@unpublished{AcharyaActisAghajanietal.2013,
author = {Acharya, B. S. and Actis, M. and Aghajani, T. and Agnetta, G. and Aguilar, J. and Aharonian, Felix A. and Ajello, M. and Akhperjanian, A. G. and Alcubierre, M. and Aleksic, J. and Alfaro, R. and Aliu, E. and Allafort, A. J. and Allan, D. and Allekotte, I. and Amato, E. and Anderson, J. and Ang{\"u}ner, Ekrem Oǧuzhan and Antonelli, L. A. and Antoranz, P. and Aravantinos, A. and Arlen, T. and Armstrong, T. and Arnaldi, H. and Arrabito, L. and Asano, K. and Ashton, T. and Asorey, H. G. and Awane, Y. and Baba, H. and Babic, A. and Baby, N. and Baehr, J. and Bais, A. and Baixeras, C. and Bajtlik, S. and Balbo, M. and Balis, D. and Balkowski, C. and Bamba, A. and Bandiera, R. and Barber, A. and Barbier, C. and Barcelo, M. and Barnacka, Anna and Barnstedt, J{\"u}rgen and Barres de Almeida, U. and Barrio, J. A. and Basili, A. and Basso, S. and Bastieri, D. and Bauer, C. and Baushev, Anton N. and Becerra Gonzalez, J. and Becherini, Yvonne and Bechtol, K. C. and Tjus, J. Becker and Beckmann, Volker and Bednarek, W. and Behera, B. and Belluso, M. and Benbow, W. and Berdugo, J. and Berger, K. and Bernard, F. and Bernardino, T. and Bernl{\"o}hr, K. and Bhat, N. and Bhattacharyya, S. and Bigongiari, C. and Biland, A. and Billotta, S. and Bird, T. and Birsin, E. and Bissaldi, E. and Biteau, Jonathan and Bitossi, M. and Blake, S. and Blanch Bigas, O. and Blasi, P. and Bobkov, A. A. and Boccone, V. and Boettcher, Markus and Bogacz, L. and Bogart, J. and Bogdan, M. and Boisson, Catherine and Boix Gargallo, J. and Bolmont, J. and Bonanno, G. and Bonardi, A. and Bonev, T. and Bonifacio, P. and Bonnoli, G. and Bordas, Pol and Borgland, A. W. and Borkowski, Janett and Bose, R. and Botner, O. and Bottani, A. and Bouchet, L. and Bourgeat, M. and Boutonnet, C. and Bouvier, A. and Brau-Nogue, S. and Braun, I. and Bretz, T. and Briggs, M. S. and Bringmann, T. and Brook, P. and Brun, Pierre and Brunetti, L. and Buanes, T. and Buckley, J. H. and Buehler, R. and Bugaev, V. and Bulgarelli, A. and Bulik, Tomasz and Busetto, G. and Buson, S. and Byrum, K. and Cailles, M. and Cameron, R. A. and Camprecios, J. and Canestrari, R. and Cantu, S. and Capalbi, M. and Caraveo, P. A. and Carmona, E. and Carosi, A. and Carr, John and Carton, P. H. and Casanova, Sabrina and Casiraghi, M. and Catalano, O. and Cavazzani, S. and Cazaux, S. and Cerruti, M. and Chabanne, E. and Chadwick, Paula M. and Champion, C. and Chen, Andrew and Chiang, J. and Chiappetti, L. and Chikawa, M. and Chitnis, V. R. and Chollet, F. and Chudoba, J. and Cieslar, M. and Cillis, A. N. and Cohen-Tanugi, J. and Colafrancesco, Sergio and Colin, P. and Calome, J. and Colonges, S. and Compin, M. and Conconi, P. and Conforti, V. and Connaughton, V. and Conrad, Jan and Contreras, J. L. and Coppi, P. and Corona, P. and Corti, D. and Cortina, J. and Cossio, L. and Costantini, H. and Cotter, G. and Courty, B. and Couturier, S. and Covino, S. and Crimi, G. and Criswell, S. J. and Croston, J. and Cusumano, G. and Dafonseca, M. and Dale, O. and Daniel, M. and Darling, J. and Davids, I. and Dazzi, F. and De Angelis, A. and De Caprio, V. and De Frondat, F. and de Gouveia Dal Pino, E. M. and de la Calle, I. and De La Vega, G. A. and Lopez, R. de los Reyes and De Lotto, B. and De Luca, A. and de Mello Neto, J. R. T. and de Naurois, M. and de Oliveira, Y. and de Ona Wilhelmi, E. and de Souza, V. and Decerprit, G. and Decock, G. and Deil, C. and Delagnes, E. and Deleglise, G. and Delgado, C. and Della Volpe, D. and Demange, P. and Depaola, G. and Dettlaff, A. and Di Paola, A. and Di Pierro, F. and Diaz, C. and Dick, J. and Dickherber, R. and Dickinson, H. and Diez-Blanco, V. and Digel, S. and Dimitrov, D. and Disset, G. and Djannati-Ata{\"i}, A. and Doert, M. and Dohmke, M. and Domainko, W. and Prester, Dijana Dominis and Donat, A. and Dorner, D. and Doro, M. and Dournaux, J-L. and Drake, G. and Dravins, D. and Drury, L. and Dubois, F. and Dubois, R. and Dubus, G. and Dufour, C. and Dumas, D. and Dumm, J. and Durand, D. and Dyks, J. and Dyrda, M. and Ebr, J. and Edy, E. and Egberts, Kathrin and Eger, P. and Einecke, S. and Eleftheriadis, C. and Elles, S. and Emmanoulopoulos, D. and Engelhaupt, D. and Enomoto, R. and Ernenwein, J-P and Errando, M. and Etchegoyen, A. and Evans, P. and Falcone, A. and Fantinel, D. and Farakos, K. and Farnier, C. and Fasola, G. and Favill, B. and Fede, E. and Federici, S. and Fegan, S. and Feinstein, F. and Ferenc, D. and Ferrando, P. and Fesquet, M. and Fiasson, A. and Fillin-Martino, E. and Fink, D. and Finley, C. and Finley, J. P. and Fiorini, M. and Firpo Curcoll, R. and Flores, H. and Florin, D. and Focke, W. and Foehr, C. and Fokitis, E. and Font, L. and Fontaine, G. and Fornasa, M. and Foerster, A. and Fortson, L. and Fouque, N. and Franckowiak, A. and Fransson, C. and Fraser, G. and Frei, R. and Albuquerque, I. F. M. and Fresnillo, L. and Fruck, C. and Fujita, Y. and Fukazawa, Y. and Fukui, Y. and Funk, S. and Gaebele, W. and Gabici, S. and Gabriele, R. and Gadola, A. and Galante, N. and Gall, D. and Gallant, Y. and Gamez-Garcia, J. and Garcia, B. and Garcia Lopez, R. and Gardiol, D. and Garrido, D. and Garrido, L. and Gascon, D. and Gaug, M. and Gaweda, J. and Gebremedhin, L. and Geffroy, N. and Gerard, L. and Ghedina, A. and Ghigo, M. and Giannakaki, E. and Gianotti, F. and Giarrusso, S. and Giavitto, G. and Giebels, B. and Gika, V. and Giommi, P. and Girard, N. and Giro, E. and Giuliani, A. and Glanzman, T. and Glicenstein, J. -F. and Godinovic, N. and Golev, V. and Gomez Berisso, M. and Gomez-Ortega, J. and Gonzalez, M. M. and Gonzalez, A. and Gonzalez, F. and Gonzalez Munoz, A. and Gothe, K. S. and Gougerot, M. and Graciani, R. and Grandi, P. and Granena, F. and Granot, J. and Grasseau, G. and Gredig, R. and Green, A. and Greenshaw, T. and Gregoire, T. and Grimm, O. and Grube, J. and Grudzinska, M. and Gruev, V. and Gruenewald, S. and Grygorczuk, J. and Guarino, V. and Gunji, S. and Gyuk, G. and Hadasch, D. and Hagiwara, R. and Hahn, J. and Hakansson, N. and Hallgren, A. and Hamer Heras, N. and Hara, S. and Hardcastle, M. J. and Harris, J. and Hassan, T. and Hatanaka, K. and Haubold, T. and Haupt, A. and Hayakawa, T. and Hayashida, M. and Heller, R. and Henault, F. and Henri, G. and Hermann, G. and Hermel, R. and Herrero, A. and Hidaka, N. and Hinton, J. and Hoffmann, D. and Hofmann, W. and Hofverberg, P. and Holder, J. and Horns, D. and Horville, D. and Houles, J. and Hrabovsky, M. and Hrupec, D. and Huan, H. and Huber, B. and Huet, J. -M. and Hughes, G. and Humensky, T. B. and Huovelin, J. and Ibarra, A. and Illa, J. M. and Impiombato, D. and Incorvaia, S. and Inoue, S. and Inoue, Y. and Ioka, K. and Ismailova, E. and Jablonski, C. and Jacholkowska, A. and Jamrozy, M. and Janiak, M. and Jean, P. and Jeanney, C. and Jimenez, J. J. and Jogler, T. and Johnson, T. and Journet, L. and Juffroy, C. and Jung, I. and Kaaret, P. and Kabuki, S. and Kagaya, M. and Kakuwa, J. and Kalkuhl, C. and Kankanyan, R. and Karastergiou, A. and Kaercher, K. and Karczewski, M. and Karkar, S. and Kasperek, Aci. and Kastana, D. and Katagiri, H. and Kataoka, J. and Katarzynski, K. and Katz, U. and Kawanaka, N. and Kellner-Leidel, B. and Kelly, H. and Kendziorra, E. and Khelifi, B. and Kieda, D. B. and Kifune, T. and Kihm, T. and Kishimoto, T. and Kitamoto, K. and Kluzniak, W. and Knapic, C. and Knapp, J. w and Knoedlseder, J. and Koeck, F. and Kocot, J. and Kodani, K. and Koehne, J. -H. and Kohri, K. and Kokkotas, K. and Kolitzus, D. and Komin, N. and Kominis, I. and Konno, Y. and Koeppel, H. and Korohoda, P. and Kosack, K. and Koss, G. and Kossakowski, R. and Kostka, P. and Koul, R. and Kowal, G. and Koyama, S. and Koziol, J. and Kraehenbuehl, T. and Krause, J. and Krawzcynski, H. and Krennrich, F. and Krepps, A. and Kretzschmann, A. and Krobot, R. and Krueger, P. and Kubo, H. and Kudryavtsev, V. A. and Kushida, J. and Kuznetsov, A. and La Barbera, A. and La Palombara, N. and La Parola, V. and La Rosa, G. and Lacombe, K. and Lamanna, G. and Lande, J. and Languignon, D. and Lapington, J. and Laporte, P. and Lavalley, C. and Le Flour, T. and Le Padellec, A. and Lee, S. -H. and Lee, W. H. and Leigui de Oliveira, M. A. and Lelas, D. and Lenain, J. -P. and Leopold, D. J. and Lerch, T. and Lessio, L. and Lieunard, B. and Lindfors, E. and Liolios, A. and Lipniacka, A. and Lockart, H. and Lohse, T. and Lombardi, S. and Lopatin, A. and Lopez, M. and Lopez-Coto, R. and Lopez-Oramas, A. and Lorca, A. and Lorenz, E. and Lubinski, P. and Lucarelli, F. and Luedecke, H. and Ludwin, J. and Luque-Escamilla, P. L. and Lustermann, W. and Luz, O. and Lyard, E. and Maccarone, M. C. and Maccarone, T. J. and Madejski, G. M. and Madhavan, A. and Mahabir, M. and Maier, G. and Majumdar, P. and Malaguti, G. and Maltezos, S. and Manalaysay, A. and Mancilla, A. and Mandat, D. and Maneva, G. and Mangano, A. and Manigot, P. and Mannheim, K. and Manthos, I. and Maragos, N. and Marcowith, Alexandre and Mariotti, M. and Marisaldi, M. and Markoff, S. and Marszalek, A. and