Barnacka, A.
    Becherini, Y.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, Hugh J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O ' C
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, Christian
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Stockholm University, Faculty of Science, Department of Physics.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    TeV gamma-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with HESS2014In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 441, no 1, p. 790-799Article in journal (Refereed)
    Abstract [en]

    The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E > 0.1 TeV) gamma-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a unique opportunity to study the earliest stages of SNR evolution in the VHE domain. The purpose of this work is to probe the level of VHE gamma-ray emission from both SNRs and use this to constrain their physical properties. Observations were conducted with the H. E. S. S. (High Energy Stereoscopic System) Cherenkov Telescope Array over a more than six-year period spanning 2004-2010. The obtained data have effective livetimes of 67 h for G1.9+0.3 and 16 h for G330.2+1.0. The data are analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant gamma-ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Gamma = 2.5 were set at 5.6 x 10(-1)3 cm(-2) s(-1) above 0.26 TeV and 3.2 x 10(-12) cm(-2) s(-1) above 0.38 TeV, respectively. In a one-zone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to B-G1.9 greater than or similar to 12 mu G for G1.9+0.3 and to B-G330 greater than or similar to 8 mu G for G330.2+1.0. In a hadronic scenario, the low ambient densities and the large distances to the SNRs result in very low predicted fluxes, for which the H.E.S.S. upper limits are not constraining.

  • 15. Abramowski, A.
    et al.
    Aharonian, F.
    Benkhali, F. Ait
    Akhperjanian, A. G.
    Anguener, E.
    Anton, G.
    Balenderan, S.
    Balzer, A.
    Barnacka, A.
    Becherini, Y.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, Hugh J.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Djannati-Ataie, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, Christian
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, Manuel
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    HESS J1640-465-an exceptionally luminous TeV gamma-ray supernova remnant2014In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 439, no 3, p. 2828-2836Article in journal (Refereed)
    Abstract [en]

    The results of follow-up observations of the TeV gamma-ray source HESS J1640-465 from 2004 to 2011 with the High Energy Stereoscopic System (HESS) are reported in this work. The spectrum is well described by an exponential cut-off power law with photon index Gamma = 2.11 +/- 0.09(stat) +/- 0.10(sys), and a cut-off energy of E-2 = 6.0(-1.2)(+2.0) TeV. The TeV emission is significantly extended and overlaps with the northwestern part of the shell of the SNR G338.3-0.0. The new HESS results, a re-analysis of archival XMM-Newton data and multiwavelength observations suggest that a significant part of the gamma-ray emission from HESS J1640-465 originates in the supernova remnant shell. In a hadronic scenario, as suggested by the smooth connection of the GeV and TeV spectra, the product of total proton energy and mean target density could be as high as W(p)n(H) similar to 4 x 10(52)(d/10kpc)(2) erg cm(-3).

  • 16. Abramowski, A.
    et al.
    Aharonian, F.
    Benkhali, F. Ait
    Akhperjanian, A. G.
    Anguener, E.
    Anton, G.
    Balenderan, S.
    Balzer, A.
    Barnacka, A.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O ' C
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    TeV gamma-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with HESS2014In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 441, no 1, p. 790-799Article in journal (Refereed)
    Abstract [en]

    The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E > 0.1 TeV) gamma-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a unique opportunity to study the earliest stages of SNR evolution in the VHE domain. The purpose of this work is to probe the level of VHE gamma-ray emission from both SNRs and use this to constrain their physical properties. Observations were conducted with the H. E. S. S. (High Energy Stereoscopic System) Cherenkov Telescope Array over a more than six-year period spanning 2004-2010. The obtained data have effective livetimes of 67 h for G1.9+0.3 and 16 h for G330.2+1.0. The data are analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant gamma-ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Gamma = 2.5 were set at 5.6 x 10(-1)3 cm(-2) s(-1) above 0.26 TeV and 3.2 x 10(-12) cm(-2) s(-1) above 0.38 TeV, respectively. In a one-zone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to B-G1.9 greater than or similar to 12 mu G for G1.9+0.3 and to B-G330 greater than or similar to 8 mu G for G330.2+1.0. In a hadronic scenario, the low ambient densities and the large distances to the SNRs result in very low predicted fluxes, for which the H.E.S.S. upper limits are not constraining.

  • 17.
    Abramowski, A.
    et al.
    University of Hamburg, Germany.
    Aharonian, F.
    Max Planck Institute for Nuclear Physics, Germany ; Dublin Institute for Advanced Studies, Ireland ; National Academy of Sciences of the Republic of Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Institute for Nuclear Physics, Germany.
    Akhperjanian, A. G.
    National Academy of Sciences of the Republic of Armenia, Armenia ; Yerevan Physics Institute, Armenia.
    Angüner, E.
    Humboldt-Universität zu Berlin, Germany.
    Anton, G.
    Friedrich-Alexander-Universität Erlangen-Nürnberg, Germany.
    Balenderan, S.
    University of Durham, UK.
    Balzer, A.
    DESY, Germany ; University of Potsdam, Germany.
    Barnacka, A.
    Nicolaus Copernicus Astronomical Center, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Djannati-Ataie, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Université Paris Diderot, France.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    HESS J1640-465-an exceptionally luminous TeV gamma-ray supernova remnant2014In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 439, no 3, p. 2828-2836Article in journal (Refereed)
    Abstract [en]

    The results of follow-up observations of the TeV gamma-ray source HESS J1640-465 from 2004 to 2011 with the High Energy Stereoscopic System (HESS) are reported in this work. The spectrum is well described by an exponential cut-off power law with photon index Gamma = 2.11 +/- 0.09(stat) +/- 0.10(sys), and a cut-off energy of E-2 = 6.0(-1.2)(+2.0) TeV. The TeV emission is significantly extended and overlaps with the northwestern part of the shell of the SNR G338.3-0.0. The new HESS results, a re-analysis of archival XMM-Newton data and multiwavelength observations suggest that a significant part of the gamma-ray emission from HESS J1640-465 originates in the supernova remnant shell. In a hadronic scenario, as suggested by the smooth connection of the GeV and TeV spectra, the product of total proton energy and mean target density could be as high as W(p)n(H) similar to 4 x 10(52)(d/10kpc)(2) erg cm(-3).

  • 18. Acero, F.
    et al.
    Aharonian, F.
    Akhperjanian, A. G.
    Anton, G.
    de Almeida, U. Barres
    Bazer-Bachi, A. R.
    Becherini, Y.
    Behera, B.
    Bernloehr, K.
    Bochow, A.
    Boisson, C.
    Bolmont, J.
    Borrel, V.
    Braun, I.
    Brucker, J.
    Brun, F.
    Brun, P.
    Buehler, R.
    Bulik, T.
    Buesching, I.
    Boutelier, T.
    Chadwick, P. M.
    Charbonnier, A.
    Chaves, R. C. G.
    Cheesebrough, A.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Chounet, L. -M
    Clapson, A. C.
    Coignet, G.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubois, F.
    Dubus, G.
    Dyks, J.
    Dyrda, M.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Fallon, L.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fiasson, A.
    Foerster, A.
    Fontaine, G.
    Fuessling, M.
    Gabici, S.
    Gallant, Y. A.
    Gerard, L.
    Gerbig, D.
    Giebels, B.
    Glicenstein, J. F.
    Glueck, B.
    Goret, P.
    Goering, D.
    Hauser, M.
    Heinz, S.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hinton, J. A.
    Hoffmann, A.
    Hofmann, W.
    Hofverberg, P.
    Holleran, M.
    Hoppe, S.
    Horns, D.
    Jacholkowska, A.
    de Jager, O. C.
    Jahn, C.
    Jung, I.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Kerschhaggl, M.
    Khangulyan, D.
    Khelifi, B.
    Keogh, D.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Komin, Nu.
    Kosack, K.
    Kossakowski, R.
    Lamanna, G.
    Lenain, J. -P
    Lohse, T.
    Marandon, V.
    Martineau-Huynh, O.
    Marcowith, A.
    Masbou, J.
    Maurin, D.
    McComb, T. J. L.
    Medina, M. C.
    Mehault, J.
    Moderski, R.
    Moulin, E.
    Naumann-Godo, M.
    de Naurois, M.
    Nedbal, D.
    Nekrassov, D.
    Nicholas, B.
    Niemiec, J.
    Nolan, S. J.
    Ohm, S.
    Olive, J-F
    Wilhelmi, E. de Ona
    Orford, K. J.
    Ostrowski, M.
    Panter, M.
    Arribas, M. Paz
    Pedaletti, G.
    Pelletier, G.
    Petrucci, P. -O
    Pita, S.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raubenheimer, B. C.
    Raue, M.
    Rayner, S. M.
    Reimer, O.
    Renaud, M.
    Rieger, F.
    Ripken, Joachim
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Rob, L.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Ruppel, J.
    Ryde, F.
    Sahakian, V.
    Santangelo, A.
    Schlickeiser, R.
    Schoeck, F. M.
    Schoenwald, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Shalchi, A.
    Sikora, M.
    Skilton, J. L.
    Sol, H.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Superina, G.
    Sushch, I.
    Szostek, A.
    Tam, P. H.
    Tavernet, J. -P
    Terrier, R.
    Tibolla, O.
    Tluczykont, M.
    van Eldik, C.
    Vasileiadis, G.
    Venter, C.
    Venter, L.
    Vialle, J. P.
    Vincent, P.
    Vivier, M.
    Voelk, H. J.
    Volpe, F.
    Wagner, S. J.
    Ward, M.
    Zdziarski, A. A.
    Zech, A.
    Localizing the VHE gamma-ray source at the Galactic Centre2010In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 402, no 3, p. 1877-1882Article in journal (Refereed)
    Abstract [en]

