909 results on '"Ceca, R."'
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152. Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre
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Abdalla, H., Abe, H., Abe, S., Abusleme, A., Acero, F., Acharyya, A., Acín Portella, V., Ackley, K., Adam, R., Adams, C., Adhikari, S. S., Aguado-Ruesga, I., Agudo, I., Aguilera, R., Aguirre-Santaella, A., Aharonian, F., Alberdi, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amans, J. -P, Amati, L., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Ammendola, R., Anderson, J., Anduze, M., Angüner, E. O., Antonelli, L. A., Antonuccio, V., Antoranz, P., Anutarawiramkul, R., Aragunde Gutierrez, J., Aramo, C., Araudo, A., Araya, M., Arbet-Engels, A., Arcaro, C., Arendt, V., Armand, C., Armstrong, T., Arqueros, F., Arrabito, L., Arsioli, B., Artero, M., Asano, K., Ascasíbar, Y., Aschersleben, J., Ashley, M., Attinà, P., Aubert, P., Singh, C. B., Baack, D., Babic, A., Backes, M., Baena, V., Bajtlik, S., Baktash, A., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Balmaverde, B., Bamba, A., Bandiera, R., Baquero Larriva, A., Barai, P., Barbier, C., Barbosa Martins, V., Barcelo, M., Barkov, M., Barnard, M., Baroncelli, L., Barres Almeida, U., Barrio, J. A., Bastieri, D., Batista, P. I., Batkovic, I., Bauer, C., Bautista-González, R., Baxter, J., Becciani, U., Becerra González, J., Becherini, Y., Beck, G., Becker Tjus, J., Bednarek, W., Belfiore, A., Bellizzi, L., Belmont, R., Benbow, W., Berge, D., Bernardini, E., Bernardos, M. I., Bernlöhr, K., Berti, A., Berton, M., Bertucci, B., Beshley, V., Bhatt, N., Bhattacharyya, S., Bhattacharyya, W., Bi, B., Bicknell, G., Biederbeck, N., Bigongiari, C., Biland, A., Bird, R., Bissaldi, E., Biteau, J., Bitossi, M., Blanch, O., Blank, M., Blazek, J., Bobin, J., Boccato, C., Bocchino, F., Boehm, C., Bohacova, M., Boisson, C., Boix, J., Bolle, J. -P, Bolmont, J., Bonanno, G., Bonavolontà, C., Bonneau Arbeletche, L., Bonnoli, G., Bordas, P., Borkowski, J., Bórquez, S., Bose, R., Bose, D., Bosnjak, Z., Bottacini, E., Böttcher, M., Botticella, M. T., Boutonnet, C., Bouyjou, F., Bozhilov, V., Bozzo, E., Brahimi, L., Braiding, C., Brau-Nogué, S., Breen, S., Bregeon, J., Breuhaus, M., Brill, A., Brisken, W., Brocato, E., Brown, A. M., Brügge, K., Brun, P., Brun, F., Brunetti, L., Brunetti, G., Bruno, P., Bruno, A., Bruzzese, A., Bucciantini, N., Buckley, J., Bühler, R., Bulgarelli, A., Bulik, T., Bünning, M., Bunse, M., Burton, M., Burtovoi, A., Buscemi, M., Buschjäger, S., Busetto, G., Buss, J., Byrum, K., Caccianiga, A., Cadoux, F., Calanducci, A., Calderón, C., Calvo Tovar, J., Cameron, R., Campaña, P., Canestrari, R., Cangemi, F., Cantlay, B., Capalbi, M., Capasso, M., Cappi, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Cárdenas, V., Cardiel, L., Cardillo, M., Carlile, C., Caroff, S., Carosi, R., Carosi, A., Carquín, E., Carrère, M., Casandjian, J. -M, Casanova, S., Cascone, E., Cassol, F., Castro-Tirado, A. J., Catalani, F., Catalano, O., Cauz, D., Ceccanti, A., Celestino Silva, C., Celli, S., Cerny, K., Cerruti, M., Chabanne, E., Chadwick, P., Chai, Y., Chambery, P., Champion, C., Chandra, S., Chaty, S., Chen, A., Cheng, K., Chernyakova, M., Chiaro, G., Chiavassa, A., Chikawa, M., Chitnis, V. 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V., Delagnes, E., Deleglise, G., Delfino Reznicek, M., Delgado, C., Delgado Giler, A. G., Delgado Mengual, J., Della Ceca, R., Della Valle, M., Della Volpe, D., Depaoli, D., Depouez, D., Devin, J., Di Girolamo, T., Di Giulio, C., Di Piano, A., Di Pierro, F., Di Venere, L., Díaz, C., Díaz-Bahamondes, C., Dib, C., Diebold, S., Digel, S., Dima, R., Djannati-Ataï, A., Djuvsland, J., Dmytriiev, A., Docher, K., Domínguez, A., Dominis Prester, D., Donath, A., Donini, A., Dorner, D., Doro, M., Dos Anjos, R. D. C., Dournaux, J. -L, Downes, T., Drake, G., Drass, H., Dravins, D., Duangchan, C., Duara, A., Dubus, G., Ducci, L., Duffy, C., Dumora, D., Dundas Morå, K., Durkalec, A., Dwarkadas, V. V., Ebr, J., Eckner, C., Eder, J., Ederoclite, A., Edy, E., Egberts, K., Einecke, S., Eisch, J., Eleftheriadis, C., Elsässer, D., Emery, G., Emmanoulopoulos, D., Ernenwein, J. -P, Errando, M., Escarate, P., Escudero, J., Espinoza, C., Ettori, S., Eungwanichayapant, A., Evans, P., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Falcone, A., Fallah Ramazani, V., Falomo, R., Farakos, K., Fasola, G., Fattorini, A., Favre, Y., Fedora, R., Fedorova, E., Fegan, S., Feijen, K., Feng, Q., Ferrand, G., Ferrara, G., Ferreira, O., Fesquet, M., Fiandrini, E., Fiasson, A., Filipovic, M., Fink, D., Finley, J. P., Fioretti, V., Fiorillo, D. F. G., Fiorini, M., Flis, S., Flores, H., Foffano, L., Föhr, C., Fonseca, M. V., Font, L., Fontaine, G., Fornieri, O., Fortin, P., Fortson, L., Fouque, N., Fournier, A., Fraga, B., Franceschini, A., Franco, F. 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S., Götz, D., Goulart Coelho, J., Gourgouliatos, K., Grabarczyk, T., Graciani, R., Grandi, P., Grasseau, G., Grasso, D., Green, A. J., Green, D., Green, J., Greenshaw, T., Grenier, I., Grespan, P., Grillo, A., Grondin, M. -H, Grube, J., Guarino, V., Guest, B., Gueta, O., Gündüz, M., Gunji, S., Gusdorf, A., Gyuk, G., Hackfeld, J., Hadasch, D., Haga, J., Hagge, L., Hahn, A., Hajlaoui, J. E., Hakobyan, H., Halim, A., Hamal, P., Hanlon, W., Hara, S., Harada, Y., Hardcastle, M. J., Harvey, M., Hashiyama, K., Hassan Collado, T., Haubold, T., Haupt, A., Hautmann, U. A., Havelka, M., Hayashi, K., Hayashida, M., He, H., Heckmann, L., Heller, M., Helo, J. C., Henault, F., Henri, G., Hermann, G., Hermel, R., Hernández Cadena, S., Herrera Llorente, J., Herrero, A., Hervet, O., Hinton, J., Hiramatsu, A., Hiroshima, N., Hirotani, K., Hnatyk, B., Hnatyk, R., Hoang, J. K., Hoffmann, D., Hofmann, W., Hoischen, C., Holder, J., Holler, M., Hona, B., Horan, D., Hörandel, J., Horns, D., Horvath, P., Houles, J., Hovatta, T., Hrabovsky, M., Hrupec, D., Huang, Y., Huet, J. -M, Hughes, G., Hui, D., Hull, G., Humensky, T. B., Hütten, M., Iaria, R., Iarlori, M., Illa, J. M., Imazawa, R., Impiombato, D., Inada, T., Incardona, F., Ingallinera, A., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Insolia, A., Iocco, F., Ioka, K., Ionica, M., Iori, M., Iovenitti, S., Iriarte, A., Ishio, K., Ishizaki, W., Iwamura, Y., Jablonski, C., Jacquemier, J., Jacquemont, M., Jamrozy, M., Janecek, P., Jankowsky, F., Jardin-Blicq, A., Jarnot, C., Jean, P., Jiménez Martínez, I., Jin, W., Jocou, L., Jordana, N., Josselin, M., Jouvin, L., Jung-Richardt, I., Junqueira, F. J. P. A., Juramy-Gilles, C., Jurysek, J., Kaaret, P., Kadowaki, L. H. 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H., Lee, S., Leigui Oliveira, M. A., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P, Leone, F., Leray, V., Leto, G., Leuschner, F., Levy, C., Lindemann, R., Lindfors, E., Linhoff, L., Liodakis, I., Lipniacka, A., Lloyd, S., Lobo, M., Lohse, T., Lombardi, S., Longo, F., Lopez, A., López, M., López-Coto, R., Loporchio, S., Louis, F., Louys, M., Lucarelli, F., Lucchesi, D., Ludwig Boudi, H., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Maccarone, T., Mach, E., Maciejewski, A. J., Mackey, J., Madejski, G. 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D., Mc Comb, L., Mchardy, I., Mckeague, S., Mcmuldroch, S., Medina, E., Medina Miranda, D., Melandri, A., Melioli, C., Melkumyan, D., Menchiari, S., Mender, S., Mereghetti, S., Merino Arévalo, G., Mestre, E., Meunier, J. -L, Meures, T., Meyer, M., Micanovic, S., Miceli, M., Michailidis, M., Michałowski, J., Miener, T., Mievre, I., Miller, J., Minaya, I. A., Mineo, T., Minev, M., Miranda, J. 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C., Terrier, R., Terzic, T., Teshima, M., Testa, V., Thibaut, D., Thocquenne, F., Tian, W., Tibaldo, L., Tiengo, A., Tiziani, D., Tluczykont, M., Todero Peixoto, C. J., Tokanai, F., Toma, K., Tomankova, L., Tomastik, J., Tonev, D., Tornikoski, M., Torres, D. F., Torresi, E., Tosti, G., Tosti, L., Totani, T., Tothill, N., Toussenel, F., Tovmassian, G., Travnicek, P., Trichard, C., Trifoglio, M., Trois, A., Truzzi, S., Tsiahina, A., Tsuru, T., Turk, B., Tutone, A., Uchiyama, Y., Umana, G., Utayarat, P., Vaclavek, L., Vacula, M., Vagelli, V., Vagnetti, F., Vakili, F., Valdivia, J. A., Valentino, M., Valio, A., Vallage, B., Vallania, P., Valverde Quispe, J. V., Den Berg, A. M., Driel, W., Eldik, C., Rensburg, C., Soelen, B., Vandenbroucke, J., Vanderwalt, J., Vasileiadis, G., Vassiliev, V., Vázquez Acosta, M., Vecchi, M., Vega, A., Veh, J., Veitch, P., Venault, P., Venter, C., Ventura, S., Vercellone, S., Vergani, S., Verguilov, V., Verna, G., Vernetto, S., Verzi, V., Vettolani, G. P., Veyssiere, C., Viale, I., Viana, A., Viaux, N., Vicha, J., Vignatti, J., Vigorito, C. F., Villanueva, J., Vink, J., Vitale, V., Vittorini, V., Vodeb, V., Voelk, H., Vogel, N., Voisin, V., Vorobiov, S., Vovk, I., Vrastil, M., Vuillaume, T., Wagner, S. J., Wagner, R., Wagner, P., Wakazono, K., Wakely, S. P., Walter, R., Ward, M., Warren, D., Watson, J., Webb, N., Wechakama, M., Wegner, P., Weinstein, A., Weniger, C., Werner, F., Wetteskind, H., White, M., White, R., Wierzcholska, A., Wiesand, S., Wijers, R., Wilkinson, M., Will, M., Williams, D. A., Williams, J., Williamson, T., Wolter, A., Wong, Y. W., Wood, M., Wunderlich, C., Yamamoto, T., Yamamoto, H., Yamane, Y., Yamazaki, R., Yanagita, S., Yang, L., Yoo, S., Yoshida, T., Yoshikoshi, T., Yu, P., Yusafzai, A., Zacharias, M., Zaharijas, G., Zaldivar, B., Zampieri, L., Zanmar Sanchez, R., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zenin, A., Zerwekh, A., Zhdanov, V. 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O., Antonelli, L. A., Aramo, C., Araudo, A., Armstrong, T., Arqueros, F., Asano, K., Ascas??bar, Y., Ashley, M., Balazs, C., Ballester, O., Baquero Larriva, A., Barbosa Martins, V., Barkov, M., Barres de Almeida, U., Barrio, J. A., Bastieri, D., Becerra, J., Beck, G., Becker Tjus, J., Benbow, W., Benito, M., Berge, D., Bernardini, E., Bernl??hr, K., Berti, A., Bertucci, B., Beshley, V., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Bocchino, F., Boisson, C., Bonneau Arbeletche, L., Bordas, P., Bosnjak, Z., Bottacini, E., Bozhilov, V., Bregeon, J., Brill, A., Bringmann, T., Brown, A. 