Martens, C. and Marti, J. and Martin, J-M. and Martin, P. and Martinez, G. and Martinez, F. and Martinez, M. and Masserot, A. and Mastichiadis, A. and Mathieu, A. and Matsumoto, H. and Mattana, F. and Mattiazzo, S. and Maurin, G. and Maxfield, S. and Maya, J. and Mazin, D. and Mc Comb, L. and McCubbin, N. and McHardy, I. and McKay, R. and Medina, C. and Melioli, C. and Melkumyan, D. and Mereghetti, S. and Mertsch, P. and Meucci, M. and Michalowski, J. and Micolon, P. and Mihailidis, A. and Mineo, T. and Minuti, M. and Mirabal, N. and Mirabel, F. and Miranda, J. M. and Mirzoyan, R. and Mizuno, T. and Moal, B. and Moderski, R. and Mognet, I. and Molinari, E. and Molinaro, M. and Montaruli, T. and Monteiro, I. and Moore, P. and Moralejo Olaizola, A. and Mordalska, M. and Morello, C. and Mori, K. and Mottez, F. and Moudden, Y. and Moulin, Emmanuel and Mrusek, I. and Mukherjee, R. and Munar-Adrover, P. and Muraishi, H. and Murase, K. and Murphy, A. and Nagataki, S. and Naito, T. and Nakajima, D. and Nakamori, T. and Nakayama, K. and Naumann, C. L. and Naumann, D. and Naumann-Godo, M. and Nayman, P. and Nedbal, D. and Neise, D. and Nellen, L. and Neustroev, V. and Neyroud, N. and Nicastro, L. and Nicolau-Kuklinski, J. and Niedzwiecki, A. and Niemiec, J. and Nieto, D. and Nikolaidis, A. and Nishijima, K. and Nolan, S. and Northrop, R. and Nosek, D. and Nowak, N. and Nozato, A. and O'Brien, P. and Ohira, Y. and Ohishi, M. and Ohm, S. and Ohoka, H. and Okuda, T. and Okumura, A. and Olive, J. -F. and Ong, R. A. and Orito, R. and Orr, M. and Osborne, J. and Ostrowski, M. and Otero, L. A. and Otte, N. and Ovcharov, E. and Oya, I. and Ozieblo, A. and Padilla, L. and Paiano, S. and Paillot, D. and Paizis, A. and Palanque, S. and Palatka, M. and Pallota, J. and Panagiotidis, K. and Panazol, J. -L. and Paneque, D. and Panter, M. and Paoletti, R. and Papayannis, Alexandros and Papyan, G. and Paredes, J. M. and Pareschi, G. and Parks, G. and Parraud, J. -M. and Parsons, D. and Arribas, M. Paz and Pech, M. and Pedaletti, G. and Pelassa, V. and Pelat, D. and Perez, M. D. C. and Persic, M. and Petrucci, P-O and Peyaud, B. and Pichel, A. and Pita, S. and Pizzolato, F. and Platos, L. and Platzer, R. and Pogosyan, L. and Pohl, M. and Pojmanski, G. and Ponz, J. D. and Potter, W. and Poutanen, J. and Prandini, E. and Prast, J. and Preece, R. and Profeti, F. and Prokoph, H. and Prouza, M. and Proyetti, M. and Puerto-Gimenez, I. and Puehlhofer, G. and Puljak, I. and Punch, M. and Pyziol, R. and Quel, E. J. and Quinn, J. and Quirrenbach, A. and Racero, E. and Rajda, P. J. and Ramon, P. and Rando, R. and Rannot, R. C. and Rataj, M. and Raue, M. and Reardon, P. and Reimann, O. and Reimer, A. and Reimer, O. and Reitberger, K. and Renaud, M. and Renner, S. and Reville, B. and Rhode, W. and Ribo, M. and Ribordy, M. and Richer, M. G. and Rico, J. and Ridky, J. and Rieger, F. and Ringegni, P. and Ripken, J. and Ristori, P. R. and Riviere, A. and Rivoire, S. and Rob, L. and Roeser, U. and Rohlfs, R. and Rojas, G. and Romano, Patrizia and Romaszkan, W. and Romero, G. E. and Rosen, S. and Lees, S. Rosier and Ross, D. and Rouaix, G. and Rousselle, J. and Rousselle, S. and Rovero, A. C. and Roy, F. and Royer, S. and Rudak, B. and Rulten, C. and Rupinski, M. and Russo, F. and Ryde, F. and Sacco, B. and Saemann, E. O. and Saggion, A. and Safiakian, V. and Saito, K. and Saito, T. and Saito, Y. and Sakaki, N. and Sakonaka, R. and Salini, A. and Sanchez, F. and Sanchez-Conde, M. and Sandoval, A. and Sandaker, H. and Sant'Ambrogio, E. and Santangelo, Andrea and Santos, E. M. and Sanuy, A. and Sapozhnikov, L. and Sarkar, S. and Sartore, N. and Sasaki, H. and Satalecka, K. and Sawada, M. and Scalzotto, V. and Scapin, V. and Scarcioffolo, M. and Schafer, J. and Schanz, T. and Schlenstedt, S. and Schlickeiser, R. and Schmidt, T. and Schmoll, J. and Schovanek, P. and Schroedter, M. and Schultz, C. and Schultze, J. and Schulz, A. and Schure, K. and Schwab, T. and Schwanke, U. and Schwarz, J. and Schwarzburg, S. and Schweizer, T. and Schwemmer, S. and Segreto, A. and Seiradakis, J. -H. and Sembroski, G. H. and Seweryn, K. and Sharma, M. and Shayduk, M. and Shellard, R. C. and Shi, J. and Shibata, T. and Shibuya, A. and Shum, E. and Sidoli, L. and Sidz, M. and Sieiro, J. and Sikora, M. and Silk, J. and Sillanpaa, A. and Singh, B. B. and Sitarek, J. and Skole, C. and Smareglia, R. and Smith, A. and Smith, D. and Smith, J. and Smith, N. and Sobczynska, D. and Sol, H. and Sottile, G. and Sowinski, M. and Spanier, F. and Spiga, D. and Spyrou, S. and Stamatescu, V. and Stamerra, A. and Starling, R. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steiner, S. and Stergioulas, N. and Sternberger, R. and Sterzel, M. and Stinzing, F. and Stodulski, M. and Straumann, U. and Strazzeri, E. and Stringhetti, L. and Suarez, A. and Suchenek, M. and Sugawara, R. and Sulanke, K. -H. and Sun, S. and Supanitsky, A. D. and Suric, T. and Sutcliffe, P. and Sykes, J. and Szanecki, M. and Szepieniec, T. and Szostek, A. and Tagliaferri, G. and Tajima, H. and Takahashi, H. and Takahashi, K. and Takalo, L. and Takami, H. and Talbot, C. and Tammi, J. and Tanaka, M. and Tanaka, S. and Tasan, J. and Tavani, M. and Tavernet, J. -P. and Tejedor, L. A. and Telezhinsky, Igor O. and Temnikov, P. and Tenzer, C. and Terada, Y. and Terrier, R. and Teshima, M. and Testa, V. and Tezier, D. and Thuermann, D. and Tibaldo, L. and Tibolla, O. and Tiengo, A. and Tluczykont, M. and Todero Peixoto, C. J. and Tokanai, F. and Tokarz, M. and Toma, K. and Torii, K. and Tornikoski, M. and Torres, D. F. and Torres, M. and Tosti, G. and Totani, T. and Toussenel, C. and Tovmassian, G. and Travnicek, P. and Trifoglio, M. and Troyano, I. and Tsinganos, K. and Ueno, H. and Umehara, K. and Upadhya, S. S. and Usher, T. and Uslenghi, M. and Valdes-Galicia, J. F. and Vallania, P. and Vallejo, G. and van Driel, W. and van Eldik, C. and Vandenbrouke, J. and Vanderwalt, J. and Vankov, H. and Vasileiadis, G. and Vassiliev, V. and Veberic, D. and Vegas, I. and Vercellone, S. and Vergani, S. and Veyssiere, C. and Vialle, J. P. and Viana, A. and Videla, M. and Vincent, P. and Vincent, S. and Vink, J. and Vlahakis, N. and Vlahos, L. and Vogler, P. and Vollhardt, A. and von Gunten, H. P. and Vorobiov, S. and Vuerli, C. and Waegebaert, V. and Wagner, R. and Wagner, R. G. and Wagner, S. and Wakely, S. P. and Walter, R. and Walther, T. and Warda, K. and Warwick, R. and Wawer, P. and Wawrzaszek, R. and Webb, N. and Wegner, P. and Weinstein, A. and Weitzel, Q. and Welsing, R. and Werner, M. and Wetteskind, H. and White, R. and Wierzcholska, A. and Wiesand, S. and Wilkinson, M. and Williams, D. A. and Willingale, R. and Winiarski, K. and Wischnewski, R. and Wisniewski, L. and Wood, M. and Woernlein, A. and Xiong, Q. and Yadav, K. K. and Yamamoto, H. and Yamamoto, T. and Yamazaki, R. and Yanagita, S. and Yebras, J. M. and Yelos, D. and Yoshida, A. and Yoshida, T. and Yoshikoshi, T. and Zabalza, V. and Zacharias, M. and Zajczyk, A. and Zanin, R. and Zdziarski, A. and Zech, Alraune and Zhao, A. and Zhou, X. and Zietara, K. and Ziolkowski, J. and Ziolkowski, P. and Zitelli, V. and Zurbach, C. and Zychowski, P.},
title = {Introducing the CTA concept},
series = {Astroparticle physics},
volume = {43},
journal = {Astroparticle physics},
number = {2},
publisher = {Elsevier},
address = {Amsterdam},
organization = {CTA Consortium},
issn = {0927-6505},
doi = {10.1016/j.astropartphys.2013.01.007},
pages = {3 -- 18},
year = {2013},
abstract = {The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project.},
language = {en}
}
@article{AceroAloisioAmansetal.2017,
author = {Acero, F. and Aloisio, R. and Amans, J. and Amato, Elena and Antonelli, L. A. and Aramo, C. and Armstrong, T. and Arqueros, F. and Asano, Katsuaki and Ashley, M. and Backes, M. and Balazs, C. and Balzer, A. and Bamba, Aya and Barkov, Maxim and Barrio, J. A. and Benbow, Wystan and Bernloehr, K. and Beshley, V. and Bigongiari, C. and Biland, A. and Bilinsky, A. and Bissaldi, Elisabetta and Biteau, J. and Blanch, O. and Blasi, P. and Blazek, J. and Boisson, C. and Bonanno, G. and Bonardi, A. and Bonavolonta, C. and Bonnoli, G. and Braiding, C. and Brau-Nogue, S. and Bregeon, J. and Brown, A. M. and Bugaev, V. and Bulgarelli, A. and Bulik, T. and Burton, Michael and Burtovoi, A. and Busetto, G. and Bottcher, M. and Cameron, R. and Capalbi, M. and Caproni, Anderson and Caraveo, P. and Carosi, R. and Cascone, E. and Cerruti, M. and Chaty, Sylvain and Chen, A. and Chen, X. and Chernyakova, M. and Chikawa, M. and Chudoba, J. and Cohen-Tanugi, J. and Colafrancesco, S. and Conforti, V. and Contreras, J. L. and Costa, A. and Cotter, G. and Covino, Stefano and Covone, G. and Cumani, P. and Cusumano, G. and Daniel, M. and Dazzi, F. and De Angelis, A. and De Cesare, G. and De Franco, A. and De Frondat, F. and Dal Pino, E. M. de Gouveia and De Lisio, C. and Lopez, R. de los Reyes and De Lotto, B. and de Naurois, M. and De Palma, F. and Del Santo, M. and Delgado, C. and della Volpe, D. and Di Girolamo, T. and