TY  - JOUR
A1  - Actis, M.
A1  - Agnetta, G.
A1  - Aharonian, Felix A.
A1  - Akhperjanian, A. G.
A1  - Aleksic, J.
A1  - Aliu, E.
A1  - Allan, D.
A1  - Allekotte, I.
A1  - Antico, F.
A1  - Antonelli, L. A.
A1  - Antoranz, P.
A1  - Aravantinos, A.
A1  - Arlen, T.
A1  - Arnaldi, H.
A1  - Artmann, S.
A1  - Asano, K.
A1  - Asorey, H. G.
A1  - Baehr, J.
A1  - Bais, A.
A1  - Baixeras, C.
A1  - Bajtlik, S.
A1  - Balis, D.
A1  - Bamba, A.
A1  - Barbier, C.
A1  - Barcelo, M.
A1  - Barnacka, Anna
A1  - Barnstedt, Jürgen
A1  - de Almeida, U. Barres
A1  - Barrio, J. A.
A1  - Basso, S.
A1  - Bastieri, D.
A1  - Bauer, C.
A1  - Becerra Gonzalez, J.
A1  - Becherini, Yvonne
A1  - Bechtol, K. C.
A1  - Becker, J.
A1  - Beckmann, Volker
A1  - Bednarek, W.
A1  - Behera, B.
A1  - Beilicke, M.
A1  - Belluso, M.
A1  - Benallou, M.
A1  - Benbow, W.
A1  - Berdugo, J.
A1  - Berger, K.
A1  - Bernardino, T.
A1  - Bernlöhr, K.
A1  - Biland, A.
A1  - Billotta, S.
A1  - Bird, T.
A1  - Birsin, E.
A1  - Bissaldi, E.
A1  - Blake, S.
A1  - Blanch Bigas, O.
A1  - Bobkov, A. A.
A1  - Bogacz, L.
A1  - Bogdan, M.
A1  - Boisson, Catherine
A1  - Boix Gargallo, J.
A1  - Bolmont, J.
A1  - Bonanno, G.
A1  - Bonardi, A.
A1  - Bonev, T.
A1  - Borkowski, Janett
A1  - Botner, O.
A1  - Bottani, A.
A1  - Bourgeat, M.
A1  - Boutonnet, C.
A1  - Bouvier, A.
A1  - Brau-Nogue, S.
A1  - Braun, I.
A1  - Bretz, T.
A1  - Briggs, M. S.
A1  - Brun, Pierre
A1  - Brunetti, L.
A1  - Buckley, H.
A1  - Bugaev, V.
A1  - Buehler, R.
A1  - Bulik, Tomasz
A1  - Busetto, G.
A1  - Buson, S.
A1  - Byrum, K.
A1  - Cailles, M.
A1  - Cameron, R. A.
A1  - Canestrari, R.
A1  - Cantu, S.
A1  - Carmona, E.
A1  - Carosi, A.
A1  - Carr, John
A1  - Carton, P. H.
A1  - Casiraghi, M.
A1  - Castarede, H.
A1  - Catalano, O.
A1  - Cavazzani, S.
A1  - Cazaux, S.
A1  - Cerruti, B.
A1  - Cerruti, M.
A1  - Chadwick, M.
A1  - Chiang, J.
A1  - Chikawa, M.
A1  - Cieslar, M.
A1  - Ciesielska, M.
A1  - Cillis, A. N.
A1  - Clerc, C.
A1  - Colin, P.
A1  - Colome, J.
A1  - Compin, M.
A1  - Conconi, P.
A1  - Connaughton, V.
A1  - Conrad, Jan
A1  - Contreras, J. L.
A1  - Coppi, P.
A1  - Corlier, M.
A1  - Corona, P.
A1  - Corpace, O.
A1  - Corti, D.
A1  - Cortina, J.
A1  - Costantini, H.
A1  - Cotter, G.
A1  - Courty, B.
A1  - Couturier, S.
A1  - Covino, S.
A1  - Croston, J.
A1  - Cusumano, G.
A1  - Daniel, M. K.
A1  - Dazzi, F.
A1  - Deangelis, A.
A1  - de Cea del Pozo, E.
A1  - Dal Pino, E. M. de Gouveia
A1  - de Jager, O.
A1  - de la Calle Perez, I.
A1  - De La Vega, G.
A1  - De Lotto, B.
A1  - de Naurois, M.
A1  - Wilhelmi, E. de Ona
A1  - de Souza, V.
A1  - Decerprit, B.
A1  - Deil, C.
A1  - Delagnes, E.
A1  - Deleglise, G.
A1  - Delgado, C.
A1  - Dettlaff, T.
A1  - Di Paolo, A.
A1  - Di Pierro, F.
A1  - Diaz, C.
A1  - Dick, J.
A1  - Dickinson, H.
A1  - Digel, S. W.
A1  - Dimitrov, D.
A1  - Disset, G.
A1  - Djannati-Ataï, A.
A1  - Doert, M.
A1  - Domainko, W.
A1  - Dorner, D.
A1  - Doro, M.
A1  - Dournaux, J. -L.
A1  - Dravins, D.
A1  - Drury, L.
A1  - Dubois, F.
A1  - Dubois, R.
A1  - Dubus, G.
A1  - Dufour, C.
A1  - Durand, D.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Edy, E.
A1  - Egberts, Kathrin
A1  - Eleftheriadis, C.
A1  - Elles, S.
A1  - Emmanoulopoulos, D.
A1  - Enomoto, R.
A1  - Ernenwein, J. -P.
A1  - Errando, M.
A1  - Etchegoyen, A.
A1  - Falcone, A. D.
A1  - Farakos, K.
A1  - Farnier, C.
A1  - Federici, S.
A1  - Feinstein, F.
A1  - Ferenc, D.
A1  - Fillin-Martino, E.
A1  - Fink, D.
A1  - Finley, C.
A1  - Finley, J. P.
A1  - Firpo, R.
A1  - Florin, D.
A1  - Foehr, C.
A1  - Fokitis, E.
A1  - Font, Ll.
A1  - Fontaine, G.
A1  - Fontana, A.
A1  - Foerster, A.
A1  - Fortson, L.
A1  - Fouque, N.
A1  - Fransson, C.
A1  - Fraser, G. W.
A1  - Fresnillo, L.
A1  - Fruck, C.
A1  - Fujita, Y.
A1  - Fukazawa, Y.
A1  - Funk, S.
A1  - Gaebele, W.
A1  - Gabici, S.
A1  - Gadola, A.
A1  - Galante, N.
A1  - Gallant, Y.
A1  - Garcia, B.
A1  - Garcia Lopez, R. J.
A1  - Garrido, D.
A1  - Garrido, L.
A1  - Gascon, D.
A1  - Gasq, C.
A1  - Gaug, M.
A1  - Gaweda, J.
A1  - Geffroy, N.
A1  - Ghag, C.
A1  - Ghedina, A.
A1  - Ghigo, M.
A1  - Gianakaki, E.
A1  - Giarrusso, S.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Giro, E.
A1  - Giubilato, P.
A1  - Glanzman, T.
A1  - Glicenstein, J. -F.
A1  - Gochna, M.
A1  - Golev, V.
A1  - Gomez Berisso, M.
A1  - Gonzalez, A.
A1  - Gonzalez, F.
A1  - Granena, F.
A1  - Graciani, R.
A1  - Granot, J.
A1  - Gredig, R.
A1  - Green, A.
A1  - Greenshaw, T.
A1  - Grimm, O.
A1  - Grube, J.
A1  - Grudzinska, M.
A1  - Grygorczuk, J.
A1  - Guarino, V.
A1  - Guglielmi, L.
A1  - Guilloux, F.
A1  - Gunji, S.
A1  - Gyuk, G.
A1  - Hadasch, D.
A1  - Haefner, D.
A1  - Hagiwara, R.
A1  - Hahn, J.
A1  - Hallgren, A.
A1  - Hara, S.
A1  - Hardcastle, M. J.
A1  - Hassan, T.
A1  - Haubold, T.
A1  - Hauser, M.
A1  - Hayashida, M.
A1  - Heller, R.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Herrero, A.
A1  - Hinton, James Anthony
A1  - Hoffmann, D.
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Horns, D.
A1  - Hrupec, D.
A1  - Huan, H.
A1  - Huber, B.
A1  - Huet, J. -M.
A1  - Hughes, G.
A1  - Hultquist, K.
A1  - Humensky, T. B.
A1  - Huppert, J. -F.
A1  - Ibarra, A.
A1  - Illa, J. M.
A1  - Ingjald, J.
A1  - Inoue, S.
A1  - Inoue, Y.
A1  - Ioka, K.
A1  - Jablonski, C.
A1  - Jacholkowska, A.
A1  - Janiak, M.
A1  - Jean, P.
A1  - Jensen, H.
A1  - Jogler, T.
A1  - Jung, I.
A1  - Kaaret, P.
A1  - Kabuki, S.
A1  - Kakuwa, J.
A1  - Kalkuhl, C.
A1  - Kankanyan, R.
A1  - Kapala, M.
A1  - Karastergiou, A.
A1  - Karczewski, M.
A1  - Karkar, S.
A1  - Karlsson, N.
A1  - Kasperek, J.
A1  - Katagiri, H.
A1  - Katarzynski, K.
A1  - Kawanaka, N.
A1  - Kedziora, B.
A1  - Kendziorra, E.
A1  - Khelifi, B.
A1  - Kieda, D.
A1  - Kifune, T.
A1  - Kihm, T.
A1  - Klepser, S.
A1  - Kluzniak, W.
A1  - Knapp, J.
A1  - Knappy, A. R.
A1  - Kneiske, T.
A1  - Knoedlseder, J.
A1  - Koeck, F.
A1  - Kodani, K.
A1  - Kohri, K.
A1  - Kokkotas, K.
A1  - Komin, N.
A1  - Konopelko, A.
A1  - Kosack, K.
A1  - Kossakowski, R.
A1  - Kostka, P.
A1  - Kotula, J.
A1  - Kowal, G.
A1  - Koziol, J.
A1  - Kraehenbuehl, T.
A1  - Krause, J.
A1  - Krawczynski, H.
A1  - Krennrich, F.
A1  - Kretzschmann, A.
A1  - Kubo, H.
A1  - Kudryavtsev, V. A.
A1  - Kushida, J.
A1  - La Barbera, N.
A1  - La Parola, V.
A1  - La Rosa, G.
A1  - Lopez, A.
A1  - Lamanna, G.
A1  - Laporte, P.
A1  - Lavalley, C.
A1  - Le Flour, T.
A1  - Le Padellec, A.
A1  - Lenain, J. -P.
A1  - Lessio, L.
A1  - Lieunard, B.
A1  - Lindfors, E.
A1  - Liolios, A.
A1  - Lohse, T.
A1  - Lombardi, S.
A1  - Lopatin, A.
A1  - Lorenz, E.
A1  - Lubinski, P.
A1  - Luz, O.
A1  - Lyard, E.
A1  - Maccarone, M. C.
A1  - Maccarone, T.
A1  - Maier, G.
A1  - Majumdar, P.