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B., H??tten, M., Iarlori, M., Inada, T., Inoue, S., Iocco, F., Iori, M., Jamrozy, M., Janecek, P., Jin, W., Jouvin, L., Jurysek, J., Karukes, E., Katarzy??ski, K., Kazanas, D., Kerszberg, D., Kherlakian, M. C., Kissmann, R., Kn??dlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kubo, H., Kushida, J., Lamanna, G., Lapington, J., Laporte, P., Leigui de Oliveira, M. A., Lenain, J., Leone, F., Leto, G., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., Lopez, A., L??pez, M., L??pez-Coto, R., Loporchio, S., Luque-Escamilla, P. L., Mach, E., Maggio, C., Maier, G., Mallamaci, M., Malta Nunes de Almeida, R., Mandat, D., Manganaro, M., Mangano, S., Manic??, G., Marculewicz, M., Mariotti, M., Markoff, S., Marquez, P., Mart??, J., Martinez, O., Mart??nez, M., Mart??nez, G., Mart??nez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Medina Miranda, D., Meyer, M., Miceli, M., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Montaruli, T., Moralejo, A., Morcuende-Parrilla, D., Morselli, A., Mukherjee, R., Mundell, C., Nagai, A., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Niko??ajuk, M., Ninci, D., Noda, K., Nosek, D., Nozaki, S., Ohira, Y., Ohishi, M., Ohtani, Y., Oka, T., Okumura, A., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, S., Orlando, E., Ostrowski, M., Oya, I., Pagano, I., Pagliaro, A., Palatiello, M., Pantaleo, F. R., Paredes, J. M., Pareschi, G., Parmiggiani, N., Patricelli, B., Pavleti??, L., Pe'Er, A., Pecimotika, M., P??rez-Romero, J., Persic, M., Petruk, O., Pfrang, K., Piano, G., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pintore, F., Pohl, M., Poireau, V., Prado, R. R., Prandini, E., Prast, J., Principe, G., Prokoph, H., Prouza, M., Przybilski, H., P??hlhofer, G., Pumo, M. L., Queiroz, F., Quirrenbach, A., Rain??, S., Rando, R., Razzaque, S., Recchia, S., Reimer, O., Reisenegger, A., Renier, Y., Rhode, W., Ribeiro, D., Rib??, M., Richtler, T., Rico, J., Rieger, F., Rinchiuso, L., Rizi, V., Rodriguez, J., Rodriguez Fernandez, G., Rodriguez Ramirez, J. C., Rojas, G., Romano, P., Romeo, G., Rosado, J., Rowell, G., Rudak, B., Russo, F., Sadeh, I., S??ther Hatlen, E., Safi-Harb, S., Salesa Greus, F., Salina, G., Sanchez, D., S??nchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Santos-Lima, R., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Seglar-Arroyo, M., Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Silk, J., Siqueira, C., Sliusar, V., S??owikowska, A., Sokolenko, A., Sol, H., Spencer, S., Stamerra, A., Stani??, S., Starling, R., Stolarczyk, T., Straumann, U., Stri??kovi??, J., Suda, Y., Suomijarvi, T., wierk, P., Tavecchio, F., Taylor, L., Tejedor, L. A., Teshima, M., Testa, V., Tibaldo, L., Todero Peixoto, C. J., Tokanai, F., Tonev, D., Tosti, G., Tosti, L., Tothill, N., Truzzi, S., Travnicek, P., Vagelli, V., Vallage, B., Vallania, P., van Eldik, C., Vandenbroucke, J., Varner, G. S., Vassiliev, V., V??zquez Acosta, M., Vecchi, M., Ventura, S., Vercellone, S., Vergani, S., Verna, G., Viana, A., Vigorito, C. F., Vink, J., Vitale, V., Vorobiov, S., Vovk, I., Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., Weniger, C., White, R., White, M., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zakaria, A. A., Zampieri, L., Zanin, R., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., ivec, M., ITA, USA, GBR, FRA, DEU, ESP, AUT, BEL, BRA, HRV, DNK, JPN, IRL, NLD, POL, SVN, CHE, High Energy Astrophys. & Astropart. Phys (API, FNWI), GRAPPA (ITFA, IoP, FNWI), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Iocco, Fabio, Anguner, E. O., Ascasibar, Y., Bernlohr, K., Colak, M., D'Ai, A., de Angelis, A., de Caprio, V., de Cassia dos Anjos, R., de Lotto, B., de Martino, D., de Ona Wilhelmi, E., de Palma, F., Dominguez, A., Elsasser, D., Gonzalez, M. M., Hernandez Cadena, S., Horandel, J., Hutten, M., Katarzynski, K., Knodlseder, J., Lopez, M., Lopez-Coto, R., Manico, G., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Nikolajuk, M., Pavletic, L., Perez-Romero, J., Puhlhofer, G., Raino, S., Ribo, M., Saether Hatlen, E., Sanchez-Conde, M., Slowikowska, A., Stanic, S., Striskovic, J., Swierk, P., Vazquez Acosta, M., Zivec, M., Consortium, The CTA, Acharyya A., Adam R., Adams C., Agudo I., Aguirre-Santaella A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amati L., Ambrosi G., Anguner E.O., Antonelli L.A., Aramo C., Araudo A., Armstrong T., Arqueros F., Asano K., Ascasibar Y., Ashley M., Balazs C., Ballester O., Baquero Larriva A., Barbosa Martins V., Barkov M., Barres de Almeida U., Barrio J.A., Bastieri D., Becerra J., Beck G., Becker Tjus J., Benbow W., Benito M., Berge D., Bernardini E., Bernlohr K., Berti A., Bertucci B., Beshley V., Biasuzzi B., Biland A., Bissaldi E., Biteau J., Blanch O., Blazek J., Bocchino F., Boisson C., Bonneau Arbeletche L., Bordas P., Bosnjak Z., Bottacini E., Bozhilov V., Bregeon J., Brill A., Bringmann T., Brown A.M., Brun P., Brun F., Bruno P., Bulgarelli A., Burton M., Burtovoi A., Buscemi M., Cameron R., Capasso M., Caproni A., Capuzzo-Dolcetta R., Caraveo P., Carosi R., Carosi A., Casanova S., Cascone E., Cassol F., Catalani F., Cauz D., Cerruti M., Chadwick P., Chaty S., Chen A., Chernyakova M., Chiaro G., Chiavassa A., Chikawa M., Chudoba J., Colak M., Conforti V., Coniglione R., Conte F., Contreras J.L., Coronado-Blazquez J., Costa A., Costantini H., Cotter G., Cristofari P., D'Ai A., D'Ammando F., Damone L.A., Daniel M.K., Dazzi F., de Angelis A., de Caprio V., de Cassia dos Anjos R., de Gouveia Dal Pino E.M., de Lotto B., de Martino D., de Ona Wilhelmi E., de Palma F., de Souza V., Delgado C., Delgado Giler A.G., della Volpe D., Depaoli D., Di Girolamo T., Di Pierro F., Di Venere L., Diebold S., Dmytriiev A., Dominguez A., Donini A., Doro M., Ebr J., Eckner C., Edwards T.D.P., Ekoume T.R.N., Elsasser D., Evoli C., Falceta-Goncalves D., Fedorova E., Fegan S., Feng Q., Ferrand G., Ferrara G., Fiandrini E., Fiasson A., Filipovic M., Fioretti V., Fiori M., Foffano L., Fontaine G., Fornieri O., Franco F.J., Fukami S., Fukui Y., Gaggero D., Galaz G., Gammaldi V., Garcia E., Garczarczyk M., Gascon D., Gent A., Ghalumyan A., Gianotti F., Giarrusso M., Giavitto G., Giglietto N., Giordano F., Giuliani A., Glicenstein J., Gnatyk R., Goldoni P., Gonzalez M.M., Gourgouliatos K., Granot J., Grasso D., Green J., Grillo A., Gueta O., Gunji S., Halim A., Hassan T., Heller M., Hernandez Cadena S., Hiroshima N., Hnatyk B., Hofmann W., Holder J., Horan D., Horandel J., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Hughes G., Humensky T.B., Hutten M., Iarlori M., Inada T., Inoue S., Iocco F., Iori M., Jamrozy M., Janecek P., Jin W., Jouvin L., Jurysek J., Karukes E., Katarzynski K., Kazanas D., Kerszberg D., Kherlakian M.C., Kissmann R., Knodlseder J., Kobayashi Y., Kohri K., Komin N., Kubo H., Kushida J., Lamanna G., Lapington J., Laporte P., Leigui de Oliveira M.A., Lenain J., Leone F., Leto G., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez A., Lopez M., Lopez-Coto R., Loporchio S., Luque-Escamilla P.L., Mach E., Maggio C., Maier G., Mallamaci M., Malta Nunes de Almeida R., Mandat D., Manganaro M., Mangano S., Manico G., Marculewicz M., Mariotti M., Markoff S., Marquez P., Marti J., Martinez O., Martinez M., Martinez G., Martinez-Huerta H., Maurin G., Mazin D., Mbarubucyeye J.D., Medina Miranda D., Meyer M., Miceli M., Miener T., Minev M., Miranda J.M., Mirzoyan R., Mizuno T., Mode B., Moderski R., Mohrmann L., Molina E., Montaruli T., Moralejo A., Morcuende-Parrilla D., Morselli A., Mukherjee R., Mundell C., Nagai A., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nikolajuk M., Ninci D., Noda K., Nosek D., Nozaki S., Ohira Y., Ohishi M., Ohtani Y., Oka T., Okumura A., Ong R.A., Orienti M., Orito R., Orlandini M., Orlando S., Orlando E., Ostrowski M., Oya I., Pagano I., Pagliaro A., Palatiello M., Pantaleo F.R., Paredes J.M., Pareschi G., Parmiggiani N., Patricelli B., Pavletic L., Pe'Er A., Pecimotika M., Perez-Romero J., Persic M., Petruk O., Pfrang K., Piano G., Piatteli P., Pietropaolo E., Pillera R., Pilszyk B., Pintore F., Pohl M., Poireau V., Prado R.R., Prandini E., Prast J., Principe G., Prokoph H., Prouza M., Przybilski H., Puhlhofer G., Pumo M.L., Queiroz F., Quirrenbach A., Raino S., Rando R., Razzaque S., Recchia S., Reimer O., Reisenegger A., Renier Y., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Rinchiuso L., Rizi V., Rodriguez J., Rodriguez Fernandez G., Rodriguez Ramirez J.C., Rojas G., Romano P., Romeo G., Rosado J., Rowell G., Rudak B., Russo F., Sadeh I., Saether Hatlen E., Safi-Harb S., Salesa Greus F., Salina G., Sanchez D., Sanchez-Conde M., Sangiorgi P., Sano H., Santander M., Santos E.M., Santos-Lima R., Sanuy A., Sarkar S., Saturni F.G., Sawangwit U., Schussler F., Schwanke U., Sciacca E., Scuderi S., Seglar-Arroyo M., Sergijenko O., Servillat M., Seweryn K., Shalchi A., Sharma P., Shellard R.C., Siejkowski H., Silk J., Siqueira C., Sliusar V., Slowikowska A., Sokolenko A., Sol H., Spencer S., Stamerra A., Stanic S., Starling R., Stolarczyk T., Straumann U., Striskovic J., Suda Y., Suomijarvi T., Swierk P., Tavecchio F., Taylor L., Tejedor L.A., Teshima M., Testa V., Tibaldo L., Todero Peixoto C.J., Tokanai F., Tonev D., Tosti G., Tosti L., Tothill N., Truzzi S., Travnicek P., Vagelli V., Vallage B., Vallania P., van Eldik C., Vandenbroucke J., Varner G.S., Vassiliev V., Vazquez Acosta M., Vecchi M., Ventura S., Vercellone S., Vergani S., Verna G., Viana A., Vigorito C.F., Vink J., Vitale V., Vorobiov S., Vovk I., Vuillaume T., Wagner S.J., Walter R., Watson J., Weniger C., White R., White M., Wiemann R., Wierzcholska A., Will M., Williams D.A., Wischnewski R., Yanagita S., Yang L., Yoshikoshi T., Zacharias M., Zaharijas G., Zakaria A.A., Zampieri L., Zanin R., Zaric D., Zavrtanik M., Zavrtanik D., Zdziarski A.A., Zech A., Zechlin H., Zhdanov V.I., and Zivec M.