    The inner 10 pc of our Galaxy contains many counterpart candidates of the very high energy (VHE; > 100 GeV) gamma-ray point source HESS J1745-290. Within the point spread function of the H.E.S.S. measurement, at least three objects are capable of accelerating particles to VHE and beyond and of providing the observed gamma-ray flux. Previous attempts to address this source confusion were hampered by the fact that the projected distances between these objects were of the order of the error circle radius of the emission centroid (34 arcsec, dominated by the pointing uncertainty of the H.E.S.S. instrument). Here we present H.E.S.S. data of the Galactic Centre region, recorded with an improved control of the instrument pointing compared to H.E.S.S. standard pointing procedures. Stars observed during gamma-ray observations by optical guiding cameras mounted on each H.E.S.S. telescope are used for off-line pointing calibration, thereby decreasing the systematic pointing uncertainties from 20 to 6 arcsec per axis. The position of HESS J1745-290 is obtained by fitting a multi-Gaussian profile to the background-subtracted gamma-ray count map. A spatial comparison of the best-fitting position of HESS J1745-290 with the position and morphology of candidate counterparts is performed. The position is, within a total error circle radius of 13 arcsec, coincident with the position of the supermassive black hole Sgr A* and the recently discovered pulsar wind nebula candidate G359.95-0.04. It is significantly displaced from the centroid of the supernova remnant Sgr A East, excluding this object with high probability as the dominant source of the VHE gamma-ray emission.

  • 19. Acero, F.
    et al.
    Aharonian, F.
    Akhperjanian, A. G.
    Anton, G.
    de Almeida, U. Barres
    Bazer-Bachi, A. R.
    Becherini, Yvonne
    Behera, B.
    Bernloehr, K.
    Bochow, A.
    Boisson, C.
    Bolmont, J.
    Borrel, V.
    Braun, I.
    Brucker, J.
    Brun, F.
    Brun, P.
    Buehler, R.
    Bulik, T.
    Buesching, I.
    Boutelier, T.
    Chadwick, P. M.
    Charbonnier, A.
    Chaves, R. C. G.
    Cheesebrough, A.
    Conrad, J.
    Chounet, L. -M
    Clapson, A. C.
    Coignet, G.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubois, F.
    Dubus, G.
    Dyks, J.
    Dyrda, M.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Fallon, L.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fiasson, A.
    Foerster, A.
    Fontaine, G.
    Fuessling, M.
    Gabici, S.
    Gallant, Y. A.
    Gerard, L.
    Gerbig, D.
    Giebels, B.
    Glicenstein, J. F.
    Glueck, B.
    Goret, P.
    Goering, D.
    Hauser, M.
    Heinz, S.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hinton, J. A.
    Hoffmann, A.
    Hofmann, W.
    Hofverberg, P.
    Holleran, M.
    Hoppe, S.
    Horns, D.
    Jacholkowska, A.
    de Jager, O. C.
    Jahn, C.
    Jung, I.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Kerschhaggl, M.
    Khangulyan, D.
    Khelifi, B.
    Keogh, D.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Komin, Nu.
    Kosack, K.
    Kossakowski, R.
    Lamanna, G.
    Lenain, J. -P
    Lohse, T.
    Marandon, V.
    Martineau-Huynh, O.
    Marcowith, A.
    Masbou, J.
    Maurin, D.
    McComb, T. J. L.
    Medina, M. C.
    Mehault, J.
    Moderski, R.
    Moulin, E.
    Naumann-Godo, M.
    de Naurois, M.
    Nedbal, D.
    Nekrassov, D.
    Nicholas, B.
    Niemiec, J.
    Nolan, S. J.
    Ohm, S.
    Olive, J-F
    Wilhelmi, E. de Ona
    Orford, K. J.
    Ostrowski, M.
    Panter, M.
    Arribas, M. Paz
    Pedaletti, G.
    Pelletier, G.
    Petrucci, P. -O
    Pita, S.
    Puehlhofer, G.
    Punch, M.
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raubenheimer, B. C.
    Raue, M.
    Rayner, S. M.
    Reimer, O.
    Renaud, M.
    Rieger, F.
    Ripken, J.
    Rob, L.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Ruppel, J.
    Ryde, F.
    Sahakian, V.
    Santangelo, A.
    Schlickeiser, R.
    Schoeck, F. M.
    Schoenwald, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Shalchi, A.
    Sikora, M.
    Skilton, J. L.
    Sol, H.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Superina, G.
    Sushch, I.
    Szostek, A.
    Tam, P. H.
    Tavernet, J. -P
    Terrier, R.
    Tibolla, O.
    Tluczykont, M.
    van Eldik, C.
    Vasileiadis, G.
    Venter, C.
    Venter, L.
    Vialle, J. P.
    Vincent, P.
    Vivier, M.
    Voelk, H. J.
    Volpe, F.
    Wagner, S. J.
    Ward, M.
    Zdziarski, A. A.
    Zech, A.
    Localizing the VHE gamma-ray source at the Galactic Centre2010In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 402, no 3, p. 1877-1882Article in journal (Refereed)
    Abstract [en]

    The inner 10 pc of our Galaxy contains many counterpart candidates of the very high energy (VHE; > 100 GeV) gamma-ray point source HESS J1745-290. Within the point spread function of the H.E.S.S. measurement, at least three objects are capable of accelerating particles to VHE and beyond and of providing the observed gamma-ray flux. Previous attempts to address this source confusion were hampered by the fact that the projected distances between these objects were of the order of the error circle radius of the emission centroid (34 arcsec, dominated by the pointing uncertainty of the H.E.S.S. instrument). Here we present H.E.S.S. data of the Galactic Centre region, recorded with an improved control of the instrument pointing compared to H.E.S.S. standard pointing procedures. Stars observed during gamma-ray observations by optical guiding cameras mounted on each H.E.S.S. telescope are used for off-line pointing calibration, thereby decreasing the systematic pointing uncertainties from 20 to 6 arcsec per axis. The position of HESS J1745-290 is obtained by fitting a multi-Gaussian profile to the background-subtracted gamma-ray count map. A spatial comparison of the best-fitting position of HESS J1745-290 with the position and morphology of candidate counterparts is performed. The position is, within a total error circle radius of 13 arcsec, coincident with the position of the supermassive black hole Sgr A* and the recently discovered pulsar wind nebula candidate G359.95-0.04. It is significantly displaced from the centroid of the supernova remnant Sgr A East, excluding this object with high probability as the dominant source of the VHE gamma-ray emission.