A1  - Maltezos, S.
A1  - Malkiewicz, P.
A1  - Mana, C.
A1  - Manalaysay, A.
A1  - Maneva, G.
A1  - Mangano, A.
A1  - Manigot, P.
A1  - Marin, J.
A1  - Mariotti, M.
A1  - Markoff, S.
A1  - Martinez, G.
A1  - Martinez, M.
A1  - Mastichiadis, A.
A1  - Matsumoto, H.
A1  - Mattiazzo, S.
A1  - Mazin, D.
A1  - McComb, T. J. L.
A1  - McCubbin, N.
A1  - McHardy, I.
A1  - Medina, C.
A1  - Melkumyan, D.
A1  - Mendes, A.
A1  - Mertsch, P.
A1  - Meucci, M.
A1  - Michalowski, J.
A1  - Micolon, P.
A1  - Mineo, T.
A1  - Mirabal, N.
A1  - Mirabel, F.
A1  - Miranda, J. M.
A1  - Mirzoyan, R.
A1  - Mizuno, T.
A1  - Moal, B.
A1  - Moderski, R.
A1  - Molinari, E.
A1  - Monteiro, I.
A1  - Moralejo, A.
A1  - Morello, C.
A1  - Mori, K.
A1  - Motta, G.
A1  - Mottez, F.
A1  - Moulin, E.
A1  - Mukherjee, R.
A1  - Munar, P.
A1  - Muraishi, H.
A1  - Murase, K.
A1  - Murphy, A. Stj.
A1  - Nagataki, S.
A1  - Naito, T.
A1  - Nakamori, T.
A1  - Nakayama, K.
A1  - Naumann, C. L.
A1  - Naumann, D.
A1  - Nayman, P.
A1  - Nedbal, D.
A1  - Niedzwiecki, A.
A1  - Niemiec, J.
A1  - Nikolaidis, A.
A1  - Nishijima, K.
A1  - Nolan, S. J.
A1  - Nowak, N.
A1  - O'Brien, P. T.
A1  - Ochoa, I.
A1  - Ohira, Y.
A1  - Ohishi, M.
A1  - Ohka, H.
A1  - Okumura, A.
A1  - Olivetto, C.
A1  - Ong, R. A.
A1  - Orito, R.
A1  - Orr, M.
A1  - Osborne, J. P.
A1  - Ostrowski, M.
A1  - Otero, L.
A1  - Otte, A. N.
A1  - Ovcharov, E.
A1  - Oya, I.
A1  - Ozieblo, A.
A1  - Paiano, S.
A1  - Pallota, J.
A1  - Panazol, J. L.
A1  - Paneque, D.
A1  - Panter, M.
A1  - Paoletti, R.
A1  - Papyan, G.
A1  - Paredes, J. M.
A1  - Pareschi, G.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pedaletti, G.
A1  - Pepato, A.
A1  - Persic, M.
A1  - Petrucci, P. O.
A1  - Peyaud, B.
A1  - Piechocki, W.
A1  - Pita, S.
A1  - Pivato, G.
A1  - Platos, L.
A1  - Platzer, R.
A1  - Pogosyan, L.
A1  - Pohl, Martin
A1  - Pojmanski, G.
A1  - Ponz, J. D.
A1  - Potter, W.
A1  - Prandini, E.
A1  - Preece, R.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quel, E.
A1  - Quirrenbach, A.
A1  - Rajda, P.
A1  - Rando, R.
A1  - Rataj, M.
A1  - Raue, M.
A1  - Reimann, C.
A1  - Reimann, O.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - Renner, S.
A1  - Reymond, J. -M.
A1  - Rhode, W.
A1  - Ribo, M.
A1  - Ribordy, M.
A1  - Rico, J.
A1  - Rieger, F.
A1  - Ringegni, P.
A1  - Ripken, J.
A1  - Ristori, P.
A1  - Rivoire, S.
A1  - Rob, L.
A1  - Rodriguez, S.
A1  - Roeser, U.
A1  - Romano, Patrizia
A1  - Romero, G. E.
A1  - Rosier-Lees, S.
A1  - Rovero, A. C.
A1  - Roy, F.
A1  - Royer, S.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Ruppel, J.
A1  - Russo, F.
A1  - Ryde, F.
A1  - Sacco, B.
A1  - Saggion, A.
A1  - Sahakian, V.
A1  - Saito, K.
A1  - Saito, T.
A1  - Sakaki, N.
A1  - Salazar, E.
A1  - Salini, A.
A1  - Sanchez, F.
A1  - Sanchez Conde, M. A.
A1  - Santangelo, A.
A1  - Santos, E. M.
A1  - Sanuy, A.
A1  - Sapozhnikov, L.
A1  - Sarkar, S.
A1  - Scalzotto, V.
A1  - Scapin, V.
A1  - Scarcioffolo, M.
A1  - Schanz, T.
A1  - Schlenstedt, S.
A1  - Schlickeiser, R.
A1  - Schmidt, T.
A1  - Schmoll, J.
A1  - Schroedter, M.
A1  - Schultz, C.
A1  - Schultze, J.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwarzburg, S.
A1  - Schweizer, T.
A1  - Seiradakis, J.
A1  - Selmane, S.
A1  - Seweryn, K.
A1  - Shayduk, M.
A1  - Shellard, R. C.
A1  - Shibata, T.
A1  - Sikora, M.
A1  - Silk, J.
A1  - Sillanpaa, A.
A1  - Sitarek, J.
A1  - Skole, C.
A1  - Smith, N.
A1  - Sobczynska, D.
A1  - Sofo Haro, M.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spiga, D.
A1  - Spyrou, S.
A1  - Stamatescu, V.
A1  - Stamerra, A.
A1  - Starling, R. L. C.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steiner, S.
A1  - Stergioulas, N.
A1  - Sternberger, R.
A1  - Stinzing, F.
A1  - Stodulski, M.
A1  - Straumann, U.
A1  - Suarez, A.
A1  - Suchenek, M.
A1  - Sugawara, R.
A1  - Sulanke, K. H.
A1  - Sun, S.
A1  - Supanitsky, A. D.
A1  - Sutcliffe, P.
A1  - Szanecki, M.
A1  - Szepieniec, T.
A1  - Szostek, A.
A1  - Szymkowiak, A.
A1  - Tagliaferri, G.
A1  - Tajima, H.
A1  - Takahashi, H.
A1  - Takahashi, K.
A1  - Takalo, L.
A1  - Takami, H.
A1  - Talbot, R. G.
A1  - Tam, P. H.
A1  - Tanaka, M.
A1  - Tanimori, T.
A1  - Tavani, M.
A1  - Tavernet, J. -P.
A1  - Tchernin, C.
A1  - Tejedor, L. A.
A1  - Telezhinsky, Igor O.
A1  - Temnikov, P.
A1  - Tenzer, C.
A1  - Terada, Y.
A1  - Terrier, R.
A1  - Teshima, M.
A1  - Testa, V.
A1  - Tibaldo, L.
A1  - Tibolla, O.
A1  - Tluczykont, M.
A1  - Peixoto, C. J. Todero
A1  - Tokanai, F.
A1  - Tokarz, M.
A1  - Toma, K.
A1  - Torres, D. F.
A1  - Tosti, G.
A1  - Totani, T.
A1  - Toussenel, F.
A1  - Vallania, P.
A1  - Vallejo, G.
A1  - van der Walt, J.
A1  - van Eldik, C.
A1  - Vandenbroucke, J.
A1  - Vankov, H.
A1  - Vasileiadis, G.
A1  - Vassiliev, V. V.
A1  - Vegas, I.
A1  - Venter, L.
A1  - Vercellone, S.
A1  - Veyssiere, C.
A1  - Vialle, J. P.
A1  - Videla, M.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Vlahakis, N.
A1  - Vlahos, L.
A1  - Vogler, P.
A1  - Vollhardt, A.
A1  - Volpe, F.
A1  - Von Gunten, H. P.
A1  - Vorobiov, S.
A1  - Wagner, S.
A1  - Wagner, R. M.
A1  - Wagner, B.
A1  - Wakely, S. P.
A1  - Walter, P.
A1  - Walter, R.
A1  - Warwick, R.
A1  - Wawer, P.
A1  - Wawrzaszek, R.
A1  - Webb, N.
A1  - Wegner, P.
A1  - Weinstein, A.
A1  - Weitzel, Q.
A1  - Welsing, R.
A1  - Wetteskind, H.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Wilkinson, M. I.
A1  - Williams, D. A.
A1  - Winde, M.
A1  - Wischnewski, R.
A1  - Wisniewski, L.
A1  - Wolczko, A.
A1  - Wood, M.
A1  - Xiong, Q.
A1  - Yamamoto, T.
A1  - Yamaoka, K.
A1  - Yamazaki, R.
A1  - Yanagita, S.
A1  - Yoffo, B.
A1  - Yonetani, M.
A1  - Yoshida, A.
A1  - Yoshida, T.
A1  - Yoshikoshi, T.
A1  - Zabalza, V.
A1  - Zagdanski, A.
A1  - Zajczyk, A.
A1  - Zdziarski, A.
A1  - Zech, Alraune
A1  - Zietara, K.
A1  - Ziolkowski, P.
A1  - Zitelli, V.
A1  - Zychowski, P.
T1  - Design concepts for the Cherenkov Telescope Array CTA an advanced facility for ground-based high-energy gamma-ray astronomy
JF  - Experimental astronomy : an international journal on astronomical instrumentation and data analysis
N2  - Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA.
KW  - Ground based gamma ray astronomy
KW  - Next generation Cherenkov telescopes
KW  - Design concepts
Y1  - 2011
U6  - https://doi.org/10.1007/s10686-011-9247-0
SN  - 0922-6435
SN  - 1572-9508
VL  - 32
IS  - 3
SP  - 193
EP  - 316
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - INPR
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T1  - Introducing the CTA concept
T2  - Astroparticle physics
N2  - 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.
KW  - TeV gamma-ray astronomy
KW  - Air showers
KW  - Cherenkov Telescopes
Y1  - 2013
U6  - https://doi.org/10.1016/j.astropartphys.2013.01.007
SN  - 0927-6505
SN  - 1873-2852
VL  - 43
IS  - 2
SP  - 3
EP  - 18
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
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A1  - Amans, J.
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A1  - Backes, M.
A1  - Balazs, C.
A1  - Balzer, A.
A1  - Bamba, Aya
A1  - Barkov, Maxim
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A1  - Beshley, V.
A1  - Bigongiari, C.
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A1  - Chaty, Sylvain
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A1  - Chernyakova, M.
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A1  - Chudoba, J.
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A1  - Colafrancesco, S.
A1  - Conforti, V.
A1  - Contreras, J. L.
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A1  - Daniel, M.
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A1  - De Cesare, G.
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A1  - Lopez, R. de los Reyes
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A1  - de Naurois, M.
A1  - De Palma, F.
A1  - Del Santo, M.
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A1  - Fedorova, E.
A1  - Fernandez-Barral, A.
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A1  - Nagataki, Shigehiro
A1  - Nagayoshi, T.
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A1  - Nakajima, D.