- Subjects
Cherenkov Telescope Array ,MATÉRIA ESCURA ,scale: TeV ,Astronomy ,atmosphere [Cherenkov counter] ,dark matter experiment ,Dark matter theory ,energy resolution ,Gamma ray experiments ,Particle ,Astrophysics ,cosmic background radiation ,01 natural sciences ,7. Clean energy ,High Energy Physics - Phenomenology (hep-ph) ,benchmark ,WIMP ,HESS ,energy: flux ,TeV [scale] ,relativistic [charged particle] ,gamma ray experiment ,MAGIC (telescope) ,Monte Carlo ,Event reconstruction ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Contraction ,spatial distribution ,track data analysis ,density [dark matter] ,Clumpy ,Astrophysics::Instrumentation and Methods for Astrophysics ,imaging ,High Energy Physics - Phenomenology ,dark matter experiments ,dark matter theory ,gamma ray experiments ,galaxy morphology ,Dark matter experiments ,Física nuclear ,VERITAS ,Astrophysics - High Energy Astrophysical Phenomena ,Simulations ,noise ,Astrophysics::High Energy Astrophysical Phenomena ,Dark matter ,satellite ,Cosmic background radiation ,FOS: Physical sciences ,Annihilation ,dark matter: density ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cherenkov counter: atmosphere ,heavy [dark matter] ,annihilation [dark matter] ,GLAST ,Galaxy morphology ,cosmic radiation [p] ,0103 physical sciences ,Cherenkov [radiation] ,Candidates ,ddc:530 ,AGN ,Cherenkov radiation ,Radiative Processes ,thermal [cross section] ,010308 nuclear & particles physics ,Física ,dark matter: annihilation ,Gamma-Ray Signals ,dark matter ,Galactic Center ,TeV gamma-ray astronomy ,Astronomy and Astrophysics ,Mass ,radiation: Cherenkov ,sensitivity ,MAGIC ,Galaxy ,Astronomía ,dark matter: heavy ,gamma ray ,p: cosmic radiation ,[PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph] ,correlation ,charged particle: relativistic ,flux [energy] ,galaxy ,supersymmetry ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,cross section: thermal - Abstract
Full list of authors: Acharyya, A.; Adam, R.; Adams, C.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, R.; Alfaro, J.; Alispach, C.; Aloisio, R.; Alves Batista, R.; Amati, L.; Ambrosi, G.; Angüner, E. O.; Antonelli, L. A.; Aramo, C.; Araudo, A.; Armstrong, T.; Arqueros, F.; Asano, K.; Ascasíbar, Y. Ashley, M.; Balazs, C.; Ballester, O.; Baquero Larriva, A.; Barbosa Martins, V.; Barkov, M.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Becerra, J.; Beck, G.; Becker Tjus, J.; Benbow, W.; Benito, M.; Berge, D.; Bernardini, E.; Bernlöhr, K.; Berti, A.; Bertucci, B.; Beshley, V.; Biasuzzi, B.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Bocchino, F.; Boisson, C.; Bonneau Arbeletche, L.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Bozhilov, V.; Bregeon, J.; Brill, A.; Bringmann, T.; Brown, A. M.; Brun, P.; Brun, F.; Bruno, P.; Bulgarelli, A.; Burton, M.; Burtovoi, A.; Buscemi, M.; Cameron, R.; Capasso, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Carosi, R.; Carosi, A.; Casanova, S.; Cascone, E.; Cassol, F.; Catalani, F.; Cauz, D.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A.; Chernyakova, M.; Chiaro, G.; Chiavassa, A.; Chikawa, M.; Chudoba, J.; Çolak, M.; Conforti, V.; Coniglione, R.; Conte, F.; Contreras, J. L.; Coronado-Blazquez, J.; Costa, A.; Costantini, H.; Cotter, G.; Cristofari, P.; D'Aimath, A.; D'Ammando, F.; Damone, L. A.; Daniel, M. K.; Dazzi, F.; De Angelis, A.; De Caprio, V.; de Cássia dos Anjos, R.; de Gouveia Dal Pino, E. M.; De Lotto, B.; De Martino, D.; de Oña Wilhelmi, E.; De Palma, F.; de Souza, V.; Delgado, C.; Delgado Giler, A. G.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Pierro, F.; Di Venere, L.; Diebold, S.; Dmytriiev, A.; Domínguez, A.; Donini, A.; Doro, M.; Ebr, J.; Eckner, C.; Edwards, T. D. P.; Ekoume, T. R. N.; Elsässer, D.; Evoli, C.; Falceta-Goncalves, D.; Fedorova, E.; Fegan, S.; Feng, Q.; Ferrand, G.; Ferrara, G.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Fiori, M.; Foffano, L.; Fontaine, G.; Fornieri, O.; Franco, F. J.; Fukami, S.; Fukui, Y.; Gaggero, D.; Galaz, G.; Gammaldi, V.; Garcia, E.; Garczarczyk, M.; Gascon, D.; Gent, A.; Ghalumyan, A.; Gianotti, F.; Giarrusso, M.; Giavitto, G.; Giglietto, N.; Giordano, F.; Giuliani, A.; Glicenstein, J.; Gnatyk, R.; Goldoni, P.; González, M. M.; Gourgouliatos, K.; Granot, J.; Grasso, D.; Green, J.; Grillo, A.; Gueta, O.; Gunji, S.; Halim, A.; Hassan, T.; Heller, M.; Hernández Cadena, S.; Hiroshima, N.; Hnatyk, B.; Hofmann, W.; Holder, J.; Horan, D.; Hörandel, J.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Hughes, G.; Humensky, T. B.; Hütten, M.; Iarlori, M.; Inada, T.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jin, W.; Jouvin, L.; Jurysek, J.; Karukes, E.; Katarzyński, K.; Kazanas, D.; Kerszberg, D.; Kherlakian, M. C.; Kissmann, R.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kubo, H.; Kushida, J.; Lamanna, G.; Lapington, J.; Laporte, P.; Leigui de Oliveira, M. A.; Lenain, J.; Leone, F.; Leto, G.; Lindfors, E.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez, A.; López, M.; López-Coto, R.; Loporchio, S.; Luque-Escamilla, P. L.; Mach, E.; Maggio, C.; Maier, G.; Mallamaci, M.; Malta Nunes de Almeida, R.; Mandat, D.; Manganaro, M.; Mangano, S.; Manicò, G.; Marculewicz, M.; Mariotti, M.; Markoff, S.; Marquez, P.; Martí, J.; Martinez, O.; Martínez, M.; Martínez, G.; Martínez-Huerta, H.; Maurin, G.; Mazin, D.; Mbarubucyeye, J. D.; Medina Miranda, D.; Meyer, M.; Miceli, M.; Miener, T.; Minev, M.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Mode, B.; Moderski, R.; Mohrmann, L.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende-Parrilla, D.; Morselli, A.; Mukherjee, R.; Mundell, C.; Nagai, A.; Nakamori, T.; Nemmen, R.; Niemiec, J.; Nieto, D.; Nikołajuk, M.; Ninci, D.; Noda, K.; Nosek, D.; Nozaki, S.; Ohira, Y.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, S.; Orlando, E.; Ostrowski, M.; Oya, I.; Pagano, I.; Pagliaro, A.; Palatiello, M.; Pantaleo, F. R.; Paredes, J. M.; Pareschi, G.; Parmiggiani, N.; Patricelli, B.; Pavletić, L.; Pe'er, A.; Pecimotika, M.; Pérez-Romero, J.; Persic, M.; Petruk, O.; Pfrang, K.; Piano, G.; Piatteli, P.; Pietropaolo, E.; Pillera, R.; Pilszyk, B.; Pintore, F.; Pohl, M.; Poireau, V.; Prado, R. R.; Prandini, E.; Prast, J.; Principe, G.; Prokoph, H.; Prouza, M.; Przybilski, H.; Pühlhofer, G.; Pumo, M. L.; Queiroz, F.; Quirrenbach, A.; Rainò, S.; Rando, R.; Razzaque, S.; Recchia, S.; Reimer, O.; Reisenegger, A.; Renier, Y.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Rinchiuso, L.; Rizi, V.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodriguez Ramirez, J. C.; Rojas, G.; Romano, P.; Romeo, G.; Rosado, J.; Rowell, G.; Rudak, B.; Russo, F.; Sadeh, I.; Sæther Hatlen, E.; Safi-Harb, S.; Salesa Greus, F.; Salina, G.; Sanchez, D.; Sánchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santos, E. M.; Santos-Lima, R.; Sanuy, A.; Sarkar, S.; Saturni, F. G.; Sawangwit, U.; Schussler, F.; Schwanke, U.; Sciacca, E.; Scuderi, S.; Seglar-Arroyo, M.; Sergijenko, O.; Servillat, M.; Seweryn, K.; Shalchi, A.; Sharma, P.; Shellard, R. C.; Siejkowski, H.; Silk, J.; Siqueira, C.; Sliusar, V.; Słowikowska, A.; Sokolenko, A.; Sol, H.; Spencer, S.; Stamerra, A.; Stanič, S.; Starling, R.; Stolarczyk, T.; Straumann, U.; Strišković, J.; Suda, Y.; Suomijarvi, T.; Świerk, P.; Tavecchio, F.; Taylor, L.; Tejedor, L. A.; Teshima, M.; Testa, V.; Tibaldo, L.; Todero Peixoto, C. J.; Tokanai, F.; Tonev, D.; Tosti, G.; Tosti, L.; Tothill, N.; Truzzi, S.; Travnicek, P.; Vagelli, V.; Vallage, B.; Vallania, P.; van Eldik, C.; Vandenbroucke, J.; Varner, G. S.; Vassiliev, V.; Vázquez Acosta, M.; Vecchi, M.; Ventura, S.; Vercellone, S.; Vergani, S.; Verna, G.; Viana, A.; Vigorito, C. F.; Vink, J.; Vitale, V.; Vorobiov, S.; Vovk, I.; Vuillaume, T.; Wagner, S. J.; Walter, R.; Watson, J.; Weniger, C.; White, R.; White, M.; Wiemann, R.; Wierzcholska, A.; Will, M.; Williams, D. A.; Wischnewski, R.; Yanagita, S.; Yang, L.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zakaria, A. A.; Zampieri, L.; Zanin, R.; Zaric, D.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V. I.; Živec, M.-- This is an open access article published by IOP Publishing Ltd on behalf of Sissa Medialab. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI., We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models given a standard cuspy profile of the dark matter density distribution. Importantly, even for a cored profile, the projected sensitivity of CTA will be sufficient to probe various well-motivated models of thermally produced dark matter at the TeV scale. This is due to CTA's unprecedented sensitivity, angular and energy resolutions, and the planned observational strategy. The survey of the inner Galaxy will cover a much larger region than corresponding previous observational campaigns with imaging atmospheric Cherenkov telescopes. CTA will map with unprecedented precision the large-scale diffuse emission in high-energy gamma rays, constituting a background for dark matter searches for which we adopt state-of-the-art models based on current data. Throughout our analysis, we use up-to-date event reconstruction Monte Carlo tools developed by the CTA consortium, and pay special attention to quantifying the level of instrumental systematic uncertainties, as well as background template systematic errors, required to probe thermally produced dark matter at these energies. © 2021 The Author(s)., We gratefully acknowledge financial support from the following agencies and organisations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Education, Science and Research, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Fundacao de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), and Instituto Serrapilheira, Brasil; Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants CATA AFB 170002, ANID PIA/APOYO AFB 180002, ACT 1406, FONDECYT-Chile grants, 1161463, 1170171, 1190886, 1171421, 1170345, 1201582, Gemini-ANID 32180007, Chile; Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croatia; Ministry of Education, Youth and Sports, MEYS LM2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Academy of Finland (grant nr.317636, 320045, 317383 and 320085), Finland; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile de France, Labex ENIGMASS, OSUG2020, P2IO and OCEVU, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, J1-9146, J1-1700, N1-0111, and the Young Researcher program, Slovenia; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; The Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through grants AYA2016-79724-C4-1-P, AYA2016-80889-P, AYA2016-76012-C3-1-P, BES-2016-076342, ESP2017-87055-C2-1-P, FPA2017-82729-C6-1-R, FPA2017-82729-C6-2-R, FPA2017-82729-C6-3-R, FPA2017-82729-C6-4-R, FPA2017-82729-C6-5-R, FPA2017-82729-C6-6-R, PGC2018-095161-B-I00, PGC2018-095512-B-I00; the \Centro de Excelencia Severo Ochoa"program through grants no. SEV-2015-0548, SEV-2016-0597, SEV-2016-0588, SEV-2017-0709; the "Unidad de Excelencia Maria de Maeztu" program through grant no. MDM-2015-0509; the "Ramon y Cajal" programme through grants RYC-2013-14511, RyC-2013-14660, RYC-2017-22665; and the MultiDark Consolider Network FPA2017-90566-REDC. Atraccion de Talento contract no. 2016-T1/TIC-1542 granted by the Comunidad de Madrid; the "Postdoctoral Junior Leader Fellowship" programme from La Caixa Banking Foundation, grants no. LCF/BQ/LI18/11630014 and LCF/BQ/PI18/11630012; the "Programa Operativo" FEDER2014-2020, Consejeria de Economia y Conocimiento de la Junta de Andalucia (ref. 1257737), PAIDI 2020 (ref. P18-FR-1580), and Universidad de Jaen; the Spanish AEI EQC2018-005094-P FEDER 2014-2020; the European Union's "Horizon 2020" research and innovation programme under Marie Sklodowska-Curie grant agreement no. 665919; and the ESCAPE project with grant no. GA:824064, Spain; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; State Secretariat for Education, Research and Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Society, Science and Technology Facilities Council, U.K.; U.S. National Science Foundation, U.S. Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, U.S.A. The research leading to these results has received funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and No 317446. This project is receiving funding from the European Union's Horizon 2020 research and innovation programs under agreement No 676134.
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153. Direct observation of an extended X-ray jet at z = 6.1
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Ighina, L., primary, Moretti, A., additional, Tavecchio, F., additional, Caccianiga, A., additional, Belladitta, S., additional, Dallacasa, D., additional, Della Ceca, R., additional, Sbarrato, T., additional, and Spingola, C., additional
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154. The evolution of the heaviest supermassive black holes in jetted AGNs
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Diana, A, primary, Caccianiga, A, additional, Ighina, L, additional, Belladitta, S, additional, Moretti, A, additional, and Della Ceca, R, additional
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155. Dramatic Changes in the Observed Velocity of the Accretion Disk Wind in MCG-03-58-007 Are Revealed by XMM-Newton and NuSTAR
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Braito, V., primary, Reeves, J. N., additional, Matzeu, G., additional, Severgnini, P., additional, Ballo, L., additional, Cicone, C., additional, Ceca, R. Della, additional, Giustini, M., additional, and Sirressi, M., additional
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156. Testing the blast-wave AGN feedback scenario in MCG-03-58-007
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Sirressi, M, Cicone, C, Severgnini, P, Braito, V, Dotti, M, Della Ceca, R, Reeves, J, Matzeu, G, Vignali, C, Ballo, L, Sirressi M., Cicone C., Severgnini P., Braito V., Dotti M., Della Ceca R., Reeves J. N., Matzeu G. A., Vignali C., Ballo L., Sirressi, M, Cicone, C, Severgnini, P, Braito, V, Dotti, M, Della Ceca, R, Reeves, J, Matzeu, G, Vignali, C, Ballo, L, Sirressi M., Cicone C., Severgnini P., Braito V., Dotti M., Della Ceca R., Reeves J. N., Matzeu G. A., Vignali C., and Ballo L.
- Abstract
We report the first Atacama large millimeter/submillimeter array observations of MCG-03- 58-007, a local (z = 0.03236 ± 0.00002, this work) AGN (LAGN ∼ 1045 erg s-1), hosting a powerful X-ray ultrafast (v = 0.1c) outflow (UFO). The CO(1-0) line emission is observed across∼18 kpc scales with a resolution of∼ 1 kpc. About 78 per cent of theCO(1-0) luminosity traces a galaxy-size rotating disc. However, after subtracting the emission due to such rotating disc, we detect with a S/N = 20 a residual emission in the central ∼4 kpc. Such residuals may trace a low velocity (vLOS = 170 km s-1) outflow. We compare the momentum rate (P ) and kinetic power (E) of such putative molecular outflow with that of the X-ray UFO and find P mol/P UFO ∼ 0.4 and Emol/ EUFO ∼ 4 × 10-3. This result is at odds with the energyconserving scenario suggested by the large momentum boosts measured in some other molecular outflows. An alternative interpretation of the residual CO emission would be a compact rotating structure, distinct from the main disc, which would be a factor of ∼10- 100 more extended and massive than typical circumnuclear discs revealed in Seyferts. In conclusion, in both scenarios, our results rule out the hypothesis of a momentum-boosted molecular outflow in this AGN, despite the presence of a powerful X-ray UFO.
- Published
- 2019
157. X-ray obscuration from a variable ionized absorber in PG 1114+445
- Author
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Serafinelli, R., primary, Braito, V., additional, Severgnini, P., additional, Tombesi, F., additional, Giani, G., additional, Piconcelli, E., additional, Della Ceca, R., additional, Vagnetti, F., additional, Gaspari, M., additional, Saturni, F. G., additional, Middei, R., additional, and Tortosa, A., additional
- Published
- 2021
- Full Text
- View/download PDF
158. The stratified disc wind of MCG-03-58-007
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Braito, V., Reeves, J. N., Severgnini, P., Della Ceca, R., Ballo, L., Cicone, C., Matzeu, G. A., Serafinelli, R., Sirressi, Mattia, Braito, V., Reeves, J. N., Severgnini, P., Della Ceca, R., Ballo, L., Cicone, C., Matzeu, G. A., Serafinelli, R., and Sirressi, Mattia
- Abstract
Past Suzaku, XMM-Newton, and NuSTAR observations of the nearby (z = 0.03233) bright Seyfert 2 galaxy MCG-03-58-007 revealed the presence of two deep and blue-shifted iron K-shell absorption line profiles. These could be explained with the presence of two phases of a highly ionized, high column density accretion disc wind outflowing with v(out1) similar to-0.1c and v(out2) similar to -0.2c. Here we present two new observations of MCG-03-58-007: one was carried out in 2016 with Chandra and one in 2018 with Swift. Both caught MCG-03-58-007 in a brighter state (F2-10 (keV) similar to 4 x 10(-12) erg cm(-2) s(-1)) confirming the presence of the fast disc wind. The multi-epoch observations of MCG-03-58-007 covering the period from 2010 to 2018 were then analysed. These data show that the lower velocity component outflowing with v(out1) similar to -0.072 +/- 0.002c is persistent and detected in all the observations, although it is variable in column density in the range N-H similar to 3-8 x 102(3) cm(-2). In the 2016 Swift observation we detected again the second faster component outflowing with v(out2) similar to-0.2c, with a column density (N-H = 7.0(-4.1)(+5.6) x 10(23) cm(-2)), similar to that seen during the Suzaku observation. However during the Chandra observation 2 yr earlier, this zone was not present (N-H < 1.5 x 10(23) cm(-2)), suggesting that this faster zone is intermittent. Overall the multi-epochs observations show that the disc wind in MCG-03-58-007 is not only powerful, but also extremely variable, hence placing MCG-03-58-007 among unique disc winds such as the one seen in the famous QSO PDS456. One of the main results of this investigation is the consideration that these winds could be extremely variable, sometime appearing and sometime disappearing; thus to reach solid and firm conclusions about their energetics multiple observations are mandatory.