  • 20. Acero, F.
    et al.
    Aharonian, F.
    Akhperjanian, A. G.
    Anton, G.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Zdziarski, A. A.
    Zech, A.
    Conrad, Jan
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Localizing the VHE gamma-ray source at the Galactic Centre2010In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 402, no 3, p. 1877-1882Article in journal (Refereed)
    Abstract [en]

    The inner 10 pc of our Galaxy contains many counterpart candidates of the very high energy (VHE; > 100 GeV) gamma-ray point source HESS J1745-290. Within the point spread function of the H.E.S.S. measurement, at least three objects are capable of accelerating particles to VHE and beyond and of providing the observed gamma-ray flux. Previous attempts to address this source confusion were hampered by the fact that the projected distances between these objects were of the order of the error circle radius of the emission centroid (34 arcsec, dominated by the pointing uncertainty of the H.E.S.S. instrument). Here we present H.E.S.S. data of the Galactic Centre region, recorded with an improved control of the instrument pointing compared to H.E.S.S. standard pointing procedures. Stars observed during gamma-ray observations by optical guiding cameras mounted on each H.E.S.S. telescope are used for off-line pointing calibration, thereby decreasing the systematic pointing uncertainties from 20 to 6 arcsec per axis. The position of HESS J1745-290 is obtained by fitting a multi-Gaussian profile to the background-subtracted gamma-ray count map. A spatial comparison of the best-fitting position of HESS J1745-290 with the position and morphology of candidate counterparts is performed. The position is, within a total error circle radius of 13 arcsec, coincident with the position of the supermassive black hole Sgr A* and the recently discovered pulsar wind nebula candidate G359.95-0.04. It is significantly displaced from the centroid of the supernova remnant Sgr A East, excluding this object with high probability as the dominant source of the VHE gamma-ray emission.

  • 21.
    Acuner, Zeynep
    et al.
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden..
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden..
    Yu, Hoi-Fung
    KTH, School of Engineering Sciences (SCI), Physics. AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.;Univ Hong Kong, Fac Sci, Pokfulam, Hong Kong, Peoples R China..
    Non-dissipative photospheres in GRBs: spectral appearance in the Fermi/GBM catalogue2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 487, no 4, p. 5508-5519Article in journal (Refereed)
    Abstract [en]

    A large fraction of gamma-ray burst (GRB) spectra are very hard below the peak. Indeed, the observed distribution of sub-peak power-law indices, alpha, has been used as an argument for a photospheric origin of GRB spectra. Here, we investigate what fraction of GRBs have spectra that are consistent with emission from a photopshere in a non-dissipative outflow. This is the simplest possible photospheric emission scenario. We create synthetic spectra, with a range of peak energies, by folding the theoretical predictions through the detector response of the FERMI/GBM detector. These simulated spectral data are fitted with typically employed empirical models. We find that the low-energy photon indices obtain values ranging -0.4 < alpha < 0.0, peaking at around -0.1, thus covering a non-negligible fraction of observed values. These values are significantly softer than the asymptotic value of the theoretical spectrum of alpha similar to 0.4. The reason for the alpha values to be much softer than expected, is the limitation of the empirical functions to capture the true curvature of the theoretical spectrum. We conclude that more than a quarter of the bursts in the GBM catalogue have at least one time-resolved spectrum, whose alpha values are consistent with spectra from a non-dissipative outflow, releasing its thermal energy at the photosphere. The fraction of spectra consistent with emission from the photosphere will increase even more if dissipation of kinetic energy in the flow occurs below the photosphere.

  • 22. Adamo, A.
    et al.
    Smith, L. J.
    Gallagher, J. S.
    Bastian, N.
    Ryon, J.
    Westmoquette, M. S.
    Konstantopoulos, I. S.
    Zackrisson, Erik
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Larsen, S. S.
    Silva-Villa, E.
    Charlton, J. C.
    Weisz, D. R.
    Revealing a ring-like cluster complex in a tidal tail of the starburst galaxy NGC 21462012In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 426, no 2, p. 1185-1194Article in journal (Refereed)
    Abstract [en]

    We report the discovery of a ring-like cluster complex in the starburst galaxy NGC?2146. The Ruby Ring, so named due to its appearance, shows a clear ring-like distribution of star clusters around a central object. It is located in one of the tidal streams that surround the galaxy. NGC?2146 is part of the Snapshot Hubble U-band Cluster Survey (SHUCS). The WFC3/F336W data have added critical information to the available archival Hubble Space Telescope imaging set of NGC?2146, allowing us to determine ages, masses and extinctions of the clusters in the Ruby Ring. These properties have then been used to investigate the formation of this extraordinary system. We find evidence of a spatial and temporal correlation between the central cluster and the clusters in the ring. The latter are about 4?Myr younger than the central cluster, which has an age of 7?Myr. This result is supported by the Ha emission which is strongly coincident with the ring, and weaker at the position of the central cluster. From the derived total Ha luminosity of the system, we constrain the star formation rate density to be quite high (SSFR = 0.47?M??yr-1?kpc-2). The Ruby Ring is the product of an intense and localized burst of star formation, similar to the extended cluster complexes observed in M?51 and the Antennae, but more impressive because it is quite isolated. The central cluster contains only 5 per cent of the total stellar mass in the clusters that are determined within the complex. The ring-like morphology, the age spread and the mass ratio support a triggering formation scenario for this complex. We discuss the formation of the Ruby Ring in a collect and collapse framework. The predictions made by this model agree quite well with the estimated bubble radius and expansion velocity produced by the feedback from the central cluster, making the Ruby Ring an interesting case of triggered star formation.

  • 23. Adamo, A.
    et al.
    Östlin, G.
    Zackrisson, E.
    Papaderos, P.
    Bergvall, Nils
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
    Rich, R. M.
    Micheva, G.
    Star cluster formation and evolution in Mrk 930: properties of a metal-poor starburst2011In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 415, no 3, p. 2388-2406Article in journal (Refereed)
    Abstract [en]

    We present the analysis of the large population of star clusters in the blue compact galaxy (BCG) Mrk 930. The study has been conducted by means of a photometric analysis of multiband data obtained with the Hubble Space Telescope (HST). We have reconstructed the spectral energy distributions of the star clusters and estimated the age, mass and extinction for a representative sample. Similar to previous studies of star clusters in BCGs, we observe a very young cluster population with 70 per cent of the systems formed less than 10 Myr ago. In Mrk 930, the peak in the star cluster age distribution at 4 Myr is corroborated by the presence of Wolf-Rayet spectral features, and by the observed optical and infrared (IR) line ratios [OIII]/H beta and [Ne III]/[Ne II]. The recovered extinction in these very young clusters shows large variations, with a decrease at older ages. It is likely that our analysis is limited to the optically brightest objects (i.e. systems only partially embedded in their natal cocoons; the deeply embedded clusters being undetected). We map the extinction across the galaxy using low-resolution spectra and the H alpha-to-H beta ratio, as obtained from ground-based narrow band imaging. These results are compared with the extinction distribution recovered from the clusters. We find that the mean optical extinction derived in the starburst regions is close to the averaged value observed in the clusters [more than 80 per cent of the systems have E(B - V) <= 0.2mag], but locally, do not trace the more extinguished clusters. Previous HST studies of BCGs have revealed a population of young and extremely red super star clusters. We detect a considerable fraction of clusters affected by a red excess also in Mrk 930. The nature of the red excess, which turns up at near-IR wavelengths (I band and longwards), remains unknown. We compare the cluster formation history and the star formation history, the latter derived from the fit of spectral population synthesis models to the spectra. We find a general agreement between the two independently estimated quantities. Using the cluster properties, we perform a study of the host environmental properties. We find that the cluster formation efficiency (the fraction of star formation happening in clusters) is significantly higher, suggesting a key role of the environment for the formation of these massive objects.

