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1. H.E.S.S. first public test data release

Author: Abdalla, H., Abramowski, A., Aharonian, F., Ait Benkhali, F., Angüner, E.O., Arakawa, M., Arcaro, C., Armand, C., Arrieta, M., Backes, M., Barnard, M., Becherini, Y., Becker Tjus, J., Berge, D., Bernhard, S., Bernlöhr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bordas, P., Bregeon, J., Brun, F., Brun, P., Bryan, M., Büchele, 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., Decock, J., Deil, C., Devin, J., DeWilt, P., Dirson, L., Djannati-Ataï, A., Donath, A., Drury, L.O'C., Dyks, J., Edwards, T., Egberts, K., Emery, G., Ernenwein, J.-P., Eschbach, S., Fegan, S., Fiasson, A., Fontaine, G., Funk, S., Füßling, M., Gabici, S., Gallant, Y.A., Garrigoux, T., Gaté, 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., Katz, U., Katsuragawa, M., Kerszberg, D., Khangulyan, D., Khélif, B., King, J., Klepser, S., Kluzniak, W., Komin, Nu, Kosack, K., Krakau, S., Kraus, M., Krüger, P.P., Lamanna, G., Lau, J., Lefaucheur, J., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leser, E., Lohse, T., Lorentz, M., Liu, R., López-Coto, R., Lypova, I., Malyshev, D., Marandon, V., Marcowith, A., Mariaud, C., Marx, R., Maurin, G., Meintjes, P.J., Mitchell, 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., Prokhorov, D.A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reimer, A., Reimer, O., Renaud, M., De Los Reyes, R., 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., Schüssler, F., Schulz, A., Schwanke, U., Seglar-Arroyo, M., Seyffert, A.S., Shafi, N., Shiningayamwe, K., Simoni, R., Sol, H., Spanier, F., Stawarz, Ł, 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., Venter, C., Viana, A., Vincent, P., Vink, J., Voisin, F., Völk, H.J., Vuillaume, T., Wadiasingh, Z., Wagner, S.J., Wagner, P., Wagner, R.M., White, R., Wierzcholska, A., Wörnlein, A., Yang, R., Zaborov, D., Zacharias, M., Zanin, R., Zdziarski, A.A., Zech, A., Zefi, F., Ziegler, A., Zorn, J., Zywucka, N., Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), H.E.S.S., Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, background, FOS: Physical sciences, imaging, Cherenkov counter: atmosphere, quality, gamma ray, HESS, spectral, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The High Energy Stereoscopic System (H.E.S.S.) is an array of ground-based imaging atmospheric Cherenkov telescopes in Namibia. For the first time, the H.E.S.S. collaboration is releasing a small dataset of event lists and instrument response information. This is a test data release, with the motivation to support the ongoing efforts to define open high-level data models and associated formats, as well as open-source science tools for gamma-ray astronomy. The data are in FITS format. Open-source science tools that support this format exist already. The release data consists of 27.9 hours in total of observations of the Crab nebula, PKS 2155-304, MSH 15-52 and RX J1713.7-3946 taken with the H.E.S.S. 1 array. Most data are from 2004, the PKS 2155-304 data are from 2006 and 2008. In addition, 20.7 hours of off observations of empty fields of view are included. The targets and observations were chosen to be suitable for common analysis use cases, including point-like and extended sources for spectral and morphology measurements, as well as a variable source (PKS 2155-304) and the off dataset for background studies. The total size of the files in this data release is 42.8 MB. This is a very small subset of the thousands of hours of H.E.S.S. 1 observations taken since 2004. The quality of this dataset, and measurements derived from this data, does not reflect the state of the art for H.E.S.S. publications, e.g. the event reconstruction and gamma-hadron separation method used here is a very basic one., Comment: This is the release notes document. See https://www.mpi-hd.mpg.de/hfm/HESS/pages/dl3-dr1/ for further information
Published: 2018

2. Searches for gamma-ray lines and ‘pure WIMP’ spectra from Dark Matter annihilations in dwarf galaxies with H.E.S.S.

Author: Cirelli, M., primary, Panci, P., additional, Sala, F., additional, Silk, J., additional, Taoso, M., additional, Abdalla, H., additional, Aharonian, F., additional, Benkhali, F. Ait, additional, Angüner, E.O., additional, Arakawa, M., additional, Arcaro, C., additional, Armand, C., additional, Arrieta, M., additional, Backes, M., additional, Barnard, M., additional, Becherini, Y., additional, Tjus, J. Becker, additional, Berge, D., additional, Bernhard, S., additional, Bernlöhr, K., additional, Blackwell, R., additional, Böttcher, M., additional, Boisson, C., additional, Bolmont, J., additional, Bonnefoy, S., additional, Bordas, P., additional, Bregeon, J., additional, Brun, F., additional, Brun, P., additional, Bryan, M., additional, Büchele, M., additional, Bulik, T., additional, Bylund, T., additional, Capasso, M., additional, Caroff, S., additional, Carosi, A., additional, Casanova, S., additional, Cerruti, M., additional, Chakraborty, N., additional, Chandra, S., additional, Chaves, R.C.G., additional, Chen, A., additional, Colafrancesco, S., additional, Condon, B., additional, Davids, I.D., additional, Deil, C., additional, Devin, J., additional, deWilt, P., additional, Dirson, L., additional, Djannati-Ataï, A., additional, Dmytriiev, A., additional, Donath, A., additional, Doroshenko, V., additional, Drury, L.O'C., additional, Dyks, J., additional, Egberts, K., additional, Emery, G., additional, Ernenwein, J.-P., additional, Eschbach, S., additional, Fegan, S., additional, Fiasson, A., additional, Fontaine, G., additional, Funk, S., additional, Füßling, M., additional, Gabici, S., additional, Gallant, Y.A., additional, Gaté, F., additional, Giavitto, G., additional, Glawion, D., additional, Glicenstein, J.F., additional, Gottschall, D., additional, Grondin, M.-H., additional, Hahn, J., additional, Haupt, M., additional, Heinzelmann, G., additional, Henri, G., additional, Hermann, G., additional, Hinton, J.A., additional, Hofmann, W., additional, Hoischen, C., additional, Holch, T. L., additional, Holler, M., additional, Horns, D., additional, Huber, D., additional, Iwasaki, H., additional, Jacholkowska, A., additional, Jamrozy, M., additional, Jankowsky, D., additional, Jankowsky, F., additional, Jouvin, L., additional, Jung-Richardt, I., additional, Kastendieck, M.A., additional, Katarzyński, K., additional, Katsuragawa, M., additional, Katz, U., additional, Kerszberg, D., additional, Khangulyan, D., additional, Khélifi, B., additional, King, J., additional, Klepser, S., additional, Kluźniak, W., additional, Komin, Nu., additional, Kosack, K., additional, Krakau, S., additional, Kraus, M., additional, Krüger, P.P., additional, Lamanna, G., additional, Lau, J., additional, Lefaucheur, J., additional, Lemière, A., additional, Lemoine-Goumard, M., additional, Lenain, J.-P., additional, Leser, E., additional, Lohse, T., additional, Lorentz, M., additional, López-Coto, R., additional, Lypova, I., additional, Malyshev, D., additional, Marandon, V., additional, Marcowith, A., additional, Mariaud, C., additional, Martí-Devesa, G., additional, Marx, R., additional, Maurin, G., additional, Meintjes, P.J., additional, Mitchell, A.M.W., additional, Moderski, R., additional, Mohamed, M., additional, Mohrmann, L., additional, Moulin, E., additional, Murach, T., additional, Nakashima, S., additional, de Naurois, M., additional, Ndiyavala, H., additional, Niederwanger, F., additional, Niemiec, J., additional, Oakes, L., additional, O'Brien, P., additional, Odaka, H., additional, Ohm, S., additional, Ostrowski, M., additional, Oya, I., additional, Padovani, M., additional, Panter, M., additional, Parsons, R.D., additional, Perennes, C., additional, Petrucci, P.-O., additional, Peyaud, B., additional, Piel, Q., additional, Pita, S., additional, Poireau, V., additional, Noel, A. Priyana, additional, Prokhorov, D.A., additional, Prokoph, H., additional, Pühlhofer, G., additional, Punch, M., additional, Quirrenbach, A., additional, Raab, S., additional, Rauth, R., additional, Reimer, A., additional, Reimer, O., additional, Renaud, M., additional, Rieger, F., additional, Rinchiuso, L., additional, Romoli, C., additional, Rowell, G., additional, Rudak, B., additional, Ruiz-Velasco, E., additional, Sahakian, V., additional, Saito, S., additional, Sanchez, D.A., additional, Santangelo, A., additional, Sasaki, M., additional, Schlickeiser, R., additional, Schüssler, F., additional, Schulz, A., additional, Schwanke, U., additional, Schwemmer, S., additional, Seglar-Arroyo, M., additional, Senniappan, M., additional, Seyffert, A.S., additional, Shafi, N., additional, Shilon, I., additional, Shiningayamwe, K., additional, Simoni, R., additional, Sinha, A., additional, Sol, H., additional, Spanier, F., additional, Specovius, A., additional, Spir-Jacob, M., additional, Stawarz, Ł., additional, Steenkamp, R., additional, Stegmann, C., additional, Steppa, C., additional, Takahashi, T., additional, Tavernet, J.-P., additional, Tavernier, T., additional, Taylor, A.M., additional, Terrier, R., additional, Tibaldo, L., additional, Tiziani, D., additional, Tluczykont, M., additional, Trichard, C., additional, Tsirou, M., additional, Tsuji, N., additional, Tuffs, R., additional, Uchiyama, Y., additional, Walt, D.J. van der, additional, Eldik, C. van, additional, Rensburg, C. van, additional, Soelen, B. van, additional, Vasileiadis, G., additional, Veh, J., additional, Venter, C., additional, Viana, A., additional, Vincent, P., additional, Vink, J., additional, Voisin, F., additional, Völk, H.J., additional, Vuillaume, T., additional, Wadiasingh, Z., additional, Wagner, S.J., additional, Wagner, R.M., additional, White, R., additional, Wierzcholska, A., additional, Yang, R., additional, Zaborov, D., additional, Zacharias, M., additional, Zanin, R., additional, Zdziarski, A.A., additional, Zech, A., additional, Zefi, F., additional, Ziegler, A., additional, Zorn, J., additional, and Żywucka, N., additional
Published: 2018
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3. Detection of variable VHE γ-ray emission from the extra-galactic γ-ray binary LMC P3

Author: 24420530 - Böttcher, Markus, 26909995 - Garrigoux, Tania, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 26403366 - Ndiyavala, Hambeleleni, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 20574266 - Barnard, Monica, 26598973 - Abdalla, Hassan, Abdalla, H., Barnard, M., Böttcher, M., Garrigoux, T., Ivascenko, A., Krüger, P.P., Ndiyavala, H., Pekeur, N.W., Seyffert, A.S., Spanier, F., Sushch, I., Van der Walt, D.J., Van Rensburg, C., Venter, C., Wadiasingh, Z., Zacharias, M., H.E.S.S. Collaboration, 24420530 - Böttcher, Markus, 26909995 - Garrigoux, Tania, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 26403366 - Ndiyavala, Hambeleleni, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 20574266 - Barnard, Monica, 26598973 - Abdalla, Hassan, Abdalla, H., Barnard, M., Böttcher, M., Garrigoux, T., Ivascenko, A., Krüger, P.P., Ndiyavala, H., Pekeur, N.W., Seyffert, A.S., Spanier, F., Sushch, I., Van der Walt, D.J., Van Rensburg, C., Venter, C., Wadiasingh, Z., Zacharias, M., and H.E.S.S. Collaboration
Abstract: Context. Recently, the high-energy (HE, 0.1–100 GeV) γ-ray emission from the object LMC P3 in the Large Magellanic Cloud (LMC) has been discovered to be modulated with a 10.3-day period, making it the first extra-galactic γ-ray binary. Aim. This work aims at the detection of very-high-energy (VHE, >100 GeV) γ-ray emission and the search for modulation of the VHE signal with the orbital period of the binary system. Methods. LMC P3 has been observed with the High Energy Stereoscopic System (H.E.S.S.); the acceptance-corrected exposure time is 100 h. The data set has been folded with the known orbital period of the system in order to test for variability of the emission. Results. VHE γ-ray emission is detected with a statistical significance of 6.4 σ. The data clearly show variability which is phase-locked to the orbital period of the system. Periodicity cannot be deduced from the H.E.S.S. data set alone. The orbit-averaged luminosity in the 1–10 TeV energy range is (1.4 ± 0.2) × 1035 erg s−1. A luminosity of (5 ± 1) × 1035 erg s−1 is reached during 20% of the orbit. HE and VHE γ-ray emissions are anti-correlated. LMC P3 is the most luminous γ-ray binary known so far
Published: 2018