Di Giulio, C. and Di Pierro, F. and Di Venere, L. and Doro, M. and Dournaux, J. and Dumas, D. and Dwarkadas, Vikram V. and Diaz, C. and Ebr, J. and Egberts, Kathrin and Einecke, S. and Elsaesser, D. and Eschbach, S. and Falceta-Goncalves, D. and Fasola, G. and Fedorova, E. and Fernandez-Barral, A. and Ferrand, Gilles and Fesquet, M. and Fiandrini, E. and Fiasson, A. and Filipovic, Miroslav D. and Fioretti, V. and Font, L. and Fontaine, Gilles and Franco, F. J. and Freixas Coromina, L. and Fujita, Yutaka and Fukui, Y. and Funk, S. and Forster, A. and Gadola, A. and Lopez, R. Garcia and Garczarczyk, M. and Giglietto, N. and Giordano, F. and Giuliani, A. and Glicenstein, J. and Gnatyk, R. and Goldoni, P. and Grabarczyk, T. and Graciani, R. and Graham, J. and Grandi, P. and Granot, Jonathan and Green, A. J. and Griffiths, S. and Gunji, S. and Hakobyan, H. and Hara, S. and Hassan, T. and Hayashida, M. and Heller, M. and Helo, J. C. and Hinton, J. and Hnatyk, B. and Huet, J. and Huetten, M. and Humensky, T. B. and Hussein, M. and Horandel, J. and Ikeno, Y. and Inada, T. and Inome, Y. and Inoue, S. and Inoue, T. and Inoue, Y. and Ioka, K. and Iori, Maurizio and Jacquemier, J. and Janecek, P. and Jankowsky, D. and Jung, I. and Kaaret, P. and Katagiri, H. and Kimeswenger, S. and Kimura, Shigeo S. and Knodlseder, J. and Koch, B. and Kocot, J. and Kohri, K. and Komin, N. and Konno, Y. and Kosack, K. and Koyama, S. and Kraus, Michaela and Kubo, Hidetoshi and Mezek, G. Kukec and Kushida, J. and La Palombara, N. and Lalik, K. and Lamanna, G. and Landt, H. and Lapington, J. and Laporte, P. and Lee, S. and Lees, J. and Lefaucheur, J. and Lenain, J. -P. and Leto, Giuseppe and Lindfors, E. and Lohse, T. and Lombardi, S. and Longo, F. and Lopez, M. and Lucarelli, F. and Luque-Escamilla, Pedro Luis and Lopez-Coto, R. and Maccarone, M. C. and Maier, G. and Malaguti, G. and Mandat, D. and Maneva, G. and Mangano, S. and Marcowith, Alexandre and Marti, J. and Martinez, M. and Martinez, G. and Masuda, S. and Maurin, G. and Maxted, N. and Melioli, Claudio and Mineo, T. and Mirabal, N. and Mizuno, T. and Moderski, R. and Mohammed, M. and Montaruli, T. and Moralejo, A. and Mori, K. and Morlino, G. and Morselli, A. and Moulin, Emmanuel and Mukherjee, R. and Mundell, C. and Muraishi, H. and Murase, Kohta and Nagataki, Shigehiro and Nagayoshi, T. and Naito, T. and Nakajima, D. and Nakamori, T. and Nemmen, R. and Niemiec, Jacek and Nieto, D. and Nievas-Rosillo, M. and Nikolajuk, M. and Nishijima, K. and Noda, K. and Nogues, L. and Nosek, D. and Novosyadlyj, B. and Nozaki, S. and Ohira, Yutaka and Ohishi, M. and Ohm, S. and Okumura, A. and Ong, R. A. and Orito, R. and Orlati, A. and Ostrowski, M. and Oya, I. and Padovani, Marco and Palacio, J. and Palatka, M. and Paredes, Josep M. and Pavy, S. and Persic, M. and Petrucci, P. and Petruk, Oleh and Pisarski, A. and Pohl, Martin and Porcelli, A. and Prandini, E. and Prast, J. and Principe, G. and Prouza, M. and Pueschel, Elisa and Puelhofer, G. and Quirrenbach, A. and Rameez, M. and Reimer, O. and Renaud, M. and Ribo, M. and Rico, J. and Rizi, V. and Rodriguez, J. and Fernandez, G. Rodriguez and Rodriguez Vazquez, J. J. and Romano, Patrizia and Romeo, G. and Rosado, J. and Rousselle, J. and Rowell, G. and Rudak, B. and Sadeh, I. and Safi-Harb, S. and Saito, T. and Sakaki, N. and Sanchez, D. and Sangiorgi, P. and Sano, H. and Santander, M. and Sarkar, S. and Sawada, M. and Schioppa, E. J. and Schoorlemmer, H. and Schovanek, P. and Schussler, F. and Sergijenko, O. and Servillat, M. and Shalchi, A. and Shellard, R. C. and Siejkowski, H. and Sillanpaa, A. and Simone, D. and Sliusar, V. and Sol, H. and Stanic, S. and Starling, R. and Stawarz, L. and Stefanik, S. and Stephan, M. and Stolarczyk, T. and Szanecki, M. and Szepieniec, T. and Tagliaferri, G. and Tajima, H. and Takahashi, M. and Takeda, J. and Tanaka, M. and Tanaka, S. and Tejedor, L. A. and Telezhinsky, Igor O. and Temnikov, P. and Terada, Y. and Tescaro, D. and Teshima, M. and Testa, V. and Thoudam, S. and Tokanai, F. and Torres, D. F. and Torresi, E. and Tosti, G. and Townsley, C. and Travnicek, P. and Trichard, C. and Trifoglio, M. and Tsujimoto, S. and Vagelli, V. and Vallania, P. and Valore, L. and van Driel, W. and van Eldik, C. and Vandenbroucke, Justin and Vassiliev, V. and Vecchi, M. and Vercellone, Stefano and Vergani, S. and Vigorito, C. and Vorobiov, S. and Vrastil, M. and Vazquez Acosta, M. L. and Wagner, S. J. and Wagner, R. and Wakely, S. P. and Walter, R. and Ward, J. E. and Watson, J. J. and Weinstein, A. and White, M. and White, R. and Wierzcholska, A. and Wilcox, P. and Williams, D. A. and Wischnewski, R. and Wojcik, P. and Yamamoto, T. and Yamamoto, H. and Yamazaki, Ryo and Yanagita, S. and Yang, L. and Yoshida, T. and Yoshida, M. and Yoshiike, S. and Yoshikoshi, T. and Zacharias, M. and Zampieri, L. and Zanin, R. and Zavrtanik, M. and Zavrtanik, D. and Zdziarski, A. and Zech, Alraune and Zechlin, Hannes and Zhdanov, V. and Ziegler, A. and Zorn, J.},
title = {Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7-3946},
series = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
volume = {840},
journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
number = {2},
publisher = {IOP Publ. Ltd.},
address = {Bristol},
issn = {0004-637X},
doi = {10.3847/1538-4357/aa6d67},
pages = {14},
year = {2017},
abstract = {We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7-3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti) correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H I emission. We present a series of simulated images of RX J1713.7-3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton, whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H I observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator.},
language = {en}
}
@article{AbdallaAdamAharonianetal.2020,
author = {Abdalla, H. and Adam, R. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arcaro, C. and Armand, C. and Armstrong, T. and Ashkar, H. and Backes, M. and Baghmanyan, V. and Martins, V. Barbosa and Barnacka, A. and Barnard, M. and Becherini, Y. and Berge, D. and Bernlohr, K. and Bi, B. and Bottcher, M. and Boisson, C. and Bolmont, J. and de Lavergne, M. de Bony and Bordas, Pol and Breuhaus, M. and Brun, F. and Brun, P. and Bryan, M. and Buchele, M. and Bulik, T. and Bylund, T. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Chand, T. and Chandra, S. and Chen, A. and Cotter, G. and Curylo, M. and Mbarubucyeye, J. Damascene and Davids, I. D. and Davies, J. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V. and Duffy, C. and Dyks, J. and Egberts, Kathrin and Eichhorn, F. and Einecke, S. and Emery, G. and Ernenwein, J. -P. and Feijen, K. and Fegan, S. and Fiasson, A. and de Clairfontaine, G. Fichet and Fontaine, G. and Funk, S. and Fussling, Matthias and Gabici, S. and Gallant, Y. A. and Giavitto, G. and Giunti, L. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M. -H. and Hahn, J. and Haupt, M. and Hermann, G. and Hinton, J. A. and Hofmann, W. and Hoischen, Clemens and Holch, T. L. and Holler, M. and Horbe, M. and Horns, D. and Huber, D. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jardin-Blicq, A. and Joshi, V. and Jung-Richardt, I. and Kasai, E. and Kastendieck, M. A. and Katarzynski, K. and Katz, U. and Khangulyan, D. and Khelifi, B. and Klepser, S. and Kluzniak, W. and Komin, Nu. and Konno, R. and Kosack, K. and Kostunin, D. and Kreter, M. and Lamanna, G. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J. -P. and Levy, C. and Lohse, T. and Lypova, I. and Mackey, J. and Majumdar, J. and Malyshev, D. and Malyshev, D. and Marandon, V. and Marchegiani, P. and Marcowith, Alexandre and Mares, A. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Meyer, M. and Mitchell, A. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Montanari, A. and Moore, C. and Morris, P. and Moulin, Emmanuel and Muller, J. and Murach, T. and Nakashima, K. and Nayerhoda, A. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and O'Brien, Patrick and Odaka, H. and Ohm, S. and Olivera-Nieto, L. and Wilhelmi, E. de Ona and Ostrowski, M. and Oya, I. and Panter, M. and Panny, S. and Parsons, R. D. and Peron, G. and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V. and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puhlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reichherzer, P. and Reimer, A. and Reimer, O. and Remy, Q. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V. and Sailer, S. and Sanchez, D. A. and Santangelo, Andrea and Sasaki, M. and Scalici, M. and Schussler, F. and Schutte, H. M. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spencer, S. and Spir-Jacob, M. and Stawarz, L. and Sun, L. and Steenkamp, R. and Stegmann, C. and Steinmassl, S. and Steppa, C. and Takahashi, T. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tiziani, D. and Tluczykont, M. and Tomankova, L. and Trichard, C. and Tsirou, M. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Volk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Watson, J. and Werner, F. and White, R. and Wierzcholska, A. and Wong, Yu Wun and Yusafzai, A. and Zacharias, M. and Zanin, R. and Zargaryan, D. and Zdziarski, A. A. and Zech, Alraune and Zhu, S. J. and Ziegler, A. and Zorn, J. and Zouari, S. and Zywucka, N.},