A1  - Nakamori, T.
A1  - Nemmen, R.
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A1  - Nikolajuk, M.
A1  - Nishijima, K.
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A1  - Ohishi, M.
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A1  - Telezhinsky, Igor O.
A1  - Temnikov, P.
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A1  - Vandenbroucke, Justin
A1  - Vassiliev, V.
A1  - Vecchi, M.
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A1  - Vergani, S.
A1  - Vigorito, C.
A1  - Vorobiov, S.
A1  - Vrastil, M.
A1  - Vazquez Acosta, M. L.
A1  - Wagner, S. J.
A1  - Wagner, R.
A1  - Wakely, S. P.
A1  - Walter, R.
A1  - Ward, J. E.
A1  - Watson, J. J.
A1  - Weinstein, A.
A1  - White, M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Wilcox, P.
A1  - Williams, D. A.
A1  - Wischnewski, R.
A1  - Wojcik, P.
A1  - Yamamoto, T.
A1  - Yamamoto, H.
A1  - Yamazaki, Ryo
A1  - Yanagita, S.
A1  - Yang, L.
A1  - Yoshida, T.
A1  - Yoshida, M.
A1  - Yoshiike, S.
A1  - Yoshikoshi, T.
A1  - Zacharias, M.
A1  - Zampieri, L.
A1  - Zanin, R.
A1  - Zavrtanik, M.
A1  - Zavrtanik, D.
A1  - Zdziarski, A.
A1  - Zech, Alraune
A1  - Zechlin, Hannes
A1  - Zhdanov, V.
A1  - Ziegler, A.
A1  - Zorn, J.
T1  - Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7-3946
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - 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.
KW  - cosmic rays
KW  - gamma rays: ISM
KW  - ISM: individual objects (RX J1713.7-3946, G347.3-0.5)
Y1  - 2017
U6  - https://doi.org/10.3847/1538-4357/aa6d67
SN  - 0004-637X
SN  - 1538-4357
VL  - 840
IS  - 2
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - De Angelis, A.
A1  - Tatischeff, V.
A1  - Grenier, I. A.
A1  - McEnery, J.
A1  - Mallamaci, Manuela
A1  - Tavani, M.
A1  - Oberlack, U.
A1  - Hanlon, L.
A1  - Walter, R.
A1  - Argan, A.
A1  - Von Ballmoos, P.
A1  - Bulgarelli, A.
A1  - Bykov, A.
A1  - Hernanz, M.
A1  - Kanbach, G.
A1  - Kuvvetli, I.
A1  - Pearce, M.
A1  - Zdziarski, A.
A1  - Conrad, J.
A1  - Ghisellini, G.
A1  - Harding, A.
A1  - Isern, J.
A1  - Leising, M.
A1  - Longo, F.
A1  - Madejski, G.
A1  - Martinez, M.
A1  - Mazziotta, Mario Nicola
A1  - Paredes, J. M.
A1  - Pohl, Martin
A1  - Rando, R.
A1  - Razzano, M.
A1  - Aboudan, A.
A1  - Ackermann, M.
A1  - Addazi, A.
A1  - Ajello, M.
A1  - Albertus, C.
A1  - Alvarez, J. M.
A1  - Ambrosi, G.
A1  - Anton, S.
A1  - Antonelli, L. A.
A1  - Babic, A.
A1  - Baibussinov, B.
A1  - Balbom, M.
A1  - Baldini, L.
A1  - Balman, S.
A1  - Bambi, C.
A1  - Barres de Almeida, U.
A1  - Barrio, J. A.
A1  - Bartels, R.
A1  - Bastieri, D.
A1  - Bednarek, W.
A1  - Bernard, D.
A1  - Bernardini, E.
A1  - Bernasconi, T.
A1  - Bertucci, B.
A1  - Biland, A.
A1  - Bissaldi, E.
A1  - Boettcher, M.
A1  - Bonvicini, V.
A1  - Bosch-Ramon, V.
A1  - Bottacini, E.
A1  - Bozhilov, V.
A1  - Bretz, T.
A1  - Branchesi, M.
A1  - Brdar, V.
A1  - Bringmann, T.
A1  - Brogna, A.
A1  - Jorgensen, C. Budtz
A1  - Busetto, G.
A1  - Buson, S.
A1  - Busso, M.
A1  - Caccianiga, A.
A1  - Camera, S.
A1  - Campana, R.
A1  - Caraveo, P.
A1  - Cardillo, M.
A1  - Carlson, P.
A1  - Celestin, S.
A1  - Cermeno, M.
A1  - Chen, A.
A1  - Cheung, C. C.
A1  - Churazov, E.
A1  - Ciprini, S.
A1  - Coc, A.
A1  - Colafrancesco, S.
A1  - Coleiro, A.
A1  - Collmar, W.
A1  - Coppi, P.
A1  - Curado da Silva, R.
A1  - Cutini, S.
A1  - De Lotto, B.
A1  - de Martino, D.
A1  - De Rosa, A.
A1  - Del Santo, M.
A1  - Delgado, L.
A1  - Diehl, R.
A1  - Dietrich, S.
A1  - Dolgov, A. D.
A1  - Dominguez, A.
A1  - Prester, D. Dominis
A1  - Donnarumma, I.
A1  - Dorner, D.
A1  - Doro, M.
A1  - Dutra, M.
A1  - Elsaesser, D.
A1  - Fabrizio, M.
A1  - Fernandez-Barral, A.
A1  - Fioretti, V.
A1  - Foffano, L.
A1  - Formato, V.
A1  - Fornengo, N.
A1  - Foschini, L.
A1  - Franceschini, A.
A1  - Franckowiak, A.
A1  - Funk, S.
A1  - Fuschino, F.
A1  - Gaggero, D.
A1  - Galanti, G.
A1  - Gargano, F.
A1  - Gasparrini, D.
A1  - Gehrz, R.
A1  - Giammaria, P.
A1  - Giglietto, N.
A1  - Giommi, P.
A1  - Giordano, F.
A1  - Giroletti, M.
A1  - Ghirlanda, G.
A1  - Godinovic, N.
A1  - Gouiffes, C.
A1  - Grove, J. E.
A1  - Hamadache, C.
A1  - Hartmann, D. H.
A1  - Hayashida, M.
A1  - Hryczuk, A.
A1  - Jean, P.
A1  - Johnson, T.
A1  - Jose, J.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Kiener, J.
A1  - Knodlseder, J.
A1  - Kolem, M.
A1  - Kopp, J.
A1  - Kozhuharov, V.
A1  - Labanti, C.
A1  - Lalkovski, S.
A1  - Laurent, P.
A1  - Limousin, O.
A1  - Linares, M.
A1  - Lindfors, E.
A1  - Lindner, M.
A1  - Liu, J.
A1  - Lombardi, S.
A1  - Loparco, F.
A1  - Lopez-Coto, R.
A1  - Lopez Moya, M.
A1  - Lott, B.
A1  - Lubrano, P.
A1  - Malyshev, D.
A1  - Mankuzhiyil, N.
A1  - Mannheim, K.
A1  - Marcha, M. J.
A1  - Marciano, A.
A1  - Marcote, B.
A1  - Mariotti, M.
A1  - Marisaldi, M.
A1  - McBreen, S.
A1  - Mereghetti, S.
A1  - Merle, A.
A1  - Mignani, R.
A1  - Minervini, G.
A1  - Moiseev, A.
A1  - Morselli, A.
A1  - Moura, F.
A1  - Nakazawa, K.
A1  - Nava, L.
A1  - Nieto, D.
A1  - Orienti, M.
A1  - Orio, M.
A1  - Orlando, E.
A1  - Orleanski, P.
A1  - Paiano, S.
A1  - Paoletti, R.
A1  - Papitto, A.
A1  - Pasquato, M.
A1  - Patricelli, B.
A1  - Perez-Garcia, M. A.
A1  - Persic, M.
A1  - Piano, G.
A1  - Pichel, A.
A1  - Pimenta, M.
A1  - Pittori, C.
A1  - Porter, T.
A1  - Poutanen, J.
A1  - Prandini, E.
A1  - Prantzos, N.
A1  - Produit, N.
A1  - Profumo, S.
A1  - Queiroz, F. S.
A1  - Raino, S.
A1  - Raklev, A.
A1  - Regis, M.
A1  - Reichardt, I.
A1  - Rephaeli, Y.
A1  - Rico, J.
A1  - Rodejohann, W.
A1  - Fernandez, G. Rodriguez
A1  - Roncadelli, M.
A1  - Roso, L.
A1  - Rovero, A.
A1  - Ruffini, R.
A1  - Sala, G.
A1  - Sanchez-Conde, M. A.
A1  - Santangelo, A.
A1  - Parkinson, P. Saz
A1  - Sbarrato, T.
A1  - Shearer, A.
A1  - Shellard, R.
A1  - Short, K.
A1  - Siegert, T.
A1  - Siqueira, C.
A1  - Spinelli, P.
A1  - Stamerra, A.
A1  - Starrfield, S.
A1  - Strong, A.
A1  - Strumke, I.
A1  - Tavecchio, F.
A1  - Taverna, R.
A1  - Terzic, T.
A1  - Thompson, D. J.
A1  - Tibolla, O.
A1  - Torres, D. F.
A1  - Turolla, R.
A1  - Ulyanov, A.
A1  - Ursi, A.
A1  - Vacchi, A.
A1  - Van den Abeele, J.
A1  - Vankova-Kirilovai, G.
A1  - Venter, C.
A1  - Verrecchia, F.
A1  - Vincent, P.
A1  - Wang, X.
A1  - Weniger, C.
A1  - Wu, X.
A1  - Zaharijas, G.
A1  - Zampieri, L.
A1  - Zane, S.
A1  - Zimmer, S.
A1  - Zoglauer, A.
T1  - Science with e-ASTROGAM A space mission for MeV-GeV gamma-ray astrophysics
JF  - Journal of High Energy Astrophysics
Y1  - 2018
U6  - https://doi.org/10.1016/j.jheap.2018.07.001
SN  - 2214-4048
SN  - 2214-4056
VL  - 19
SP  - 1
EP  - 106
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Ahnen, M. L.
A1  - Ansoldi, S.
A1  - Antonelli, L. A.
A1  - Arcaro, C.
A1  - Babic, A.
A1  - Banerjee, B.
A1  - Bangale, P.
A1  - Barres de Almeida, U.
A1  - Barrio, J. A.
A1  - Gonzalez, J. Becerra
A1  - Bednarek, W.
A1  - Bernardini, E.
A1  - Berti, A.
A1  - Bhattacharyya, W.
A1  - Blanch, O.
A1  - Bonnoli, G.
A1  - Carosi, R.
A1  - Carosi, A.
A1  - Chatterjee, A.
A1  - Colak, S. M.
A1  - Colin, P.
A1  - Colombo, E.
A1  - Contreras, J. L.
A1  - Cortina, J.
A1  - Covino, S.
A1  - Cumani, P.
A1  - Da Vela, P.
A1  - Dazzi, F.
A1  - De Angelis, A.
A1  - De Lotto, B.
A1  - Delfino, M.