- Published
- 2021
- Full Text
- View/download PDF
159. Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation
- Author
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Abdalla, H., Abe, H., Acero, F., Acharyya, A., Adam, R., Agudo, I, Aguirre-Santaella, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Batista, R. Alves, Amati, L., Amato, E., Ambrosi, G., Anguner, E. O., Araudo, A., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ascasibar, Y., Ashley, M., Backes, M., Balazs, C., Balbo, M., Balmaverde, B., Baquero Larriva, A., Martins, V. Barbosa, Barkov, M., Baroncelli, L., de Almeida, U. Barres, Barrio, J. A., Batista, P-, I, Becerra Gonzalez, J., Becherini, Yvonne, Beck, G., Tjus, J. Becker, Belmont, R., Benbow, W., Bernardini, E., Berti, A., Berton, M., Bertucci, B., Beshley, V, Bi, B., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Bocchino, F., Boisson, C., Bolmont, J., Bonanno, G., Arbeletche, L. Bonneau, Bonnoli, G., Bordas, P., Bottacini, E., Bottcher, M., Bozhilov, V, Bregeon, J., Brill, A., Brown, A. M., Bruno, P., Bruno, A., Bulgarelli, A., Burton, M., Buscemi, M., Caccianiga, A., Cameron, R., Capasso, M., Caprai, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Carosi, R., Carosi, A., Casanova, S., Cascone, E., Cauz, D., Cerny, K., Cerruti, M., Chadwick, P., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Chiavassa, A., Chytka, L., Conforti, V, Conte, F., Contreras, J. L., Coronado-Blazquez, J., Cortina, J., Costa, A., Costantini, H., Covino, S., Cristofari, P., Cuevas, O., D'Ammando, F., Daniel, M. K., Davies, J., Dazzi, F., De Angelis, A., de Lavergne, M. de Bony, De Caprio, V, dos Anjos, R. de Cassia, Dal Pino, E. M. de Gouveia, De Lotto, B., De Martino, D., de Naurois, M., Wilhelmi, E. de Ona, De Palma, F., de Souza, V, Delgado, C., Della Ceca, R., della Volpe, D., Depaoli, D., Di Girolamo, T., Di Pierro, F., Diaz, C., Diaz-Bahamondes, C., Diebold, S., Djannati-Atai, A., Dmytriiev, A., Dominguez, A., Donini, A., Dorner, D., Doro, M., Dournaux, J., Dwarkadas, V. V., Ebr, J., Eckner, C., Einecke, S., Ekoume, T. R. N., Elsaesser, D., Emery, G., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Fioretti, V, Foffano, L., Fonseca, M. , V, Font, L., Fontaine, G., Franco, F. J., Freixas Coromina, L., Fukami, S., Fukazawa, Y., Fukui, Y., Gaggero, D., Galanti, G., Gammaldi, V, Garcia, E., Garczarczyk, M., Gascon, D., Gaug, M., Gent, A., Ghalumyan, A., Ghirlanda, G., Gianotti, F., Giarrusso, M., Giavitto, G., Giglietto, N., Giordano, F., Glicenstein, J., Goldoni, P., Gonzalez, J. M., Gourgouliatos, K., Grabarczyk, T., Grandi, P., Granot, J., Grasso, D., Green, J., Grube, J., Gueta, O., Gunji, S., Halim, A., Harvey, M., Collado, T. Hassan, Hayashi, K., Heller, M., Cadena, S. Hernandez, Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hnatyk, R., Hoffmann, D., Hofmann, W., Holder, J., Horan, D., Horandel, J., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Hughes, G., Hutten, M., Iarlori, M., Inada, T., Inoue, S., Insolia, A., Ionica, M., Iori, M., Jacquemont, M., Jamrozy, M., Janecek, P., Jimenez Martinez, I, Jin, W., Jung-Richardt, I, Jurysek, J., Kaaret, P., Karas, V, Karkar, S., Kawanaka, N., Kerszberg, D., Khelifi, B., Kissmann, R., Knodlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kong, A., Kosack, K., Kubo, H., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Laporte, P., Lefaucheur, J., Lemoine-Goumard, M., Lenain, J., Leone, F., Leto, G., Leuschner, F., Lindfors, E., Lloyd, S., Lohse, T., Lombardi, S., Longo, F., Lopez, A., Lopez, M., Lopez-Coto, R., Loporchio, S., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maggio, C., Majczyna, A., Makariev, M., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Manico, G., Marcowith, A., Marculewicz, M., Markoff, S., Marquez, P., Marti, J., Martinez, O., Martinez, M., Martinez, G., Martinez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Miranda, D. Medina, Meyer, M., Micanovic, S., Miener, T., Minev, M., Miranda, J. M., Mitchell, A., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Montaruli, T., Moralejo, A., Morales Merino, J., Morcuende-Parrilla, D., Morselli, A., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Nagai, A., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas, M., Nikolajuk, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., Ohira, Y., Ohishi, M., Oka, T., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, E., Osborne, J. P., Ostrowski, M., Oya, I, Pagliaro, A., Palatka, M., Paneque, D., Pantaleo, F. R., Paredes, J. M., Parmiggiani, N., Patricelli, B., Pavletic, L., Pe'er, A., Pech, M., Pecimotika, M., Peresano, M., Persic, M., Petruk, O., Pfrang, K., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pimentel, D., Pintore, F., Pita, S., Pohl, M., Poireau, V, Polo, M., Prado, R. R., Prast, J., Principe, G., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Pueschel, E., Puehlhofer, G., Pumo, M. L., Punch, Michael, Queiroz, F., Quirrenbach, A., Rando, R., Razzaque, S., Rebert, E., Recchia, S., Reichherzer, P., Reimer, O., Reimer, A., Renier, Y., Reposeur, T., Rhode, W., Ribeiro, D., Ribo, M., Richtler, T., Rico, J., Rieger, F., Rizi, V, Rodriguez, J., Fernandez, G. Rodriguez, Ramirez, J. C. Rodriguez, Rodriguez Vazquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., de Leon, A. Rosales, Rowell, G., Rudak, B., Rujopakarn, W., Russo, F., Sadeh, I, Saha, L., Saito, T., Greus, F. Salesa, Sanchez, D., Sanchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Scherer, A., Schleicher, B., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Arroyo, M. Seglar, Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Sinha, A., Sliusar, V, Slowikowska, A., Sokolenko, A., Sol, H., Specovius, A., Spencer, S., Spiga, D., Stamerra, A., Starling, R., Stolarczyk, T., Straumann, U., Striskovic, J., Suda, Y., Tagliaferri, G., Takahashi, H., Takahashi, M., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terrier, R., Terzic, T., Testa, V, Tian, W., Tibaldo, L., Tonev, D., Torres, D. F., Torresi, E., Tosti, L., Tothill, N., Tovmassian, G., Travnicek, P., Truzzi, S., Tuossenel, F., Umana, G., Vacula, M., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., van Eldik, C., Varner, G. S., Vassiliev, V., Vazquez Acosta, M., Vecchi, M., Veh, J., Vercellone, S., Vergani, S., Verguilov, V., Vettolani, G. P., Viana, A., Vigorito, C. F., Vitale, V., Vorobiov, S., Vovk, I, Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., White, M., White, R., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Wolter, A., Yamazaki, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. , I, Zivec, M., Abdalla, H., Abe, H., Acero, F., Acharyya, A., Adam, R., Agudo, I, Aguirre-Santaella, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Batista, R. Alves, Amati, L., Amato, E., Ambrosi, G., Anguner, E. O., Araudo, A., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ascasibar, Y., Ashley, M., Backes, M., Balazs, C., Balbo, M., Balmaverde, B., Baquero Larriva, A., Martins, V. Barbosa, Barkov, M., Baroncelli, L., de Almeida, U. Barres, Barrio, J. A., Batista, P-, I, Becerra Gonzalez, J., Becherini, Yvonne, Beck, G., Tjus, J. Becker, Belmont, R., Benbow, W., Bernardini, E., Berti, A., Berton, M., Bertucci, B., Beshley, V, Bi, B., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Bocchino, F., Boisson, C., Bolmont, J., Bonanno, G., Arbeletche, L. Bonneau, Bonnoli, G., Bordas, P., Bottacini, E., Bottcher, M., Bozhilov, V, Bregeon, J., Brill, A., Brown, A. M., Bruno, P., Bruno, A., Bulgarelli, A., Burton, M., Buscemi, M., Caccianiga, A., Cameron, R., Capasso, M., Caprai, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Carosi, R., Carosi, A., Casanova, S., Cascone, E., Cauz, D., Cerny, K., Cerruti, M., Chadwick, P., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Chiavassa, A., Chytka, L., Conforti, V, Conte, F., Contreras, J. L., Coronado-Blazquez, J., Cortina, J., Costa, A., Costantini, H., Covino, S., Cristofari, P., Cuevas, O., D'Ammando, F., Daniel, M. K., Davies, J., Dazzi, F., De Angelis, A., de Lavergne, M. de Bony, De Caprio, V, dos Anjos, R. de Cassia, Dal Pino, E. M. de Gouveia, De Lotto, B., De Martino, D., de Naurois, M., Wilhelmi, E. de Ona, De Palma, F., de Souza, V, Delgado, C., Della Ceca, R., della Volpe, D., Depaoli, D., Di Girolamo, T., Di Pierro, F., Diaz, C., Diaz-Bahamondes, C., Diebold, S., Djannati-Atai, A., Dmytriiev, A., Dominguez, A., Donini, A., Dorner, D., Doro, M., Dournaux, J., Dwarkadas, V. V., Ebr, J., Eckner, C., Einecke, S., Ekoume, T. R. N., Elsaesser, D., Emery, G., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Fioretti, V, Foffano, L., Fonseca, M. , V, Font, L., Fontaine, G., Franco, F. J., Freixas Coromina, L., Fukami, S., Fukazawa, Y., Fukui, Y., Gaggero, D., Galanti, G., Gammaldi, V, Garcia, E., Garczarczyk, M., Gascon, D., Gaug, M., Gent, A., Ghalumyan, A., Ghirlanda, G., Gianotti, F., Giarrusso, M., Giavitto, G., Giglietto, N., Giordano, F., Glicenstein, J., Goldoni, P., Gonzalez, J. M., Gourgouliatos, K., Grabarczyk, T., Grandi, P., Granot, J., Grasso, D., Green, J., Grube, J., Gueta, O., Gunji, S., Halim, A., Harvey, M., Collado, T. Hassan, Hayashi, K., Heller, M., Cadena, S. Hernandez, Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hnatyk, R., Hoffmann, D., Hofmann, W., Holder, J., Horan, D., Horandel, J., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Hughes, G., Hutten, M., Iarlori, M., Inada, T., Inoue, S., Insolia, A., Ionica, M., Iori, M., Jacquemont, M., Jamrozy, M., Janecek, P., Jimenez Martinez, I, Jin, W., Jung-Richardt, I, Jurysek, J., Kaaret, P., Karas, V, Karkar, S., Kawanaka, N., Kerszberg, D., Khelifi, B., Kissmann, R., Knodlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kong, A., Kosack, K., Kubo, H., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Laporte, P., Lefaucheur, J., Lemoine-Goumard, M., Lenain, J., Leone, F., Leto, G., Leuschner, F., Lindfors, E., Lloyd, S., Lohse, T., Lombardi, S., Longo, F., Lopez, A., Lopez, M., Lopez-Coto, R., Loporchio, S., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maggio, C., Majczyna, A., Makariev, M., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Manico, G., Marcowith, A., Marculewicz, M., Markoff, S., Marquez, P., Marti, J., Martinez, O., Martinez, M., Martinez, G., Martinez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Miranda, D. Medina, Meyer, M., Micanovic, S., Miener, T., Minev, M., Miranda, J. M., Mitchell, A., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Montaruli, T., Moralejo, A., Morales Merino, J., Morcuende-Parrilla, D., Morselli, A., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Nagai, A., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas, M., Nikolajuk, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., Ohira, Y., Ohishi, M., Oka, T., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, E., Osborne, J. P., Ostrowski, M., Oya, I, Pagliaro, A., Palatka, M., Paneque, D., Pantaleo, F. R., Paredes, J. M., Parmiggiani, N., Patricelli, B., Pavletic, L., Pe'er, A., Pech, M., Pecimotika, M., Peresano, M., Persic, M., Petruk, O., Pfrang, K., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pimentel, D., Pintore, F., Pita, S., Pohl, M., Poireau, V, Polo, M., Prado, R. R., Prast, J., Principe, G., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Pueschel, E., Puehlhofer, G., Pumo, M. L., Punch, Michael, Queiroz, F., Quirrenbach, A., Rando, R., Razzaque, S., Rebert, E., Recchia, S., Reichherzer, P., Reimer, O., Reimer, A., Renier, Y., Reposeur, T., Rhode, W., Ribeiro, D., Ribo, M., Richtler, T., Rico, J., Rieger, F., Rizi, V, Rodriguez, J., Fernandez, G. Rodriguez, Ramirez, J. C. Rodriguez, Rodriguez Vazquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., de Leon, A. Rosales, Rowell, G., Rudak, B., Rujopakarn, W., Russo, F., Sadeh, I, Saha, L., Saito, T., Greus, F. Salesa, Sanchez, D., Sanchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Scherer, A., Schleicher, B., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Arroyo, M. Seglar, Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Sinha, A., Sliusar, V, Slowikowska, A., Sokolenko, A., Sol, H., Specovius, A., Spencer, S., Spiga, D., Stamerra, A., Starling, R., Stolarczyk, T., Straumann, U., Striskovic, J., Suda, Y., Tagliaferri, G., Takahashi, H., Takahashi, M., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terrier, R., Terzic, T., Testa, V, Tian, W., Tibaldo, L., Tonev, D., Torres, D. F., Torresi, E., Tosti, L., Tothill, N., Tovmassian, G., Travnicek, P., Truzzi, S., Tuossenel, F., Umana, G., Vacula, M., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., van Eldik, C., Varner, G. S., Vassiliev, V., Vazquez Acosta, M., Vecchi, M., Veh, J., Vercellone, S., Vergani, S., Verguilov, V., Vettolani, G. P., Viana, A., Vigorito, C. F., Vitale, V., Vorobiov, S., Vovk, I, Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., White, M., White, R., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Wolter, A., Yamazaki, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. , I, and Zivec, M.