title = {An extreme particle accelerator in the Galactic plane},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {644},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {0004-6361},
doi = {10.1051/0004-6361/202038851},
pages = {8},
year = {2020},
abstract = {The unidentified very-high-energy (VHE; E > 0.1 TeV) gamma -ray source, HESS J1826-130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady gamma -ray flux from HESS J1826-130, which appears extended with a half-width of 0.21 degrees +/- 0.02
(stat)degrees
stat degrees +/- 0.05
(sys)degrees sys degrees . The source spectrum is best fit with either a power-law function with a spectral index Gamma = 1.78 +/- 0.10(stat) +/- 0.20(sys) and an exponential cut-off at 15.2
(+5.5)(-3.2) -3.2+5.5 TeV, or a broken power-law with Gamma (1) = 1.96 +/- 0.06(stat) +/- 0.20(sys), Gamma (2) = 3.59 +/- 0.69(stat) +/- 0.20(sys) for energies below and above E-br = 11.2 +/- 2.7 TeV, respectively. The VHE flux from HESS J1826-130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, HESS J1825-137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826-130 VHE emission related to PSR J1826-1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826-130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to greater than or similar to 200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2018,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, M. and Barnard, M. and Becherini, Y. and Tjus, J. Becker and Berge, D. and Bernhard, S. and Bernloehr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Dei, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J. -P. and Eschbach, S. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and F{\"u}ssling, Matthias and Gabici, S. and Gallant, Y. A. and Garrigoux, T. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M. -H. and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, J. A. and Hofmann, W. and Hoischen, Clemens and Holch, T. L. and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I. and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Kerszberg, D. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu. and Kosack, K. and Krakau, S. and Kraus, M. and Kruger, R. R. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J. -P. and Leser, Eva and Lohse, T. and Lorentz, M. and Lopez-Coto, R. and Lypova, I. and Malyshev, D. and Marandon, V. and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitche, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I. and Padovani, M. and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P. -O. and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V. and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V. and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Spanier, F. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Sushch, Iurii and Takahashi, T. and Tavernet, J. -P. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Viana, A. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, P. and Wagner, R. M. and White, R. and Wierzcholska, A. and Woernlein, A. and Yang, R. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Zefi, F. and Ziegler, A. and Zorn, J. and Zywucka, N.},
title = {VHE gamma-ray discovery and multiwavelength study of the blazar 1ES 2322-409},
series = {Monthly notices of the Royal Astronomical Society},
volume = {482},
journal = {Monthly notices of the Royal Astronomical Society},
number = {3},
publisher = {Oxford Univ. Press},
address = {Oxford},
organization = {HESS Collaboration},
issn = {0035-8711},
doi = {10.1093/mnras/sty2686},
pages = {3011 -- 3022},
year = {2018},
abstract = {A hotspot at a position compatible with the BL. Lac object 1ES 2322-409 was serendipitously detected with H.E.S.S. during observations performed in 2004 and 2006 on the blazar PKS 2316-423. Additional data on 1ES 2322-409 were taken in 2011 and 2012, leading to a total live-time of 22.3 h. Point-like very-high-energy (VHE; E > 100 GeV) gamma-ray emission is detected from a source centred on the IFS 2322-409 position, with an excess of 116.7 events at a significance of 6.0 sigma. The average VHE gamma-ray spectrum is well described with a power law with a photon index Gamma = 3.40 +/- 0.66(stat) +/- 0.20(sys) and an integral flux Phi(E > 200 GeV) = (3.11 +/- 0.71(stat) 0.62(sys)) x 10(-2)cm(-2)s(-1), which corresponds to 1.1 per cent of the Crab nebula flux above 200 GeV. Multiwavelength data obtained with Fermi LAT, Swift XRT and UVOT, RXTE PCA, ATOM, and additional data from WISE, GROND, and Catalina are also used to characterize the broad-band non-thermal emission of lES 2322-409. The multiwavelength behaviour indicates day-scale variability. Swift UVOT and XRT data show strong variability at longer scales. A spectral energy distribution (SED) is built from contemporaneous observations obtained around a high state identified in Swift data. A modelling of the SED is performed with a stationary homogeneous one-zone synchrotronself-Compton leptonic model. The redshift of the source being unknown, two plausible values were tested for the modelling. A systematic scan of the model parameters space is performed, resulting in a well-constrained combination of values providing a good description of the broad-band behaviour of 1ES 2322-409.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2019,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, M. and Barnard, M. and Becherini, Y. and Tjus, J. Becker and Berge, D. and Bernloehr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buchele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chand, T. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V. and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J. -P. and Eschbach, S. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M. -H. and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, James Anthony and Hofmann, W. and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I. and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu. and Kosack, K. and Kraus, M. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J. -P. and Leser, Eva and Lohse, T. and Lopez-Coto, R. and Lorentz, M. and Lypova, I. and Malyshev, D. and Marandon, V. and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moore, C. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I. and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P. -O. and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V. and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V. and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schutte, H. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernet, J. -P. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, R. M. and White, R. and Wierzcholska, A. and Yang, R. and Yoneda, H. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Ziegler, A. and Zorn, J. and Zywucka, N.},
title = {H.E.S.S. observations of the flaring gravitationally lensed galaxy PKS 1830-211},
series = {Monthly notices of the Royal Astronomical Society},
volume = {486},
journal = {Monthly notices of the Royal Astronomical Society},
number = {3},
publisher = {Oxford Univ. Press},
address = {Oxford},
organization = {H E S S Collaboration},
issn = {0035-8711},
doi = {10.1093/mnras/stz1031},
pages = {3886 -- 3891},
year = {2019},
abstract = {PKS 1830-211 is a known macrolensed quasar located at a redshift of z = 2.5. Its highenergy gamma-ray emission has been detected with the Fermi-Large Area Telescope (LAT) instrument and evidence for lensing was obtained by several authors from its high-energy data. Observations of PKS 1830-211 were taken with the High Energy Stereoscopic System (H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014 August, following a flare alert by the Fermi-LAT Collaboration. The H.E.S.S observations were aimed at detecting a gamma-ray flare delayed by 20-27 d from the alert flare, as expected from observations at other wavelengths. More than 12 h of good-quality data were taken with an analysis threshold of similar to 67 GeV. The significance of a potential signal is computed as a function of the date and the average significance over the whole period. Data are compared to simultaneous observations by Fermi-LAT. No photon excess or significant signal is detected. An upper limit on PKS 1830-211 flux above 67 GeV is computed and compared to the extrapolation of the Fermi-LAT flare spectrum.},
language = {en}
}
@article{AbdallaAdamAharonianetal.2019,