  • 24.
    Adamo, Angela
    et al.
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Kruijssen, J. M. D.
    Bastian, N.
    Silva-Villa, E.
    Ryon, J.
    Probing the role of the galactic environment in the formation of stellar clusters, using M83 as a test bench2015In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 452, no 1, p. 246-260Article in journal (Refereed)
    Abstract [en]

    We present a study of the M83 cluster population, covering the disc of the galaxy between radii of 0.45 and 4.5 kpc. We aim to probe the properties of the cluster population as a function of distance from the galactic centre. We observe a net decline in cluster formation efficiency (Gamma, i.e. amount of star formation happening in bound clusters) from about 26 per cent in the inner region to 8 per cent in the outer part of the galaxy. The recovered Gamma values within different regions of M83 follow the same Gamma versus star formation rate density relation observed for entire galaxies. We also probe the initial cluster mass function (ICMF) as a function of galactocentric distance. We observe a significant steepening of the ICMF in the outer regions (from -1.90 +/- 0.11 to -2.70 +/- 0.14) and for the whole galactic cluster population (slope of -2.18 +/- 0.07) of M83. We show that this change of slope reflects a more fundamental change of the 'truncation mass' at the high-mass end of the distribution. This can be modelled as a Schechter function of slope -2 with an exponential cutoff mass (M-c) that decreases significantly from the inner to the outer regions (from 4.00 to 0.25 x 10(5) M-circle dot) while the galactic M-c is approximate to 1.60 x 10(5) M-circle dot. The trends in Gamma and ICMF are consistent with the observed radial decrease of the Sigma (H-2), hence in gas pressure. As gas pressure declines, cluster formation becomes less efficient. We conclude that the host galaxy environment appears to regulate (1) the fraction of stars locked in clusters and (2) the upper mass limit of the ICMF, consistently described by a near-universal slope -2 truncated at the high-mass end.

  • 25.
    Adamo, Angela
    et al.
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Östlin, Göran
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Zackrisson, Erik
    Stockholm University, Faculty of Science, Department of Astronomy.
    Probing cluster formation under extreme conditions: massive star clusters in blue compact galaxies2011In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 417, no 3, p. 1904-1912Article in journal (Refereed)
    Abstract [en]

    The numerous and massive young star clusters in blue compact galaxies (BCGs) are used to investigate the properties of their hosts. We test whether BCGs follow claimed relations between cluster populations and their hosts, such as the fraction of the total luminosity contributed by the clusters as function of the mean star formation rate (SFR) density, the V-band luminosity of the brightest youngest cluster as related to the mean host SFR and the cluster formation efficiency (i.e. the fraction of star formation happening in star clusters) versus the density of the SFR. We find that BCGs follow the trends, supporting a scenario where cluster formation and environmental properties of the host are correlated. They occupy, in all the diagrams, the regions of higher SFRs, as expected by the extreme nature of the starbursts operating in these systems. We find that the star clusters contribute almost to the 20 per cent of the UV luminosity of the hosts. We suggest that the BCG starburst environment has most likely favoured the compression and collapse of the giant molecular clouds, enhancing the local star formation efficiency, so that massive clusters have been formed. The estimated cluster formation efficiency supports this scenario. BCGs have a cluster formation efficiency comparable to luminous IR galaxies and spiral starburst nuclei (the averaged value is similar to 35 per cent) which is much higher than the 8-10 per cent reported for quiescent spirals and dwarf star-forming galaxies.

  • 26.
    Adamo, Angela
    et al.
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Östlin, Göran
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Zackrisson, Erik
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Hayes, Matthew
    The Massive Star Clusters in the Dwarf Merger ESO 185-IG13: is the Red Excess Ubiquitous in Starbursts?2011In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 414, no 3, p. 1793-1812Article in journal (Other academic)
    Abstract [en]

    We have investigated the starburst properties of the luminous blue compact galaxy ESO 185-IG13. The galaxy has been imaged with the high resolution cameras onboard to the Hubble Space Telescope. From the UV to the IR, the data reveal a system shaped by hundreds of young star clusters, and fine structures, like a tidal stream and a shell. The presence of numerous clusters and the perturbed morphology indicate that the galaxy has been involved in a recent merger event. Using previous simulations of shell formation in galaxy mergers we constrain potential progenitors of ESO 185-IG13. The analysis of the star cluster population is used to investigate the properties of the present starburst and to date the final merger event, which has produced hundreds of clusters younger than 100 Myr. We have found a peak of cluster formation only 3.5 Myr old. A large fraction of these clusters will not survive after 10-20 Myr, due to the "infant mortality" caused by gas expulsion. However, this sample of clusters represents an unique chance to investigate the youngest phases of cluster evolution. As already observed in the analog blue compact galaxy Haro 11, a fraction of young clusters are affected by a flux excess at wavelengths longer than 8000 \AA. Ages, masses, and extinctions of clusters with this NIR excess are estimated from UV and optical data. We discuss similarities and differences of the observed NIR excess in ESO 185-IG13 clusters with other cases in the literature. The cluster ages and masses are used to distinguish among the potential causes of the excess. We observe, as in Haro 11, that the use of the IR and the (commonly used) I band data results in overestimates of age and mass in clusters affected by the NIR excess. This has important implications for a number of related studies of star clusters.

  • 27.
    Adamo, Angela
    et al.
    Stockholm University, Faculty of Science, Department of Astronomy.
    Östlin, Göran
    Stockholm University, Faculty of Science, Department of Astronomy.
    Zackrisson, Erik
    Stockholm University, Faculty of Science, Department of Astronomy.
    Hayes, Matthew
    Observatoire Astronomique de l'Université de Genève.
    Cumming, Robert
    Stockholm University, Faculty of Science, Department of Astronomy.
    Micheva, Genoveva
    Stockholm University, Faculty of Science, Department of Astronomy.
    Super star clusters in Haro 11: properties of a very young starburst and evidence for a near-infrared flux excess2010In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, MNRAS, Vol. 407, no 2, p. 870-890Article in journal (Refereed)
    Abstract [en]

    We have used multiband imaging to investigate the nature of an extreme starburst environment in the nearby Lyman break galaxy analogue Haro 11 (ESO350-IG038) by means of its stellar cluster population. The central starburst region has been observed in eight different high-resolution Hubble Space Telescope (HST) wavebands, sampling the stellar and gas components from UV to near-infrared. Photometric imaging of the galaxy was also carried out at 2.16μm by NaCo AO instrument at the ESO Very Large Telescope. We constructed integrated spectral energy distributions (SEDs) for about 200 star clusters located in the active star-forming regions and compared them with single stellar population models (suitable for physical properties of very young cluster population) in order to derive ages, masses and extinctions of the star clusters. The cluster age distribution we recover confirms that the present starburst has lasted for 40Myr, and shows a peak of cluster formation only 3.5 Myr old. With such an extremely young cluster population, Haro 11 represents a unique opportunity to investigate the youngest phase of the cluster formation process and evolution in starburst systems. We looked for possible relations between cluster ages, extinctions and masses. Extinction tends to diminish as a function of the cluster age, but the spread is large and reaches the highest dispersion for clusters in partial embedded phases (<5Myr). A fraction of low-mass (below 104 Msolar), very young (1-3Myr) clusters is missing, either because they are embedded in the parental molecular cloud and heavily extinguished, or because of blending with neighbouring clusters. The range of the cluster masses is wide; we observe that more than 30 per cent of the clusters have masses above 105 Msolar, qualifying them as super star clusters. Almost half of the cluster sample is affected by flux excesses at wavelengths >8000Å which cannot be explained by simple stellar evolutionary models. Fitting SED models over all wavebands leads to systematic overestimates of cluster ages and incorrect masses for the stellar population supplying the light in these clusters. We show that the red excess affects also the HST F814W filter, which is typically used to constrain cluster physical properties. The clusters which show the red excess are younger than 40Myr we discuss possible physical explanations for the phenomenon. Finally, we estimate that Haro 11 has produced bound clusters at a rate almost a factor of 10 higher than the massive and regular spirals, like the Milky Way. The present cluster formation efficiency is ~38 per cent of the galactic star formation rate.