A1  - Delgado, Jose Miguel Martins
A1  - Di Pierro, F.
A1  - Doert, M.
A1  - Dominguez, A.
A1  - Prester, D. Dominis
A1  - Doro, M.
A1  - Glawion, D. Eisenacher
A1  - Engelkemeier, M.
A1  - Ramazani, V. Fallah
A1  - Fernandez-Barral, A.
A1  - Fidalgo, D.
A1  - Fonseca, M. V.
A1  - Font, L.
A1  - Fruck, C.
A1  - Galindo, D.
A1  - Lopez, R. J. Garcia
A1  - Garczarczyk, M.
A1  - Gaug, M.
A1  - Giammaria, P.
A1  - Godinovic, N.
A1  - Gora, D.
A1  - Guberman, D.
A1  - Hadasch, D.
A1  - Hahn, A.
A1  - Hassan, T.
A1  - Hayashida, M.
A1  - Herrera, J.
A1  - Hose, J.
A1  - Hrupec, D.
A1  - Ishio, K.
A1  - Konno, Y.
A1  - Kubo, H.
A1  - Kushida, J.
A1  - Kuvezdic, D.
A1  - Lelas, D.
A1  - Lindfors, E.
A1  - Lombardi, S.
A1  - Longo, F.
A1  - Lopez, M.
A1  - Maggio, C.
A1  - Majumdar, P.
A1  - Makariev, M.
A1  - Maneva, G.
A1  - Manganaro, M.
A1  - Maraschi, L.
A1  - Mariotti, M.
A1  - Martinez, M.
A1  - Mazin, D.
A1  - Menzel, U.
A1  - Minev, M.
A1  - Miranda, J. M.
A1  - Mirzoyan, R.
A1  - Moralejo, A.
A1  - Moreno, V.
A1  - Moretti, E.
A1  - Nagayoshi, T.
A1  - Neustroev, V.
A1  - Niedzwiecki, A.
A1  - Nievas Rosillo, M.
A1  - Nigro, C.
A1  - Nilsson, K.
A1  - Ninci, D.
A1  - Nishijima, K.
A1  - Noda, K.
A1  - Nogues, L.
A1  - Paiano, S.
A1  - Palacio, J.
A1  - Paneque, D.
A1  - Paoletti, R.
A1  - Paredes, J. M.
A1  - Pedaletti, G.
A1  - Peresano, M.
A1  - Perri, L.
A1  - Persic, M.
A1  - Moroni, P. G. Prada
A1  - Prandini, E.
A1  - Puljak, I.
A1  - Garcia, J. R.
A1  - Reichardt, I.
A1  - Ribo, M.
A1  - Rico, J.
A1  - Righi, C.
A1  - Rugliancich, A.
A1  - Saito, T.
A1  - Satalecka, K.
A1  - Schroeder, S.
A1  - Schweizer, T.
A1  - Shore, S. N.
A1  - Sitarek, J.
A1  - Snidaric, I.
A1  - Sobczynska, D.
A1  - Stamerra, A.
A1  - Strzys, M.
A1  - Suric, T.
A1  - Takalo, L.
A1  - Tavecchio, F.
A1  - Temnikov, P.
A1  - Terzic, T.
A1  - Teshima, M.
A1  - Torres-Alba, N.
A1  - Treves, A.
A1  - Tsujimoto, S.
A1  - Vanzo, G.
A1  - Vazquez Acosta, M.
A1  - Vovk, I.
A1  - Ward, J. E.
A1  - Will, M.
A1  - Zaric, D.
A1  - Arbet-Engels, A.
A1  - Baack, D.
A1  - Balbo, M.
A1  - Biland, A.
A1  - Blank, M.
A1  - Bretz, T.
A1  - Bruegge, K.
A1  - Bulinski, M.
A1  - Buss, J.
A1  - Dmytriiev, A.
A1  - Dorner, D.
A1  - Einecke, S.
A1  - Elsaesser, D.
A1  - Herbst, T.
A1  - Hildebrand, D.
A1  - Kortmann, L.
A1  - Linhoff, L.
A1  - Mahlke, M.
A1  - Mannheim, K.
A1  - Mueller, S. A.
A1  - Neise, D.
A1  - Neronov, A.
A1  - Noethe, M.
A1  - Oberkirch, J.
A1  - Paravac, A.
A1  - Rhode, W.
A1  - Schleicher, B.
A1  - Schulz, F.
A1  - Sedlaczek, K.
A1  - Shukla, A.
A1  - Sliusar, V.
A1  - Walter, R.
A1  - Archer, A.
A1  - Benbow, W.
A1  - Bird, R.
A1  - Brose, Robert
A1  - Buckley, J. H.
A1  - Bugaev, V.
A1  - Christiansen, J. L.
A1  - Cui, W.
A1  - Daniel, M. K.
A1  - Falcone, A.
A1  - Feng, Q.
A1  - Finley, J. P.
A1  - Gillanders, G. H.
A1  - Gueta, O.
A1  - Hanna, D.
A1  - Hervet, O.
A1  - Holder, J.
A1  - Hughes, G.
A1  - Huetten, M.
A1  - Humensky, T. B.
A1  - Johnson, C. A.
A1  - Kaaret, P.
A1  - Kar, P.
A1  - Kelley-Hoskins, N.
A1  - Kertzman, M.
A1  - Kieda, D.
A1  - Krause, M.
A1  - Krennrich, F.
A1  - Kumar, S.
A1  - Lang, M. J.
A1  - Lin, T. T. Y.
A1  - Maier, G.
A1  - McArthur, S.
A1  - Moriarty, P.
A1  - Mukherjee, R.
A1  - Ong, R. A.
A1  - Otte, A. N.
A1  - Park, N.
A1  - Petrashyk, A.
A1  - Pichel, A.
A1  - Pohl, Martin
A1  - Quinn, J.
A1  - Ragan, K.
A1  - Reynolds, P. T.
A1  - Richards, G. T.
A1  - Roache, E.
A1  - Rovero, A. C.
A1  - Rulten, C.
A1  - Sadeh, I.
A1  - Santander, M.
A1  - Sembroski, G. H.
A1  - Shahinyan, K.
A1  - Sushch, Iurii
A1  - Tyler, J.
A1  - Wakely, S. P.
A1  - Weinstein, A.
A1  - Wells, R. M.
A1  - Wilcox, P.
A1  - Wilhel, A.
A1  - Williams, D. A.
A1  - Williamson, T. J.
A1  - Zitzer, B.
A1  - Perri, M.
A1  - Verrecchia, F.
A1  - Leto, C.
A1  - Villata, M.
A1  - Raiteri, C. M.
A1  - Jorstad, S. G.
A1  - Larionov, V. M.
A1  - Blinov, D. A.
A1  - Grishina, T. S.
A1  - Kopatskaya, E. N.
A1  - Larionova, E. G.
A1  - Nikiforova, A. A.
A1  - Morozova, D. A.
A1  - Troitskaya, Yu. V.
A1  - Troitsky, I. S.
A1  - Kurtanidze, O. M.
A1  - Nikolashvili, M. G.
A1  - Kurtanidze, S. O.
A1  - Kimeridze, G. N.
A1  - Chigladze, R. A.
A1  - Strigachev, A.
A1  - Sadun, A. C.
T1  - Extreme HBL behavior of Markarian 501 during 2012
JF  - Astronomy and astrophysics : an international weekly journal / European Southern Observatory (ESO)
N2  - Aims. We aim to characterize the multiwavelength emission from Markarian 501 (Mrk 501), quantify the energy-dependent variability, study the potential multiband correlations, and describe the temporal evolution of the broadband emission within leptonic theoretical scenarios. Methods. We organized a multiwavelength campaign to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Results. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0.2 TeV of similar to 0.5 times the Crab Nebula flux (CU) for most of the campaign. The highest activity occurred on 2012 June 9, when the VHE flux was similar to 3 CU, and the peak of the high-energy spectral component was found to be at similar to 2 TeV. Both the X-ray and VHE gamma-ray spectral slopes were measured to be extremely hard, with spectral indices <2 during most of the observing campaign, regardless of the X-ray and VHE flux. This study reports the hardest Mrk 501 VHE spectra measured to date. The fractional variability was found to increase with energy, with the highest variability occurring at VHE. Using the complete data set, we found correlation between the X-ray and VHE bands; however, if the June 9 flare is excluded, the correlation disappears (significance <3 sigma) despite the existence of substantial variability in the X-ray and VHE bands throughout the campaign. Conclusions. The unprecedentedly hard X-ray and VHE spectra measured imply that their low- and high-energy components peaked above 5 keV and 0.5 TeV, respectively, during a large fraction of the observing campaign, and hence that Mrk 501 behaved like an extreme high-frequency-peaked blazar (EHBL) throughout the 2012 observing season. This suggests that being an EHBL may not be a permanent characteristic of a blazar, but rather a state which may change over time. The data set acquired shows that the broadband spectral energy distribution (SED) of Mrk 501, and its transient evolution, is very complex, requiring, within the framework of synchrotron self-Compton (SSC) models, various emission regions for a satisfactory description. Nevertheless the one-zone SSC scenario can successfully describe the segments of the SED where most energy is emitted, with a significant correlation between the electron energy density and the VHE gamma-ray activity, suggesting that most of the variability may be explained by the injection of high-energy electrons. The one-zone SSC scenario used reproduces the behavior seen between the measured X-ray and VHE gamma-ray fluxes, and predicts that the correlation becomes stronger with increasing energy of the X-rays.
KW  - astroparticle physics
KW  - acceleration of particles
KW  - radiation mechanisms: non-thermal
KW  - BL Lacertae objects: general
KW  - BL Lacertae objects: individual: Mrk501
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201833704
SN  - 1432-0746
VL  - 620
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - De Angelis, A.
A1  - Tatischeff, V.
A1  - Tavani, M.
A1  - Oberlack, U.
A1  - Grenier, I.
A1  - Hanloni, L.
A1  - Walter, R.
A1  - Argan, A.
A1  - Von Ballmoos, P.
A1  - Bulgarelli, A.
A1  - Donnarumma, I.
A1  - Hernanz, M.
A1  - Kuvvetli, I.
A1  - Pearce, M.
A1  - Zdziarski, A.
A1  - Aboudan, A.
A1  - Ajello, M.
A1  - Ambrosi, G.
A1  - Bernard, D.
A1  - Bernardini, E.
A1  - Bonvicini, V.
A1  - Brogna, A.
A1  - Branchesi, M.
A1  - Budtz-Jorgensen, C.
A1  - Bykov, A. M.
A1  - Campana, R.
A1  - Cardillo, M.
A1  - Coppi, P.
A1  - De Martino, D.
A1  - Diehl, R.
A1  - Doro, M.
A1  - Fioretti, V.
A1  - Funk, S.
A1  - Ghisellini, G.
A1  - Grove, E.
A1  - Hamadache, C.
A1  - Hartmann, D. H.
A1  - Hayashida, M.
A1  - Isern, J.
A1  - Kanbach, G.
A1  - Kiener, J.
A1  - Knodlseder, J.
A1  - Labanti, C.
A1  - Laurent, P.