author = {Abdalla, Hassan E. and Adam, R. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Ashkar, H. and Backes, M. and Martins, V. Barbosa and Barnard, M. and Becherini, Y. and Berge, D. and Bernloehr, K. and Bissaldi, E. and Blackwell, R. and Boettcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bregeon, J. and Breuhaus, M. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chand, T. and Chandra, S. and Chen, A. and Colafrancesco, S. and Curylo, M. and Davids, I. D. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Feijen, K. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fussling, Matthias and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Giunti, L. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, J. A. and Hofmann, W. and Hoischen, Clemens and Holch, T. L. and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jardin-Blicq, A. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Kostunin, D. and Kreter, M. and Lamanna, G. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Levy, C. and Lohse, T. and Lypova, I and Mackey, J. and Majumdar, J. and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mares, A. and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moore, C. and Moulin, Emmanuel and Muller, J. and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Wilhelmi, E. de Ona and Ostrowski, M. and Oya, I and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Remy, Q. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Sailer, S. and Saito, S. and Sanchez, D. A. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schutte, H. M. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and White, R. and Wierzcholska, A. and Yang, R. and Yoneda, H. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Ziegler, A. and Zorn, J. and Zywucka, N. and de Palma, F. and Axelsson, M. and Roberts, O. J.},
title = {A very-high-energy component deep in the gamma-ray burst afterglow},
series = {Nature : the international weekly journal of science},
volume = {575},
journal = {Nature : the international weekly journal of science},
number = {7783},
publisher = {Nature Publ. Group},
address = {London},
issn = {0028-0836},
doi = {10.1038/s41586-019-1743-9},
pages = {464 -- +},
year = {2019},
abstract = {Gamma-ray bursts (GRBs) are brief flashes of gamma-rays and are considered to be the most energetic explosive phenomena in the Universe(1). The emission from GRBs comprises a short (typically tens of seconds) and bright prompt emission, followed by a much longer afterglow phase. During the afterglow phase, the shocked outflow-produced by the interaction between the ejected matter and the circumburst medium-slows down, and a gradual decrease in brightness is observed(2). GRBs typically emit most of their energy via.-rays with energies in the kiloelectronvolt-to-megaelectronvolt range, but a few photons with energies of tens of gigaelectronvolts have been detected by space-based instruments(3). However, the origins of such high-energy (above one gigaelectronvolt) photons and the presence of very-high-energy (more than 100 gigaelectronvolts) emission have remained elusive(4). Here we report observations of very-high-energy emission in the bright GRB 180720B deep in the GRB afterglow-ten hours after the end of the prompt emission phase, when the X-ray flux had already decayed by four orders of magnitude. Two possible explanations exist for the observed radiation: inverse Compton emission and synchrotron emission of ultrarelativistic electrons. Our observations show that the energy fluxes in the X-ray and gamma-ray range and their photon indices remain comparable to each other throughout the afterglow. This discovery places distinct constraints on the GRB environment for both emission mechanisms, with the inverse Compton explanation alleviating the particle energy requirements for the emission observed at late times. The late timing of this detection has consequences for the future observations of GRBs at the highest energies.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2018,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, M. and Barnard, M. and Becherini, Y. and Tjus, J. Becker and Berge, D. and Bernhard, S. and Bernlohr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chandra, S. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, J. A. and Hofmann, W. and Hoischen, Clemens and Holch, T. L. and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Kerszberg, D. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Krakau, S. and Kraus, M. and Kr{\"u}ger, P. P. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Lohse, T. and Lorentz, M. and Lopez-Coto, R. and Lypova, I and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I and Padovani, M. and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, D. A. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Spanier, F. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernet, J-P and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, R. M. and White, R. and Wierzcholska, A. and Yang, R. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Zefi, F. and Ziegler, A. and Zorn, J. and Zywucka, N. and Kerr, M. and Johnston, S. and Shannon, R. M.},
title = {First ground-based measurement of sub-20 GeV to 100 GeV gamma-Rays from the Vela pulsar with HESS II},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {620},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {1432-0746},
doi = {10.1051/0004-6361/201732153},
pages = {14},
year = {2018},
abstract = {Aims. We report on the measurement and investigation of pulsed high-energy y-ray emission from the Vela pulsar, PSR B0833-45, based on observations with the largest telescope of H.E.S.S., CT5, in monoscopic mode, and on data obtained with the Fermi-LAT. Methods. Data from 40.3 h of observations carried out with the H.E.S.S. II array from 2013 to 2015 have been used. A dedicated very low-threshold event reconstruction and analysis pipeline was developed to achieve the lowest possible energy threshold. Eight years of Fermi-LAT data were analysed and also used as reference to validate the CT5 telescope response model and analysis methods. Results. A pulsed gamma-ray signal at a significance level of more than 15 sigma is detected from the P2 peak of the Vela pulsar light curve. Of a total of 15 835 events, more than 6000 lie at an energy below 20 GeV, implying a significant overlap between H.E.S.S. II-CT5 and the Fermi-LAT. While the investigation of the pulsar light curve with the LAT confirms characteristics previously known up to 20 GeV in the tens of GeV energy range, CT5 data show a change in the pulse morphology of P2, i.e. an extreme sharpening of its trailing edge, together with the possible onset of a new component at 3.4 sigma significance level. Assuming a power-law model for the P2 spectrum, an excellent agreement is found for the photon indices (Gamma similar or equal to 4.1) obtained with the two telescopes above 10 GeV and an upper bound of 8\% is derived on the relative offset between their energy scales. Using data from both instruments, it is shown however that the spectrum of P2 in the 10-100 GeV has a pronounced curvature; this is a confirmation of the sub-exponential cut-off form found at lower energies with the LAT. This is further supported by weak evidence of an emission above 100 GeV obtained with CT5. In contrast, converging indications are found from both CT5 and LAT data for the emergence of a hard component above 50 GeV in the leading wing (LW2) of P2, which possibly extends beyond 100 GeV. Conclusions. The detection demonstrates the performance and understanding of CT5 from 100 GeV down to the sub-20 GeV domain, i.e. unprecedented low energy for ground-based gamma-ray astronomy. The extreme sharpening of the trailing edge of the P2 peak found in the H.E.S.S. II light curve of the Vela pulsar and the possible extension beyond 100 GeV of at least one of its features, LW2, provide further constraints to models of gamma-Ray emission from pulsars.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2018,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, M. and Barnard, M. and Becherini, Y. and Tjus, J. Becker and Berge, D. and Bernhard, S. and Bernloehr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Dei, C. and Devin, J. and dewilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Garrigoux, T. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, J. A. and Hofmann, W. and Hoischen, Clemens and Holch, T. L. and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Kerszberg, D. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Krakau, S. and Kraus, M. and Kruger, P. P. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Lohse, T. and Lorentz, M. and Lopez-Coto, R. and Lypova, I and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I and Padovani, M. and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowel, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, D. A. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Spanier, F. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Sushch, I and Takahashi, T. and Tavernet, J-P and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Viana, A. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, P. and Wagner, R. M. and White, R. and Wierzcholska, A. and Woernlein, A. and Yang, R. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Zefi, F. and Ziegler, A. and Zorn, J. and Zywucka, N.},