  • 28.
    Adamo, Angela
    et al.
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Östlin, Göran
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Zackrisson, Erik
    Stockholm University, Faculty of Science, Department of Astronomy.
    Papaderos, P.
    Bergvall, N.
    Rich, R. M.
    Micheva, Genoveva
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Star cluster formation and evolution in Mrk 930: properties of a metal-poor starburst2011In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 415, no 3, p. 2388-2406Article in journal (Refereed)
    Abstract [en]

    We present the analysis of the large population of star clusters in the blue compact galaxy (BCG) Mrk 930. The study has been conducted by means of a photometric analysis of multiband data obtained with the Hubble Space Telescope (HST). We have reconstructed the spectral energy distributions of the star clusters and estimated the age, mass and extinction for a representative sample. Similar to previous studies of star clusters in BCGs, we observe a very young cluster population with 70 per cent of the systems formed less than 10 Myr ago. In Mrk 930, the peak in the star cluster age distribution at 4 Myr is corroborated by the presence of Wolf-Rayet spectral features, and by the observed optical and infrared (IR) line ratios [OIII]/H beta and [Ne III]/[Ne II]. The recovered extinction in these very young clusters shows large variations, with a decrease at older ages. It is likely that our analysis is limited to the optically brightest objects (i.e. systems only partially embedded in their natal cocoons; the deeply embedded clusters being undetected). We map the extinction across the galaxy using low-resolution spectra and the H alpha-to-H beta ratio, as obtained from ground-based narrow band imaging. These results are compared with the extinction distribution recovered from the clusters. We find that the mean optical extinction derived in the starburst regions is close to the averaged value observed in the clusters [more than 80 per cent of the systems have E(B - V) <= 0.2mag], but locally, do not trace the more extinguished clusters. Previous HST studies of BCGs have revealed a population of young and extremely red super star clusters. We detect a considerable fraction of clusters affected by a red excess also in Mrk 930. The nature of the red excess, which turns up at near-IR wavelengths (I band and longwards), remains unknown. We compare the cluster formation history and the star formation history, the latter derived from the fit of spectral population synthesis models to the spectra. We find a general agreement between the two independently estimated quantities. Using the cluster properties, we perform a study of the host environmental properties. We find that the cluster formation efficiency (the fraction of star formation happening in clusters) is significantly higher, suggesting a key role of the environment for the formation of these massive objects.

  • 29.
    Agarwal, Bhaskar
    et al.
    Yale Univ, Dept Astron, 52 Hillhouse Ave,Steinbach Hall, New Haven, CT 06511 USA..
    Johnson, Jarrett L.
    Los Alamos Natl Lab, Theoret Div X, Los Alamos, NM 87545 USA..
    Zackrisson, Erik
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
    Labbe, Ivo
    Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands..
    van den Bosch, Frank C.
    Yale Univ, Dept Astron, 52 Hillhouse Ave,Steinbach Hall, New Haven, CT 06511 USA..
    Natarajan, Priyamvada
    Yale Univ, Dept Astron, 52 Hillhouse Ave,Steinbach Hall, New Haven, CT 06511 USA..
    Khochfar, Sadegh
    Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland..
    Detecting direct collapse black holes: making the case for CR72016In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 460, no 4, p. 4003-4010Article in journal (Refereed)
    Abstract [en]

    We propose that one of the sources in the recently detected system CR7 by Sobral et al. through spectrophotometric measurements at z=6.6 harbours a direct collapse black hole (DCBH). We argue that the LW radiation field required for direct collapse in source A is provided by sources B and C.By tracing the LW production history and star formation rate over cosmic time for the halo hosting CR7 in a ACDM universe, we demonstrate that a DCBH could have formed at z similar to 20. The spectrum of source A is well fit by nebular emission from primordial gas around a BH with MBH similar to 4.4x10(6)M(circle dot) accreting at a 40 per cent of the Eddington rate, which strongly supports our interpretation of the data. Combining these lines of evidence, we argue that CR7 might well be the first DCBH candidate.

  • 30.
    Agarwal, Bhaskar
    et al.
    Heidelberg Univ, Inst Theoret Phys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany..
    Regan, John
    Heidelberg Univ, Inst Theoret Phys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.;Dublin City Univ, Sch Math Sci, Ctr Astrophys & Relat, Dublin D09 Y5N0, Ireland..
    Klessen, Ralf S.
    Heidelberg Univ, Inst Theoret Phys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany..
    Downes, Turlough P.
    Dublin City Univ, Sch Math Sci, Ctr Astrophys & Relat, Dublin D09 Y5N0, Ireland..
    Zackrisson, Erik
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy. Uppsala Univ, Dept Phys & Astron, Box 515, SE-75120 Uppsala, Sweden..
    An analytic resolution to the competition between Lyman-Werner radiation and metal winds in direct collapse black hole hosts2017In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 470, no 4, p. 4034-4038Article in journal (Refereed)
    Abstract [en]

    A near pristine atomic cooling halo close to a star forming galaxy offers a natural pathway for forming massive direct collapse black hole (DCBH) seeds, which could be the progenitors of the z > 6 redshift quasars. The close proximity of the haloes enables a sufficient Lyman-Werner flux to effectively dissociate H-2 in the core of the atomic cooling halo. A mild background may also be required to delay star formation in the atomic cooling halo, often attributed to distant background galaxies. In this paper, we investigate the impact of metal pollution from both the background galaxies and the close star forming galaxy under extremely unfavourable conditions such as instantaneous metal mixing. We find that within the time window of DCBH formation, the level of pollution never exceeds the critical threshold (Z(cr) similar to 1 x 10(-5) Z(circle dot)) and attains a maximum metallicity of Z similar to 2 x 10(- 6) Z(circle dot). As the system evolves, the metallicity eventually exceeds the critical threshold, long after the DCBH has formed.

  • 31.
    Agarwal, Jessica
    et al.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    A'Hearn, M. F.
    Univ Maryland, Dept Astron, College Pk, MD 20742 USA..
    Vincent, J. -B
    Guettler, C.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Hoefner, S.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Sierks, H.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Tubiana, C.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Barbieri, C.
    Univ Padua, Dept Phys & Astron G Galilei, Vic Osservat 3, I-35122 Padua, Italy..
    Lamy, P. L.
    Aix Marseille Univ, Lab Astrophys Marseille, CNRS, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France..
    Rodrigo, R.
    CSIC, Ctr Astrobiol, INTA, European Space Agcy,ESAC, POB 78, E-28691 Madrid, Spain.;Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland..
    Koschny, D.
    European Space Agcy, Res & Sci Support Dept, NL-2201 Noordwijk, Netherlands..
    Rickman, Hans
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics. PAS Space Res Ctr, Poland..
    Barucci, M. A.
    Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA,Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France..
    Bertaux, J. -L
    Bertini, I.
    Univ Padua, Ctr Ateneo Studi Attivita Spaziali Giuseppe Colom, Via Venezia 15, I-35131 Padua, Italy..
    Boudreault, S.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Cremonese, G.
    INAF Osservat Astron Padova, Vicolo Osservat 5, I-35122 Padua, Italy..
    Da Deppo, V.
    CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy..
    Davidsson, B.
    Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA..
    Debei, S.
    Univ Padua, Dept Ind Engn, Via Venezia 1, I-35131 Padua, Italy..
    De Cecco, M.
    Univ Trento, Via Sommarive 9, I-38123 Trento, Italy..
    Deller, J.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Fornasier, S.
    Univ Paris Diderot, UPMC Univ Paris 06, CNRS, LESIA,Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France..
    Fulle, M.
    INAF Osservat Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy..
    Gicquel, A.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Groussin, O.
    Aix Marseille Univ, LAM, CNRS, UMR 7326, F-13388 Marseille, France..
    Gutierrez, P. J.
    CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain..
    Hofmann, M.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Hviid, S. F.
    DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany..
    Ip, W. -H
    Jorda, L.
    Aix Marseille Univ, LAM, CNRS, UMR 7326, F-13388 Marseille, France..
    Keller, H. U.
    TU Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany..
    Knollenberg, J.
    DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany..
    Kramm, J. -R
    Kuehrt, E.
    DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany..
    Kueppers, M.
    ESA ESAC, POB 78, E-28691 Villanueva De La Cananda, Spain..
    Lara, L. M.
    CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain..
    Lazzarin, M.
    Univ Padua, Dept Phys & Astron G Galilei, Vic Osservat 3, I-35122 Padua, Italy..
    Lopez Moreno, J. J.
    CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain..
    Marzari, F.
    Univ Padua, Dept Phys & Astron G Galilei, Vic Osservat 3, I-35122 Padua, Italy..
    Naletto, G.
    Univ Padua, Ctr Ateneo Studi Attivita Spaziali Giuseppe Colom, Via Venezia 15, I-35131 Padua, Italy.;CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.;Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy..
    Oklay, N.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Shi, X.
    Max Planck Inst Sonnensyst Forsch, Justus Von Liebig Weg 3, D-37077 Gottingen, Germany..
    Thomas, N.
    Univ Bern, Phys Inst, Sidlerstr 5, CH-3012 Bern, Switzerland..
    Acceleration of individual, decimetre-sized aggregates in the lower coma of comet 67P/Churyumov-Gerasimenko2016In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 462, p. S78-S88Article in journal (Refereed)
    Abstract [en]

    We present observations of decimetre-sized, likely ice-containing aggregates ejected from a confined region on the surface of comet 67P/Churyumov-Gerasimenko. The images were obtained with the narrow angle camera of the Optical, Spectroscopic, and Infrared Remote Imaging System on board the Rosetta spacecraft in 2016 January when the comet was at 2 au from the Sun outbound from perihelion. We measure the acceleration of individual aggregates through a 2 h image series. Approximately 50 per cent of the aggregates are accelerated away from the nucleus, and 50 per cent towards it, and likewise towards either horizontal direction. The accelerations are up to one order of magnitude stronger than local gravity, and are most simply explained by the combined effect of gas drag accelerating all aggregates upwards, and the recoil force from asymmetric outgassing, either from rotating aggregates with randomly oriented spin axes and sufficient thermal inertia to shift the temperature maximum away from an aggregate's subsolar region, or from aggregates with variable ice content. At least 10 per cent of the aggregates will escape the gravity field of the nucleus and feed the comet's debris trail, while others may fall back to the surface and contribute to the deposits covering parts of the Northern hemisphere. The rocket force plays a crucial role in pushing these aggregates back towards the surface. Our observations show the future back fall material in the process of ejection, and provide the first direct measurement of the acceleration of aggregates in the innermost coma (<2 km) of a comet, where gas drag is still significant.