4. A polarized fast radio burst at low Galactic latitude

Author: Petroff, E., primary, Burke-Spolaor, S., additional, Keane, E. F., additional, McLaughlin, M. A., additional, Miller, R., additional, Andreoni, I., additional, Bailes, M., additional, Barr, E. D., additional, Bernard, S. R., additional, Bhandari, S., additional, Bhat, N. D. R., additional, Burgay, M., additional, Caleb, M., additional, Champion, D., additional, Chandra, P., additional, Cooke, J., additional, Dhillon, V. S., additional, Farnes, J. S., additional, Hardy, L. K., additional, Jaroenjittichai, P., additional, Johnston, S., additional, Kasliwal, M., additional, Kramer, M., additional, Littlefair, S. P., additional, Macquart, J. P., additional, Mickaliger, M., additional, Possenti, A., additional, Pritchard, T., additional, Ravi, V., additional, Rest, A., additional, Rowlinson, A., additional, Sawangwit, U., additional, Stappers, B., additional, Sullivan, M., additional, Tiburzi, C., additional, van Straten, W., additional, Albert, A., additional, André, M., additional, Anghinolfi, M., additional, Anton, G., additional, Ardid, M., additional, Aubert, J.-J., additional, Avgitas, T., additional, Baret, B., additional, Barrios-Martí, J., additional, Basa, S., additional, Bertin, V., additional, Biagi, S., additional, Bormuth, R., additional, Bourret, S., additional, Bouwhuis, M.C., additional, Bruijn, R., additional, Brunner, J., additional, Busto, J., additional, Capone, A., additional, Caramete, L., additional, Carr, J., additional, Celli, S., additional, Chiarusi, T., additional, Circella, M., additional, Coelho, J.A.B., additional, Coleiro, A., additional, Coniglione, R., additional, Costantini, H., additional, Coyle, P., additional, Creusot, A., additional, Deschamps, A., additional, De Bonis, G., additional, Distefano, C., additional, Palma, I. Di, additional, Donzaud, C., additional, Dornic, D., additional, Drouhin, D., additional, Eberl, T., additional, El Bojaddaini, I., additional, Elsässer, D., additional, Enzenhöfer, A., additional, Felis, I., additional, Fusco, L.A., additional, Galatà, S., additional, Gay, P., additional, Geißelsöder, S., additional, Geyer, K., additional, Giordano, V., additional, Gleixner, A., additional, Glotin, H., additional, Grégoire, T., additional, Gracia-Ruiz, R., additional, Graf, K., additional, Hallmann, S., additional, van Haren, H., additional, Heijboer, A.J., additional, Hello, Y., additional, Hernández-Rey, J.J., additional, Hößl, J., additional, Hofestädt, J., additional, Hugon, C., additional, Illuminati, G., additional, James, C.W, additional, de Jong, M., additional, Jongen, M., additional, Kadler, M., additional, Kalekin, O., additional, Katz, U., additional, Kießling, D., additional, Kouchner, A., additional, Kreter, M., additional, Kreykenbohm, I., additional, Kulikovskiy, V., additional, Lachaud, C., additional, Lahmann, R., additional, Lefèvre, D., additional, Leonora, E., additional, Lotze, M., additional, Loucatos, S., additional, Marcelin, M., additional, Margiotta, A., additional, Marinelli, A., additional, Martínez-Mora, J.A., additional, Mathieu, A., additional, Mele, R., additional, Melis, K., additional, Michael, T., additional, Migliozzi, P., additional, Moussa, A., additional, Mueller, C., additional, Nezri, E., additional, Păvălaş, G.E., additional, Pellegrino, C., additional, Perrina, C., additional, Piattelli, P., additional, Popa, V., additional, Pradier, T., additional, Quinn, L., additional, Racca, C., additional, Riccobene, G., additional, Roensch, K., additional, Sánchez-Losa, A., additional, Saldaña, M., additional, Salvadori, I., additional, Samtleben, D. F. E., additional, Sanguineti, M., additional, Sapienza, P., additional, Schnabel, J., additional, Seitz, T., additional, Sieger, C., additional, Spurio, M., additional, Stolarczyk, Th., additional, Taiuti, M., additional, Tayalati, Y., additional, Trovato, A., additional, Tselengidou, M., additional, Turpin, D., additional, Tönnis, C., additional, Vallage, B., additional, Vallée, C., additional, Van Elewyck, V., additional, Vivolo, D., additional, Vizzoca, A., additional, Wagner, S., additional, Wilms, J., additional, Zornoza, J.D., additional, Zúñiga, J., additional, Abdalla, H., additional, Abramowski, A., additional, Aharonian, F., additional, Benkhali, F. Ait, additional, Akhperjanian, A.G., additional, Andersson, T., additional, Angüner, E.O., additional, Arrieta, M., additional, Aubert, P., additional, Backes, M., additional, Balzer, A., additional, Barnard, M., additional, Becherini, Y., additional, Becker Tjus, J., additional, Berge, D., additional, Bernhard, S., additional, Bernlöhr, K., additional, Blackwell, R., additional, Böttcher, M., additional, Boisson, C., additional, Bolmont, J., additional, Bordas, P., additional, Bregeon, J., additional, Brun, F., additional, Brun, P., additional, Bryan, M., additional, Bulik, T., additional, Capasso, M., additional, Casanova, S., additional, Cerruti, M., additional, Chakraborty, N., additional, Chalme-Calvet, R., additional, Chaves, R.C.G., additional, Chen, A., additional, Chevalier, J., additional, Chrétien, M., additional, Colafrancesco, S., additional, Cologna, G., additional, Condon, B., additional, Conrad, J., additional, Cui, Y., additional, Davids, I.D., additional, Decock, J., additional, Degrange, B., additional, Deil, C., additional, Devin, J., additional, deWilt, P., additional, Dirson, L., additional, Djannati-Ataï, A., additional, Domainko, W., additional, Donath, A., additional, Drury, L.O’C., additional, Dubus, G., additional, Dutson, K., additional, Dyks, J., additional, Edwards, T., additional, Egberts, K., additional, Eger, P., additional, Ernenwein, J.-P., additional, Eschbach, S., additional, Farnier, C., additional, Fegan, S., additional, Fernandes, M.V., additional, Fiasson, A., additional, Fontaine, G., additional, Förster, A., additional, Funk, S., additional, Füßling, M., additional, Gabici, S., additional, Gajdus, M., additional, Gallant, Y.A., additional, Garrigoux, T., additional, Giavitto, G., additional, Giebels, B., additional, Glicenstein, J.F., additional, Gottschall, D., additional, Goyal, A., additional, Grondin, M.-H., additional, Hadasch, D., additional, Hahn, J., additional, Haupt, M., additional, Hawkes, J., additional, Heinzelmann, G., additional, Henri, G., additional, Hermann, G., additional, Hervet, O., additional, Hinton, J.A., additional, Hofmann, W., additional, Hoischen, C., additional, Holler, M., additional, Horns, D., additional, Ivascenko, A., additional, Jacholkowska, A., additional, Jamrozy, M., additional, Janiak, M., additional, Jankowsky, D., additional, Jankowsky, F., additional, Jingo, M., additional, Jogler, T., additional, Jouvin, L., additional, Jung-Richardt, I., additional, Kastendieck, M.A., additional, Katarzyński, K., additional, Kerszberg, D., additional, Khélifi, B., additional, Kieffer, M., additional, King, J., additional, Klepser, S., additional, Klochkov, D., additional, Kluźniak, W., additional, Kolitzus, D., additional, Komin, Nu., additional, Kosack, K., additional, Krakau, S., additional, Kraus, M., additional, Krayzel, F., additional, Krüger, P.P., additional, Laffon, H., additional, Lamanna, G., additional, Lau, J., additional, Lees, J.-P., additional, Lefaucheur, J., additional, Lefranc, V., additional, Lemière, A., additional, Lemoine-Goumard, M., additional, Lenain, J.-P., additional, Leser, E., additional, Lohse, T., additional, Lorentz, M., additional, Liu, R., additional, López-Coto, R., additional, Lypova, I., additional, Marandon, V., additional, Marcowith, A., additional, Mariaud, C., additional, Marx, R., additional, Maurin, G., additional, Maxted, N., additional, Mayer, M., additional, Meintjes, P.J., additional, Meyer, M., additional, Mitchell, A.M.W., additional, Moderski, R., additional, Mohamed, M., additional, Mohrmann, L., additional, Morå, K., additional, Moulin, E., additional, Murach, T., additional, de Naurois, M., additional, Niederwanger, F., additional, Niemiec, J., additional, Oakes, L., additional, O’Brien, P., additional, Odaka, H., additional, Öttl, S., additional, Ohm, S., additional, Ostrowski, M., additional, Oya, I., additional, Padovani, M., additional, Panter, M., additional, Parsons, R.D., additional, Pekeur, N.W., additional, Pelletier, G., additional, Perennes, C., additional, Petrucci, P.-O., additional, Peyaud, B., additional, Piel, Q., additional, Pita, S., additional, Poon, H., additional, Prokhorov, D., additional, Prokoph, H., additional, Pühlhofer, G., additional, Punch, M., additional, Quirrenbach, A., additional, Raab, S., additional, Reimer, A., additional, Reimer, O., additional, Renaud, M., additional, Reyes, R. de los, additional, Rieger, F., additional, Romoli, C., additional, Rosier-Lees, S., additional, Rowell, G., additional, Rudak, B., additional, Rulten, C.B., additional, Sahakian, V., additional, Salek, D., additional, Sanchez, D.A., additional, Santangelo, A., additional, Sasaki, M., additional, Schlickeiser, R., additional, Schulz, A., additional, Schüssler, F., additional, Schwanke, U., additional, Schwemmer, S., additional, Settimo, M., additional, Seyffert, A.S., additional, Shafi, N., additional, Shilon, I., additional, Simoni, R., additional, Sol, H., additional, Spanier, F., additional, Spengler, G., additional, Spies, F., additional, Stawarz, Ł., additional, Steenkamp, R., additional, Stegmann, C., additional, Stinzing, F., additional, Stycz, K., additional, Sushch, I., additional, Tavernet, J.-P., additional, Tavernier, T., additional, Taylor, A.M., additional, Terrier, R., additional, Tibaldo, L., additional, Tiziani, D., additional, Tluczykont, M., additional, Trichard, C., additional, Tuffs, R., additional, Uchiyama, Y., additional, Walt, D.J. van der, additional, van Eldik, C., additional, van Rensburg, C., additional, van Soelen, B., additional, Vasileiadis, G., additional, Veh, J., additional, Venter, C., additional, Viana, A., additional, Vincent, P., additional, Vink, J., additional, Voisin, F., additional, Völk, H.J., additional, Vuillaume, T., additional, Wadiasingh, Z., additional, Wagner, S.J., additional, Wagner, P., additional, Wagner, R.M., additional, White, R., additional, Wierzcholska, A., additional, Willmann, P., additional, Wörnlein, A., additional, Wouters, D., additional, Yang, R., additional, Zabalza, V., additional, Zaborov, D., additional, Zacharias, M., additional, Zanin, R., additional, Zdziarski, A.A., additional, Zech, A., additional, Zefi, F., additional, Ziegler, A., additional, and Żywucka, N., additional
Published: 2017
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5. TeV gamma-ray observations of the binary neutron star merger GW170817 with H.E.S.S.

Author: 24420530 - Böttcher, Markus, 26909995 - Garrigoux, Tania, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 26403366 - Ndiyavala, Hambeleleni, 26598973 - Abdalla, Hassan, 20574266 - Barnard, Monica, Abdalla, H., Barnard, M., Böttcher, M., Garrigoux, T., Ivascenko, A., Krüger, P.P., Ndiyavala, H., Pekeur, N.W., Seyffert, A.S., Spanier, F., Sushch, I., Van der Walt, D.J., Van Rensburg, C., Venter, C., Wadiasingh, Z., Zacharias, M., H.E.S.S. Collaboration, 24420530 - Böttcher, Markus, 26909995 - Garrigoux, Tania, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 26403366 - Ndiyavala, Hambeleleni, 26598973 - Abdalla, Hassan, 20574266 - Barnard, Monica, Abdalla, H., Barnard, M., Böttcher, M., Garrigoux, T., Ivascenko, A., Krüger, P.P., Ndiyavala, H., Pekeur, N.W., Seyffert, A.S., Spanier, F., Sushch, I., Van der Walt, D.J., Van Rensburg, C., Venter, C., Wadiasingh, Z., Zacharias, M., and H.E.S.S. Collaboration
Abstract: We search for high-energy gamma-ray emission from the binary neutron star merger GW170817 with the H.E.S.S. Imaging Air Cherenkov Telescopes. The observations presented here have been obtained starting only 5.3 hr after GW170817. The H.E.S.S. target selection identified regions of high probability to find a counterpart of the gravitational-wave event. The first of these regions contained the counterpart SSS17a that has been identified in the optical range several hours after our observations. We can therefore present the first data obtained by a groundbased pointing instrument on this object. A subsequent monitoring campaign with the H.E.S.S. telescopes extended over several days, covering timescales from 0.22 to 5.2 days and energy ranges between 270 GeV to 8.55 TeV. No significant gamma-ray emission has been found. The derived upper limits on the very-high-energy gamma-ray flux for the first time constrain non-thermal, high-energy emission following the merger of a confirmed binary neutron star system
Published: 2017

6. The high-energy γ-ray emission of AP Librae

Author: H.E.S.S.Collaboration, Abramowski, A., Aharonian, F., Ait Benkhali, F., Akhperjanian, A.G., Angüner, E., Anton, G., Backes, M., Balenderan, S., Balzer, A., Barnacka, A., Becherini, Y., Becker Tjus, J., Bernlöhr, K., Birsin, E., Bissaldi, E., Biteau, J., Böttcher, M., Boisson, C., Bolmont, J., Bordas, P., Brucker, J., Brun, F., Brun, P., Bulik, T., Carrigan, S., Casanova, S., Chadwick, P.M., Chalme-Calvet, R., Chaves, R.C.G., Cheesebrough, A., Chrétien, 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-Ataï, 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., Förster, A., Füßling, M., Gajdus, M., Gallant, Y.A., Garrigoux, T., Giavitto, G., Giebels, B., Glicenstein, J.F., Grondin, M.-H., Grudzińska, M., Häffner, 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., Katarzyński, K., Katz, U., Kaufmann, S., Khélifi, B., Kieffer, M., Klepser, S., Klochkov, D., Kluźniak, W., Kneiske, T., Kolitzus, D., Komin, Nu., Kosack, K., Krakau, S., Krayzel, F., Krüger, P.P., Laffon, H., Lamanna, G., Lefaucheur, J., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Lohse, T., Lopatin, A., Lu, C.-C., Marandon, V., Marcowith, A., Marx, R., Maurin, G., Maxted, N., Mayer, M., McComb, T.J.L., Méhault, J., Meintjes, P.J., Menzler, U., Meyer, M., Moderski, R., Mohamed, M., Moulin, E., Murach, T., Naumann, C.L., Naurois, M. de, Niemiec, J., Nolan, S.J., Oakes, L., Odaka, H., Ohm, S., Oña Wilhelmi, E. de, Opitz, B., Ostrowski, M., Oya, I., Panter, M., Parsons, R.D., Paz Arribas, M., Pekeur, N.W., Pelletier, G., Perez, J., Petrucci, P.-O., Peyaud, B., Pita, S., Poon, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Raue, M., Reichardt, I., Reimer, A., Reimer, O., Renaud, M., Reyes, R. de los, 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., Schüssler, F., Schulz, A., Schwanke, U., Schwarzburg, S., Schwemmer, S., Sol, H., Spengler, G., Spies, F., Stawarz, Ł., Steenkamp, R., Stegmann, C., Stinzing, F., Stycz, K., Sushch, I., 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., Völk, H.J., Volpe, F., Vorster, M., Vuillaume, T., Wagner, S.J., Wagner, P., Wagner, R.M., Ward, M., Weidinger, M., Weitze, Q., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Yang, R., Zabalza, V., Zacharias, M., Zdziarski, A.A., Zech, A., Zechlin, H.-S., Finke, J., Fortin, P., Horan, D., 24420530 - Böttcher, Markus, 23909196 - Casanova, Sabrina, 13146629 - Davids, Isak Delberth, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 24922986 - Sushch, Iurii, 12006653 - Venter, Christo, and 12792322 - Vorster, Michael Johannes
Subjects: Physics, Spectral index, Range (particle radiation), galaxies. [Gamma rays], active [Galaxies], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics, Type (model theory), Light curve, 7. Clean energy, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, galaxies [gamma rays], individual: AP Librae [BL Lacertae objects], Spectral energy distribution, High Energy Physics::Experiment, 010303 astronomy & astrophysics, Energy (signal processing), Fermi Gamma-ray Space Telescope
Abstract: The $\gamma$-ray spectrum of the low-frequency-peaked BL Lac (LBL) object AP Librae is studied, following the discovery of very-high-energy (VHE; $E>100\,{\rm GeV}$) $\gamma$-ray emission up to the TeV range by the H.E.S.S. experiment. This makes AP Librae one of the few VHE emitters of the LBL type. The measured spectrum yields a flux of $(8.8 \pm 1.5_{\rm stat} \pm 1.8_{\rm sys}) \times 10^{-12}\ {\rm cm}^{-2} {\rm s}^{-1}$ above 130 GeV and a spectral index of $\Gamma = 2.65\pm0.19_{\rm stat}\pm0.20_{\rm sys}$. This study also makes use of \textit{Fermi}-LAT, observations in the high energy (HE, E$>$100 MeV) range, providing the longest continuous light curve (5 years) ever published on this source. The source underwent a flaring event between MJD 56306-56376 in the HE range, with a flux increase of a factor 3.5 in the 14-day bin light curve and no significant variation in spectral shape with respect to the low-flux state. While the H.E.S.S., and (low state) \textit{Fermi}-LAT fluxes are in good agreement where they overlap, a spectral curvature between the steep VHE spectrum and the \textit{Fermi}-LAT, spectrum is observed. The maximum of the $\gamma$-ray emission in the spectral energy distribution is located below the GeV energy range.
Published: 2015