A1  - Limousin, O.
A1  - Longo, F.
A1  - Mannheim, K.
A1  - Marisaldi, M.
A1  - Martinez, M.
A1  - Mazziotta, Mario Nicola
A1  - McEnery, J.
A1  - Mereghetti, S.
A1  - Minervini, G.
A1  - Moiseev, A.
A1  - Morselli, A.
A1  - Nakazawa, K.
A1  - Orleanski, P.
A1  - Paredes, J. M.
A1  - Patricelli, B.
A1  - Pevre, J.
A1  - Piano, G.
A1  - Pohl, Martin
A1  - Ramarijaona, H.
A1  - Rando, R.
A1  - Reichardt, I.
A1  - Roncadelli, M.
A1  - Silva, R.
A1  - Tavecchio, F.
A1  - Thompson, D. J.
A1  - Turolla, R.
A1  - Ulyanov, A.
A1  - Vacchi, A.
A1  - Wu, X.
A1  - Zoglauer, A.
T1  - The e-ASTROGAM mission Exploring the extreme Universe with gamma rays in the MeV - GeV range
JF  - Experimental astronomy : an international journal on astronomical instrumentation and data analysis
N2  - e-ASTROGAM (‘enhanced ASTROGAM’) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV – the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.
KW  - High-Energy Gamma-Ray Astronomy
KW  - High-Energy Astrophysics
KW  - Nuclear Astrophysics
KW  - Compton and Pair Creation Telescope
KW  - Gamma-Ray Bursts
KW  - Active Galactic Nuclei
KW  - Jets
KW  - Outflows
KW  - Multiwavelength Observations of the Universe
KW  - Counterparts of gravitational waves
KW  - Fermi
KW  - Dark Matter
KW  - Nucleosynthesis
KW  - Early Universe
KW  - Supernovae
KW  - Cosmic Rays
KW  - Cosmic Antimatter
Y1  - 2017
U6  - https://doi.org/10.1007/s10686-017-9533-6
SN  - 0922-6435
SN  - 1572-9508
VL  - 44
SP  - 25
EP  - 82
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - CHAP
A1  - Tatischeff, V.
A1  - De Angelis, A.
A1  - Tavani, M.
A1  - Grenier, I.
A1  - Oberlack, U.
A1  - Hanlon, L.
A1  - Walter, R.
A1  - Argan, A.
A1  - von Ballmoos, P.
A1  - Bulgarelli, A.
A1  - Donnarumma, I.
A1  - Hernanz, Margarita
A1  - Kuvvetli, I.
A1  - Mallamaci, M.
A1  - Pearce, M.
A1  - Zdziarski, A.
A1  - Aboudan, A.
A1  - Ajello, M.
A1  - Ambrosi, G.
A1  - Bernard, D.
A1  - Bernardini, E.
A1  - Bonvicini, V.
A1  - Brogna, A.
A1  - Branchesi, M.
A1  - Budtz-Jorgensen, C.
A1  - Bykov, A.
A1  - Campana, R.
A1  - Cardillo, M.
A1  - Ciprini, S.
A1  - Coppi, P.
A1  - Cumani, P.
A1  - da Silva, R. M. Curado
A1  - De Martino, D.
A1  - Diehl, R.
A1  - Doro, M.
A1  - Fioretti, V.
A1  - Funk, S.
A1  - Ghisellini, G.
A1  - Giordano, F.
A1  - Grove, J. E.
A1  - Hamadache, C.
A1  - Hartmann, D. H.
A1  - Hayashida, M.
A1  - Isern, J.
A1  - Kanbach, G.
A1  - Kiener, J.
A1  - Knodlseder, J.
A1  - Labanti, C.
A1  - Laurent, P.
A1  - Leising, M.
A1  - Limousin, O.
A1  - Longo, F.
A1  - Mannheim, K.
A1  - Marisaldi, M.
A1  - Martinez, M.
A1  - Mazziotta, M. N.
A1  - McEnery, J. E.
A1  - Mereghetti, S.
A1  - Minervini, G.
A1  - Moiseev, A.
A1  - Morselli, A.
A1  - Nakazawa, K.
A1  - Orleanski, P.
A1  - Paredes, J. M.
A1  - Patricelli, B.
A1  - Peyre, J.
A1  - Piano, G.
A1  - Pohl, Martin
A1  - Rando, R.
A1  - Roncadelli, M.
A1  - Tavecchio, F.
A1  - Thompson, D. J.
A1  - Turolla, R.
A1  - Ulyanov, A.
A1  - Vacchi, A.
A1  - Wu, X.
A1  - Zoglauer, A.
ED  - DenHerder, JWA Nikzad
T1  - The e-ASTROGAM gamma-ray space observatory for the multimessenger astronomy of the 2030s
T2  - Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray
N2  - e-ASTROGAM is a concept for a breakthrough observatory space mission carrying a gamma-ray telescope dedicated to the study of the non-thermal Universe in the photon energy range from 0.15 MeV to 3 GeV. The lower energy limit can be pushed down to energies as low as 30 keV for gamma-ray burst detection with the calorimeter. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with remarkable polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous and current generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will be a major player of the multiwavelength, multimessenger time-domain astronomy of the 2030s, and provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LISA, LIGO, Virgo, KAGRA, the Einstein Telescope and the Cosmic Explorer, IceCube-Gen2 and KM3NeT, SKA, ALMA, JWST, E-ELT, LSST, Athena, and the Cherenkov Telescope Array.
KW  - Gamma-ray astronomy
KW  - time-domain astronomy
KW  - space mission
KW  - Compton and pair creation telescope
KW  - gamma-ray polarization
KW  - high-energy astrophysical phenomena
Y1  - 2018
SN  - 978-1-5106-1952-4
U6  - https://doi.org/10.1117/12.2315151
SN  - 0277-786X
SN  - 1996-756X
VL  - 10699
PB  - SPIE - The International Society for Optical Engineering
CY  - Bellingham
ER  - 
TY  - JOUR
A1  - Krohn, Arne
A1  - Materne, Stefanie
A1  - Schlutow, A.
A1  - Wilhelm, R.
A1  - Metzdorf, R.
A1  - Wilk, B.
A1  - Förster, B.
A1  - Schade, Bernd
A1  - Kitzig, Angelika
A1  - Müller, Jörg
A1  - Haase, Walter
A1  - Rückert-John, Jana
T1  - Agenda 21-Prozesse für zukunftsfähige Kommunen in Brandenburg
N2  - Agenda 21-Prozesse für zukunftsfähige Kommunen in Brandenburg KROHN, A.: Stadtentwicklung und Lokale Agenda 21 – Zwei Seiten einer Medaille ; MATERNE, S.: Agenda 21 in Oranienburg – die Entwicklung eines Leitbildes ; SCHLUTOW, A.; WILHELM, B.; METZDORF, R.; WILK, B., FÖRSTER, B.: Interessengemeinschaft "Ökologie 2000 - Unternehmer für die Umwelt" – Anstoß der Wirtschaft für eine lokale Agenda 21 in Strausberg ; SCHADE, B.: Agenda 21 im Landkreis Potsdam-Mittelmark – Rahmen für lokale Aktivitäten ; KITZIG, A.: Potsdam, Stadt der Toleranz – unterwegs mit Geschichts- und Verantwortungsbewußtsein für die Zukunft. Die Lokale Agenda 21 ; MÜLLER, J.: Umsetzung eines Klimaschutzkonzeptes – Schritte zu einer nachhaltigen Entwicklung der Stadt Eberswalde , HAASE, W.: Eine lokale Agenda 21 für Kleinmachnow , RÜCKERT-JOHN, J.: Auf dem Weg zur Nachhaltigkeit. Ergebnisse einer Dorfstudie
Y1  - 1999
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-4120
ER  - 
TY  - JOUR
A1  - Zorn, Edgar Ulrich
A1  - Le Corvec, Nicolas
A1  - Varley, Nick R.
A1  - Salzer, Jacqueline T.
A1  - Walter, Thomas R.
A1  - Navarro-Ochoa, Carlos
A1  - Vargas-Bracamontes, Dulce M.
A1  - Thiele, Samuel T.
A1  - Arámbula Mendoza, Raúl
T1  - Load stress controls on directional lava dome growth at Volcan de Colima, Mexico
JF  - Frontiers in Earth Science
N2  - During eruptive activity of andesitic stratovolcanoes, the extrusion of lava domes, their collapse and intermittent explosions are common volcanic hazards. Many lava domes grow in a preferred direction, in turn affecting the direction of lava flows and pyroclastic density currents. Access to active lava domes is difficult and hazardous, so detailed data characterizing lava dome growth are typically limited, keeping the processes controlling the directionality of extrusions unclear. Here we combine TerraSAR-X satellite radar observations with high-resolution airborne photogrammetry to assess morphological changes, and perform finite element modeling to investigate the impact of loading stress on shallow magma ascent directions associated with lava dome extrusion and crater formation at Volcan de Colima, Mexico. The TerraSAR-X data, acquired in similar to 1-m resolution spotlight mode, enable us to derive a chronology of the eruptive processes from intensity-based time-lapse observations of the general crater and dome evolution. The satellite images are complemented by close-range airborne photos, processed by the Structure-from-Motion workflow. This allows the derivation of high-resolution digital elevation models, providing insight into detailed loading and unloading features. During the observation period from Jan-2013 to Feb-2016, we identify a dominantly W-directed dome growth and lava flow production until Jan-2015. In Feb-2015, following the removal of the active summit dome, the surface crater widened and elongated along a NE-SW axis. Later in May-2015, a new dome grew toward the SW of the crater while a separate vent developed in the NE of the crater, reflecting a change in the direction of magma ascent and possible conduit bifurcation. Finite element models show a significant stress change in agreement with the observed magma ascent direction changes in response to the changing surface loads, both for loading (dome growth) and unloading (crater forming excavation) cases. These results allow insight into shallow dome growth dynamics and the migration of magma ascent in response to changing volcano summit morphology. They further highlight the importance of detailed volcano summit morphology surveillance, as changes in direction or location of dome extrusion may have major implications regarding the directions of potential volcanic hazards, such as pyroclastic density currents generated by dome collapse.
KW  - lava dome
KW  - load stress
KW  - Volcan de Colima
KW  - TerraSAR-X
KW  - photogrammetry
KW  - finite element modeling
Y1  - 2019
U6  - https://doi.org/10.3389/feart.2019.00084
SN  - 2296-6463
VL  - 7
PB  - Frontiers Media
CY  - Lausanne
ER  - 
TY  - JOUR
A1  - Bozzo, Enrico
A1  - Bhalerao, V.
A1  - Pradhan, Prajal
A1  - Tomsick, J.
A1  - Romano, Patrizia
A1  - Ferrigno, Carlo
A1  - Chaty, S.
A1  - Oskinova, Lida
A1  - Manousakis, A.
A1  - Walter, R.
A1  - Falanga, M.
A1  - Campana, S.
A1  - Stella, L.
A1  - Ramolla, M.
A1  - Chini, R.