title = {The starburst galaxy NGC 253 revisited by HESS and Fermi-LAT},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {617},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {1432-0746},
doi = {10.1051/0004-6361/201833202},
pages = {7},
year = {2018},
abstract = {Context. NGC 253 is one of only two starburst galaxies found to emit gamma-rays from hundreds of MeV to multi-TeV energies. Accurate measurements of the very-high-energy (VHE; E> 100 GeV) and high-energy (HE; E > 60 MeV) spectra are crucial to study the underlying particle accelerators, probe the dominant emission mechanism(s) and to study cosmic-ray interaction and transport. Aims. The measurement of the VHE gamma-ray emission of NGC 253 published in 2012 by H.E.S.S. was limited by large systematic uncertainties. Here, the most up to date measurement of the gamma-ray spectrum of NGC 253 is investigated in both HE and VHE gamma-rays. Assuming a hadronic origin of the gamma-ray emission, the measurement uncertainties are propagated into the interpretation of the accelerated particle population. Methods. The data of H.E.S.S. observations are reanalysed using an updated calibration and analysis chain. The improved Fermi-LAT analysis employs more than 8 yr of data processed using pass 8. The cosmic-ray particle population is evaluated from the combined HE-VHE gamma-ray spectrum using NAIMA in the optically thin case. Results. The VHE gamma-ray energy spectrum is best fit by a power-law distribution with a flux normalisation of (1.34 +/- 0.14(stat) +/- 0.27(sys)) x 10(-13) cm(-2) s(-1) TeV-1 at 1 TeV - about 40\% above, but compatible with the value obtained in Abramowski et al. (2012). The spectral index Gamma = 2.39 +/- 0.14(stat) +/- 0.25(sys) is slightly softer than but consistent with the previous measurement within systematic errors. In the Fermi energy range an integral flux of F(E > 60 MeV) = (1.56 +/- 0.28(stat) +/- 0.15(sys)) x 10(-8) cm(-2) s(-1) is obtained. At energies above similar to 3 GeV the HE spectrum is consistent with a power-law ranging into the VHE part of the spectrum measured by H.E.S.S. with an overall spectral index Gamma = 2.22 +/- 0.06(stat). Conclusions. Two scenarios for the starburst nucleus are tested, in which the gas in the starburst nucleus acts as either a thin or a thick target for hadronic cosmic rays accelerated by the individual sources in the nucleus. In these two models, the level to which NGC 253 acts as a calorimeter is estimated to a range of f(cal) = 0.1 to 1 while accounting for the measurement uncertainties. The presented spectrum is likely to remain the most accurate measurements until the Cherenkov Telescope Array (CTA) has collected a substantial set of data towards NGC 253.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2019,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Anguener, E. O. and Arakawa, M. and Arcaro, C. and Armand, C. and Ashkar, H. and Backes, M. and Martins, V. Barbosa and Barnard, M. and Becherini, Y. and Berge, D. and Bernloehr, K. and Blackwell, R. and Boettcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bregeon, J. and Breuhaus, M. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chand, T. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Curylo, M. and Davids, I. D. and Deil, C. and Devin, J. and de Wilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-p and Eschbach, S. and Feijen, K. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, James Anthony and Hofmann, W. and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Kostunin, D. and Kraus, M. and Lamanna, G. and Lau, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Levy, C. and Lohse, T. and Lopez-Coto, R. and Lypova, I and Mackey, J. and Majumdar, J. and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mares, A. and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Muller, J. and Moore, C. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Wilhelmi, E. de Ona and Ostrowski, M. and Oya, I and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Remy, Q. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schutte, H. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and White, R. and Wierzcholska, A. and Yang, R. and Yoneda, H. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Ziegler, A. and Zorn, J. and Zywucka, N. and Maxted, N.},
title = {Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S.},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {626},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {1432-0746},
doi = {10.1051/0004-6361/201935242},
pages = {11},
year = {2019},
abstract = {Young core-collapse supernovae with dense-wind progenitors may be able to accelerate cosmic-ray hadrons beyond the knee of the cosmic-ray spectrum, and this may result in measurable gamma-ray emission. We searched for gamma-ray emission from ten super- novae observed with the High Energy Stereoscopic System (H.E.S.S.) within a year of the supernova event. Nine supernovae were observed serendipitously in the H.E.S.S. data collected between December 2003 and December 2014, with exposure times ranging from 1.4 to 53 h. In addition we observed SN 2016adj as a target of opportunity in February 2016 for 13 h. No significant gamma-ray emission has been detected for any of the objects, and upper limits on the >1 TeV gamma-ray flux of the order of similar to 10(-13) cm(-)(2)s(-1) are established, corresponding to upper limits on the luminosities in the range similar to 2 x 10(39) to similar to 1 x 10(42) erg s(-1). These values are used to place model-dependent constraints on the mass-loss rates of the progenitor stars, implying upper limits between similar to 2 x 10(-5) and similar to 2 x 10(-3) M-circle dot yr(-1) under reasonable assumptions on the particle acceleration parameters.},
language = {en}
}
@article{AbdallaAdamAharonianetal.2019,
author = {Abdalla, Hassan E. and Adam, R. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Ashkar, H. and Backes, M. and Martins, V. Barbosa and Barnard, M. and Becherini, Y. and Berge, D. and Bernloehr, K. and Blackwell, R. and B{\"o}ttcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bregeon, J. and Breuhaus, M. and Brun, F. and Brun, P. and Bryan, M. and B{\"u}chele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chand, T. and Chandra, S. and Chen, A. and Colafrancesco, S. and Curylo, M. and Davids, I. D. and Deil, C. and Devin, J. and DeWilt, P. and Dirson, L. and Djannati-Ata, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Feijen, K. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and F{\"u}ßling, Matthias and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, James Anthony and Hofmann, W. and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jardin-Blicq, A. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Kostunin, D. and Kraus, M. and Lamanna, G. and Lau, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Levy, C. and Lohse, T. and Lypova, I and Mackey, J. and Majumdar, J. and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mares, A. and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moore, C. and Moulin, Emmanuel and Muller, J. and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Wilhelmi, E. de Ona and Ostrowski, M. and Oya, I and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Priyana Noel, A. and Prokhorov, D. A. and Prokoph, H. and P{\"u}hlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Remy, Q. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Sch{\"u}ssler, F. and Schulz, A. and Schutte, H. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van Der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and White, R. and Wierzcholska, A. and Yang, R. and Yoneda, H. and Zacharias, Michael and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Ziegler, A. and Zorn, J. and Zywucka, N. and Meyer, M.},
title = {Constraints on the emission region of 3C 279 during strong flares in 2014 and 2015 through VHE gamma-ray observations with HESS},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {627},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {1432-0746},
doi = {10.1051/0004-6361/201935704},
pages = {19},
year = {2019},
abstract = {The flat spectrum radio quasar 3C 279 is known to exhibit pronounced variability in the high-energy (100MeV < E < 100 GeV) gamma-ray band, which is continuously monitored with Fermi-LAT. During two periods of high activity in April 2014 and June 2015 target-of-opportunity observations were undertaken with the High Energy Stereoscopic System (H.E.S.S.) in the very-high-energy (VHE, E > 100 GeV) gamma-ray domain. While the observation in 2014 provides an upper limit, the observation in 2015 results in a signal with 8 : 7 sigma significance above an energy threshold of 66 GeV. No VHE variability was detected during the 2015 observations. The VHE photon spectrum is soft and described by a power-law index of 4.2 +/- 0.3. The H.E.S.S. data along with a detailed and contemporaneous multiwavelength data set provide constraints on the physical parameters of the emission region. The minimum distance of the emission region from the central black hole was estimated using two plausible geometries of the broad-line region and three potential intrinsic spectra. The emission region is confidently placed at r greater than or similar to 1 : 7 X 1017 cm from the black hole, that is beyond the assumed distance of the broad-line region. Time-dependent leptonic and lepto-hadronic one-zone models were used to describe the evolution of the 2015 flare. Neither model can fully reproduce the observations, despite testing various parameter sets. Furthermore, the H.E.S.S. data were used to derive constraints on Lorentz invariance violation given the large redshift of 3C 279.},