7. Acceleration of petaelectronvolt protons in the Galactic Centre

Author: 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 23909196 - Casanova, Sabrina, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 25161814 - Spanier, Felix Alexander, 12006653 - Venter, Christo, 24922986 - Sushch, Iurii, Abramowski, A., Böttcher, M., Casanova, S., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Spanier, F., Sushch, I., Venter, C., Davids, I.D., H.E.S.S. Collaboration, 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 23909196 - Casanova, Sabrina, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 25161814 - Spanier, Felix Alexander, 12006653 - Venter, Christo, 24922986 - Sushch, Iurii, Abramowski, A., Böttcher, M., Casanova, S., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Spanier, F., Sushch, I., Venter, C., Davids, I.D., and H.E.S.S. Collaboration
Abstract: Galactic cosmic rays reach energies of at least a few petaelectronvolts1 (of the order of 1015 electronvolts). This implies that our Galaxy contains petaelectronvolt accelerators (‘PeVatrons’), but all proposed models of Galactic cosmic-ray accelerators encounter difficulties at exactly these energies2. Dozens of Galactic accelerators capable of accelerating particles to energies of tens of teraelectronvolts (of the order of 1013 electronvolts) were inferred from recent γ-ray observations3. However, none of the currently known accelerators—not even the handful of shell-type supernova remnants commonly believed to supply most Galactic cosmic rays—has shown the characteristic tracers of petaelectronvolt particles, namely, power-law spectra of γ-rays extending without a cut-off or a spectral break to tens of teraelectronvolts4. Here we report deep γ-ray observations with arcminute angular resolution of the region surrounding the Galactic Centre, which show the expected tracer of the presence of petaelectronvolt protons within the central 10 parsecs of the Galaxy. We propose that the supermassive black hole Sagittarius A* is linked to this PeVatron. Sagittarius A* went through active phases in the past, as demonstrated by X-ray outbursts5and an outflow from the Galactic Centre6. Although its current rate of particle acceleration is not sufficient to provide a substantial contribution to Galactic cosmic rays, Sagittarius A* could have plausibly been more active over the last 106–107 years, and therefore should be considered as a viable alternative to supernova remnants as a source of petaelectronvolt Galactic cosmic rays.
Published: 2016

8. Search for dark matter annihilations towards the inner Galactic halo from 10 years of observations with H.E.S.S.

Author: 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 26909995 - Garrigoux, Tania, 20574266 - Barnard, Monica, 26598973 - Abdalla, Hassan, Abdallah, H., Barnard, M., Böttcher, M., Davids, I.D., Garrigoux, T., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Seyffert, A.S., Spanier, F., Van der Walt, D.J., Venter, C., H.E.S.S. Collaboration, 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 20126999 - Seyffert, Albertus Stefanus, 25161814 - Spanier, Felix Alexander, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 26909995 - Garrigoux, Tania, 20574266 - Barnard, Monica, 26598973 - Abdalla, Hassan, Abdallah, H., Barnard, M., Böttcher, M., Davids, I.D., Garrigoux, T., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Seyffert, A.S., Spanier, F., Van der Walt, D.J., Venter, C., and H.E.S.S. Collaboration
Abstract: The inner region of the Milky Way halo harbors a large amount of dark matter (DM). Given its proximity, it is one of the most promising targets to look for DM. We report on a search for the annihilations of DM particles using γ-ray observations towards the inner 300 parsecs of the Milky Way, with the H.E.S.S. array of ground-based Cherenkov telescopes. The analysis is based on a 2D maximum likelihood method using Galactic center (GC) data accumulated by H.E.S.S. over the last 10 years (2004-2014), and does not show any significant γ-ray signal above background. Assuming Einasto and Navarro-Frenk-White DM density profiles at the GC, we derive upper limits on the annihilation cross section ⟨σv⟩. These constraints are the strongest obtained so far in the TeV DM mass range and improve upon previous limits by a factor 5. For the Einasto profile, the constraints reach ⟨σv⟩ values of 6×10−26cm3s−1 in the W+W− channel for a DM particle mass of 1.5 TeV, and 2×10−26cm3s−1 in the τ+τ− channel for 1 TeV mass. For the first time, ground-based γ-ray observations have reached sufficient sensitivity to probe ⟨σv⟩ values expected from the thermal relic density for TeV DM particles
Published: 2016

9. Discovery of the hard spectrum VHE γ-ray source HESS J1641-463

Author: Abramowski, A., Böttcher, M., Davids, I.D., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Spanier, F., Sushch, I., Venter, C., and Vorster, M.
Subjects: Cosmic rays, general [gamma rays], individual objects (SNR G338.3−0.0, SNR G338.5+0.1) [ISM]
Abstract: This Letter reports the discovery of a remarkably hard spectrum source, HESS J1641–463, by the High Energy Stereoscopic System (H.E.S.S.) in the very high energy (VHE) domain. HESS J1641–463 remained unnoticed by the usual analysis techniques due to confusion with the bright nearby source HESS J1640–465. It emerged at a significance level of 8.5 standard deviations after restricting the analysis to events with energies above 4 TeV. It shows a moderate flux level of phgr(E>1 TeV) = (3.64 ± 0.44stat ± 0.73sys) × 10–13 cm–2 s–1, corresponding to 1.8% of the Crab Nebula flux above the same energy, and a hard spectrum with a photon index of Γ = 2.07 ± 0.11stat ± 0.20sys. It is a point-like source, although an extension up to a Gaussian width of σ = 3 arcmin cannot be discounted due to uncertainties in the H.E.S.S. point-spread function. The VHE γ-ray flux of HESS J1641–463 is found to be constant over the observed period when checking time binnings from the year-by-year to the 28 minute exposure timescales. HESS J1641–463 is positionally coincident with the radio supernova remnant SNR G338.5+0.1. No X-ray candidate stands out as a clear association; however, Chandra and XMM-Newton data reveal some potential weak counterparts. Various VHE γ-ray production scenarios are discussed. If the emission from HESS J1641–463 is produced by cosmic ray protons colliding with the ambient gas, then their spectrum must extend close to 1 PeV. This object may represent a source population contributing significantly to the galactic cosmic ray flux around the knee http://dx.doi.org/10.1088/2041-8205/794/1/L1 http://iopscience.iop.org/0004-637X German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRSIN2P3, and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the PolishMinistry of Science and Higher Education, the SouthAfrican Department of Science and Technology and National Research Foundation, and by the University of Namibia.
Published: 2014

10. HESS J1640−465 – an exceptionally luminous TeV γ -ray supernova remnant

Author: Abramowski, A., Casanova, S., Davids, I.D., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., and Böttcher, M.
Subjects: non-thermal [Radiation mechanisms], supernova remnants [ISM], individual objects: G338.3−0.0 [ISM]
Abstract: The results of follow-up observations of the TeV γ-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 Γ = 2.11 ± 0.09stat ± 0.10sys, and a cut-off energy of Ec=6.0+2.0−1.2 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 γ-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 WpnH ∼ 4 × 1052(d/10kpc)2 erg cm−3 http://mnras.oxfordjournals.org/ http://dx.doi.org/10.1093/mnras/stu139 German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation and the University of Namibia
Published: 2014

11. TeV ° ray observations of the young synchrotrondominated SNRs G1.9+0.3 and G330.2+1.0 with H.E.S.S

Author: Abramowski, A., Böttcher, M., Casanova, S., Davids, I.D., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., and Vorster, M.
Subjects: non-thermal [Radiation mechanisms], individual objects: SNR G330.2+1.0 [ISM], individual objects: SNR G1.9+0.3 [ISM], supernova remnants [ISM], magnetic fields [ISM], ISM [gamma-rays]
Abstract: The nonthermal nature of the Xray emission from the shelltype 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 veryhighenergy (VHE; E > 0.1 TeV) γ 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 γ 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 sixyear 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 γ 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 Ŵ = 2.5 were set at 5.6 × 10−13 cm−2 s−1 above 0.26 TeV and 3.2 × 10−12 cm−2 s−1 above 0.38 TeV, respectively. In a onezone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to BG1.9 & 12 μG for G1.9+0.3 and to BG330 & 8 μG 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 http://mnras.oxfordjournals.org/ German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRSIN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Particle Physics and Astronomy Research Council (PPARC), the IPNP of the Charles University, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia
Published: 2014

12. HESSJ1818–154, a new composite supernova remnant discovered in TeV gamma rays and X-rays

Author: Abramowski, A., Böttcher, M., Casanova, S., Davids, I.D., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., and Vorster, M.
Subjects: individual: HESS J1818-154 [supernovae], individuals: G15.4+0.1 [X-rays], general [X-rays], observational [methods], general [gamma rays]
Abstract: Composite supernova remnants (SNRs) constitute a small subclass of the remnants of massive stellar explosions where non-thermal radiation is observed from both the expanding shell-like shock front and from a pulsar wind nebula (PWN) located inside of the SNR. These systems represent a unique evolutionary phase of SNRs where observations in the radio, X-ray, and -ray regimes allow the study of the co-evolution of both these energetic phenomena. In this article, we report results from observations of the shell-type SNR G15.4+0.1 performed with the High Energy Stereoscopic System (H.E.S.S.) and XMM-Newton. A compact TeV -ray source, HESS J1818-154, located in the center and contained within the shell of G15.4+0.1 is detected by H.E.S.S. and featurs a spectrum best represented by a power-law model with a spectral index of -2:3 ± 0:3stat ± 0:2sys and an integral flux of F(>0:42 TeV) = (0:9 ± 0:3stat ± 0:2sys) x 10-12 cm-2 s-1. Furthermore, a recent observation with XMM-Newton reveals extended X-ray emission strongly peaked in the center of G15.4+0.1. The X-ray source shows indications of an energydependent morphology featuring a compact core at energies above 4 keV and more extended emission that fills the entire region within the SNR at lower energies. Together, the X-ray and VHE -ray emission provide strong evidence of a PWN located inside the shell of G15.4+0.1 and this SNR can therefore be classified as a composite based on these observations. The radio, X-ray, and -ray emission from the PWN is compatible with a one-zone leptonic model that requires a low average magnetic field inside the emission region. An unambiguous counterpart to the putative pulsar, which is thought to power the PWN, has been detected neither in radio nor in X-ray observations of G15.4+0.1 http://www.aanda.org/ http://dx.doi.org/10.1051/0004-6361/201322914 The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and the University of Namibia.
Published: 2014

13. Long-term monitoring of PKS2155-304 with ATOM and H.E.S.S.: investigation of optical/y-ray correlations in different spectral states

Author: Abramowski, A., Böttcher, M., Davids, I.D., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Spanier, F., Sushch, I., Venter, C., and Vorster, M.
Subjects: non-thermal [Radiation mechanisms], active [galaxies], black hole physics, galaxies [gamma rays], jets [galaxies], individual: PKS 2155-304 [BL Lacertae objects]
Abstract: In this paper we report on the analysis of all the available optical and very high-energy y-ray (>200 GeV) data for the BL Lac object PKS 2155-304, collected simultaneously with the ATOM and H.E.S.S. telescopes from 2007 until 2009. This study also includes X-ray (RXTE, Swift) and high-energy y-ray (Fermi-LAT) data. During the period analysed, the source was transitioning from its flaring to quiescent optical states, and was characterized by only moderate flux changes at different wavelengths on the timescales of days and months. A flattening of the optical continuum with an increasing optical flux can be noted in the collected dataset, but only occasionally and only at higher flux levels. We did not find any universal relation between the very high-energy y-ray and optical flux changes on the timescales from days and weeks up to several years. On the other hand, we noted that at higher flux levels the source can follow two distinct tracks in the optical flux–colour diagrams, which seem to be related to distinct y-ray states of the blazar. The obtained results therefore indicate a complex scaling between the optical and y-ray emission of PKS 2155-304, with different correlation patterns holding at different epochs, and a y-ray flux depending on the combination of an optical flux and colour rather than a flux alone http://dx.doi.org/10.1051/0004-6361/201424142 http://www.aanda.org/ The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia.
Published: 2014