- Abstract
The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for gamma-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of gamma-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of gamma-ray absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift z = 2 and to constrain or detect gamma-ray halos up to intergalactic-magnetic-field strengths of at least 0.3 pG. Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from gamma-ray astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of gamma-ray cosmology.
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- 2021
- Full Text
- View/download PDF
160. The impact of the CMB on the evolution of high-z blazars
- Author
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Ighina, L, primary, Caccianiga, A, additional, Moretti, A, additional, Belladitta, S, additional, Della Ceca, R, additional, and Diana, A, additional
- Published
- 2021
- Full Text
- View/download PDF
161. The TESIS Project: Revealing Massive Early-Type Galaxies at z > 1
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Saracco, P., Longhetti, M., Severgnini, P., Della Ceca, R., Braito, V., Bender, R., Drory, N., Feulner, G., Hopp, U., Mannucci, F., Maraston, C., Renzini, Alvio, editor, and Bender, Ralf, editor
- Published
- 2005
- Full Text
- View/download PDF
162. The TESIS Project: Are Type 2 QSO Hidden in X-Ray Emitting EROs?
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Severgnini, P., Della Ceca, R., Braito, V., Saracco, P., Longhetti, M., Bender, R., Drory, N., Feulner, G., Hopp, U., Mannucci, F., Maraston, C., Renzini, Alvio, editor, and Bender, Ralf, editor
- Published
- 2005
- Full Text
- View/download PDF
163. Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation
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Abdalla, H., primary, Abe, H., additional, Acero, F., additional, Acharyya, A., additional, Adam, R., additional, Agudo, I., additional, Aguirre-Santaella, A., additional, Alfaro, R., additional, Alfaro, J., additional, Alispach, C., additional, Aloisio, R., additional, Batista, R. Alves, additional, Amati, L., additional, Amato, E., additional, Ambrosi, G., additional, Angüner, E.O., additional, Araudo, A., additional, Armstrong, T., additional, Arqueros, F., additional, Arrabito, L., additional, Asano, K., additional, Ascasíbar, Y., additional, Ashley, M., additional, Backes, M., additional, Balazs, C., additional, Balbo, M., additional, Balmaverde, B., additional, Larriva, A. Baquero, additional, Martins, V. Barbosa, additional, Barkov, M., additional, Baroncelli, L., additional, de Almeida, U. Barres, additional, Barrio, J.A., additional, Batista, P.-I., additional, González, J. Becerra, additional, Becherini, Y., additional, Beck, G., additional, Tjus, J. Becker, additional, Belmont, R., additional, Benbow, W., additional, Bernardini, E., additional, Berti, A., additional, Berton, M., additional, Bertucci, B., additional, Beshley, V., additional, Bi, B., additional, Biasuzzi, B., additional, Biland, A., additional, Bissaldi, E., additional, Biteau, J., additional, Blanch, O., additional, Bocchino, F., additional, Boisson, C., additional, Bolmont, J., additional, Bonanno, G., additional, Arbeletche, L. Bonneau, additional, Bonnoli, G., additional, Bordas, P., additional, Bottacini, E., additional, Böttcher, M., additional, Bozhilov, V., additional, Bregeon, J., additional, Brill, A., additional, Brown, A.M., additional, Bruno, P., additional, Bruno, A., additional, Bulgarelli, A., additional, Burton, M., additional, Buscemi, M., additional, Caccianiga, A., additional, Cameron, R., additional, Capasso, M., additional, Caprai, M., additional, Caproni, A., additional, Capuzzo-Dolcetta, R., additional, Caraveo, P., additional, Carosi, R., additional, Carosi, A., additional, Casanova, S., additional, Cascone, E., additional, Cauz, D., additional, Cerny, K., additional, Cerruti, M., additional, Chadwick, P., additional, Chaty, S., additional, Chen, A., additional, Chernyakova, M., additional, Chiaro, G., additional, Chiavassa, A., additional, Chytka, L., additional, Conforti, V., additional, Conte, F., additional, Contreras, J.L., additional, Coronado-Blazquez, J., additional, Cortina, J., additional, Costa, A., additional, Costantini, H., additional, Covino, S., additional, Cristofari, P., additional, Cuevas, O., additional, D'Ammando, F., additional, Daniel, M.K., additional, Davies, J., additional, Dazzi, F., additional, Angelis, A. De, additional, de Lavergne, M. de Bony, additional, Caprio, V. De, additional, Anjos, R. de Cássia dos, additional, Pino, E.M. de Gouveia Dal, additional, Lotto, B. De, additional, Martino, D. De, additional, de Naurois, M., additional, Wilhelmi, E. de Oña, additional, Palma, F. De, additional, de Souza, V., additional, Delgado, C., additional, Ceca, R. Della, additional, Volpe, D. della, additional, Depaoli, D., additional, Girolamo, T. Di, additional, Pierro, F. Di, additional, Díaz, C., additional, Díaz-Bahamondes, C., additional, Diebold, S., additional, Djannati-Ataï, A., additional, Dmytriiev, A., additional, Domínguez, A., additional, Donini, A., additional, Dorner, D., additional, Doro, M., additional, Dournaux, J., additional, Dwarkadas, V.V., additional, Ebr, J., additional, Eckner, C., additional, Einecke, S., additional, Ekoume, T.R.N., additional, Elsässer, D., additional, Emery, G., additional, Evoli, C., additional, Fairbairn, M., additional, Falceta-Goncalves, D., additional, Fegan, S., additional, Feng, Q., additional, Ferrand, G., additional, Fiandrini, E., additional, Fiasson, A., additional, Fioretti, V., additional, Foffano, L., additional, Fonseca, M.V., additional, Font, L., additional, Fontaine, G., additional, Franco, F.J., additional, Coromina, L. Freixas, additional, Fukami, S., additional, Fukazawa, Y., additional, Fukui, Y., additional, Gaggero, D., additional, Galanti, G., additional, Gammaldi, V., additional, Garcia, E., additional, Garczarczyk, M., additional, Gascon, D., additional, Gaug, M., additional, Gent, A., additional, Ghalumyan, A., additional, Ghirlanda, G., additional, Gianotti, F., additional, Giarrusso, M., additional, Giavitto, G., additional, Giglietto, N., additional, Giordano, F., additional, Glicenstein, J., additional, Goldoni, P., additional, González, J.M., additional, Gourgouliatos, K., additional, Grabarczyk, T., additional, Grandi, P., additional, Granot, J., additional, Grasso, D., additional, Green, J., additional, Grube, J., additional, Gueta, O., additional, Gunji, S., additional, Halim, A., additional, Harvey, M., additional, Collado, T. Hassan, additional, Hayashi, K., additional, Heller, M., additional, Cadena, S. Hernández, additional, Hervet, O., additional, Hinton, J., additional, Hiroshima, N., additional, Hnatyk, B., additional, Hnatyk, R., additional, Hoffmann, D., additional, Hofmann, W., additional, Holder, J., additional, Horan, D., additional, Hörandel, J., additional, Horvath, P., additional, Hovatta, T., additional, Hrabovsky, M., additional, Hrupec, D., additional, Hughes, G., additional, Hütten, M., additional, Iarlori, M., additional, Inada, T., additional, Inoue, S., additional, Insolia, A., additional, Ionica, M., additional, Iori, M., additional, Jacquemont, M., additional, Jamrozy, M., additional, Janecek, P., additional, Martínez, I. Jiménez, additional, Jin, W., additional, Jung-Richardt, I., additional, Jurysek, J., additional, Kaaret, P., additional, Karas, V., additional, Karkar, S., additional, Kawanaka, N., additional, Kerszberg, D., additional, Khélifi, B., additional, Kissmann, R., additional, Knödlseder, J., additional, Kobayashi, Y., additional, Kohri, K., additional, Komin, N., additional, Kong, A., additional, Kosack, K., additional, Kubo, H., additional, Palombara, N. La, additional, Lamanna, G., additional, Lang, R.G., additional, Lapington, J., additional, Laporte, P., additional, Lefaucheur, J., additional, Lemoine-Goumard, M., additional, Lenain, J., additional, Leone, F., additional, Leto, G., additional, Leuschner, F., additional, Lindfors, E., additional, Lloyd, S., additional, Lohse, T., additional, Lombardi, S., additional, Longo, F., additional, Lopez, A., additional, López, M., additional, López-Coto, R., additional, Loporchio, S., additional, Lucarelli, F., additional, Luque-Escamilla, P.L., additional, Lyard, E., additional, Maggio, C., additional, Majczyna, A., additional, Makariev, M., additional, Mallamaci, M., additional, Mandat, D., additional, Maneva, G., additional, Manganaro, M., additional, Manicò, G., additional, Marcowith, A., additional, Marculewicz, M., additional, Markoff, S., additional, Marquez, P., additional, Martí, J., additional, Martinez, O., additional, Martínez, M., additional, Martínez, G., additional, Martínez-Huerta, H., additional, Maurin, G., additional, Mazin, D., additional, Mbarubucyeye, J.D., additional, Miranda, D. Medina, additional, Meyer, M., additional, Micanovic, S., additional, Miener, T., additional, Minev, M., additional, Miranda, J.M., additional, Mitchell, A., additional, Mizuno, T., additional, Mode, B., additional, Moderski, R., additional, Mohrmann, L., additional, Molina, E., additional, Montaruli, T., additional, Moralejo, A., additional, Merino, J. Morales, additional, Morcuende-Parrilla, D., additional, Morselli, A., additional, Mukherjee, R., additional, Mundell, C., additional, Murach, T., additional, Muraishi, H., additional, Nagai, A., additional, Nakamori, T., additional, Nemmen, R., additional, Niemiec, J., additional, Nieto, D., additional, Nievas, M., additional, Nikolajuk, M., additional, Nishijima, K., additional, Noda, K., additional, Nosek, D., additional, Nozaki, S., additional, O'Brien, P., additional, Ohira, Y., additional, Ohishi, M., additional, Oka, T., additional, Ong, R.A., additional, Orienti, M., additional, Orito, R., additional, Orlandini, M., additional, Orlando, E., additional, Osborne, J.P., additional, Ostrowski, M., additional, Oya, I., additional, Pagliaro, A., additional, Palatka, M., additional, Paneque, D., additional, Pantaleo, F.R., additional, Paredes, J.M., additional, Parmiggiani, N., additional, Patricelli, B., additional, Pavletić, L., additional, Pe'er, A., additional, Pech, M., additional, Pecimotika, M., additional, Peresano, M., additional, Persic, M., additional, Petruk, O., additional, Pfrang, K., additional, Piatteli, P., additional, Pietropaolo, E., additional, Pillera, R., additional, Pilszyk, B., additional, Pimentel, D., additional, Pintore, F., additional, Pita, S., additional, Pohl, M., additional, Poireau, V., additional, Polo, M., additional, Prado, R.R., additional, Prast, J., additional, Principe, G., additional, Produit, N., additional, Prokoph, H., additional, Prouza, M., additional, Przybilski, H., additional, Pueschel, E., additional, Pühlhofer, G., additional, Pumo, M.L., additional, Punch, M., additional, Queiroz, F., additional, Quirrenbach, A., additional, Rando, R., additional, Razzaque, S., additional, Rebert, E., additional, Recchia, S., additional, Reichherzer, P., additional, Reimer, O., additional, Reimer, A., additional, Renier, Y., additional, Reposeur, T., additional, Rhode, W., additional, Ribeiro, D., additional, Ribó, M., additional, Richtler, T., additional, Rico, J., additional, Rieger, F., additional, Rizi, V., additional, Rodriguez, J., additional, Fernandez, G. Rodriguez, additional, Ramirez, J.C. Rodriguez, additional, Vázquez, J.J. Rodríguez, additional, Romano, P., additional, Romeo, G., additional, Roncadelli, M., additional, Rosado, J., additional, de