T1  - Multi-wavelength observations of IGR J17544-2619 from quiescence to outburst
JF  - Journal of geophysical research : Earth surface
N2  - In this paper we report on a long multi-wavelength observational campaign of the supergiant fast X-ray transient prototype IGR J17544-2619. A 150 ks-long observation was carried out simultaneously with XMM-Newton and NuSTAR, catching the source in an initial faint X-ray state and then undergoing a bright X-ray outburst lasting approximately 7 ks. We studied the spectral variability during outburst and quiescence by using a thermal and bulk Comptonization model that is typically adopted to describe the X-ray spectral energy distribution of young pulsars in high mass X-ray binaries. Although the statistics of the collected X-ray data were relatively high, we could neither confirm the presence of a cyclotron line in the broad-band spectrum of the source (0.5-40 keV), nor detect any of the previously reported tentative detections of the source spin period. The monitoring carried out with Swift/XRT during the same orbit of the system observed by XMM-Newton and NuSTAR revealed that the source remained in a low emission state for most of the time, in agreement with the known property of all supergiant fast X-ray transients being significantly sub-luminous compared to other supergiant X-ray binaries. Optical and infrared observations were carried out for a total of a few thousand seconds during the quiescence state of the source detected by XMM-Newton and NuSTAR. The measured optical and infrared magnitudes were slightly lower than previous values reported in the literature, but compatible with the known micro-variability of supergiant stars. UV observations obtained with the UVOT telescope on-board Swift did not reveal significant changes in the magnitude of the source in this energy domain compared to previously reported values.
KW  - X-rays: binaries
Y1  - 2016
U6  - https://doi.org/10.1051/0004-6361/201629311
SN  - 1432-0746
VL  - 596
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Barden, Marco
A1  - Rix, Hans-Walter
A1  - Somerville, Rachel S.
A1  - Bell, Eric F.
A1  - Häußler, Boris
A1  - Peng, Chen Y.
A1  - Borch, Andrea
A1  - Beckwith, Steven V. W.
A1  - Caldwell, John A. R.
A1  - Heymans, Catherine
A1  - Jahnke, Knud
A1  - Jogee, Shardha
A1  - McIntosh, Daniel H.
A1  - Meisenheimer, Klaus
A1  - Sanchez, Sebastian F.
A1  - Wisotzki, Lutz
A1  - Wolf, C.
T1  - GEMS : the surface brightness and surface mass density evolution of disk galaxies
N2  - We combine HST imaging from the GEMS ( Galaxy Evolution from Morphologies and SEDs) survey with photometric redshifts from COMBO-17 to explore the evolution of disk-dominated galaxies since z less than or similar to 1.1. The sample is composed of all GEMS galaxies with Sersic indices n < 2.5, derived from fits to the galaxy images. We account fully for selection effects through careful analysis of image simulations; we are limited by the depth of the redshift and HST data to the study of galaxies with M-V less than or similar to -20, or equivalently, log (M/M-circle dot) greater than or similar to 10. We find strong evolution in the magnitude-size scaling relation for galaxies with M-V less than or similar to -20, corresponding to a brightening of similar to 1 mag arcsec(-2) in rest-frame V band by z similar to 1. Yet disks at a given absolute magnitude are bluer and have lower stellar mass-to-light ratios at z similar to 1 than at the present day. As a result, our findings indicate weak or no evolution in the relation between stellar mass and effective disk size for galaxies with log (M/M-circle dot) greater than or similar to 10 over the same time interval. This is strongly inconsistent with the most naive theoretical expectation, in which disk size scales in proportion to the halo virial radius, which would predict that disks are a factor of 2 denser at fixed mass at z similar to 1. The lack of evolution in the stellar mass-size relation is consistent with an "inside-out'' growth of galaxy disks on average (galaxies increasing in size as they grow more massive), although we cannot rule out more complex evolutionary scenarios
Y1  - 2005
ER  - 
TY  - JOUR
A1  - Jahnke, Knud
A1  - Sanchez, Sebastian F.
A1  - Wisotzki, Lutz
A1  - Barden, Marco
A1  - Beckwith, Steven V. W.
A1  - Bell, Eric F.
A1  - Borch, Andrea
A1  - Caldwell, John A. R.
A1  - Häußler, Boris
A1  - Heymans, Catherine
A1  - Jogee, Shardha
A1  - McIntosh, Daniel H.
A1  - Meisenheimer, Klaus
A1  - Peng, Chen Y.
A1  - Rix, Hans-Walter
A1  - Somerville, Rachel S.
A1  - Wolf, C.
T1  - Ultraviolet light from young stars in GEMS quasar host galaxies at 1.8 < z < 2.75
N2  - We have performed Hubble Space Telescope imaging of a sample of 23 high-redshift (1.8<z<2.75) active galactic nuclei (AGNs), drawn from the COMBO-17 survey. The sample contains moderately luminous quasars (M(B)similar to-23). The data are part of the Galaxy Evolution from Morphologies and SEDs imaging survey that provides high-resolution optical images obtained with the Advanced Camera for Surveys in two bands (F606W and F850LP), sampling the rest-frame UV flux of the targets. To deblend the AGN images into nuclear and resolved (host galaxy) components, we use a point-spread function subtraction technique that is strictly conservative with respect to the flux of the host galaxy. We resolve the host galaxies in both filter bands in nine of the 23 AGNs, whereas the remaining 14 objects are considered nondetections, with upper limits of less than 5% of the nuclear flux. However, when we co-add the unresolved AGN images into a single high signal-to-noise ratio composite image, we find again an unambiguously resolved host galaxy. The recovered host galaxies have apparent magnitudes of 23.0<F606W<26.0 and 22.5<F850LP<24.5, with rest-frame UV colors in the range -0.2<(F606W-F850LP)(obs)<2.3. The rest-frame absolute magnitudes at 200 nm are -20.0<M-200 nm<-22.2. The photometric properties of the composite host are consistent with the individual resolved host galaxies. We find that the UV colors of all host galaxies are substantially bluer than expected from an old population of stars with formation redshift z<=5, independent of the assumed metallicities. These UV colors and luminosities range up to the values found for Lyman break galaxies (LBGs) at z=3. Our results suggest either a recent starburst of, e. g., a few percent of the total stellar mass at 100 Myr before observation, with mass fraction and age strongly degenerate, or the possibility that the detected UV emission may be due to young stars forming continuously. For the latter case we estimate star formation rates of typically &SIM;6 M&ODOT; yr(-1) (uncorrected for internal dust attenuation), which again lies in the range of rates implied from the UV flux of LBGs. Our results agree with the recent discovery of enhanced blue stellar light in AGN hosts at lower redshifts
Y1  - 2004
SN  - 0004-637X
ER  - 
TY  - JOUR
A1  - Sanchez, Sebastian F.
A1  - Jahnke, Knud
A1  - Wisotzki, Lutz
A1  - McIntosh, Daniel H.
A1  - Bell, Eric F.
A1  - Barden, Marko
A1  - Beckwith, Steven V. W.
A1  - Borch, Andrea
A1  - Caldwell, John A. R.
A1  - Haussler, Boris
A1  - Jogee, Shardha
A1  - Meisenheimer, Klaus
A1  - Peng, Chen Y.
A1  - Rix, Hans-Walter
A1  - Somerville, Rachel S.
A1  - Wolf, C.
T1  - Colors of active galactic nucleus host galaxies at 0.5 < z < 1.1 from the GEMS survey
N2  - We present the results from a study of the host galaxies of 15 optically selected active galactic nuclei (AGNs) with 0.5<z<1.1 from the Galaxy Evolution from Morphology and SEDs project (GEMS). GEMS is a Hubble Space Telescope imaging survey of a similar to28' x 28' contiguous field centered on the Chandra Deep Field-South in the F606W and F850LP filter bands. It incorporates the spectral energy distributions and redshifts of similar to10,000 objects, obtained by the COMBO-17 project. We have detected the host galaxies of all 15 AGNs in the F850LP band (and 13 of 15 in the F606W band), recovering their fluxes, morphologies, and structural parameters. We find that 80% of the host galaxies have early-type (bulge-dominated) morphologies, while the rest have structures characteristic of late-type (disk-dominated) galaxies. We find that 25% of the early types and 30% of the late types exhibit disturbances consistent with galaxy interactions. The hosts show a wide range of colors, from those of red-sequence galaxies to blue colors consistent with ongoing star formation. Roughly 70% of the morphologically early-type hosts have rest-frame blue colors, a much larger fraction than those typical of nonactive morphologically early-type galaxies in this redshift and luminosity range. Yet, we find that the early-type hosts are structurally similar to red-sequence elliptical galaxies, inasmuch as they follow an absolute magnitude versus half-light size correlation that is consistent with the mean relation for early-type galaxies at similar redshifts
Y1  - 2004
SN  - 0004-637X
ER  - 
TY  - JOUR
A1  - Jäger, Matthias
A1  - Stegemann, George I.
A1  - Brinker, Walter
A1  - Yilmaz, Sükrü
A1  - Bauer, Siegfried
A1  - Horsthuis, W. H. G.
A1  - Moehlmann, Gustaaf R.
T1  - Comparison of quasi-phase-matching geometries for second-harmonic generation in poled polymer channel waveguides at 1.5 æm
Y1  - 1996
ER  - 
TY  - JOUR
A1  - Bathke, Hannes
A1  - Sudhaus, H.
A1  - Holohan, E. P.
A1  - Walter, T. R.
A1  - Shirzaei, M.
T1  - An active ring fault detected at Tendurek volcano by using InSAR
JF  - JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
N2  - Although ring faults are present at many ancient, deeply eroded volcanoes, they have been detected at only very few modern volcanic centers. At the so far little studied Tendurek volcano in eastern Turkey, we generated an ascending and a descending InSAR time series of its surface displacement field for the period from 2003 to 2010. We detected a large (similar to 105km(2)) region that underwent subsidence at the rate of similar to 1cm/yr during this period. Source modeling results show that the observed signal fits best to simulations of a near-horizontal contracting sill located at around 4.5km below the volcano summit. Intriguingly, the residual displacement velocity field contains a steep gradient that systematically follows a system of arcuate fractures visible on the volcano&rsquo;s midflanks. RapidEye satellite optical images show that this fracture system has deflected Holocene lava flows, thus indicating its presence for at least several millennia. We interpret the arcuate fracture system as the surface expression of an inherited ring fault that has been slowly reactivated during the detected recent subsidence. These results show that volcano ring faults may not only slip rapidly during eruptive or intrusive phases, but also slowly during dormant phases.
KW  - Tendurek volcano
KW  - caldera subsidence
KW  - arcuate fracture system
KW  - fault reactivation
Y1  - 2013
U6  - https://doi.org/10.1002/jgrb.50305
SN  - 2169-9313
VL  - 118
IS  - 8
SP  - 4488
EP  - 4502
PB  - AMER GEOPHYSICAL UNION
CY  - WASHINGTON
ER  - 
TY  - JOUR
A1  - Homolka, R. Walter
T1  - Back to the Ice Age? : The Roman Catholic Church and Judaism
N2  - Until well into the twentieth century, Jews and Christians had no mutual basis for discourse. The Christian- Jewish dialogue and the rapprochement between the Holy See and the State of Israel are owed in essence to feelings of shame regarding the Shoah. The Second Vatican Council and the pontificate of John Paul II signified substantial breakthroughs. Since then, though, the sense of guilt has eased, and the Roman Catholic Church's awareness of the injustice of its role as fellow traveller to, and henchman of, the Third Reich has diminished. Under the current Pope, Benedict XVI, the relationship between Jews and Catholics has noticeably deteriorated. After five years of his pontificate, Joseph Ratzinger has lost a great deal of trust, and not only among Jews.