  • 32.
    Ahlgren, Björn
    et al.
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Larsson, Josefin
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Ahlberg, Erik
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Lundman, Christoffer
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Pe'er, Asaf
    Testing a model for subphotospheric dissipation in GRBs: fits to Fermi data constrain the dissipation scenario2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 485, p. 474-497Article in journal (Refereed)
    Abstract [en]

    It has been suggested that the prompt emission in gamma-ray bursts (GRBs) could be described by radiation from the photosphere in a hot fireball. Such models must be tested by directly fitting them to data. In this work we use data from the Fermi Gamma-ray Space Telescope and consider a specific photospheric model, in which the kinetic energy of a low-magnetization outflow is dissipated locally by internal shocks below the photosphere. We construct a table model with a physically motivated parameter space and fit it to time-resolved spectra of the 36 brightest Fermi GRBs with a known redshift. We find that about two-thirds of the examined spectra cannot be described by the model, as it typically underpredicts the observed flux. However, since the sample is strongly biased towards bright GRBs, we argue that this fraction will be significantly lowered when considering the full population. From the successful fits we find that the model can reproduce the full range of spectral slopes present in the sample. For these cases we also find that the dissipation consistently occurs at a radius of ∼1012 cm and that only a few per cent efficiency is required. Furthermore, we find a positive correlation between the fireball luminosity and the Lorentz factor. Such a correlation has been previously reported by independent methods. We conclude that if GRB spectra are due to photospheric emission, the dissipation cannot only be the specific scenario we consider here.

  • 33.
    Ahnen, M. L.
    et al.
    Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland..
    Jóhannesson, Gudlaugur
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Larsson, Stefan
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Yassine, M.
    Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.;Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy..
    et al.,
    MAGIC and Fermi-LAT gamma-ray results on unassociated HAWC sources2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 485, no 1, p. 356-366Article in journal (Refereed)
    Abstract [en]

    The HAWC Collaboration released the 2HWC catalogue of TeV sources, in which 19 show no association with any known high-energy (HE; E greater than or similar to 10 GeV) or very-high-energy (VHE; E greater than or similar to 300 GeV) sources. This catalogue motivated follow-up studies by both the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) and Fermi-LAT (Large Area Telescope) observatories with the aim of investigating gamma-ray emission over a broad energy band. In this paper, we report the results from the first joint work between High Altitude Water Cherenkov (HAWC), MAGIC, and Fermi-LAT on three unassociated HAWC sources: 2HWC J2006+341, 2HWC J1907+084*, and 2HWC J1852+013*. Although no significant detection was found in the HE and VHE regimes, this investigation shows that a minimum 1 degrees extension (at 95 per cent confidence level) and harder spectrum in the GeV than the one extrapolated from HAWC results are required in the case of 2HWC J1852+013*, whilst a simply minimum extension of 0.16 degrees (at 95 per cent confidence level) can already explain the scenario proposed by HAWC for the remaining sources. Moreover, the hypothesis that these sources are pulsar wind nebulae is also investigated in detail.

  • 34. Alentiev, D.
    et al.
    Kochukhov, Oleg
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
    Ryabchikova, T.
    Cunha, M.
    Tsymbal, V.
    Weiss, W.
    Discovery of the longest period rapidly oscillating Ap star HD1777652012In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 421, no 1, p. L82-L86Article in journal (Refereed)
    Abstract [en]

    We present the discovery of a long-period, rapidly oscillating Ap (roAp) star, HD177765. Using high-resolution time-series observations obtained with the Ultraviolet and Visual Echelle Spectrograph at the European Southern Observatory Very Large Telescope, we found radial velocity variations with amplitudes 7-150 ms(-1) and a period of 23.6 min, exceeding that of any previously known roAp star. The largest pulsation amplitudes are observed for Eu III, Ce III and for the narrow core of H alpha. We derived the atmospheric parameters and chemical composition of HD177765, showing this star to be similar to other long-period roAp stars. Comparison with theoretical pulsational models indicates an advanced evolutionary state for HD177765. Abundance analyses of this and other roAp stars suggest a systematic variation with age of the rare-earth line anomalies seen in cool Ap stars.

  • 35.
    Algeri, Sara
    et al.
    Stockholm University, Faculty of Science, Department of Physics. Imperial College London, UK.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Imperial College London, UK.
    van Dyk, David A.
    A method for comparing non-nested models with application to astrophysical searches for new physics2016In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 458, no 1, p. L84-L88Article in journal (Refereed)
    Abstract [en]

    Searches for unknown physics and decisions between competing astrophysical models to explain data both rely on statistical hypothesis testing. The usual approach in searches for new physical phenomena is based on the statistical likelihood ratio test and its asymptotic properties. In the common situation, when neither of the two models under comparison is a special case of the other i.e. when the hypotheses are non-nested, this test is not applicable. In astrophysics, this problem occurs when two models that reside in different parameter spaces are to be compared. An important example is the recently reported excess emission in astrophysical gamma-rays and the question whether its origin is known astrophysics or dark matter. We develop and study a new, simple, generally applicable, frequentist method and validate its statistical properties using a suite of simulations studies. We exemplify it on realistic simulated data of the Fermi-Large Area Telescope gamma-ray satellite, where non-nested hypotheses testing appears in the search for particle dark matter.

  • 36.
    Alsing, Justin
    et al.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Flatiron Institute, USA; Imperial College London, UK.
    Charnock, Tom
    Feeney, Stephen
    Wandelt, Benjamin
    Fast likelihood-free cosmology with neural density estimators and active learning2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 488, no 3, p. 4440-4458Article in journal (Refereed)
    Abstract [en]

    Likelihood-free inference provides a framework for performing rigorous Bayesian inference using only forward simulations, properly accounting for all physical and observational effects that can be successfully included in the simulations, The key challenge for likelihood-free applications in cosmology, where simulation is typically expensive, is developing methods that can achieve high-fidelity posterior inference with as few simulations as possible. Density estimation likelihood-free inference (DELFI) methods turn inference into a density-estimation task on a set of simulated data-parameter pairs, and give orders of magnitude improvements over traditional Approximate Bayesian Computation approaches to likelihood-free inference. In this paper, we use neural density estimators (NDEs) to learn the likelihood function from a set of simulated data sets, with active learning to adaptively acquire simulations in the most relevant regions of parameter space on the fly. We demonstrate the approach on a number of cosmological case studies, showing that for typical problems high-fidelity posterior inference can be achieved with just 0(103) simulations or fewer. In addition to enabling efficient simulation-based inference, for simple problems where the form of the likelihood is known, DELFI offers a fast alternative to Markov Chain Monte Carlo (MCMC) sampling, giving orders of magnitude speed-up in some cases. Finally, we introduce PYDELFI a flexible public implementation of DELFI with NDFs and active learning - available at haps://github.com/justinalsing/pydelfi.