Leon, A. Rosales, additional, Rowell, G., additional, Rudak, B., additional, Rujopakarn, W., additional, Russo, F., additional, Sadeh, I., additional, Saha, L., additional, Saito, T., additional, Greus, F. Salesa, additional, Sanchez, D., additional, Sánchez-Conde, M., additional, Sangiorgi, P., additional, Sano, H., additional, Santander, M., additional, Santos, E.M., additional, Sanuy, A., additional, Sarkar, S., additional, Saturni, F.G., additional, Sawangwit, U., additional, Scherer, A., additional, Schleicher, B., additional, Schovanek, P., additional, Schussler, F., additional, Schwanke, U., additional, Sciacca, E., additional, Scuderi, S., additional, Arroyo, M. Seglar, additional, Sergijenko, O., additional, Servillat, M., additional, Seweryn, K., additional, Shalchi, A., additional, Sharma, P., additional, Shellard, R.C., additional, Siejkowski, H., additional, Sinha, A., additional, Sliusar, V., additional, Slowikowska, A., additional, Sokolenko, A., additional, Sol, H., additional, Specovius, A., additional, Spencer, S., additional, Spiga, D., additional, Stamerra, A., additional, Stanič, S., additional, Starling, R., additional, Stolarczyk, T., additional, Straumann, U., additional, Strišković, J., additional, Suda, Y., additional, Świerk, P., additional, Tagliaferri, G., additional, Takahashi, H., additional, Takahashi, M., additional, Tavecchio, F., additional, Taylor, L., additional, Tejedor, L.A., additional, Temnikov, P., additional, Terrier, R., additional, Terzic, T., additional, Testa, V., additional, Tian, W., additional, Tibaldo, L., additional, Tonev, D., additional, Torres, D.F., additional, Torresi, E., additional, Tosti, L., additional, Tothill, N., additional, Tovmassian, G., additional, Travnicek, P., additional, Truzzi, S., additional, Tuossenel, F., additional, Umana, G., additional, Vacula, M., additional, Vagelli, V., additional, Valentino, M., additional, Vallage, B., additional, Vallania, P., additional, Eldik, C. van, additional, Varner, G.S., additional, Vassiliev, V., additional, Acosta, M. Vázquez, additional, Vecchi, M., additional, Veh, J., additional, Vercellone, S., additional, Vergani, S., additional, Verguilov, V., additional, Vettolani, G.P., additional, Viana, A., additional, Vigorito, C.F., additional, Vitale, V., additional, Vorobiov, S., additional, Vovk, I., additional, Vuillaume, T., additional, Wagner, S.J., additional, Walter, R., additional, Watson, J., additional, White, M., additional, White, R., additional, Wiemann, R., additional, Wierzcholska, A., additional, Will, M., additional, Williams, D.A., additional, Wischnewski, R., additional, Wolter, A., additional, Yamazaki, R., additional, Yanagita, S., additional, Yang, L., additional, Yoshikoshi, T., additional, Zacharias, M., additional, Zaharijas, G., additional, Zaric, D., additional, Zavrtanik, M., additional, Zavrtanik, D., additional, Zdziarski, A.A., additional, Zech, A., additional, Zechlin, H., additional, Zhdanov, V.I., additional, and Živec, M., additional
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- 2021
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164. A possible sub-kiloparsec dual AGN buried behind the galaxy curtain
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Severgnini, P., primary, Braito, V., additional, Cicone, C., additional, Saracco, P., additional, Vignali, C., additional, Serafinelli, R., additional, Della Ceca, R., additional, Dotti, M., additional, Cusano, F., additional, Paris, D., additional, Pruto, G., additional, Zaino, A., additional, Ballo, L., additional, and Landoni, M., additional
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- 2021
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165. The stratified disc wind of MCG-03-58-007
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Braito, V, primary, Reeves, J N, additional, Severgnini, P, additional, Della Ceca, R, additional, Ballo, L, additional, Cicone, C, additional, Matzeu, G A, additional, Serafinelli, R, additional, and Sirressi, M, additional
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- 2020
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166. The first blazar observed at z > 6
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Belladitta, S., primary, Moretti, A., additional, Caccianiga, A., additional, Spingola, C., additional, Severgnini, P., additional, Della Ceca, R., additional, Ghisellini, G., additional, Dallacasa, D., additional, Sbarrato, T., additional, Cicone, C., additional, Cassarà, L. P., additional, and Pedani, M., additional
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- 2020
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167. Dust-to-gas ratio in a complete sample of type-1 AGN
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Ordovás-Pascual, I., Mateos, Silvia, Carrera, Francisco J., Caccianiga, A., Della Ceca, R., Severgnini, P., Moretti, A., Ballo, Lucía, and Corral, Amalia
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Resumen del póster presentado al XIII Scientific Meeting of the Spanish Astronomical Society, celebrado en la Universidad de Salamanca del 16 al 20 de julio de 2018., According to the Unified Model of Active Galactic Nuclei (AGN), unobscured AGN based on its optical spectrum (detection of rest-frame UV-optical broad emission lines, type-1 AGN) should appear as X-ray unabsorbed AGN. However, there is an important fraction (10-30%) of AGN whose optical and X-ray classifications do not match, and the origin of the discrepancy is not clear. To provide insight into this topic, we have conducted a statistical analysis of the optical obscuration and X-ray absorption properties of the optically type1 AGN from the Bright Ultra-hard XMM-Newton Survey (BUXS) with L2−10keV >1042 erg s−1 and z=0.05-1. We have high-quality spectra from XMM-Newton and either SDSS spectra or proprietary observations for the selected sample. In order to provide the most complete sample as possible, we have conducted a detailed analysis of the emission lines to provide a reliable classification of the AGNs. We derive the X-ray absorption by fitting their XMM-Newton spectra and the optical extinction using UV/optical spectral continuum fits. As BUXS is a flux limited X-ray selected sample at hard energies (f4.510keV ≤6×10−14 ergs−1cm−2), it is complete for NH column densities up to the Compton-thick limit (∼1024cm−2). Our preliminary results show that most type-1 AGN in our sample show consistent optical and X-ray classification, but there is a large fraction ( 20%) of objects with large NH column densities (NH >4×1021 cm−2).
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- 2019
168. Arcsecond Scale Polarization of BL Lac Objects
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Stanghellini, C., Cassaro, P., Bondi, M., Dallacasa, D., Ceca, R. Della, Zappalà, R. A., Ekers, R., editor, Fanti, C., editor, and Padrielli, L., editor
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- 1996
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169. Extended Emission in BL Lac Objects
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Bondi, M., Dallacasa, D., Stanghellini, C., Ceca, R. Della, Ekers, R., editor, Fanti, C., editor, and Padrielli, L., editor
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- 1996
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170. The Ultra Luminous Infrared Galaxy Mrk 231: new clues from BeppoSAX and XMM- Newton
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Braito, V., Della Ceca, R., Piconcelli, E., Severgnini, P., Bassani, L., Cappi, M., Franceschini, A., Iwasawa, K., Malaguti, G., Marziani, P., Palumbo, G.G.C., Persic, M., Risaliti, G., and Salvati, M.
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- 2004
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171. Arp 299: a second merging system with two active nuclei?
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Ballo, L., Braito, V., Della Ceca, R., Maraschi, L., Tavecchio, F., and Dadina, M.
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- 2004
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172. AGNs with discordant optical and X-ray classification are not a physical family: diverse origin in two AGNs
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Carrera, F., Ordovás-Pascual, I., Mateos, S., Wiersema, K., Barcons, X., Braito, V., Caccianiga, A., Del Moro, A., Ceca, R., Severgnini, P., Della Ceca, R., National Science Foundation (US), Alfred P. Sloan Foundation, Agenzia Spaziale Italiana, European Commission, Ministerio de Economía y Competitividad (España), Fundações de Amparo à Pesquisa (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Department of Energy (US), National Aeronautics and Space Administration (US), Higher Education Funding Council for England, Max Planck Institute for Astrophysics, Japan Science and Technology Agency, and Universidad de Cantabria
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Seyfert [Galaxies] ,Galaxies: Seyfert ,active [Galaxies] ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Library science ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Web site ,Galaxies: nuclei ,Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Galaxies: active ,Astrophysics - Astrophysics of Galaxies ,galaxies [X-rays] ,X-rays: galaxies ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,nuclei [Galaxies] ,Christian ministry ,Administration (government) - Abstract
Approximately 3-17 per cent of active galactic nuclei (AGNs) without detected rest-frame UV/optical broad emission lines (type-2 AGN) do not show absorption in X-rays. The physical origin behind the apparently discordant optical/X-ray properties is not fully understood. Our study aims at providing insight into this issue by conducting a detailed analysis of the nuclear dust extinction and X-ray absorption properties of two AGNs with low X-ray absorption and with high optical extinction, for which a rich set of high-quality spectroscopic data is available from XMM-Newton archive data in X-rays and XSHOOTER proprietary data at UV-to-NIR wavelengths. In order to unveil the apparent mismatch, we have determined the AV/NH and both the supermassive black hole and the host galaxy masses. We find that the mismatch is caused in one case by an abnormally high dust-to-gas ratio that makes the UV/optical emission to appear more obscured than in the X-rays. For the other object, we find that the dust-to-gas ratio is similar to the Galactic one but the AGN is hosted by a very massive galaxy so that the broad emission lines and the nuclear continuum are swamped by the star light and difficult to detect., IO-P and FJC acknowledge financial support through grant AYA2015-64346-C2-1-P (MINECO/FEDER). SM acknowledges financial support by the Spanish Ministry of Economy and Competitiveness through grant AYA2016-76730-P (MINECO/FEDER). AC, RD, PS and VB acknowledge financial support by the Italian Space Agency (contract ASI-INAF I/037/12/0). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss.org/. The STARLIGHT project is supported by the Brazilian agencies CNPq, CAPES and FAPESP and by the France-Brazil CAPES/Cofecub program.