14. Flux upper limits for 47 AGN observed with H.E.S.S. in 2004-2011

Author: Abramowski, A., Casanova, S., Davids, I.D., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., and Vorster, M.
Subjects: galaxies [Gamma rays], active [galaxies]
Abstract: Context. About 40% of the observation time of the High Energy Stereoscopic System (H.E.S.S.) is dedicated to studying active galactic nuclei (AGN), with the aim of increasing the sample of known extragalactic very-high-energy (VHE, E > 100 GeV) sources and constraining the physical processes at play in potential emitters. Aims. H.E.S.S. observations of AGN, spanning a period from April 2004 to December 2011, are investigated to constrain their -ray fluxes. Only the 47 sources without significant excess detected at the position of the targets are presented. Methods. Upper limits on VHE fluxes of the targets were computed and a search for variability was performed on the nightly time scale. Results. For 41 objects, the flux upper limits we derived are the most constraining reported to date. These constraints at VHE are compared with the flux level expected from extrapolations of Fermi-LAT measurements in the two-year catalog of AGN. The H.E.S.S. upper limits are at least a factor of two lower than the extrapolated Fermi-LAT fluxes for 11 objects. Taking into account the attenuation by the extragalactic background light reduces the tension for all but two of them, suggesting intrinsic curvature in the high-energy spectra of these two AGN. Conclusions. Compilation e orts led by current VHE instruments are of critical importance for target-selection strategies before the advent of the Cherenkov Telescope Array (CTA). http://www.aanda.org/ The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support of the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia.
Published: 2014

15. Search for extended γ-ray emission around AGN with H.E.S.S. and Fermi-LAT

Author: Abramowski, A., Böttcher, M., Davids, I.D., Krüger, P.P., Pekeur, N.W., Sushch, I., and Venter, C.
Subjects: galaxies [Gamma rays], magnetic fields [galaxies], individual: 1ES 0229+200 [BL Lacertae objects], intergalactic medium, individual: 1ES 1101-232 [BL Lacertae objects], individual: PKS 2155-304 [BL Lacertae objects]
Abstract: Context. Very-high-energy (VHE; E > 100 GeV) γ-ray emission from blazars inevitably gives rise to electron-positron pair production through the interaction of these γ-rays with the extragalactic background light (EBL). Depending on the magnetic fields in the proximity of the source, the cascade initiated from pair production can result in either an isotropic halo around an initially beamed source or a magnetically broadened cascade flux. Aims. Both extended pair-halo (PH) and magnetically broadened cascade (MBC) emission from regions surrounding the blazars 1ES 1101-232, 1ES 0229+200, and PKS 2155-304 were searched for using VHE γ-ray data taken with the High Energy Stereoscopic System (H.E.S.S.) and high-energy (HE; 100 MeV < E < 100 GeV) γ-ray data with the Fermi Large Area Telescope (LAT). Methods. By comparing the angular distributions of the reconstructed γ-ray events to the angular profiles calculated from detailed theoretical models, the presence of PH and MBC was investigated. Results. Upper limits on the extended emission around 1ES 1101-232, 1ES 0229+200, and PKS 2155-304 are found to be at a level of a few per cent of the Crab nebula flux above 1 TeV, depending on the assumed photon index of the cascade emission. Assuming strong extra-Galactic magnetic field (EGMF) values, >10−12 G, this limits the production of pair haloes developing from electromagnetic cascades. For weaker magnetic fields, in which electromagnetic cascades would result inMBCs, EGMF strengths in the range (0.3−3) ×10−15 G were excluded for PKS 2155-304 at the 99% confidence level, under the assumption of a 1Mpc coherence length. http://www.aanda.org/ The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), theMax Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the PolishMinistry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia.
Published: 2014

16. Constraints on axionlike particles with H.E.S.S. from the irregularity of the PKS 2155-304 energy spectrum

Author: Abramowski, A., Acero, F., Aharonian, F., Ait Benkhali, F., Akhperjanian, A.G., Angüner, E., Anton, G., Balenderan, S., Balzer, A., Barnacka, A., Becherini, Y., Becker Tjus, J., Bernlöhr, 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., Chrétien, 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-Ataï, 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., Förster, A., Fußling, M., Gajdus, M., Gallant, Y.A., Garrigoux, T., Gast, H., Giebels, B., Glicenstein, J.F., Göring, D., Grondin, M.-H., Grudzińska, M., Häffner, 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., Katarzyński, K., Katz, U., Kaufmann, S., Khélifi, B., Kieffer, M., Klepser, S., Klochkov, D., Kluźniak, W., Kneiske, T., Kolitzus, D., Komin, Nu., Kosack, K., Krakau, S., Krayzel, F., Krüger, 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., Marx, R., Maurin, G., Maxted, N., Mayer, M., McComb, T.J.L., Medina, M.C., Méhault, 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., de Oña Wilhelmi, E., Opitz, B., Ostrowski, M., Oya, I., Panter, M., Parsons, R.D., Paz Arribas, M., Pekeur, N.W., Pelletier, G., Perez, J., Petrucci, P.-O., Peyaud, B., Pita, S., Poon, H., Pühlhofer, 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., Schüssler, 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., Völk, H.J., Volpe, F., Vorster, M., Wagner, S.J., Wagner, P., Ward, M., Weidinger, M., Weitzel, Q., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Zacharias, M., Zajczyk, A., Zdziarski, A.A., Zech, A., Zechlin, H.-S., H.E.S.S. Collaboration, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), HESS, A., Abramowski, F., Acero, F., Aharonian, F. A., Benkhali, A. G., Akhperjanian, E., Anguener, G., Anton, S., Balenderan, A., Balzer, A., Barnacka, Y., Becherini, J. B., Tju, K., Bernloehr, E., Birsin, Bissaldi, Elisabetta, J., Biteau, C., Boisson, J., Bolmont, P., Borda, J., Brucker, F., Brun, P., Brun, T., Bulik, S., Carrigan, S., Casanova, M., Cerruti, P. M., Chadwick, R., Chalme Calvet, R. C., G., A., Cheesebrough, M., Chretien, S., Colafrancesco, G., Cologna, J., Conrad, C., Couturier, M., Dalton, M. K., Daniel, I. D., David, B., Degrange, C., Deil, P., Dewilt, H. J., Dickinson, A., Djannati Atai, W., Domainko, L. O., '., G., Dubu, K., Dutson, J., Dyk, M., Dyrda, T., Edward, K., Egbert, P., Eger, P., Espigat, C., Farnier, S., Fegan, F., Feinstein, M. V., Fernande, D., Fernandez, A., Fiasson, G., Fontaine, A., Foerster, M., Fuessling, M., Gajdu, Y. A., Gallant, T., Garrigoux, H., Gast, B., Giebel, J. F., Glicenstein, D., Goering, M. . ., H., M., Grudzinska, S., Haeffner, J. D., Hague, J., Hahn, J., Harri, G., Heinzelmann, G., Henri, G., Hermann, O., Hervet, A., Hillert, J. A., Hinton, W., Hofmann, P., Hofverberg, M., Holler, D., Horn, A., Jacholkowska, C., Jahn, M., Jamrozy, M., Janiak, F., Jankowsky, I., Jung, M. A., Kastendieck, K., Katarzynski, U., Katz, S., Kaufmann, B., Khelifi, M., Kieffer, S., Klepser, D., Klochkov, W., Kluzniak, T., Kneiske, D., Kolitzu, N., Komin, K., Kosack, S., Krakau, F., Krayzel, P. P., Krueger, H., Laffon, G., Lamanna, J., Lefaucheur, M., Lemoine Goumard, J. . ., P., D., Lennarz, T., Lohse, A., Lopatin, C. . ., C., V., Marandon, A., Marcowith, R., Marx, G., Maurin, N., Maxted, M., Mayer, T. J., L., M. C., Medina, J., Mehault, U., Menzler, M., Meyer, R., Moderski, M., Mohamed, E., Moulin, T., Murach, C. L., Naumann, M. d., Nauroi, D., Nedbal, J., Niemiec, S. J., Nolan, L., Oake, S., Ohm, E. d., Ona, B., Opitz, M., Ostrowski, I., Oya, M., Panter, R. D., Parson, M. P., Arriba, N. W., Pekeur, G., Pelletier, J., Perez, P. . ., O., B., Peyaud, S., Pita, H., Poon, G., Puehlhofer, M., Punch, A., Quirrenbach, S., Raab, M., Raue, A., Reimer, O., Reimer, M., Renaud, R. d., Lo, F., Rieger, L., Rob, S., Rosier Lee, G., Rowell, B., Rudak, C. B., Rulten, V., Sahakian, D. A., Sanchez, A., Santangelo, R., Schlickeiser, F., Schuessler, A., Schulz, U., Schwanke, S., Schwarzburg, S., Schwemmer, H., Sol, G., Spengler, F., Spie, L., Stawarz, R., Steenkamp, C., Stegmann, F., Stinzing, K., Stycz, I., Sushch, A., Szostek, R., Terrier, M., Tluczykont, C., Trichard, K., Valeriu, C. v., Eldik, G., Vasileiadi, C., Venter, A., Viana, P., Vincent, H. J., Voelk, F., Volpe, M., Vorster, S. J., Wagner, P., Wagner, M., Ward, M., Weidinger, Q., Weitzel, R., White, A., Wierzcholska, P., Willmann, A., Woernlein, D., Wouter, M., Zacharia, A., Zajczyk, A. A., Zdziarski, A., Zech, H. . ., S., The H.E.S.S. Collaboration, Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), and Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules)
Subjects: Electromagnetic field, Nuclear and High Energy Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Física de Partículas y Campos, 01 natural sciences, 7. Clean energy, Standard Model, Physics::Geophysics, High Energy Physics - Experiment, purl.org/becyt/ford/1 [https], High Energy Physics - Experiment (hep-ex), 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], ddc:530, gamma-ray, 010303 astronomy & astrophysics, Boson, Physics, PKS 2155-304, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma rays, Gamma ray, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Axionlike particles, Pseudoscalar, Astrophysics - High Energy Astrophysical Phenomena, Gamma emission, CIENCIAS NATURALES Y EXACTAS, BL Lac object, H.E.S.S, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Axionlike particles (ALPs) are hypothetical light (sub-eV) bosons predicted in some extensions of the Standard Model of particle physics. In astrophysical environments comprising high-energy gamma rays and turbulent magnetic fields, the existence of ALPs can modify the energy spectrum of the gamma rays for a sufficiently large coupling between ALPs and photons. This modification would take the form of an irregular behavior of the energy spectrum in a limited energy range. Data from the H.E.S.S. observations of the distant BL Lac object PKS 2155-304 (z = 0.116) are used to derive upper limits at the 95% C.L. on the strength of the ALP coupling to photons, $g_{\gamma a} < 2.1\times 10^{-11}$ GeV$^{-1}$ for an ALP mass between 15 neV and 60 neV. The results depend on assumptions on the magnetic field around the source, which are chosen conservatively. The derived constraints apply to both light pseudoscalar and scalar bosons that couple to the electromagnetic field., Comment: 13 pages, 7 figures, to appear in Phys.Rev.D
Published: 2013
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17. Search for very-high-energy γ-ray emission from galactic globular clusters with H.E.S.S

Author: Abramowski, S., Casanova, S., Krüger, P.P, Pekeur, N.W., Sheidaei, F., and Venter, C.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, general [Globular clusters], non-thermal [radiation mechanisms], general [pulsars], general [gamma rays], Astrophysics::Galaxy Astrophysics
Abstract: Context: Globular clusters (GCs) are established emitters of high-energy (HE, 100 MeV < E < 100 GeV) γ-ray radiation which could originate from the cumulative emission of the numerous millisecond pulsars (msPSRs) in the clusters’ cores or from inverse Compton (IC) scattering of relativistic leptons accelerated in the GC environment. These stellar clusters could also constitute a new class of sources in the very-high-energy (VHE, E > 100 GeV) γ-ray regime, judging from the recent detection of a signal from the direction of Terzan 5 with the H.E.S.S. telescope array. Aims: To search for VHE γ-ray sources associated with other GCs, and to put constraints on leptonic emission models, we systematically analyzed the observations towards 15 GCs taken with the H.E.S.S. array of imaging atmospheric Cherenkov telescopes. Methods: We searched for point-like and extended VHE γ-ray emission from each GC in our sample and also performed a stacking analysis combining the data from all GCs to investigate the hypothesis of a population of faint emitters. Assuming IC emission as the origin of the VHE γ-ray signal from the direction of Terzan 5, we calculated the expected γ-ray flux from each of the 15 GCs, based on their number of millisecond pulsars, their optical brightness and the energy density of background photon fields. Results: We did not detect significant VHE γ-ray emission from any of the 15 GCs in either of the two analyses. Given the uncertainties related to the parameter determinations, the obtained flux upper limits allow to rule out the simple IC/msPSR scaling model for NGC 6388 and NGC 7078. The upper limits derived from the stacking analyses are factors between 2 and 50 below the flux predicted by the simple leptonic scaling model, depending on the assumed source extent and the dominant target photon fields. Therefore, Terzan 5 still remains exceptional among all GCs, as the VHE γ-ray emission either arises from extra-ordinarily efficient leptonic processes, or from a recent catastrophic event, or is even unrelated to the GC itself. http://dx.doi.org/10.1051/0004-6361/201220719 http://www.aanda.org/articles/aa/pdf/2013/03/aa20719-12.pdf
Published: 2013

18. H.E.S.S. reveals a lack of TeV emission from the supernova remnant Puppis A

Author: 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 12006653 - Venter, Christo, 12792322 - Vorster, Michael Johannes, Abramowski, A., Böttcher, M., Davids, I.D., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Spanier, F., Sushch, I., Venter, C., Vorster, M., H.E.S.S. Collaboration, 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 12006653 - Venter, Christo, 12792322 - Vorster, Michael Johannes, Abramowski, A., Böttcher, M., Davids, I.D., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Spanier, F., Sushch, I., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: Context: Puppis A is an interesting ~4 kyr-old supernova remnant (SNR) that shows strong evidence of interaction between the forward shock and a molecular cloud. It has been studied in detail from radio frequencies to high-energy (HE, 0.1−100 GeV) γ-rays. An analysis of the Fermi-LAT data has shown extended HE γ-ray emission with a 0.2−100 GeV spectrum exhibiting no significant deviation from a power law, unlike most of the GeV-emitting SNRs known to be interacting with molecular clouds. This makes it a promising target for imaging atmospheric Cherenkov telescopes (IACTs) to probe the γ-ray emission above 100 GeV. Aims: Very-high-energy (VHE, E ≥ 0.1 TeV) γ-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (H.E.S.S.). Methods: Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the direction and energy of the incident γ-rays in order to produce sky images and source spectra. The profile likelihood method is applied to find constraints on the existence of a potential break or cutoff in the photon spectrum. Results: The analysis of the H.E.S.S. data does not reveal any significant emission towards Puppis A. The derived upper limits on the differential photon flux imply that its broadband γ-ray spectrum must exhibit a spectral break or cutoff. By combining Fermi-LAT and H.E.S.S. measurements, the 99% confidence-level upper limits on such a cutoff are found to be 450 and 280 GeV, assuming a power law with a simple exponential and a sub-exponential cutoff, respectively. It is concluded that none of the standard limitations (age, size, radiative losses) on the particle acceleration mechanism, assumed to be continuing at present, can explain the lack of VHE signal. The scenario in which particle acceleration has ceased some time ago is considered as an alternative explanation. The HE/VHE spectrum of Puppis A could then exhibit a break of non-radiative origin (as observed
Published: 2015