Y1  - 2010
UR  - http://www.informaworld.com/openurl?genre=journal&issn=1353-7121
U6  - https://doi.org/10.1080/13537121.2010.511800
SN  - 1353-7121
ER  - 
TY  - JOUR
A1  - Tu, Rui
A1  - Wang, Rongjiang
A1  - Walter, Thomas R.
A1  - Diao, FaQi
T1  - Adaptive recognition and correction of baseline shifts from collocated GPS and accelerometer using two phases Kalman filter
JF  - Advances in space research
N2  - The real-time recognition and precise correction of baseline shifts in strong-motion records is a critical issue for GPS and accelerometer combined processing. This paper proposes a method to adaptively recognize and correct baseline shifts in strong-motion records by utilizing GPS measurements using two phases Kalman filter. By defining four kinds of learning statistics and criteria, the time series of estimated baseline shifts can be divided into four time intervals: initialization, static, transient and permanent. During the time interval in which the transient baseline shift is recognized, the dynamic noise of the Kalman filter system and the length of the baseline shifts estimation window are adaptively adjusted to yield a robust integration solution. The validations from an experimental and real datasets show that acceleration baseline shifts can be precisely recognized and corrected, thus, the combined system adaptively adjusted the estimation strategy to get a more robust solution. (C) 2014 COSPAR. Published by Elsevier Ltd. All rights reserved.
KW  - GPS
KW  - Strong-motion
KW  - Baseline shift
KW  - Kalman filter
KW  - Integration
Y1  - 2014
U6  - https://doi.org/10.1016/j.asr.2014.07.008
SN  - 0273-1177
SN  - 1879-1948
VL  - 54
IS  - 9
SP  - 1924
EP  - 1932
PB  - Elsevier
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Tu, Rui
A1  - Ge, Maorong
A1  - Wang, Rongjiang
A1  - Walter, Thomas R.
T1  - A new algorithm for tight integration of real-time GPS and strong-motion records, demonstrated on simulated, experimental, and real seismic data
JF  - Journal of seismology
N2  - The complementary advantages of GPS and seismic measurements are well recognized in seismotectonic monitoring studies. Therefore, integrated processing of the two data streams has been proposed recently in an attempt to obtain accurate and reliable information of surface displacements associated with earthquakes. A hitherto still critical issue in the integrated processing is real-time detection and precise estimation of the transient baseline error in the seismic records. Here, we report on a new approach by introducing the seismic acceleration corrected by baseline errors into the state equation system. The correction is performed and regularly updated in short epochs (with increments which may be as short as seconds), so that station position, velocity, and acceleration can be constrained very tightly and baseline error can be estimated as a random-walk process. With the adapted state equation system, our study highlights the use of a new approach developed for integrated processing of GPS and seismic data by means of sequential least-squares adjustment. The efficiency of our approach is demonstrated and validated using simulated, experimental, and real datasets. The latter were collected at collocated GPS and seismic stations around the 4 April 2010, E1 Mayor-Cucapah earthquake (Mw, 7.2). The results have shown that baseline errors of the strong-motion sensors are corrected precisely and high-precision seismic displacements are real-timely obtained by the new approach.
KW  - High-rateGPS
KW  - Strong-motion records
KW  - Baseline error
KW  - Tight integration
KW  - Precise point positioning
Y1  - 2014
U6  - https://doi.org/10.1007/s10950-013-9408-x
SN  - 1383-4649
SN  - 1573-157X
VL  - 18
IS  - 1
SP  - 151
EP  - 161
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - JOUR
A1  - Lisdat, Fred
A1  - Utepbergenov, D.
A1  - Haseloff, R. F.
A1  - Blasig, Ingolf E.
A1  - Stöcklein, Walter F. M.
A1  - Scheller, Frieder W.
A1  - Brigelius-Flohé, Regina
T1  - An optical method for the detection of oxidative stress using protein-RNA interaction
Y1  - 2001
ER  - 
TY  - JOUR
A1  - Renteria, Miguel E.
A1  - Schmaal, L.
A1  - Hibar, D. P.
A1  - Couvy-Duchesne, B.
A1  - Strike, L. T.
A1  - Mills, N. T.
A1  - de Zubicaray, Greig. I.
A1  - McMahon, Katie. L.
A1  - Medland, Sarah E.
A1  - Gillespie, N. A.
A1  - Hatton, S. N.
A1  - Lagopoulos, J.
A1  - Veltman, D. J.
A1  - van der Wee, N.
A1  - van Erp, T. G. M.
A1  - Wittfeld, K.
A1  - Grabe, H. J.
A1  - Block, Andrea
A1  - Hegenscheid, K.
A1  - Voelzke, H.
A1  - Veer, I. M.
A1  - Walter, H.
A1  - Schnell, K.
A1  - Schramm, E.
A1  - Normann, C.
A1  - Schoepf, Dieter
A1  - Konrad, C.
A1  - Zurowski, B.
A1  - Godlewska, B. R.
A1  - Cowen, P. J.
A1  - Penninx, B. W. J. H.
A1  - Jahanshad, N.
A1  - Thompson, Paul M.
A1  - Wright, M. J.
A1  - Martin, N. G.
A1  - Christensen, H.
A1  - Hickie, I. B.
T1  - Subcortical brain structure and suicidal behaviour in major depressive disorder: a meta-analysis from the ENIGMA-MDD working group
JF  - Translational Psychiatry
Y1  - 2017
U6  - https://doi.org/10.1038/tp.2017.84
SN  - 2158-3188
VL  - 7
SP  - 2301
EP  - 2320
PB  - Nature Publ. Group
CY  - New York
ER  - 
TY  - CHAP
A1  - Walter, R.
A1  - Zurita-Heras, J.
A1  - Leyder, J.-C.
T1  - Probing clumpy stellar winds with a neutron star
N2  - INTEGRAL tripled the number of super-giant high-mass X-ray binaries (sgHMXB) known in the Galaxy by revealing absorbed and fast transient (SFXT) systems. Quantitative constraints on the wind clumping of massive stars can be obtained from the study of the hard X-ray variability of SFXT. A large fraction of the hard X-ray emission is emitted in the form of flares with a typical duration of 3 ksec, frequency of 7 days and luminosity of $10^{36}$ erg/s. Such flares are most probably emitted by the interaction of a compact object orbiting at $\sim10~R_*$ with wind clumps ($10^{22 ... 23}$ g) representing a large fraction of the stellar mass-loss rate. The density ratio between the clumps and the inter-clump medium is $10^{2 ... 4}$. The parameters of the clumps and of the inter-clump medium, derived from the SFXT flaring behavior, are in good agreement with macro-clumping scenario and line-driven instability simulations. SFXT are likely to have larger orbital radius than classical sgHMXB.
Y1  - 2007
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-18024
ER  - 
TY  - JOUR
A1  - Namiki, Atsuko
A1  - Rivalta, Eleonora
A1  - Woith, Heiko
A1  - Willey, Timothy
A1  - Parolai, Stefano
A1  - Walter, Thomas R.
T1  - Volcanic activities triggered or inhibited by resonance of volcanic edifices to large earthquakes
JF  - Geology
N2  - The existence of a causal link between large earthquakes and volcanic unrest is widely accepted. Recent observations have also revealed counterintuitive negative responses of volcanoes to large earthquakes, including decreased gas emissions and subsidence in volcanic areas. In order to explore the mechanisms that could simultaneously explain both the positive and negative responses of volcanic activity to earthquakes, we here focus on the role played by topography. In the laboratory, we shook a volcanic edifice analogue, made of gel, previously injected with a buoyant fluid. We find that shaking triggers rapid migration of the buoyant fluid upward, downward, or laterally, depending on the fluid’s buoyancy and storage depth; bubbly fluids stored at shallow depth ascend, while low-buoyancy fluids descend or migrate laterally. The migration of fluids induced by shaking is two orders of magnitude faster than without shaking. Downward or lateral fluid migration may decrease volcanic gas emissions and cause subsidence as a negative response, while upward migration is consistent both with an increase in volcanic activity and immediate unrest (deformation and seismicity) after large earthquakes. The fluid migration is more efficient when the oscillation frequency is close to the resonance frequency of the edifice. The resonance frequency for a 30-km-wide volcanic mountain range, such as those where subsidence was observed, is ∼0.07 Hz. Only large earthquakes are able to cause oscillation at such low frequencies.
Y1  - 2018
U6  - https://doi.org/10.1130/G45323.1
SN  - 0091-7613
SN  - 1943-2682
VL  - 47
IS  - 1
SP  - 67
EP  - 70
PB  - American Institute of Physics
CY  - Boulder
ER  - 
TY  - JOUR
A1  - Eibl, Eva P. S.
A1  - Hainzl, Sebastian
A1  - Vesely, Nele I. K.
A1  - Walter, Thomas R.
A1  - Jousset, Philippe
A1  - Hersir, Gylfi Pall
A1  - Dahm, Torsten
T1  - Eruption interval monitoring at strokkur Geyser, Iceland
JF  - Geophysical research letters
N2  - Geysers are hot springs whose frequency of water eruptions remain poorly understood. We set up a local broadband seismic network for 1 year at Strokkur geyser, Iceland, and developed an unprecedented catalog of 73,466 eruptions. We detected 50,135 single eruptions but find that the geyser is also characterized by sets of up to six eruptions in quick succession. The number of single to sextuple eruptions exponentially decreased, while the mean waiting time after an eruption linearly increased (3.7 to 16.4 min). While secondary eruptions within double to sextuple eruptions have a smaller mean seismic amplitude, the amplitude of the first eruption is comparable for all eruption types. We statistically model the eruption frequency assuming discharges proportional to the eruption multiplicity and a constant probability for subsequent events within a multituple eruption. The waiting time after an eruption is predictable but not the type or amplitude of the next one. <br /> Plain Language Summary Geysers are springs that often erupt in hot water fountains. They erupt more often than volcanoes but are quite similar. Nevertheless, it is poorly understood how often volcanoes and also geysers erupt. We created a list of 73,466 eruption times of Strokkur geyser, Iceland, from 1 year of seismic data. The geyser erupted one to six times in quick succession. We found 50,135 single eruptions but only 1 sextuple eruption, while the mean waiting time increased from 3.7 min after single eruptions to 16.4 min after sextuple eruptions. Mean amplitudes of each eruption type were higher for single eruptions, but all first eruptions in a succession were similar in height. Assuming a constant heat inflow at depth, we can predict the waiting time after an eruption but not the type or amplitude of the next one.