language = {en}
}
@article{AbdallaAharonianAitBenkhalietal.2018,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Ait Benkhali, Faical and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, Michael and Barnard, M. and Becherini, Yvonne and Tjus, J. Becker and Berge, D. and Bernhard, S. and Bernl{\"o}hr, Konrad and Blackwell, R. and B{\"o}ttcher, Markus and Boisson, C. and Bolmont, Julien and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and B{\"u}chele, M. and Bulik, Tomasz and Bylund, Tomas and Capasso, Massimo and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, Matteo and Chakraborty, Nachiketa and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, Sergio and Condon, B. and Davids, Isak and Deil, Christoph and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, Axel and Doroshenko, Victor and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J. -P. and Eschbach, Stefan and Fegan, S. and Fiasson, Armand and Fontaine, G. and Funk, Sebastian and F{\"u}ßling, Matthias and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, Gianluca and Eisenacher Glawion, Dorit and Glicenstein, Jean-Fran{\c{c}}ois and Gottschall, D. and Grondin, Marie-H{\´e}l{\`e}ne and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, Gilles and Hermann, G. and Hinton, James Anthony and Hofmann, Werner and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, David and Jankowsky, Felix and Jouvin, L. and Jung-Richardt, I. and Kastendieck, M. A. and Katarzyński, Krzysztof and Katsuragawa, M. and Katz, U. and Kerszberg, D. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu. and Kosack, K. and Krakau, S. and Kraus, M. and Kruger, P. P. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J. -P. and Leser, Eva and Lohse, T. and Lorentz, M. and Lopez-Coto, R. and Lypova, I. and Malyshev, D. and Marandon, V. and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I. and Padovani, M. and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P. -O. and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V. and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V. and Saito, S. and Sanchez, D. A. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I. and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Spanier, F. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernet, J. -P. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Viana, A. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, R. M. and White, R. and Wierzcholska, A. and Yang, R. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. and Zech, Alraune and Zefi, F. and Ziegler, A. and Zorn, J. and Zywucka, N. and Cirelli, M. and Panci, P. and Sala, F. and Silk, J. and Taoso, M.},
title = {Searches for gamma-ray lines and 'pure WIMP' spectra from Dark Matter annihilations in dwarf galaxies with H.E.S.S.},
series = {Journal of cosmology and astroparticle physics},
journal = {Journal of cosmology and astroparticle physics},
number = {11},
publisher = {IOP Publishing Ltd. (Bristol)},
address = {Bristol},
organization = {HESS Collaboration},
issn = {1475-7516},
doi = {10.1088/1475-7516/2018/11/037},
pages = {22},
year = {2018},
abstract = {Dwarf spheroidal galaxies are among the most promising targets for detecting signals of Dark Matter (DM) annihilations. The H.E.S.S. experiment has observed five of these systems for a total of about 130 hours. The data are re-analyzed here, and, in the absence of any detected signals, are interpreted in terms of limits on the DM annihilation cross section. Two scenarios are considered: i) DM annihilation into mono-energetic gamma-rays and ii) DM in the form of pure WIMP multiplets that, annihilating into all electroweak bosons, produce a distinctive gamma-ray spectral shape with a high-energy peak at the DM mass and a lower-energy continuum. For case i), upper limits at 95\% confidence level of about less than or similar to 3 x 10(-25) cm(3) s(-1) are obtained in the mass range of 400 GeV to 1TeV. For case ii), the full spectral shape of the models is used and several excluded regions are identified, but the thermal masses of the candidates are not robustly ruled out.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2019,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, M. and Barnard, M. and Becherini, Y. and Tjus, J. Becker and Berge, D. and Bernloehr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chand, T. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, James Anthony and Hofmann, W. and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Kerszberg, D. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Kraus, M. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Lohse, T. and Lopez-Coto, R. and Lypova, I and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moore, C. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schutte, H. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernet, J-P and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, R. M. and White, R. and Wierzcholska, A. and Yang, R. and Yoneda, H. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Zefi, F. and Ziegler, A. and Zorn, J. and Zywucka, N.},
title = {Particle transport within the pulsar wind nebula HESS J1825-137},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {621},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {1432-0746},
doi = {10.1051/0004-6361/201834335},
pages = {18},
year = {2019},
abstract = {Context. We present a detailed view of the pulsar wind nebula (PWN) HESS J1825-137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics. Aims. The nebula was studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) gamma-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5 degrees from the pulsar, similar to 1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of similar to 100 pc, potentially the largest gamma-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of R proportional to E alpha with alpha = -0.29 +/- 0.04(stat) +/- 0.05(sys) disfavours a pure diffusion scenario for particle transport within the nebula. The total gamma-ray flux of the nebula above 1 TeV is found to be (1.12 +/- 0.03(stat) +/- 0.25(sys)) +/- 10(-11) cm(-2) s(-1), corresponding to similar to 64\% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE gamma-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2019,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Arrieta, M. and Backes, M. and Barnard, M. and Becherini, Y. and Tjus, J. Becker and Berge, D. and Bernhard, S. and Bernloehr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bordas, Pol and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Cerruti, M. and Chakraborty, N. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, James Anthony and Hofmann, W. and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Kerszberg, D. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Krakau, S. and Kraus, M. and Kruger, P. P. and Lamanna, G. and Lau, J. and Lefaucheur, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Lohse, T. and Lorentz, M. and Lopez-Coto, R. and Lypova, I and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Ostrowski, M. and Oya, I and Padovani, M. and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Spanier, F. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernet, J-P and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, R. M. and White, R. and Wierzcholska, A. and Yang, R. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Zefi, F. and Ziegler, A. and Zorn, J. and Zywucka, N.},
title = {The 2014TeV gamma-Ray Flare of Mrk 501 Seen with HESS},
series = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
volume = {870},
journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
number = {2},
publisher = {IOP Publ. Ltd.},
address = {Bristol},
organization = {HESS Collaboration},
issn = {0004-637X},
doi = {10.3847/1538-4357/aaf1c4},
pages = {9},
year = {2019},