  • 37.
    Alsing, Justin
    et al.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Flatiron Institute, USA; Imperial College London, UK.
    Wandelt, Benjamin
    Nuisance hardened data compression for fast likelihood-free inference2019In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 488, no 4, p. 5093-5103Article in journal (Refereed)
    Abstract [en]

    We show how nuisance parameter marginalized posteriors can be inferred directly from simulations in a likelihood-free setting, without having to jointly infer the higher dimensional interesting and nuisance parameter posterior first and marginalize a posteriori. The result is that for an inference task with a given number of interesting parameters, the number of simulations required to perform likelihood-free inference can be kept (roughly) the same irrespective of the number of additional nuisances to be marginalized over. To achieve this, we introduce two extensions to the standard likelihood-free inference set-up. First, we show how nuisance parameters can be recast as latent variables and hence automatically marginalized over in the likelihood-free framework. Secondly, we derive an asymptotically optimal compression from N data to n summaries - one per interesting parameter - such that the Fisher information is (asymptotically) preserved, but the summaries are insensitive to the nuisance parameters. This means that the nuisance marginalized inference task involves learning n interesting parameters from n nuisance hardened' data summaries, regardless of the presence or number of additional nuisance parameters to be marginalized over. We validate our approach on two examples from cosmology: supernovae and weak-lensing data analyses with nuisance parametrized systematics. For the supernova problem, high-fidelity posterior inference of Omega(m) and w(0) (marginalized over systematics) can be obtained from just a few hundred data simulations. For the weak-lensing problem, six cosmological parameters can be inferred from just simulations, irrespective of whether 10 additional nuisance parameters are included in the problem or not.

  • 38.
    Alvarado-Gomez, Julian D.
    et al.
    Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA..
    Hussain, Gaitee A. J.
    European Southern Observ, Karl Schwarzschild Str 1, D-85748 Garching, Germany.;Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, F-31400 Toulouse, France..
    Drake, Jeremy J.
    Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA..
    Donati, Jean-Francois
    CNRS, IRAP, 14 Ave Edouard Belin, F-31400 Toulouse, France..
    Sanz-Forcada, Jorge
    CSIC, INTA, Ctr Astrobiol, ESAC Campus, E-28692 Madrid, Spain..
    Stelzer, Beate
    Eberhard Karls Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Cohen, Ofer
    Univ Massachusetts, Dept Phys & Appl Phys, 600 Suffolk St, Lowell, MA 01854 USA..
    Amazo-Gomez, Eliana M.
    Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.;Georg August Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany..
    Grunhut, Jason H.
    Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada..
    Garraffo, Cecilia
    Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA..
    Moschou, Sofia P.
    Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA..
    Silvester, James
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy.
    Oksala, Mary E.
    Univ Paris Diderot, Sorbonne Paris Cite, Univ Paris 06,LESIA, UPMC,Sorbonne Univ,CNRS,PSL Res Univ,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.;Calif Lutheran Univ, Dept Phys, 60 West Olsen Rd 3700, Thousand Oaks, CA 91360 USA..
    Far beyond the Sun - I. The beating magnetic heart in Horologium2018In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 473, no 4, p. 4326-4338Article in journal (Refereed)
    Abstract [en]

    A former member of the Hyades cluster, iota Horologii (iota Hor) is a planet-hosting Sun-like star which displays the shortest coronal activity cycle known to date (P-cyc similar to 1.6 yr). With an age of similar to 625 Myr, iota Hor is also the youngest star with a detected activity cycle. The study of its magnetic properties holds the potential to provide fundamental information to understand the origin of cyclic activity and stellar magnetism in late-type stars. In this series of papers, we present the results of a comprehensive project aimed at studying the evolving magnetic field in this star and how this evolution influences its circumstellar environment. This paper summarizes the first stage of this investigation, with results from a long-term observing campaign of iota Hor using ground-based high-resolution spectropolarimetry. The analysis includes precise measurements of the magnetic activity and radial velocity of the star, and their multiple time-scales of variability. In combination with values reported in the literature, we show that the long-term chromospheric activity evolution of iota Hor follows a beating pattern, caused by the superposition of two periodic signals of similar amplitude at P-1 similar or equal to 1.97 +/- 0.02 yr and P-2 similar or equal to 1.41 +/- 0.01 yr. Additionally, using the most recent parameters for iota Hor b in combination with our activity and radial velocity measurements, we find that stellar activity dominates the radial velocity residuals, making the detection of additional planets in this system challenging. Finally, we report here the first measurements of the surface longitudinal magnetic field strength of iota Hor, which displays varying amplitudes within +/- 4G and served to estimate the rotation period of the star (P-rot = 7.70(-0.67)(+0.18) d).

  • 39.
    Amanullah, Rahman
    et al.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Johansson, Joel
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Goobar, Ariel
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Ferretti, Raphael
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Papadogiannakis, Seméli
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Petrushevska, Tanja
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Brown, P. J.
    Cao, Y.
    Contreras, C.
    Dahle, H.
    Elias-Rosa, N.
    Fynbo, J. P. U.
    Gorosabel, J.
    Guaita, L.
    Hangard, Laura
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Howell, D. A.
    Hsiao, E. Y.
    Kankare, E.
    Kasliwal, M.
    Leloudas, G.
    Lundqvist, Peter
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Mattila, S.
    Nugent, P.
    Phillips, M. M.
    Sandberg, Andreas
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Stanishev, V.
    Sullivan, M.
    Taddia, Francesco
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Östlin, Göran
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Asadi, Saghar
    Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Herrero-Illana, R.
    Jensen, J. J.
    Karhunen, K.
    Lazarevic, S.
    Varenius, E.
    Santos, P.
    Sridhar, S. Seethapuram
    Wallström, S. H. J.
    Wiegert, J.
    Diversity in extinction laws of Type Ia supernovae measured between 0.2 and 2 mu m2015In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 453, no 3, p. 3300-3328Article in journal (Refereed)
    Abstract [en]

    We present ultraviolet (UV) observations of six nearby Type Ia supernovae (SNe Ia) obtained with the Hubble Space Telescope, three of which were also observed in the near-IR (NIR) with Wide-Field Camera 3. UV observations with the Swift satellite, as well as ground-based optical and NIR data provide complementary information. The combined data set covers the wavelength range 0.2-2 mu m. By also including archival data of SN 2014J, we analyse a sample spanning observed colour excesses up to E(B - V) = 1.4 mag. We study the wavelength-dependent extinction of each individual SN and find a diversity of reddening laws when characterized by the total-to-selective extinction R-V. In particular, we note that for the two SNe with E(B - V) greater than or similar to 1 mag, for which the colour excess is dominated by dust extinction, we find R-V = 1.4 +/- 0.1 and R-V = 2.8 +/- 0.1. Adding UV photometry reduces the uncertainty of fitted R-V by similar to 50 per cent allowing us to also measure R-V of individual low-extinction objects which point to a similar diversity, currently not accounted for in the analyses when SNe Ia are used for studying the expansion history of the Universe.

  • 40. Amarsi, A. M.
    et al.
    Asplund, M.
    Collet, R.
    Leenaarts, Jorrit
    Stockholm University, Faculty of Science, Department of Astronomy.
    Non-LTE oxygen line formation in 3D hydrodynamic model stellar atmospheres2016In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 455, no 4, p. 3735-3751Article in journal (Refereed)
    Abstract [en]

    The O (Iota) 777 nm lines are among the most commonly used diagnostics for the oxygen abundances in the atmospheres of FGK-type stars. However, they form in conditions that are far from local thermodynamic equilibrium (LTE). We explore the departures from LTE of atomic oxygen, and their impact on O I lines, across the STAGGER-grid of three-dimensional hydrodynamic model atmospheres. For the O (Iota) 777 nm triplet, we find significant departures from LTE. These departures are larger in stars with larger effective temperatures, smaller surface gravities, and larger oxygen abundances. We present grids of predicted 3D non-LTE based equivalent widths for the O (Iota) 616 nm, [O (Iota)] 630 nm, [O (I)] 636 nm, and O (Iota) 777 nm lines, as well as abundance corrections to 1D LTE based results.