19. Discovery of variable VHE γ-ray emission from the binary system 1FGL J1018.6-5856

Author: 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 20126999 - Seyffert, Albertus Stefanus, Abramowski, A., Böttcher, M., Davids, I.D., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Seyffert, A.S., Spanier, F., Sushch, I., Van der Walt, D.J., Venter, C., H.E.S.S. Collaboration, 24420530 - Böttcher, Markus, 13146629 - Davids, Isak Delberth, 24790052 - Ivascenko, Alex, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 25161814 - Spanier, Felix Alexander, 24922986 - Sushch, Iurii, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 20126999 - Seyffert, Albertus Stefanus, Abramowski, A., Böttcher, M., Davids, I.D., Ivascenko, A., Krüger, P.P., Pekeur, N.W., Seyffert, A.S., Spanier, F., Sushch, I., Van der Walt, D.J., Venter, C., and H.E.S.S. Collaboration
Abstract: Re-observations with the HESS telescope array of the very high-energy (VHE) source HESS J1018–589 A that is coincident with the Fermi-LAT γ-ray binary 1FGL J1018.6–5856 have resulted in a source detection significance of more than 9σ and the detection of variability (χ2/ν of 238.3/155) in the emitted γ-ray flux. This variability confirms the association of HESS J1018–589 A with the high-energy γ-ray binary detected by Fermi-LAT and also confirms the point-like source as a new VHE binary system. The spectrum of HESS J1018–589 A is best fit with a power-law function with photon index Γ = 2.20 ± 0.14stat ± 0.2sys. Emission is detected up to ~20 TeV. The mean differential flux level is (2.9 ± 0.4) × 10-13 TeV-1 cm-2 s-1 at 1 TeV, equivalent to ~1% of the flux from the Crab Nebula at the same energy. Variability is clearly detected in the night-by-night light curve. When folded on the orbital period of 16.58 days, the rebinned light curve peaks in phase with the observed X-ray and high-energy phaseograms. The fit of the HESS phaseogram to a constant flux provides evidence of periodicity at the level of Nσ> 3σ. The shape of the VHE phaseogram and measured spectrum suggest a low-inclination, low-eccentricity system with amodest impact from VHE γ-ray absorption due to pair production (τ ≲ 1 at 300 GeV)
Published: 2015

20. Search for TeV Gamma-ray emission from GRB 100621A, an extremely bright GRB in X-rays, with H.E.S.S.

Author: 12006653 - Venter, Christo, 22050574 - Pekeur, Nicolette Whilna, 12792322 - Vorster, Michael Johannes, 24922986 - Sushch, Iurii, 11749903 - Krüger, Petrus Paulus, 23909196 - Casanova, Sabrina, 24420530 - Böttcher, Markus, Abramowski, A., Böttcher, M., Casanova, S., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., H.E.S.S. Collaboration, 12006653 - Venter, Christo, 22050574 - Pekeur, Nicolette Whilna, 12792322 - Vorster, Michael Johannes, 24922986 - Sushch, Iurii, 11749903 - Krüger, Petrus Paulus, 23909196 - Casanova, Sabrina, 24420530 - Böttcher, Markus, Abramowski, A., Böttcher, M., Casanova, S., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the 0:3–10 keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, >100 GeV) regime. Due to its relatively small redshift of z ~ 0:5, the favourable position in the southern sky and the relatively short follow-up time (<700 s after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the H.E.S.S. instrument. The analysis of the H.E.S.S. data shows no indication of emission and yields an integral flux upper limit above ~380 GeV of 4:2X10-12 cm-2 s-1 (95% confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the H.E.S.S. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays
Published: 2014

21. Discovery of high and very high-energy emission from the BL Lacertae object SHBL J001355.9-185406

Author: 22050574 - Pekeur, Nicolette Whilna, 12006653 - Venter, Christo, 12792322 - Vorster, Michael Johannes, 24922986 - Sushch, Iurii, 11749903 - Krüger, Petrus Paulus, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., H.E.S.S. Collaboration, 22050574 - Pekeur, Nicolette Whilna, 12006653 - Venter, Christo, 12792322 - Vorster, Michael Johannes, 24922986 - Sushch, Iurii, 11749903 - Krüger, Petrus Paulus, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: The detection of the high-frequency peaked BL Lac object (HBL) SHBL J001355.9–185406 (z = 0.095) at high (HE; 100 MeV < E < 300 GeV) and very high-energy (VHE; E > 100 GeV) with the Fermi Large Area Telescope (LAT) and the High Energy Stereoscopic System (H.E.S.S.) is reported. Dedicated observations were performed with the H.E.S.S. telescopes, leading to a detection at the 5.5σ significance level. The measured flux above 310 GeV is (8.3 ± 1.7stat ± 1.7sys) × 10−13 photons cm−2 s−1 (about 0.6% of that of the Crab Nebula), and the power-law spectrum has a photon index of Γ = 3.4 ± 0.5stat ± 0.2sys. Using 3.5 years of publicly available Fermi-LAT data, a faint counterpart has been detected in the LAT data at the 5.5σ significance level, with an integrated flux above 300 MeV of (9.3 ± 3.4stat ± 0.8sys) × 10−10 photons cm−2 s−1 and a photon index of Γ = 1.96 ± 0.20stat ± 0.08sys. X-ray observations with Swift-XRT allow the synchrotron peak energy in νFν representation to be located at ∼1.0 keV. The broadband spectral energy distribution is modelled with a one-zone synchrotron self-Compton (SSC) model and the optical data by a black-body emission describing the thermal emission of the host galaxy. The derived parameters are typical of HBLs detected at VHE, with a particle-dominated jet.
Published: 2013

22. H.E.S.S. observations of the binary system PSR B1259-63/LS 2883 around the 2010/2011 periastron passage

Author: 12006653 - Venter, Christo, 11005394 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 23909196 - Casanova, Sabrina, 22164405 - Sheidaei, Farzaneh, 12792322 - Vorster, Michael Johannes, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., H.E.S.S. Collaboration, 12006653 - Venter, Christo, 11005394 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 23909196 - Casanova, Sabrina, 22164405 - Sheidaei, Farzaneh, 12792322 - Vorster, Michael Johannes, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: Aims. We present very high energy (VHE; E > 100 GeV) data from the γ-ray binary system PSR B1259-63/LS 2883 taken around its periastron passage on 15th of December 2010 with the High Energy Stereoscopic System (H.E.S.S.) of Cherenkov Telescopes. We aim to search for a possible TeV counterpart of the GeV flare detected by the Fermi LAT. In addition, we aim to study the current periastron passage in the context of previous observations taken at similar orbital phases, testing the repetitive behaviour of the source. Methods. Observations at VHEs were conducted with H.E.S.S. from 9th to 16th of January 2011. The total dataset amounts to ~6 h of observing time. The data taken around the 2004 periastron passage were also re-analysed with the current analysis techniques in order to extend the energy spectrum above 3 TeV to fully compare observation results from 2004 and 2011. Results. The source is detected in the 2011 data at a significance level of 11.5σ revealing an averaged integral flux above 1 TeV of (1.01 ± 0.18stat ± 0.20sys) × 10-12 cm-2 s-1. The differential energy spectrum follows a power-law shape with a spectral index Γ = 2.92 ± 0.30stat ± 0.20sys and a flux normalisation at 1 TeV of N0 = (1.95 ± 0.32stat ± 0.39sys) × 10-12 TeV-1 cm-2 s-1. The measured light curve does not show any evidence for variability of the source on the daily scale. The re-analysis of the 2004 data yields results compatible with the published ones. The differential energy spectrum measured up to ~10 TeV is consistent with a power law with a spectral index Γ = 2.81 ± 0.10stat ± 0.20sys and a flux normalisation at 1 TeV of N0 = (1.29 ± 0.08stat ± 0.26sys) × 10-12 TeV-1 cm-2 s-1. Conclusions. The measured integral flux and the spectral shape of the 2011 data are compatible with the results obtained around previous periastron passages. The absence of variability in the H.E.S.S. data indicates that the GeV flare observed by Fermi LAT in the time period covered also by H.E.S.S. observations o
Published: 2013

23. Discovery of very high energy γ-ray emission from the BL Lacertae object PKS 0301-243 with H.E.S.S.

Author: 12006653 - Venter, Christo, 11005394 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 24420530 - Böttcher, Markus, 23909196 - Casanova, Sabrina, 24922986 - Sushch, Iurii, 12792322 - Vorster, Michael Johannes, Abramowski, A., Böttcher, M., Casanova, S., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., H.E.S.S. Collaboration, 12006653 - Venter, Christo, 11005394 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 24420530 - Böttcher, Markus, 23909196 - Casanova, Sabrina, 24922986 - Sushch, Iurii, 12792322 - Vorster, Michael Johannes, Abramowski, A., Böttcher, M., Casanova, S., Krüger, P.P., Pekeur, N.W., Sushch, I., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: The active galactic nucleus PKS 0301−243 (z = 0.266) is a high-synchrotron-peaked BL Lac object that is detected at high energies (HE, 100 MeV < E < 100 GeV) by Fermi/LAT. This paper reports on the discovery of PKS 0301−243 at very high energies (E > 100 GeV) by the High Energy Stereoscopic System (H.E.S.S.) from observations between September 2009 and December 2011 for a total live time of 34.9 h. Gamma rays above 200 GeV are detected at a significance of 9.4σ. A hint of variability at the 2.5σ level is found. An integral flux I(E > 200GeV) = (3.3 ± 1.1stat ± 0.7syst) × 10−12 ph cm−2 s−1 and a photon index Γ = 4.6 ± 0.7stat ± 0.2syst are measured. Multi-wavelength light curves in HE, X-ray and optical bands show strong variability, and a minimal variability timescale of eight days is estimated from the optical light curve. A single-zone leptonic synchrotron self-Compton scenario satisfactorily reproduces the multi-wavelength data. In this model, the emitting region is out of equipartition and the jet is particle dominated. Because of its high redshift compared to other sources observed at TeV energies, the very high energy emission from PKS 0301−243 is attenuated by the extragalactic background light (EBL) and the measured spectrum is used to derive an upper limit on the opacity of the EBL.
Published: 2013

24. Discovery of TeV y-ray emission from PKS 0447-439 and derivation of an upper limit on its redshift

Author: 12006653 - Venter, Christo, 11005394 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 12792322 - Vorster, Michael Johannes, 22164405 - Sheidaei, Farzaneh, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., H.E.S.S. Collaboration, 12006653 - Venter, Christo, 11005394 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 12792322 - Vorster, Michael Johannes, 22164405 - Sheidaei, Farzaneh, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: Very high-energy γ-ray emission from PKS 0447−439 was detected with the H.E.S.S. Cherenkov telescope array in December 2009. This blazar is one of the brightest extragalactic objects in the Fermi bright source list and has a hard spectrum in the MeV to GeV range. In the TeV range, a photon index of 3.89 ± 0.37 (stat) ±0.22 (sys) and a flux normalisation at 1 TeV, Φ1 TeV = (3.5 ± 1.1(stat) ± 0.9(sys)) × 10−13 cm−2 s−1 TeV−1 were found. The detection with H.E.S.S. triggered observations in the X-ray band with the Swift and RXTE telescopes. Simultaneous UV and optical data from Swift UVOT and data from the optical telescopes ATOM and ROTSE are also available. The spectrum and light curve measured with H.E.S.S. are presented and compared to the multi-wavelength data at lower energies. A rapid flare is seen in the Swift XRT and RXTE data, together with a flux variation in the UV band, at a time scale of the order of one day. A firm upper limit of z < 0.59 on the redshift of PKS 0447−439 is derived from the combined Fermi-LAT and H.E.S.S. data, given the assumptions that there is no upturn in the intrinsic spectrum above the Fermi-LAT energy range and that absorption on the extragalactic background light (EBL) is not weaker than the lower limit provided by current models. The spectral energy distribution is well described by a simple one-zone synchrotron self-Compton scenario, if the redshift of the source is less than z _ 0.4..
Published: 2013

25. H.E.S.S. discovery of VHE y-rays from the quasar PKS 1510-089

Author: 11005394 - Krüger, Petrus Paulus, 12006653 - Venter, Christo, 22050574 - Pekeur, Nicolette Whilna, 12792322 - Vorster, Michael Johannes, 22164405 - Sheidaei, Farzaneh, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., H.E.S.S. Collaboration, 11005394 - Krüger, Petrus Paulus, 12006653 - Venter, Christo, 22050574 - Pekeur, Nicolette Whilna, 12792322 - Vorster, Michael Johannes, 22164405 - Sheidaei, Farzaneh, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: The quasar PKS 1510-089 (z = 0.361) was observed with the H.E.S.S. array of imaging atmospheric Cherenkov telescopes during high states in the optical and GeV bands, to search for very high energy (VHE, defined as E ≥ 0.1 TeV) emission. VHE γ-rays were detected with a statistical significance of 9.2 standard deviations in 15.8 h of H.E.S.S. data taken during March and April 2009. A VHE integral flux of I(0.15 TeV < E < 1.0TeV) = (1.0 ± 0.2stat ± 0.2sys) × 10−11 cm−2 s−1 is measured. The best-fit power law to the VHE data has a photon index of Γ = 5.4 ± 0.7stat ± 0.3sys. The GeV and optical light curves show pronounced variability during the period of H.E.S.S. observations. However, there is insufficient evidence to claim statistically significant variability in the VHE data. Because of its relatively high redshift, the VHE flux from PKS 1510−089 should suffer considerable attenuation in the intergalactic space due to the extragalactic background light (EBL). Hence, the measured γ-ray spectrum is used to derive upper limits on the opacity due to EBL, which are found to be comparable with the previously derived limits from relatively-nearby BL Lac objects. Unlike typical VHE-detected blazars where the broadband spectrum is dominated by nonthermal radiation at all wavelengths, the quasar PKS 1510−089 has a bright thermal component in the optical to UV frequency band. Among all VHE detected blazars, PKS 1510−089 has the most luminous broad line region. The detection of VHE emission from this quasar indicates a low level of γ − γ absorption on the internal optical to UV photon field.
Published: 2013

26. Search for photon line-like signatures from dark matter annihilations with H.E.S.S

Author: 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 12006653 - Venter, Christo, 22164405 - Sheidaei, Farzaneh, 12792322 - Vorster, Michael Johannes, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., H.E.S.S. Collaboration, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 12006653 - Venter, Christo, 22164405 - Sheidaei, Farzaneh, 12792322 - Vorster, Michael Johannes, 23909196 - Casanova, Sabrina, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: Gamma-ray line signatures can be expected in the very-high-energy (VHE; E_\gamma > 100 GeV) domain due to self-annihilation or decay of dark matter (DM) particles in space. Such a signal would be readily distinguishable from astrophysical \gamma-ray sources that in most cases produce continuous spectra which span over several orders of magnitude in energy. Using data collected with the H.E.S.S. \gamma-ray instrument, upper limits on line-like emission are obtained in the energy range between ~500 GeV and ~25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. No statistically significant signal could be found. For monochromatic \gamma-ray line emission, flux limits of (2x10^-7 - 2x10^-5) m^-2 s^-1 sr^-1 and (1x10^-8 - 2x10^-6) m^-2 s^-1 sr^-1 are obtained for the central part of the Milky Way halo and extragalactic observations, respectively. For a DM particle mass of 1 TeV, limits on the velocity-averaged DM annihilation cross section < \sigma v >(\chi\chi -> \gamma\gamma) reach ~10^-27 cm^3 s^-1, based on the Einasto parametrization of the Galactic DM halo density profile
Published: 2013

27. Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.