Y1  - 2019
U6  - https://doi.org/10.1029/2019GL085266
SN  - 0094-8276
SN  - 1944-8007
VL  - 47
IS  - 1
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - JOUR
A1  - Park, H.
A1  - Walta, S.
A1  - Rosencrantz, Ruben R.
A1  - Koerner, A.
A1  - Schulte, Christoph
A1  - Elling, L.
A1  - Richtering, Walter
A1  - Böker, Alexander
T1  - Micelles from self-assembled double-hydrophilic PHEMA-glycopolymer-diblock copolymers as multivalent scaffolds for lectin binding
JF  - Polymer Chemistry
N2  - We introduce a novel double-hydrophilic hydroxyethylmethacrylate (HEMA) based diblock glycopolymer which self-assembles into homogeneous spherical micellar structures in water. The micellar structure renders surface-oriented N-acetylglucocosamine (GlcNAc) sugar moieties for strong multivalent glycan-mediated lectin binding. Structural analysis and lectin binding is performed by microscopy methods, dynamic light scattering (DLS) and two-focus fluorescence correlation spectroscopy (2fFCS), revealing a novel micellar type of multivalent sugar binding scaffold with high potential for biomedical applications.
Y1  - 2016
U6  - https://doi.org/10.1039/c5py00797f
SN  - 1759-9954
SN  - 1759-9962
VL  - 7
SP  - 878
EP  - 886
PB  - Royal Society of Chemistry
CY  - Cambridge
ER  - 
TY  - JOUR
A1  - Eibl, Eva P. S.
A1  - Müller, Daniel
A1  - Walter, Thomas R.
A1  - Allahbakhshi, Masoud
A1  - Jousset, Philippe
A1  - Hersir, Gylfi Páll
A1  - Dahm, Torsten
T1  - Eruptive cycle and bubble trap of Strokkur Geyser, Iceland
JF  - Journal of geophysical research : JGR. B: Solid earth
N2  - The eruption frequency of geysers can be studied easily on the surface. However, details of the internal structure including possible water and gas filled chambers feeding eruptions and the driving mechanisms often remain elusive. We used a multidisciplinary network of seismometers, video cameras, water pressure sensors and one tiltmeter to study the eruptive cycle, internal structure, and mechanisms driving the eruptive cycle of Strokkur geyser in June 2018. An eruptive cycle at Strokkur always consists of four phases: (1) Eruption, (2) post-eruptive conduit refilling, (3) gas filling of the bubble trap, and (4) regular bubble collapse at shallow depth in the conduit. For a typical single eruption 19 +/- 4 bubble collapses occur in Phase 3 and 8 +/- 2 collapses in Phase 4 at a mean spacing of 1.52 +/- 0.29 and 24.5 +/- 5.9 s, respectively. These collapses release latent heat to the fluid in the bubble trap (Phase 3) and later to the fluid in the conduit (Phase 4). The latter eventually reaches thermodynamic conditions for an eruption. Single to sextuple eruptions have similar spacings between bubble collapses and are likely fed from the same bubble trap at 23.7 +/- 4.4 m depth, 13-23 m west of the conduit. However, the duration of the eruption and recharging phase linearly increases likely due to a larger water, gas and heat loss from the system. Our tremor data provides documented evidence for a bubble trap beneath a pool geyser.
KW  - bubble trap
KW  - eruptive cycle
KW  - geyser
KW  - hydrothermal systems
KW  - source
KW  - location
KW  - tremor
Y1  - 2021
U6  - https://doi.org/10.1029/2020JB020769
SN  - 2169-9313
SN  - 2169-9356
VL  - 126
IS  - 4
PB  - Wiley
CY  - Hoboken, NJ
ER  - 
TY  - JOUR
A1  - Armstrong, Michael R.
A1  - Radousky, Harry B.
A1  - Austin, Ryan A.
A1  - Tschauner, Oliver
A1  - Brown, Shaughnessy
A1  - Gleason, Arianna E.
A1  - Goldman, Nir
A1  - Granados, Eduardo
A1  - Grivickas, Paulius
A1  - Holtgrewe, Nicholas
A1  - Kroonblawd, Matthew P.
A1  - Lee, Hae Ja
A1  - Lobanov, Sergey
A1  - Nagler, Bob
A1  - Nam, Inhyuk
A1  - Prakapenka, Vitali
A1  - Prescher, Clemens
A1  - Reed, Evan J.
A1  - Stavrou, Elissaios
A1  - Walter, Peter
A1  - Goncharov, Alexander F.
A1  - Belof, Jonathan L.
T1  - Highly ordered graphite (HOPG) to hexagonal diamond (lonsdaleite) phase transition observed on picosecond time scales using ultrafast x-ray diffraction
JF  - Journal of applied physics
N2  - The response of rapidly compressed highly oriented pyrolytic graphite (HOPG) normal to its basal plane was investigated at a pressure of & SIM;80 GPa. Ultrafast x-ray diffraction using & SIM;100 fs pulses at the Materials Under Extreme Conditions sector of the Linac Coherent Light Source was used to probe the changes in crystal structure resulting from picosecond timescale compression at laser drive energies ranging from 2.5 to 250 mJ. A phase transformation from HOPG to a highly textured hexagonal diamond structure is observed at the highest energy, followed by relaxation to a still highly oriented, but distorted graphite structure following release. We observe the formation of a highly oriented lonsdaleite within 20 ps, subsequent to compression. This suggests that a diffusionless martensitic mechanism may play a fundamental role in phase transition, as speculated in an early work on this system, and more recent static studies of diamonds formed in impact events. Published by AIP Publishing.
Y1  - 2022
U6  - https://doi.org/10.1063/5.0085297
SN  - 0021-8979
SN  - 1089-7550
VL  - 132
IS  - 5
PB  - AIP Publishing
CY  - Melville
ER  - 
TY  - JOUR
A1  - Beckmann, Nadine
A1  - Kadow, Stephanie
A1  - Schumacher, Fabian
A1  - Goethert, Joachim R.
A1  - Kesper, Stefanie
A1  - Draeger, Annette
A1  - Schulz-Schaeffer, Walter J.
A1  - Wang, Jiang
A1  - Becker, Jan U.
A1  - Kramer, Melanie
A1  - Kuehn, Claudine
A1  - Kleuser, Burkhard
A1  - Becker, Katrin Anne
A1  - Gulbins, Erich
A1  - Carpinteiro, Alexander
T1  - Pathological manifestations of Farber disease in a new mouse model
JF  - Biological chemistry
N2  - Farber disease (FD) is a rare lysosomal storage disorder resulting from acid ceramidase deficiency and subsequent ceramide accumulation. No treatments are clinically available and affected patients have a severely shortened lifespan. Due to the low incidence, the pathogenesis of FD is still poorly understood. Here, we report a novel acid ceramidase mutant mouse model that enables the study of pathogenic mechanisms of FD and ceramide accumulation. Asah1(tmEx1) mice were generated by deletion of the acid ceramidase signal peptide sequence. The effects on lysosomal targeting and activity of the enzyme were assessed. Ceramide and sphingomyelin levels were quantified by liquid chromatography tandem-mass spectrometry (LC-MS/MS) and disease manifestations in several organ systems were analyzed by histology and biochemistry. We show that deletion of the signal peptide sequence disrupts lysosomal targeting and enzyme activity, resulting in ceramide and sphingomyelin accumulation. The affected mice fail to thrive and die early. Histiocytic infiltrations were observed in many tissues, as well as lung inflammation, liver fibrosis, muscular disease manifestations and mild kidney injury. Our new mouse model mirrors human FD and thus offers further insights into the pathogenesis of this disease. In the future, it may also facilitate the development of urgently needed therapies.
KW  - acid ceramidase
KW  - ceramide
KW  - Farber disease
KW  - lysosomal storage disorders
Y1  - 2018
U6  - https://doi.org/10.1515/hsz-2018-0170
SN  - 1431-6730
SN  - 1437-4315
VL  - 399
IS  - 10
SP  - 1183
EP  - 1202
PB  - De Gruyter
CY  - Berlin
ER  - 
TY  - JOUR
A1  - Wirges, Werner
A1  - Przyrembel, G.
A1  - Brinker, Walter
A1  - Gerhard, Reimund
A1  - Klemberg-Sapieha, J.
A1  - Martinu, L.
A1  - Poitras, D.
A1  - Wertheimer, M. R.
T1  - Metallised viscoelastic control layers for light-valve projection displays
Y1  - 1995
ER  - 
TY  - JOUR
A1  - Brinker, Walter
A1  - Wirges, Werner
A1  - Molzow, Wolf-Dietrich
A1  - Gerhard, Reimund
A1  - Melcher, R.
A1  - Budde, W.
A1  - Fiedler, H.
T1  - Active silicon CMOS addressing matrices for light-valve projection displays
Y1  - 1995
ER  - 
TY  - JOUR
A1  - Heslop, J. K.
A1  - Winkel, Matthias
A1  - Anthony, K. M. Walter
A1  - Spencer, R. G. M.
A1  - Podgorski, D. C.
A1  - Zito, P.
A1  - Kholodov, A.
A1  - Zhang, M.
A1  - Liebner, Susanne
T1  - Increasing organic carbon biolability with depth in yedoma permafrost
BT  - ramifications for future climate change
JF  - Journal of geophysical research : Biogeosciences
N2  - Permafrost thaw subjects previously frozen organic carbon (OC) to microbial decomposition, generating the greenhouse gases (GHG) carbon dioxide (CO2) and methane (CH4) and fueling a positive climate feedback. Over one quarter of permafrost OC is stored in deep, ice-rich Pleistocene-aged yedoma permafrost deposits. We used a combination of anaerobic incubations, microbial sequencing, and ultrahigh-resolution mass spectrometry to show yedoma OC biolability increases with depth along a 12-m yedoma profile. In incubations at 3 degrees C and 13 degrees C, GHG production per unit OC at 12-versus 1.3-m depth was 4.6 and 20.5 times greater, respectively. Bacterial diversity decreased with depth and we detected methanogens at all our sampled depths, suggesting that in situ microbial communities are equipped to metabolize thawed OC into CH4. We concurrently observed an increase in the relative abundance of reduced, saturated OC compounds, which corresponded to high proportions of C mineralization and positively correlated with anaerobic GHG production potentials and higher proportions of OC being mineralized as CH4. Taking into account the higher global warming potential (GWP) of CH4 compared to CO2, thawed yedoma sediments in our study had 2 times higher GWP at 12-versus 9.0-m depth at 3 degrees C and 15 times higher GWP at 13 degrees C. Considering that yedoma is vulnerable to processes that thaw deep OC, our findings imply that it is important to account for this increasing GHG production and GWP with depth to better understand the disproportionate impact of yedoma on the magnitude of the permafrost carbon feedback.
KW  - permafrost
KW  - carbon
KW  - yedoma
KW  - Alaska
KW  - FT-ICR MS
KW  - microbes
Y1  - 2019
U6  - https://doi.org/10.1029/2018JG004712
SN  - 2169-8953
SN  - 2169-8961
VL  - 124
IS  - 7
SP  - 2021
EP  - 2038
PB  - American Geophysical Union
CY  - Washington
ER  -