  • 41. Amarsi, A. M.
    et al.
    Asplund, M.
    Collet, R.
    Leenaarts, Jorrit
    Stockholm University, Faculty of Science, Department of Astronomy.
    The Galactic chemical evolution of oxygen inferred from 3D non-LTE spectral-line-formation calculations2015In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 454, no 1, p. L11-L15Article in journal (Refereed)
    Abstract [en]

    We revisit the Galactic chemical evolution of oxygen, addressing the systematic errors inherent in classical determinations of the oxygen abundance that arise from the use of one-dimensional (1D) hydrostatic model atmospheres and from the assumption of local thermodynamic equilibrium (LTE). We perform detailed 3D non-LTE radiative-transfer calculations for atomic oxygen lines across a grid of 3D hydrodynamic STAGGER model atmospheres for dwarfs and subgiants. We apply our grid of predicted line strengths of the [O I] 630 nm and O I 777 nm lines using accurate stellar parameters from the literature. We infer a steep decay in [O/Fe] for [Fe/H] greater than or similar to -1.0, a plateau [O/Fe] approximate to 0.5 down to [Fe/H] approximate to -2.5, and an increasing trend for [Fe/H] less than or similar to -2.5. Our 3D non-LTE calculations yield overall concordant results from the two oxygen abundance diagnostics.

  • 42.
    Amarsi, A. M.
    et al.
    Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia..
    Lind, Karin
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy. Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany..
    Asplund, M.
    Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia..
    Barklem, Paul S.
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy. Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics.
    Collet, R.
    Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark..
    Non-LTE line formation of Fe in late-type stars - III. 3D non-LTE analysis of metal-poor stars2016In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 463, no 2, p. 1518-1533Article in journal (Refereed)
    Abstract [en]

    As one of the most important elements in astronomy, iron abundance determinations need to be as accurate as possible. We investigate the accuracy of spectroscopic iron abundance analyses using archetypal metal-poor stars. We perform detailed 3D non-LTE radiative transfer calculations based on 3D hydrodynamic STAGGER model atmospheres, and employ a new model atom that includes new quantum-mechanical neutral hydrogen collisional rate coefficients. With the exception of the red giant HD122563, we find that the 3D non-LTE models achieve Fe I/Fe II excitation and ionization balance as well as not having any trends with equivalent width to within modelling uncertainties of 0.05 dex, all without having to invoke any microturbulent broadening; for HD122563 we predict that the current best parallax-based surface gravity is overestimated by 0.5 dex. Using a 3D non-LTE analysis, we infer iron abundances from the 3D model atmospheres that are roughly 0.1 dex higher than corresponding abundances from 1D MARCS model atmospheres; these differences go in the same direction as the non-LTE effects themselves. We make available grids of departure coefficients, equivalent widths and abundance corrections, calculated on 1D MARCS model atmospheres and horizontally and temporally averaged 3D STAGGER model atmospheres.

  • 43.
    Andersson, Nils
    et al.
    School of Mathematics, University of Southampton.
    Haskell, Brynmore
    Astronomical Institute "Anton Pannekoek, University of Amsterdam.
    Samuelsson, Lars
    Umeå University, Faculty of Science and Technology, Department of Physics.
    Lagrangian perturbation theory for a superfluid immersed in an elastic neutron star crust2011In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 416, no 1, p. 118-132Article in journal (Refereed)
    Abstract [en]

    The inner crust of mature neutron stars, where an elastic lattice of neutron-rich nuclei coexists with a neutron superfluid, impacts on a range of astrophysical phenomena. The presence of the superfluid is key to our understanding of pulsar glitches, and is expected to affect the thermal conductivity and hence the evolution of the surface temperature. The coupling between crust and superfluid must also be accounted for in studies of neutron star dynamics, discussions of global oscillations and associated instabilities. In this paper we develop Lagrangian perturbation theory for this problem, paying attention to key issues like superfluid entrainment, potential vortex pinning, dissipative mutual friction and the star's magnetic field. We also discuss the nature of the core-crust interface. The results provide a theoretical foundation for a range of interesting astrophysical applications.

  • 44.
    André, Mats
    et al.
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.
    Odelstad, Elias
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division. Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Space Plasma Physics.
    Graham, Daniel B.
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.
    Eriksson, Anders I.
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.
    Karlsson, T.
    KTH Royal Inst Technol, Sch Elect Engn, Dept Space & Plasma Phys, Stockholm, Sweden.
    Wieser, G. Stenberg
    Swedish Inst Space Phys, Kiruna, Sweden.
    Vigren, Erik
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.
    Norgren, Cecilia
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division. Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Space Plasma Physics.
    Johansson, Fredrik L.
    Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.
    Henri, P.
    Lab Phys & Chim Environm & Espace, Orleans, France.
    Rubin, M.
    Univ Bern, Phys Inst, Bern, Switzerland.
    Richter, I.
    TU Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany.
    Lower hybrid waves at comet 67P/Churyumov-Gerasimenko2017In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 469, p. S29-S38Article in journal (Refereed)
    Abstract [en]

    We investigate the generation of waves in the lower hybrid frequency range by density gradients in the near plasma environment of comet 67P/Churyumov-Gerasimenko. When the plasma is dominated by water ions from the comet, a situation with magnetized electrons and unmagnetized ions is favourable for the generation of lower hybrid waves. These waves can transfer energy between ions and electrons and reshape the plasma environment of the comet. We consider cometocentric distances out to a few hundred km. We find that when the electron motion is not significantly interrupted by collisions with neutrals, large average gradients within tens of km of the comet, as well as often observed local large density gradients at larger distances, are often likely to be favourable for the generation of lower hybrid waves. Overall, we find that waves in the lower hybrid frequency range are likely to be common in the near plasma environment.

  • 45. André, Mats
    et al.
    Odelstad, Elias
    Graham, Daniel
    Eriksson, Anders
    Karlsson, Tomas
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Stenberg Wieser, Gabriella
    Vigren, Erik
    Norgren, Cecilia
    Johansson, Fredrik
    Henri, Pierre
    Rubin, M.
    Richter, Ingo
    Lower Hybrid Waves at Comet 67P/Churyumov-Gerasimenko2017In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 469, p. S29-S38Article in journal (Refereed)
    Abstract [en]

    We investigate the generation of waves in the lower hybrid frequency range by density gradients in the near plasma environment of comet 67P/Churyumov–Gerasimenko. When the plasma is dominated by water ions from the comet, a situation with magnetized electrons and unmagnetized ions is favourable for the generation of lower hybrid waves. These waves can transfer energy between ions and electrons and reshape the plasma environment of the comet. We consider cometocentric distances out to a few hundred km. We find that when the electron motion is not significantly interrupted by collisions with neutrals, large average gradients within tens of km of the comet, as well as often observed local large density gradients at larger distances, are often likely to be favourable for the generation of lower hybrid waves. Overall, we find that waves in the lower hybrid frequency range are likely to be common in the near plasma environment.

  • 46.
    Antipov, Sergey V.
    et al.
    Department of Chemistry and Molecular Biology, University of Gothenburg.
    Gustafsson, Magnus
    Department of Chemistry and Molecular Biology, University of Gothenburg.
    Nyman, Gunnar
    Department of Chemistry and Molecular Biology, University of Gothenburg.
    Isotope effect in the formation of carbon monoxide by radiative association2013In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 430, no 2, p. 946-950Article in journal (Refereed)
    Abstract [en]

    Rate coefficients for the formation of 12CO and 13CO isotopologues of carbon monoxide by radiative association for T = 10–20 000 K are calculated using a quantum mechanical approach. It is shown that the presence of the potential barrier on the A1Π electronic state of CO leads to different formation channels for the isotopologues at low temperatures. The corresponding rate coefficients are fitted to an analytic formula.

  • 47. Argyle, J. J.
    et al.
    Méndez-Abreu, J.
    Wild, V.
    Mortlock, Daniel J.
    Stockholm University, Faculty of Science, Department of Astronomy. Imperial College London, UK.
    Bayesian bulge-disc decomposition of galaxy images2018In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 479, no 3, p. 3076-3093Article in journal (Refereed)
    Abstract [en]

    We introduce PHI, a fully Bayesian Markov chain Monte Carlo algorithm designed for the structural decomposition of galaxy images. PHI uses a triple layer approach to effectively and efficiently explore the complex parameter space. Combining this with the use of priors to prevent non-physical models, PHI offers a number of significant advantages for estimating surface brightness profile parameters over traditional optimization algorithms. We apply PHI to a sample of synthetic galaxies with Sloan Digital Sky Survey (SDSS)-like image properties to investigate the effect of galaxy properties on our ability to recover unbiased and well-constrained structural parameters. In two-component bulge+disc galaxies, we find that the bulge structural parameters are recovered less well than those of the disc, particularly when the bulge contributes a lower fra