Author: 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 12006653 - Venter, Christo, 23909196 - Casanova, Sabrina, 22164405 - Sheidaei, Farzaneh, 12792322 - Vorster, Michael Johannes, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., H.E.S.S. Collaboration, 11749903 - Krüger, Petrus Paulus, 22050574 - Pekeur, Nicolette Whilna, 12006653 - Venter, Christo, 23909196 - Casanova, Sabrina, 22164405 - Sheidaei, Farzaneh, 12792322 - Vorster, Michael Johannes, Abramowski, A., Casanova, S., Krüger, P.P., Pekeur, N.W., Sheidaei, F., Venter, C., Vorster, M., and H.E.S.S. Collaboration
Abstract: Context. Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae, and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) γ-ray emission (HESS J0835−455) was discovered using the H.E.S.S. experiment in 2004. The VHE γ-ray emission was found to be coincident with a region of X-ray emission discovered with ROSAT above 1.5 keV (the so-called Vela X cocoon): a filamentary structure extending southwest from the pulsar to the centre of Vela X. Aims. A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the non-thermal emission from the Vela X region at TeV energies and to investigate its spectral properties. Methods. To increase the sensitivity to the faint γ-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of γ-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of γ-ray sources but with comparable observation conditions. Results. The γ-ray surface brightness over the large Vela X region reveals that the detection of non-thermal VHE γ-ray emission from the PWN HESS J0835−455 is statistically significant over a region of radius 1.2° around the position α = 08h35m00s, δ = −45°36′00′′ (J2000). The Vela X region exhibits almost uniform γ-ray spectra over its full extent: the differential energy spectrum can be described by a power-law function with a hard spectral index Γ = 1.32 ± 0.06stat ± 0.12sys and an exponential cutoff at an energy of (14.0 ± 1.6stat ± 2.6sys) TeV. Compared to the previous H.E.S.S. observations of Vela X the new analysis conf
Published: 2012

28. Cheap 0.36 dB NF broadband multipath LNA

Author: Krüger, P.P., primary
Published: 2012
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29. Reflections of Eden in Deuteronomy’s fourth commandment

Author: Haynes, M.B., Krüger, P.P., Prof, Collins, C.J., Prof, 11005394 - Krüger, Petrus Paulus (Supervisor), Krüger, P.P., and Collins, C.J.
Subjects: Discourse Analysis, Literary Analysis, Creation, Rest, Deuteronomy 5, Fourth Commandment, Promised Land, Textlinguistics, Sabbath, Exodus 20
Abstract: PhD (Old Testament), North-West University, Potchefstroom Campus This study argues that, just as in Exodus 20, the Sabbath commandment articulated in Deuteronomy 5 is grounded in creation. In doing so it also attempts to bring further insight into the overall purpose for which the Sabbath commandment was given to Israel. The study begins by discussing the ways in which authors use text–knowledge (or cognitive) frames to signal meaning to an audience—both in terms of the subject under discussion and the shared presuppositions concerning the norms of that subject. It then discusses the manner in which readers analyse complex texts by binding various pieces of information gleaned from the text into a pre-existing conceptual model. Next, it articulates a methodology for addressing hortatory texts that combines discourse analysis with various tools from literary study. This methodology recognises the text–knowledge frames used by authors and the manner in which readers go about deciphering challenging texts. The study then traces the structure of the Sabbath commandment and places it within the context of the Decalogue and Deuteronomy as a whole. The use of discourse analysis clarifies that the Sabbath day requires two things of Israel: (1) a cessation from the labour of one’s normal occupation and (2) remembering what YHWH had done in redeeming them from Egypt. Both are required to properly sanctify the day. Additionally, the Sabbath commandment is the rhetorical high point of the Decalogue; it is the only one which has commandments directly relating to self, God, and neighbour. The study suggests that the various additions and changes that are made within the Decalogue are due to the changed circumstances since the laws were given at Sinai and the wilderness generation’s passing. Moses goes to great lengths to affirm that he is still covenant mediator and that these words are every bit as binding as the first words given at Sinai. The study argues that the Decalogue forms the starting point from which the stipulations of Deuteronomy begin. Each of the commandments is expanded upon in one way or another. Five Sabbath expansions are noted in laws relating to tithing, the Sabbatical Year, the Sabbatical release of the debt-servant, the law of the firstborn male, and the festival calendar. Each of these takes the notion of rest articulated in the Sabbath commandment and applies it to Israel in various ways beyond the seventh day of the week. Next, Deuteronomy is set within the context of the Pentateuch as a whole. It is argued that the text–knowledge frames that Deuteronomy uses presuppose familiarity with the other books of the Pentateuch and the laws described therein. The themes of rest, Israel as a reflection of the garden of Eden, and the Sabbath idea are traced throughout the Pentateuch. It is argued that Adam and Eve’s labour in the garden of Eden was a “restful” labour that was subsequently destroyed by their disobedience in Genesis 3. Since that time, humanity has longed for rest, and, in various ways, the Pentateuch describes how God is intent on bringing humanity back to rest. This is done primarily through Israel, whose life in the promised land was intended to reflect life in the garden of Eden. The Sabbath day is thus to be enjoyed by them as a taste of what life was intended to be in the garden. Doctoral
Published: 2018

30. Kinderopvoeding in die boek Deuteronomium : 'n eksegetiese en openbaringshistoriese studie

Author: Jooste, Christiaan, Krüger, P.P., and 10103449 - Krüger, Petrus Paulus (Supervisor)
Subjects: Deuteronomy 6, Childrearing, Vassal Treaties, Sjema, Deuteronomy, Children, Covenant, Covenant Teaching
Abstract: PhD (Old Testament), North-West University, Potchefstroom Campus At the end of Israel’s forty year sojum in the wilderness they were at the point of taking possession of the promised land. In the book of Deuteronomy Moses addresses the people one last time, with the specific purpose to renew the covenant the Lord has made with them at Mount Horeb. The children are not overlooked in this speech. Parents are called to live in obedience to the demands of the covenant and to teach it to their children through repetition and inculcation. In this study, the research is focussing, through exegetical investigation, on the Old Testament Theological aspects and principles derived from Deuteronomy with regard to the upbringing and covenant-teaching of children. Chapter two examines the state of research on education and upbringing of children in Deuteronomy. However, the exegetical studies were done long ago and studies which include the upbringing of children in Deuteronomy in its entirety is lacking. The investigation also reflected on a possible interdependence between the vassal treaties of the Ancient Near East and Deuteronomy with regard to the upbringing and education of children. Although treaties mention the conveyance of covenant provisions to the next generation, there is no instruction to teach. Further research must determine whether a pedagogical element is present in the treaties, especially in the historical prologue. The historical background of Deuteronomy, the family and the upbringing and education of children are examined in chapter three. Moses as the implied author and Israel as the implied audience is the starting point of the exegesis. The purpose of Deuteronomy is related to the concept of תּוֹרָה and intend the renewal of the covenant. The covenant and its terms should be passed on to future generations within a patriarchal society. In this, with the support of the mother, the father plays a leading role. Since the command to teach their children, explicated in Deuteronomy 6:1-25, this passage in Scripture had been examined exegetically in chapter four. The exegesis confirms, as stated in Deuteronomy 6, the principle of covenant teaching that the Lord is an unique and only Lord (Deut.6:4). The Israelites have to internalise His commandments and decrees which results in obedience, love and reverence for Him and consequently externalise it in their daily conduct. It is the responsibility of the parents to impart this principle to the succeeding generations through communication, repetition and inculcation. Covenant teaching is thus teaching trough own conduct, which starts with the parents’ own obedience. The principles revealed in Deuteronomy 6 are supported by various passages in Deuteronomy (Deut. 4:9-10, 11:18-21, 31:9-13) and other passages in the Old Testament (Ps. 78:1-8, Ex. 12:26-28, 13:14-16, Josh. 4:21-24, Prov. 3:1-12). In chapter five the secondary passages in Deuteronomy, and in chapter six the other passages in the Old Testament are interpreted. The principles contained in Deuteronomy 6 are repeated in different contexts throughout the book and highlights the importance of future observance of the covenant terms. The research found that the principles given in the primary section are repeated in new contexts, expanded and supplemented in other parts of Scripture. The theological nature and implications of covenant teaching in this research are formulated in chapter seven. * The unity and uniqueness of the Lord, as revealed to His people, is the basis for covenant upbringing and teaching. * The upbringing and teaching don’t only have an effect on the children of these parents but also on the future generations in the Promised Land. * Firstly the parent and child need to internalise the covenant (write it on their hearts) and subsequently externalise it through conversation and living in obedience, privately and in society. * There is a move from the concrete to the abstract in upbringing and teaching. One where children will ask about the meaning of concrete actions, ceremonies and memorials, and through historical events will be taught and lead by parents to the abstract such as faith, love and reverence for the Lord. * Although the upbringing and teaching of children are primarily the responsibility of parents, the covenant community is not excluded from this responsibility. Doctoral
Published: 2021

31. Conceptual metaphor as exegetical tool in the Psalter: a case study of Psalm 74

Author: Niemand, Johannes Maguldies Gerhardus, Maré, L.P., Krüger, P.P., 22685014 - Maré, Leonard Philippus (Supervisor), and 10103449 - Krüger, Petrus Paulus (Supervisor)
Subjects: Biblical Hebrew poetic interpretation, Dead metaphor theory, Psalm 74, Figurative language, Psychological trauma, Metaphor, Conceptual metaphor theory, Communal lament, Deliberative metaphor, Biblical exegesis, Trauma theory and biblical studies, Babylonian exile, Cultural trauma
Abstract: PhD (Biblical Studies), North-West University, Potchefstroom Campus In their seminal work, Metaphors We Live By (1980), Lakoff and Johnson make a strong case that metaphors are much more than poetic embellishment. Human beings’ very cognition and conceptualisation depend on the metaphor phenomenon. Without it, we would not be able to think abstractly, engage in the complex interaction of diverse knowledge systems, or think of something in terms of something else. In other words, metaphor is foundational to our very meaning making processes. This dissertation seeks to explore the application of conceptual metaphor theory as proposed by Lakoff and Johnson in the exegesis of Psalm 74. Since no exegetical model using conceptual metaphor theory as a point of departure existed during the writing of this dissertation, a workable model was first extracted from recent developments in the theory of metaphor. This model was applied in exegesis of Psalm 74, a communal lament. The model proved to be sufficiently productive in aiding exegesis and using the model’s various levels of interpretation resulted in a very thorough reading of the Hebrew text of Psalm 74. These levels of interpretation are: 1) poetic metaphors, 2) conceptual metaphors, 3) image schemata and, 4) idealised cognitive models. In conclusion, the use of conceptual metaphor theory highlighted the possible use of Psalm 74 and the other psalms of Asaph in aiding the post-exilic Israelite community (communities) in reorienting their worldview while dealing with the national trauma of the Babylonian exile. Modern trauma theory was particularly helpful in understanding the possible use of the ancient texts during and after the Babylonian exile. Doctoral
Published: 2020