abstract = {The blazar Mrk 501 (z = 0.034) was observed at very-high-energy (VHE, E greater than or similar to 100 GeV) gamma-ray wavelengths during a bright flare on the night of 2014 June 23-24 (MJD 56832) with the H.E.S.S. phase-II array of Cherenkov telescopes. Data taken that night by H.E.S.S. at large zenith angle reveal an exceptional number of gamma-ray photons at multi-TeV energies, with rapid flux variability and an energy coverage extending significantly up to 20 TeV. This data set is used to constrain Lorentz invariance violation (LIV) using two independent channels: a temporal approach considers the possibility of an energy dependence in the arrival time of gamma-rays, whereas a spectral approach considers the possibility of modifications to the interaction of VHE gamma-rays with extragalactic background light (EBL) photons. The non-detection of energy-dependent time delays and the non-observation of deviations between the measured spectrum and that of a supposed power-law intrinsic spectrum with standard EBL attenuation are used independently to derive strong constraints on the energy scale of LIV (E-QG) in the subluminal scenario for linear and quadratic perturbations in the dispersion relation of photons. For the case of linear perturbations, the 95\% confidence level limits obtained are E-QG,E-1 > 3.6 x 10(17) GeV using the temporal approach and E-QG,E-1 > 2.6 x 10(19) GeV using the spectral approach. For the case of quadratic perturbations, the limits obtained are E-QG,E-2 > 8.5 x 10(10) GeV using the temporal approach and E-QG,E-2 > 7.8 x 10(11) GeV using the spectral approach.},
language = {en}
}
@article{AbdallaAharonianBenkhalietal.2019,
author = {Abdalla, Hassan E. and Aharonian, Felix A. and Benkhali, F. Ait and Ang{\"u}ner, Ekrem Oǧuzhan and Arakawa, M. and Arcaro, C. and Armand, C. and Backes, M. and Barnard, M. and Becherini, Y. and Berge, D. and Bernloehr, K. and Blackwell, R. and Bottcher, M. and Boisson, C. and Bolmont, J. and Bonnefoy, S. and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Buechele, M. and Bulik, T. and Bylund, T. and Capasso, M. and Caroff, S. and Carosi, A. and Casanova, Sabrina and Cerruti, M. and Chakraborty, N. and Chand, T. and Chandra, S. and Chaves, R. C. G. and Chen, A. and Colafrancesco, S. and Condon, B. and Davids, I. D. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and Djannati-Atai, A. and Dmytriiev, A. and Donath, A. and Doroshenko, V and Dyks, J. and Egberts, Kathrin and Emery, G. and Ernenwein, J-P and Eschbach, S. and Feijen, K. and Fegan, S. and Fiasson, A. and Fontaine, G. and Funk, S. and Fuessling, M. and Gabici, S. and Gallant, Y. A. and Gate, F. and Giavitto, G. and Glawion, D. and Glicenstein, J. F. and Gottschall, D. and Grondin, M-H and Hahn, J. and Haupt, M. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hinton, James Anthony and Hofmann, W. and Hoischen, Clemens and Holch, Tim Lukas and Holler, M. and Horns, D. and Huber, D. and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and Jankowsky, D. and Jankowsky, F. and Jouvin, L. and Jung-Richardt, I and Kastendieck, M. A. and Katarzynski, K. and Katsuragawa, M. and Katz, U. and Khangulyan, D. and Khelifi, B. and King, J. and Klepser, S. and Kluzniak, W. and Komin, Nu and Kosack, K. and Kostunin, D. and Kraus, M. and Lamanna, G. and Lau, J. and Lemiere, A. and Lemoine-Goumard, M. and Lenain, J-P and Leser, Eva and Lohse, T. and Lopez-Coto, R. and Lypova, I and Malyshev, D. and Marandon, V and Marcowith, Alexandre and Mariaud, C. and Marti-Devesa, G. and Marx, R. and Maurin, G. and Maxted, N. and Meintjes, P. J. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Moore, C. and Moulin, Emmanuel and Murach, T. and Nakashima, S. and de Naurois, M. and Ndiyavala, H. and Niederwanger, F. and Niemiec, J. and Oakes, L. and Odaka, H. and Ohm, S. and Wilhelmi, E. de Ona and Ostrowski, M. and Oya, I and Panter, M. and Parsons, R. D. and Perennes, C. and Petrucci, P-O and Peyaud, B. and Piel, Q. and Pita, S. and Poireau, V and Noel, A. Priyana and Prokhorov, D. A. and Prokoph, H. and Puehlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Rauth, R. and Reimer, A. and Reimer, O. and Renaud, M. and Rieger, F. and Rinchiuso, L. and Romoli, C. and Rowell, G. and Rudak, B. and Ruiz-Velasco, E. and Sahakian, V and Saito, S. and Sanchez, David M. and Santangelo, Andrea and Sasaki, M. and Schlickeiser, R. and Schussler, F. and Schulz, A. and Schutte, H. and Schwanke, U. and Schwemmer, S. and Seglar-Arroyo, M. and Senniappan, M. and Seyffert, A. S. and Shafi, N. and Shilon, I and Shiningayamwe, K. and Simoni, R. and Sinha, A. and Sol, H. and Specovius, A. and Spir-Jacob, M. and Stawarz, L. and Steenkamp, R. and Stegmann, Christian and Steppa, Constantin Beverly and Takahashi, T. and Tavernet, J-P and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, Luigi and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tsirou, M. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Vincent, P. and Vink, J. and Voisin, F. and Voelk, H. J. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and White, R. and Wierzcholska, A. and Yang, R. and Yoneda, H. and Zaborov, D. and Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech, Alraune and Ziegler, A. and Zorn, J. and Zywucka, N.},
title = {H.E.S.S. and Suzaku observations of the Vela X pulsar wind nebula},
series = {Astronomy and astrophysics : an international weekly journal},
volume = {627},
journal = {Astronomy and astrophysics : an international weekly journal},
publisher = {EDP Sciences},
address = {Les Ulis},
organization = {HESS Collaboration},
issn = {1432-0746},
doi = {10.1051/0004-6361/201935458},
pages = {16},
year = {2019},
abstract = {Context. Pulsar wind nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission towards an elongated structure called the cocoon. Aims. Since TeV emission is likely inverse-Compton emission of electrons, predominantly from interactions with the cosmic microwave background, while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. Methods. We used data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3 to 4 pc from the pulsar along the cocoon. We obtained gamma-ray spectra of the same regions from H.E.S.S. observations and fitted a radiative model to the multi-wavelength spectra. Results. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order 10(-12) erg cm(-3). The data indicate the presence of a cutoff in the electron spectrum at energies of similar to 100 TeV and a magnetic field strength of similar to 6 mu G. Constraints on the presence of turbulent magnetic fields are weak. Conclusions. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component to balance the pulsar wind at the termination shock. Sub-TeV electrons cannot completely account for the missing pressure, which may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion, but for the latter the role of radiative losses near the termination shock needs to be further investigated in the light of the measured cutoff energies. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range greater than or similar to 10 keV.},
language = {en}
}
@article{QiuKruegerWilkeetal.2016,
author = {Qiu, C. and Kr{\"u}ger, Y. and Wilke, Max and Marti, D. and Ricka, J. and Frenz, M.},
title = {Exploration of the phase diagram of liquid water in the low-temperature metastable region using synthetic fluid inclusions},
series = {Physical chemistry, chemical physics : a journal of European Chemical Societies},
volume = {18},
journal = {Physical chemistry, chemical physics : a journal of European Chemical Societies},
publisher = {Royal Society of Chemistry},
address = {Cambridge},
issn = {1463-9076},
doi = {10.1039/c6cp04250c},
pages = {28227 -- 28241},
year = {2016},
abstract = {We present new experimental data of the low-temperature metastable region of liquid water derived from high-density synthetic fluid inclusions (996-916 kg m(-3)) in quartz. Microthermometric measurements include: (i) prograde (upon heating) and retrograde (upon cooling) liquid-vapour homogenisation. We used single ultrashort laser pulses to stimulate vapour bubble nucleation in initially monophase liquid inclusions. Water densities were calculated based on prograde homogenisation temperatures using the IAPWS-95 formulation. We found retrograde liquid-vapour homogenisation temperatures in excellent agreement with IAPWS-95. (ii) Retrograde ice nucleation. Raman spectroscopy was used to determine the nucleation of ice in the absence of the vapour bubble. Our ice nucleation data in the doubly metastable region are inconsistent with the low-temperature trend of the spinodal predicted by IAPWS-95, as liquid water with a density of 921 kg m(-3) remains in a homogeneous state during cooling down to a temperature of -30.5 degrees C, where it is transformed into ice whose density corresponds to zero pressure. (iii) Ice melting. Ice melting temperatures of up to 6.8 degrees C were measured in the absence of the vapour bubble, i.e. in the negative pressure region. (iv) Spontaneous retrograde and, for the first time, prograde vapour bubble nucleation. Prograde bubble nucleation occurred upon heating at temperatures above ice melting. The occurrence of prograde and retrograde vapour bubble nucleation in the same inclusions indicates a maximum of the bubble nucleation curve in the R-T plane at around 40 degrees C. The new experimental data represent valuable benchmarks to evaluate and further improve theoretical models describing the p-V-T properties of metastable water in the low-temperature region.},
language = {en}
}