32. A polarized fast radio burst at low Galactic latitude

Author: M. de Jong, Michael Punch, Mansi M. Kasliwal, T. A. Pritchard, S. Galatà, K. Egberts, S. Loucatos, C. Tönnis, S. Öttl, G. Pelletier, Ivan Felis, Mitchell B. Mickaliger, Jacek Niemiec, G. Cologna, Robert Wagner, A. Gleixner, C. Racca, P. J. Meintjes, Thomas Lohse, Jamie Farnes, Olaf Reimer, F. Ait Benkhali, L. O'c. Drury, P. de Wilt, R. Chalme-Calvet, I. Salvadori, Kay Graf, Karel Melis, A. Vizzoca, I. El Bojaddaini, G. Heinzelmann, C. B. Rulten, Bruny Baret, Heinrich J. Völk, Manami Sasaki, S. Schwemmer, Q. Piel, Andrea Santangelo, Thomas Vuillaume, Guillaume Dubus, A. Jacholkowska, Simon Johnston, J. Chevalier, Julien Lefaucheur, M. Renaud, K. Dutson, F. Spies, D. Dornic, C. Farnier, A. Trovato, E. Leser, Tanya Edwards, Jean-Pierre Macquart, L. Tibaldo, Thomas Murach, C. Lachaud, A. Marinelli, I. D. Davids, Ramin Marx, M. Panter, U. Katz, Silvia Celli, Timothée Grégoire, D. Kiessling, Antoine Kouchner, Marco Padovani, Matthias Kadler, Francois Brun, A. Ivascenko, E. D. Barr, C. W. James, Daniela Hadasch, C. Perrina, Maria Tselengidou, G. Hermann, Regis Terrier, D. Klochkov, Johan Bregeon, W. Kluzniak, M. Kieffer, P. Vincent, Y. Cui, S. Bernhard, L. Stawarz, A. Ziegler, M.C. Bouwhuis, C. Romoli, Dieter Horns, Mateusz Janiak, B. van Soelen, B. Rudak, T. Michael, Nachiketa Chakraborty, Caterina Tiburzi, N. Zywucka, Alison Mitchell, B. Degrange, Santiago Pita, R. Blackwell, Reinhard Schlickeiser, I. Kreykenbohm, Annarita Margiotta, Jutta Schnabel, M. Jingo, R. J. White, Thomas Eberl, H. Laffon, M. Lotze, Christo Venter, Tommaso Chiarusi, M. Anghinolfi, Maura McLaughlin, Zorawar Wadiasingh, B. Condon, D. A. Sanchez, M. Mayer, V. Lefranc, H. Abdalla, M. A. Kastendieck, S. Bourret, G. Vasileiadis, Iryna Lypova, Yvonne Becherini, G. Illuminati, Clemens Hoischen, A. A. Zdziarski, S. Geisselsoder, I. Shilon, E. O. Angüner, Domenico Tiziani, K. Kosack, Konrad Bernlöhr, A. Enzenhöfer, R. Moderski, V. S. Dhillon, Evan Keane, G. Lamanna, Riaan Steenkamp, Matthew Bailes, M. Füssling, A. Zech, V. Van Elewyck, M. Taiuti, J. Decock, Ullrich Schwanke, Monica Barnard, D. Zaborov, O. Kalekin, M. Circella, Y. A. Gallant, N. D. R. Bhat, A. Creusot, Victor Zabalza, Th. Stolarczyk, B. Vallage, N. Maxted, Dominique Lefèvre, L. Dirson, E. Petroff, D. Jankowsky, M.-H. Grondin, C. Perennes, Markus Böttcher, E. Nezri, A. G. Akhperjanian, Maria Haupt, Jürgen Brunner, G. Pühlhofer, S. Klepser, A. Wörnlein, Denis Wouters, Armin Rest, A. Possenti, R. C. G. Chaves, C. Mueller, P. Coyle, F. Zefi, Poonam Chandra, F. Niederwanger, R. D. Parsons, Anne Deschamps, T. Seitz, Daniele Vivolo, D. J. Champion, C. Sieger, J. Dyks, F. Schüssler, L. Caramete, A. Reimer, Felix Spanier, Dominik Elsässer, H. van Haren, S. R. Bernard, T. Garrigoux, K. Morå, I. Di Palma, L. K. Hardy, David Salek, E. Moulin, Justine Devin, Michal Ostrowski, Tomasz Bulik, J.-P. Lenain, Luigi Antonio Fusco, Thomas Tavernier, Matteo Sanguineti, A. Sánchez-Losa, M. Capasso, S. J. Fegan, A. Djannati-Ataï, G. Riccobene, Gianluca Giavitto, Benjamin Stappers, Gilles Maurin, I. Oya, L. Quinn, Axel Donath, Jacco Vink, A. W. Chen, J. Zúñiga, A. S. Seyffert, R. Miller, Pierre-Henri Aubert, Nu. Komin, Sabrina Casanova, Andrew M. Taylor, Jörn Wilms, M. Kreter, Mark Sullivan, Michael Kramer, S. Krakau, V. Sahakian, R. Bruijn, Andreas Quirrenbach, J-J. Aubert, R. Borrnuth, M. Saldaña, Aion Viana, C. Mariaud, Joao A B Coelho, J. P. Lees, P. Migliozzi, D. J. van der Walt, M. Settimo, C. Vallée, Christian Stegmann, Stefan Wagner, Gisela Anton, Bruno Khelifi, Jan Conrad, M. Marcelin, V. Giordano, M. Lorentz, M. Kraus, D. Kerszberg, T. Avgitas, Rachel Simoni, Helen Poon, J.A. Martínez-Mora, Alexis Coleiro, Antonia Rowlinson, S. Raab, Stefan Funk, Alicja Wierzcholska, B. Peyaud, Yasunobu Uchiyama, R. J. Tuffs, L. Mohrmann, Juan José Hernández-Rey, T. Jogler, D.A. Prokhorov, Michel André, Frank M. Rieger, J.D. Zornoza, A. Schulz, T. Pradier, S. Wagner, A. Abramowski, R. Mele, S. Rosier-Lees, G. Spengler, Yann Hello, J. Lau, C. van Rensburg, M. Holler, R. Coniglione, Arnauld Albert, Emanuele Leonora, A. Balzer, Michael Zacharias, M. Mohamed, Yahya Tayalati, J. Carr, I. Jung-Richardt, A. Mathieu, A. Fiasson, Roberta Zanin, P. Willmann, Hervé Glotin, K. Geyer, K. Roensch, Michael Backes, Alexandre Marcowith, J. King, J. Hofestädt, P. P. Krüger, K. Stycz, Jeff Cooke, S. P. Littlefair, H. Odaka, Felix Jankowsky, N. Shafi, M. de Naurois, Krzysztof Katarzynski, Jim Hinton, Matteo Cerruti, P. Bordas, Robert Lahmann, F. Krayzel, V. Bertin, J. Barrios-Martí, R. Liu, Stefan Ohm, W. van Straten, Christoph Deil, J. Hossl, P. Jaroenjittichai, Léa Jouvin, R. Gracia-Ruiz, T. Andersson, W. Domainko, Gerard Fontaine, Felix Aharonian, J. F. Glicenstein, Maurizio Spurio, V. Popa, Catherine Boisson, D. Drouhin, Paolo Piattelli, Olivier Hervet, Pierre Brun, F. Voisin, M. Jongen, D. Kolitzus, C. Trichard, M. Arrieta, Utane Sawangwit, Heike Prokoph, P. T. O'Brien, Paolo Sapienza, A. Förster, Ruben Lopez-Coto, M. Lemoine-Goumard, Abdelilah Moussa, S. Eschbach, M. V. Fernandes, A.J. Heijboer, Steffen Hallmann, C. Hugon, Ruizhi Yang, D. Turpin, Werner Hofmann, Stefano Gabici, S.F. Biagi, P. Wagner, V. Marandon, Jean-Pierre Ernenwein, C. Distefano, S. Colafrancesco, D. F. E. Samtleben, Vladimir Kulikovskiy, Marek Jamrozy, I. Andreoni, Corinne Donzaud, Vikram Ravi, Joachim Hahn, Shivani Bhandari, L. Oakes, Johannes Veh, M. Tluczykont, M. Caleb, Gilles Henri, J. Bolmont, J. Hawkes, I. Sushch, S. Basa, M. Chrétien, Sarah Burke-Spolaor, M. Gajdus, G.E. Păvălaş, C. Pellegrino, H. Costantini, Peter Eger, F. Stinzing, C. van Eldik, D. Berge, G. De Bonis, B. Giebels, A. Capone, Helene Sol, J. Busto, J. Becker Tjus, J.-P. Tavernet, Gavin Rowell, M. Bryan, R. de los Reyes, P.-O. Petrucci, N. W. Pekeur, Manuel Meyer, A. Goya, M. Burgay, Miguel Ardid, D. Gottschall, Anne Lemiere, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Petroff, E, Burke-Spolaor, S, Keane, Ef, Mclaughlin, Ma, Miller, R, Andreoni, I, Bailes, M, Barr, Ed, Bernard, Sr, Bhandari, S, Bhat, Ndr, Burgay, M, Caleb, M, Champion, D, Chandra, P, Cooke, J, Dhillon, V, Farnes, J, Hardy, Lk, Jaroenjittichai, P, Johnston, S, Kasliwal, M, Kramer, M, Littlefair, Sp, Macquart, Jp, Mickaliger, M, Possenti, A, Pritchard, T, Ravi, V, Rest, A, Rowlinson, A, Sawangwit, U, Stappers, B, Sullivan, M, Tiburzi, C, van Straten, W, Albert, A, Andre, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, Jj, Avgitas, T, Baret, B, Barrios-Marti, J, Basa, S, Bertin, V, Biagi, S, Borrnuth, R, Bourret, S, Bouwhuis, Mc, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chiarusi, T, Circella, M, Coelho, Jab, Coleiro, A, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Deschamps, A, De Bonis, G, Distefano, C, Di Palma, I, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, Elsasser, D, Enzenhofer, A, Felis, I, Fusco, La, Galata, S, Gay, P, Geisselsoder, S, Geyer, K, Giordano, V, Gleixner, A, Glotin, H, Gregoire, T, Gracia-Ruiz, R, Graf, K, Hallmann, S, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Hugon, C, Illuminati, G, James, Cwcw, de Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Kiessling, D, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefevre, D, Leonora, E, Lotze, M, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Martinez-Mora, Ja, Mathieu, A, Mele, R, Melis, K, Michael, T, Migliozzi, P, Moussa, A, Mueller, C, Nezri, E, Pavalas, Ge, Pellegrino, C, Perrina, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Riccobene, G, Roensch, K, Sanchez-Losa, A, Saldana, M, Salvadori, I, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schnabel, J, Seitz, T, Sieger, C, Spurio, M, Stolarczyk, T, Taiuti, M, Tayalati, Y, Trovato, A, Tselengidou, M, Turpin, D, Tonnis, C, Vallage, B, Vallee, C, Van Elewyck, V, Vivolo, D, Vizzoca, A, Wagner, S, Wilms, J, Zornoza, Jd, Zuniga, J, Abdalla, H, Abramowski, A, Aharonian, F, Benkhali, Fa, Akhperjanian, Ag, Andersson, T, Anguner, Eo, Arrieta, M, Aubert, P, Backes, M, Balzer, A, Barnard, M, Becherini, Y, Tjus, Jb, Berge, D, Bernhard, S, Bernlohr, K, Blackwell, R, Bottcher, M, Boisson, C, Bolmont, J, Bordas, P, Bregeon, J, Brun, F, Brun, P, Bryan, M, Bulik, T, Capasso, M, Casanova, S, Cerruti, M, Chakraborty, N, Chalme-Calvet, R, Chaves, Rcg, Chen, A, Chevalier, J, Chretien, M, Colafrancesco, S, Cologna, G, Condon, B, Conrad, J, Cui, Y, Davids, Id, Decock, J, Degrange, B, Deil, C, Devin, J, de Wilt, P, Dirson, L, Djannati-Atai, A, Domainko, W, Donath, A, Drury, Lo, Dubus, G, Dutson, K, Dyks, J, Edwards, T, Egberts, K, Eger, P, Ernenwein, Jp, Eschbach, S, Farnier, C, Fegan, S, Fernandes, Mv, Fiasson, A, Fontaine, G, Forster, A, Funk, S, Fussling, M, Gabici, S, Gajdus, M, Gallant, Ya, Garrigoux, T, Giavitto, G, Giebels, B, Glicenstein, Jf, Gottschall, D, Goya, A, Grondin, Mh, Hadasch, D, Hahn, J, Haupt, M, Hawkes, J, Heinzelmann, G, Henri, G, Hermann, G, Hervet, O, Hinton, Ja, Hofmann, W, Hoischen, C, Holler, M, Horns, D, Ivascenko, A, Jacholkowska, A, Jamrozy, M, Janiak, M, Jankowsky, D, Jankowsky, F, Jingo, M, Jogler, T, Jouvin, L, Jung-Richardt, I, Kastendieck, Ma, Katarzynski, K, Kerszberg, D, Khelifi, B, Kieffer, M, King, J, Klepser, S, Klochkov, D, Kluzniak, W, Kolitzus, D, Komin, N, Kosack, K, Krakau, S, Kraus, M, Krayzel, F, Kruger, Pp, Laffon, H, Lamanna, G, Lau, J, Lees, Jp, Lefaucheur, J, Lefranc, V, Lemiere, A, Lemoine-Goumard, M, Lenain, Jp, Leser, E, Lohse, T, Lorentz, M, Liu, R, Lopez-Coto, R, Lypova, I, Marandon, V, Marcowith, A, Mariaud, C, Marx, R, Maurin, G, Maxted, N, Mayer, M, Meintjes, Pj, Meyer, M, Mitchell, Amw, Moderski, R, Mohamed, M, Mohrmann, L, Mora, K, Moulin, E, Murach, T, de Naurois, M, Niederwanger, F, Niemiec, J, Oakes, L, O'Brien, P, Odaka, H, Ottl, S, Ohm, S, Ostrowski, M, Oya, I, Padovani, M, Panter, M, Parsons, Rd, Pekeur, Nw, Pelletier, G, Perennes, C, Petrucci, Po, Peyaud, B, Piel, Q, Pita, S, Poon, H, Prokhorov, D, Prokoph, H, Puhlhofer, G, Punch, M, Quirrenbach, A, Raab, S, Reimer, A, Reimer, O, Renaud, M, de los Reyes, R, Rieger, F, Romoli, C, Rosier-Lees, S, Rowell, G, Rudak, B, Rulten, Cb, Sahakian, V, Salek, D, Sanchez, Da, Santangelo, A, Sasaki, M, Schlickeiser, R, Schulz, A, Schussler, F, Schwanke, U, Schwemmer, S, Settimo, M, Seyffert, A, Shafi, N, Shilon, I, Simoni, R, Sol, H, Spanier, F, Spengler, G, Spies, F, Stawarz, L, Steenkamp, R, Stegmann, C, Stinzing, F, Stycz, K, Sushch, I, Tavernet, Jp, Tavernier, T, Taylor, Am, Terrier, R, Tibaldo, L, Tiziani, D, Tluczykont, M, Trichard, C, Tuffs, R, Uchiyama, Y, van der Walt, Dj, van Eldik, C, van Rensburg, C, van Soelen, B, Vasileiadis, G, Veh, J, Venter, C, Viana, A, Vincent, P, Vink, J, Voisin, F, Volk, Hj, Vuillaume, T, Wadiasingh, Z, Wagner, Sj, Wagner, P, Wagner, Rm, White, R, Wierzcholska, A, Willmann, P, Wornlein, A, Wouters, D, Yang, R, Zabalza, V, Zaborov, D, Zacharias, M, Zanin, R, Zdziarski, Aa, Zech, A, Zefi, F, Ziegler, A, Zywucka, N, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Petroff, E., Burke-Spolaor, S., Keane, E. F., Mclaughlin, M. A., Miller, R., Andreoni, I., Bailes, M., Barr, E. D., Bernard, S. R., Bhandari, S., Bhat, N. D. R., Burgay, M., Caleb, M., Champion, D., Chandra, P., Cooke, J., Dhillon, V. S., Farnes, J. S., Hardy, L. K., Jaroenjittichai, P., Johnston, S., Kasliwal, M., Kramer, M., Littlefair, S. P., Macquart, J. P., Mickaliger, M., Possenti, A., Pritchard, T., Ravi, V., Rest, A., Rowlinson, A., Sawangwit, U., Stappers, B., Sullivan, M., Tiburzi, C., van Straten, W., Albert, A., André, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J.-J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Bertin, V., Biagi, S., Bormuth, R., Bourret, S., Bouwhuis, M.C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chiarusi, T., Circella, M., Coelho, J.A.B., Coleiro, A., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Deschamps, A., De Bonis, G., Distefano, C., Palma, I. Di, Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., Elsässer, D., Enzenhöfer, A., Felis, I., Fusco, L.A., Galatà, S., Gay, P., Geißelsöder, S., Geyer, K., Giordano, V., Gleixner, A., Glotin, H., Grégoire, T., Gracia-Ruiz, R., Graf, K., Hallmann, S., van Haren, H., Heijboer, A.J., Hello, Y., Hernández-Rey, J.J., Hößl, J., Hofestädt, J., Hugon, C., Illuminati, G., James, C.W, de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Kießling, D., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefèvre, D., Leonora, E., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J.A., Mathieu, A., Mele, R., Melis, K., Michael, T., Migliozzi, P., Moussa, A., Mueller, C., Nezri, E., Păvălaş, G.E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Riccobene, G., Roensch, K., Sánchez-Losa, A., Saldaña, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schnabel, J., Seitz, T., Sieger, C., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Tselengidou, M., Turpin, D., Tönnis, C., Vallage, B., Vallée, C., Van Elewyck, V., Vivolo, D., Vizzoca, A., Wagner, S., Wilms, J., Zornoza, J.D., Zúñiga, J., Abdalla, H., Abramowski, A., Aharonian, F., Benkhali, F. Ait, Akhperjanian, A.G., Andersson, T., Angüner, E.O., Arrieta, M., Aubert, P., Backes, M., Balzer, A., Barnard, M., Becherini, Y., Becker Tjus, J., Berge, D., Bernhard, S., Bernlöhr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bordas, P., Bregeon, J., Brun, F., Brun, P., Bryan, M., Bulik, T., Capasso, M., Casanova, S., Cerruti, M., Chakraborty, N., Chalme-Calvet, R., Chaves, R.C.G., Chen, A., Chevalier, J., Chrétien, M., Colafrancesco, S., Cologna, G., Condon, B., Conrad, J., Cui, Y., Davids, I.D., Decock, J., Degrange, B., Deil, C., Devin, J., Dewilt, P., Dirson, L., Djannati-Ataï, A., Domainko, W., Donath, A., Drury, L.O’C., Dubus, G., Dutson, K., Dyks, J., Edwards, T., Egberts, K., Eger, P., Ernenwein, J.-P., Eschbach, S., Farnier, C., Fegan, S., Fernandes, M.V., Fiasson, A., Fontaine, G., Förster, A., Funk, S., Füßling, M., Gabici, S., Gajdus, M., Gallant, Y.A., Garrigoux, T., Giavitto, G., Giebels, B., Glicenstein, J.F., Gottschall, D., Goyal, A., Grondin, M.-H., Hadasch, D., Hahn, J., Haupt, M., Hawkes, J., Heinzelmann, G., Henri, G., Hermann, G., Hervet, O., Hinton, J.A., Hofmann, W., Hoischen, C., Holler, M., Horns, D., Ivascenko, A., Jacholkowska, A., Jamrozy, M., Janiak, M., Jankowsky, D., Jankowsky, F., Jingo, M., Jogler, T., Jouvin, L., Jung-Richardt, I., Kastendieck, M.A., Katarzyński, K., Kerszberg, D., Khélifi, B., Kieffer, M., King, J., Klepser, S., Klochkov, D., Kluźniak, W., Kolitzus, D., Komin, Nu., Kosack, K., Krakau, S., Kraus, M., Krayzel, F., Krüger, P.P., Laffon, H., Lamanna, G., Lau, J., Lees, J.-P., Lefaucheur, J., Lefranc, V., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leser, E., Lohse, T., Lorentz, M., Liu, R., López-Coto, R., Lypova, I., Marandon, V., Marcowith, A., Mariaud, C., Marx, R., Maurin, G., Maxted, N., Mayer, M., Meintjes, P.J., Meyer, M., Mitchell, A.M.W., Moderski, R., Mohamed, M., Mohrmann, L., Morå, K., Moulin, E., Murach, T., de Naurois, M., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Odaka, H., Öttl, S., Ohm, S., Ostrowski, M., Oya, I., Padovani, M., Panter, M., Parsons, R.D., Pekeur, N.W., Pelletier, G., Perennes, C., Petrucci, P.-O., Peyaud, B., Piel, Q., Pita, S., Poon, H., Prokhorov, D., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Reimer, A., Reimer, O., Renaud, M., Reyes, R. de lo, Rieger, F., Romoli, C., Rosier-Lees, S., Rowell, G., Rudak, B., Rulten, C.B., Sahakian, V., Salek, D., Sanchez, D.A., Santangelo, A., Sasaki, M., Schlickeiser, R., Schulz, A., Schüssler, F., Schwanke, U., Schwemmer, S., Settimo, M., Seyffert, A.S., Shafi, N., Shilon, I., Simoni, R., Sol, H., Spanier, F., Spengler, G., Spies, F., Stawarz, Ł., Steenkamp, R., Stegmann, C., Stinzing, F., Stycz, K., Sushch, I., Tavernet, J.-P., Tavernier, T., Taylor, A.M., Terrier, R., Tibaldo, L., Tiziani, D., Tluczykont, M., Trichard, C., Tuffs, R., Uchiyama, Y., Walt, D.J. van der, van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Voisin, F., Völk, H.J., Vuillaume, T., Wadiasingh, Z., Wagner, S.J., Wagner, P., Wagner, R.M., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Yang, R., Zabalza, V., Zaborov, D., Zacharias, M., Zanin, R., Zdziarski, A.A., Zech, A., Zefi, F., Ziegler, A., Żywucka, N., High Energy Astrophys. & Astropart. Phys (API, FNWI), KM3NeT (IHEF, IoP, FNWI), Faculty of Science, Gravitation and Astroparticle Physics Amsterdam, ATLAS (IHEF, IoP, FNWI), GRAPPA (ITFA, IoP, FNWI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Andre, M., Aubert, J. -J., Barrios-Marti, J., Bouwhuis, M. C., Coelho, J. A. B., Di Palma, I., Elsasser, D., Enzenhofer, A., Fusco, L. A., Galata, S., Geisselsoder, S., Gregoire, T., Heijboer, A. J., Hernandez-Rey, J. J., Hobl, J., Hofestadt, J., James, C. W., Kiebling, D., Lefevre, D., Martinez-Mora, J. A., Pavalas, G. E., Sanchez-Losa, A., Saldana, M., Stolarczyk, T., Tonnis, C., Vallee, C., Zornoza, J. D., Zuniga, J., Ait Benkhali, F., Akhperjanian, A. G., Anguner, E. O., Bernlohr, K., Bottcher, M., Chaves, R. C. G., Chretien, M., Davids, I. D., Djannati-Atai, A., Drury, L. O'C., Ernenwein, J. -P., Fernandes, M. V., Forster, A., Fubling, M., Gallant, Y. A., Glicenstein, J. F., Grondin, M. -H., Hinton, J. A., Kastendieck, M. A., Katarzynski, K., Khelifi, B., Kluzniak, W., Komin, N., Kruger, P. P., Lees, J. -P., Lemiere, A., Lenain, J. -P., Lopez-Coto, R., Meintjes, P. J., Mitchell, A. M. W., Mora, K., O'Brien, P., Ottl, S., Parsons, R. D., Pekeur, N. W., Petrucci, P. -O., Puhlhofer, G., de los Reyes, R., Rulten, C. B., Sanchez, D. A., Schussler, F., Seyffert, A. S., Stawarz, L., Tavernet, J. -P., Taylor, A. M., van der Walt, D. J., Volk, H. J., Wagner, S. J., Wagner, R. M., Wornlein, A., Zdziarski, A. A., Zywucka, N., Centre Tecnològic de Vilanova i la Geltrú, and Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques
Subjects: Astrofísica, Astronomy, Astrophysics, Surveys, ISM: structure, Methods: data analysis, Polarization, Astronomy and Astrophysics, Space and Planetary Science, 01 natural sciences, Radio telescopes, data analysis [Methods], 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Line-of-sight, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Linear polarization, Fast radio burst, Galactic Center, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - High Energy Astrophysical Phenomena, polarization–methods, dataanalysis–surveys–ISM, structure, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, 0103 physical sciences, Neutrins, Neutrinos, Astrophysics::Galaxy Astrophysics, Astroparticle physics, Telescopis, 010308 nuclear & particles physics, Galactic plane, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], FISICA APLICADA, ddc:520, polarization – methods: data analysis – surveys – ISM: structure, structure [ISM], Methods: data analysi
Abstract: Monthly notices of the Royal Astronomical Society 469(4), 4465 – 4482 (2017). doi:10.1093/mnras/stx1098, We report on the discovery of a new fast radio burst (FRB), FRB 150215, with the Parkes radio telescope on 2015 February 15. The burst was detected in real time with a dispersion measure (DM) of 1105.6 ± 0.8 pc cm$^{−3}$, a pulse duration of 2.8 $^{+1.2}_{-0.5}$ ms, and a measured peak flux density assuming that the burst was at beam centre of 0.7$^{+0.2}_{-0.1}$ Jy. The FRB originated at a Galactic longitude and latitude of 24.66°, 5.28° and 25° away from the Galactic Center. The burst was found to be 43 ± 5 per cent linearly polarized with a rotation measure (RM) in the range −9, Published by Oxford Univ. Press, Oxford
Published: 2017
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33. Spectral modelling of H.E.S.S.- detected pulsar wind nebulae

Author: Van Rensburg, Carlo, Krüger, P.P., Venter, C., and 10103449 - Krüger, Petrus Paulus (Supervisor)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Non-thermal emission mechanisms, Gamma rays, Pulsar wind nebulae, H.E.S.S, Spectral modelling
Abstract: MSc (Space Physics), North-West University, Potchefstroom Campus, 2016 In the last decade, ground-based Imaging Atmospheric Cherenkov Telescopes have discovered about 175 very-high-energy (VHE; E > 100 GeV) gamma-ray sources, with more to follow with the development of H.E.S.S. II and CTA. Nearly 40 of these are confirmed pulsar wind nebulae (PWNe). We present results from a leptonic emission code that models the spectral energy density of a PWN by solving a Fokker-Planck-type transport equation and calculating inverse Compton and synchrotron emissivities. Although models such as these have been developed before, most of them model the geometry of a PWN as that of a single sphere. We have created a time-dependent, multi-zone model to investigate changes in the particle spectrum as the particles traverse through the PWN, by considering a time and spatially-dependent magnetic field, spatially-dependent bulk particle motion causing convection, diffusion, and energy losses (SR, IC and adiabatic). Our code predicts the radiation spectrum at different positions in the nebula, yielding novel results, e.g., the surface brightness versus the radius and the PWN size as function of energy. We calibrated our new model against more basic models using the observed spectrum of PWN G0.9+0.1, incorporating data from H.E.S.S. as well as radio and X-ray experiments. We fit our predicted radiation spectra to data from G21.5-0.9, G54.1+0.3, and HESS J1356-645 and found that our model yields reasonable results for young PWNe. We next performed a parameter study which gave significant insight into the behaviour of the PWN for different scenarios. Our model is now ready to be applied to a population of PWNe to probe possible trends such as the surface brightness as a function of spin-down of the pulsar. Masters
Published: 2016

34. The Sabbath commandment in Exodus 20:8-11 in the light of the first creation account

Author: Haynes, Matthew Brian, Krüger, P.P., Simango, D., 10103449 - Krüger, Petrus Paulus (Supervisor), and 12038016 - Sinango, Daniel (Supervisor)
Subjects: Genesis 2, Genesis 1, Rest, Garden, Fourth Commandment, Sabbath, Exodus 20
Abstract: MTh (Old Testament), North-West University, Potchefstroom Campus, 2015 This study is an attempt to define more clearly the Sabbath institution as it is presented in Exodus 20:8-11. It begins by describing the big-picture contours of the Sabbath institution as it has been depicted by various scholars during the last century. Many of these studies focus on delineating what proper Sabbath observance entails or describing how Sabbath rest mirrors God’s rest on the seventh day of creation. However, little investigation has been conducted into the relationship between the fourth commandment in Exodus 20 and the shape of humanity’s task and relationship with God on the seventh day. The study then examines the nature of God’s rest in the first creation account, describing what “rest” entailed for God, and the work from which he rested. It suggests that this “rest” is from the creational activity of the first six days and that it continues on into the present. It also discusses the relationship between the concept of rest offered by the first creation account and the concept of rest in the understanding of the Ancient Near East and Israel. Humanity’s role in the created order is also examined. While humans share some qualities with other creatures, such as an embodied existence, they are also distinct from the rest of creation. Only humans are created in the image of God. As such, they are given tasks unique to their status: subduing the earth, exercising dominion over the creatures of the earth, and expanding the borders of the garden as they multiply and fill the earth. These form the heart of their God-given task that they will carry out as God enjoys his seventh-day rest. Next, the study investigates the particulars of Exodus 20:8-11 and suggests a reading of these particulars against the backdrop of the seventh day as it is described in chapters 3-4. While the rationale for the Sabbath commandment is grounded in the events of the first creation account, the commandment itself also needs to be understood in the context of the Decalogue and, in turn, in the context of the law’s reception at Sinai. The law, and hence the fourth commandment, are central to the calling and purpose of Israel. As Israel fulfils its mandate to be a light to the nations, it will reflect the ideals of the seventh day as they are encapsulated in the law. Far from simply mirroring God’s rest, the fourth commandment reflects the relationship between God and humanity and humanity’s role on the seventh day of creation. The study concludes by drawing together various pieces of the argument and makes suggestions for further research. Masters
Published: 2015

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34 results on '"Krüger, P.P."'

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2. Searches for gamma-ray lines and ‘pure WIMP’ spectra from Dark Matter annihilations in dwarf galaxies with H.E.S.S.

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8. Search for dark matter annihilations towards the inner Galactic halo from 10 years of observations with H.E.S.S.

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34. The Sabbath commandment in Exodus 20:8-11 in the light of the first creation account

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34 results on '"Krüger, P.P."'

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