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- 2017
173. An X-ray analysis of high-z blazar candidates
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Ighina, Luca, Caccianiga, A., Moretti, A., Belladitta, S., Ballo, L., Cicone, C., Della Ceca, R., Severgnini, P., and Dallacasa, D.
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Astrophysics::High Energy Astrophysical Phenomena ,high redshift ,Active Galactic Nuclei ,AGN ,blazar - Abstract
We present the results of a systematic X-ray analysis of a complete and well-defined sample of 23 high-z (z=4-5.5) blazar candidates selected from the CLASS radio survey. In particular, we have complemented the existing archival data (mostly Chandra) with dedicated Swift-XRT observations reaching an almost complete X-ray coverage of the sample. Our aim is to the determination of the nature of all the objects in the sample using X-ray data, since a strong and flat (Gamma
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- 2018
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174. Evidence Of A Clumpy Disc-Wind In The Star Forming Galaxy Mcg–03–58–007
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Matzeu, Gabriele, A., Braito, V., Reeves, J. N., Severgnini, P., Ballo, L., Caccianiga, A., Campana, S., Cicone, C., Della Ceca, R., Parker, M. L., Santos-Lleó, M., and Schartel, N.
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X-rays: galaxies ,Seyfert 2: individual: MCG-03-58-007 ,Active Galactic Nuclei ,AGN ,Black hole physics - Abstract
We report the result of a detailed analysis from a deep simultaneous130 ks XMM-Newton & NuSTAR observation of the nearby (z = 0.0315)and bright starburst-AGN system: MCG-03-58-007. Rapid X-ray spectralvariability has been detected, which may be caused by an obscurationevent. We show that most of the observed variability may be caused by aninhomogeneous, highly ionized fast (vw,1~0.10c and vw,2~0.35c)disc-wind rather than a neutral absorber embedded in the clumpy torus.Suchdramatic and fast variability of the wind, places MCG–3–58-007among the unique objects such as the luminous quasar PDS 456, whichis considered the prototype of fast disc-wind. We also show that most ofthe scattered soft X-ray emission in MCG–03–58–007 originates formthe larger scale photoionized plasma, possibly associated with NLR gas,as seen from the presence of several narrow emission lines in the RGSspectra.
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- 2018
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175. Des0141-54: A Very Powerful Radio-Loud Quasar At Z=5. Blazar Or Not?
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Belladitta, Silvia, Moretti, A., Caccianiga, A., Cicone, C., Ghisellini, G., Sbarrato, T., Severgnini, P., and Della Ceca, R.
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galaxies: high-redshift ,Astrophysics::High Energy Astrophysical Phenomena ,Quasar: supermassive black holes ,Active Galactic Nuclei ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Quasars: individual: DES0141-54 ,AGN ,Astrophysics::Galaxy Astrophysics - Abstract
Looking for Active Galactic Nuclei (AGNs) in the first Gyr of the Universe is crucial to understand when and how the first super massive black holes (SMBHs) formed, how they are related to galaxy formation and what is their role in the re-ionisation process. Explaining how such massive systems could be built up in the short (< 1Gyr) available cosmic time is still an open issue. Selecting high-z AGN candidates requires a multi-wavelength approach. In particular, we are carrying out a project which combines optical, IR, and radio datasets to identify radio loud AGNs at redshift z>4.5. I will present the newly discovered extremely radio loud quasar DES0141-54 at z=5.0, selected by combining the very recently data release (DR1) of the Dark Energy Survey (DES) with the Sydney University Molonglo Sky Survey (SUMSS) radio catalog. Rest-frame UV-optical spectra were obtained for this object using EFOSC2 at the NTT and X-Shooter at the VLT. This object is extremely bright in the radio band and its radio–loudness (ratio of the radio to optical flux) is one of the largest ever measured (R>10000) at this redshift. However, puzzlingly, the X-ray emission measured by the XMM-Newton and Swift satellites is weaker compared to what expected from a such large radio emission. 
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- 2018
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176. ROSAT Observations of Einstein EMSS AGNs
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Cappi, M., primary, Palumbo, G. G. C., additional, Della Ceca, R., additional, and Maccacaro, T., additional
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- 1994
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177. Te-REX: a sample of extragalactic TeV-emitting candidates
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Balmaverde, Barbara, primary, Caccianiga, A, additional, Della Ceca, R, additional, Wolter, A, additional, Belfiore, A, additional, Ballo, L, additional, Berton, M, additional, Gioia, I, additional, Maccacaro, T, additional, and Sbarufatti, B, additional
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- 2019
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178. Water masers in Compton-thick AGN
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Castangia, P., primary, Surcis, G., additional, Tarchi, A., additional, Caccianiga, A., additional, Severgnini, P., additional, and Della Ceca, R., additional
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- 2019
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179. X-ray properties of z > 4 blazars
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Ighina, L, primary, Caccianiga, A, additional, Moretti, A, additional, Belladitta, S, additional, Della Ceca, R, additional, Ballo, L, additional, and Dallacasa, D, additional
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- 2019
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180. Testing the blast-wave AGN feedback scenario in MCG-03-58-007
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Sirressi, M, primary, Cicone, C, additional, Severgnini, P, additional, Braito, V, additional, Dotti, M, additional, Della Ceca, R, additional, Reeves, J N, additional, Matzeu, G A, additional, Vignali, C, additional, and Ballo, L, additional
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- 2019
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181. The space density ofz > 4 blazars
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Caccianiga, A, primary, Moretti, A, additional, Belladitta, S, additional, Della Ceca, R, additional, Antón, S, additional, Ballo, L, additional, Cicone, C, additional, Dallacasa, D, additional, Gargiulo, A, additional, Ighina, L, additional, Marchã, M J, additional, and Severgnini, P, additional
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- 2019
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182. The stratified disc wind of MCG-03-58-007.
- Author
-
Braito, V, Reeves, J N, Severgnini, P, Della Ceca, R, Ballo, L, Cicone, C, Matzeu, G A, Serafinelli, R, and Sirressi, M
- Subjects
SEYFERT galaxies ,ACTIVE galaxies - Abstract
Past Suzaku, XMM–Newton , and NuSTAR observations of the nearby (z = 0.03233) bright Seyfert 2 galaxy MCG-03-58-007 revealed the presence of two deep and blue-shifted iron K-shell absorption line profiles. These could be explained with the presence of two phases of a highly ionized, high column density accretion disc wind outflowing with v
out1 ∼ −0.1 c and vout2 ∼ −0.2 c. Here we present two new observations of MCG-03-58-007: one was carried out in 2016 with Chandra and one in 2018 with Swift. Both caught MCG-03-58-007 in a brighter state (|$F_{{\mathrm{2}-10\, keV}} \sim 4 \times 10^{-12}$| erg cm−2 s−1 ) confirming the presence of the fast disc wind. The multi-epoch observations of MCG-03-58-007 covering the period from 2010 to 2018 were then analysed. These data show that the lower velocity component outflowing with vout1 ∼ −0.072 ± 0.002 c is persistent and detected in all the observations, although it is variable in column density in the range NH ∼ 3–8 × 1023 cm−2 . In the 2016 Swift observation we detected again the second faster component outflowing with vout2 ∼ −0.2 c , with a column density (|$N_{\mbox{H}}=7.0^{+5.6}_{-4.1}\times 10^{23}$| cm−2 ), similar to that seen during the Suzaku observation. However during the Chandra observation 2 yr earlier, this zone was not present (NH < 1.5 × 1023 cm−2 ), suggesting that this faster zone is intermittent. Overall the multi-epochs observations show that the disc wind in MCG-03-58-007 is not only powerful, but also extremely variable, hence placing MCG-03-58-007 among unique disc winds such as the one seen in the famous QSO PDS456. One of the main results of this investigation is the consideration that these winds could be extremely variable, sometime appearing and sometime disappearing; thus to reach solid and firm conclusions about their energetics multiple observations are mandatory. [ABSTRACT FROM AUTHOR]- Published
- 2021
- Full Text
- View/download PDF
183. The N H distribution of Seyfert 2 galaxies and the X-ray background
- Author
-
Maiolino, R., Bassani, L., Comastri, A., Dadina, M., Della Ceca, R., Gilli, R., Matt, G., Risaliti, G., Salvati, M., and Zamorani, G.
- Published
- 2000
- Full Text
- View/download PDF
184. Te-REX: a sample of extragalactic TeV-emitting candidates.
- Author
-
Balmaverde, Barbara, Caccianiga, A, Della Ceca, R, Wolter, A, Belfiore, A, Ballo, L, Berton, M, Gioia, I, Maccacaro, T, and Sbarufatti, B
- Subjects
SPECTRAL energy distribution ,GAMMA ray astronomy ,BL Lacertae objects ,ASTRONOMICAL surveys ,ACTIVE galaxies - Abstract
The REX (Radio-Emitting X-ray sources) is a catalogue produced by cross-matching X-ray data from the ROSAT -PSPC archive of pointed observations and radio data from the NRAO VLA Sky Survey, aimed at the selection of blazars. From the REX catalogue, we select a well-defined and statistically complete sample of high-energy peaked BL Lac (HBL). HBL are expected to be the most numerous class of extragalactic TeV-emitting sources. Specifically, we have considered only the REX sources in the currently planned CTA extragalactic survey area satisfying specific criteria and with an optical spectroscopic confirmation. We obtain 46 HBL candidates that we called Te-REX (TeV-emitting REX). We estimate the very high-energy gamma-ray emission, in the TeV domain, using an empirical approach i.e. using specific statistical relations between gamma-rays (at GeV energies) and radio/X-rays properties observed in bright HBL from the literature. We compare the spectral energy distributions (SEDs) with the sensitivities of current and upcoming Cherenkov telescopes and we predict that 14 Te-REX could be detectable with 50 h of observations of CTA and 7 of them also with current Cherenkov facilities in 50 h. By extrapolating these numbers on the total extragalactic sky, we predict that about 800 HBL could be visible in pointed CTA observations and ∼400 with current Cherenkov telescopes in 50 h. Interestingly, our predictions show that a non-negligible fraction (∼30 per cent) of the HBL that will be detectable by CTA is composed of relatively weak objects whose optical nuclear emission is swamped by the host-galaxy light and not (yet) detected by Fermi -LAT. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
- View/download PDF
185. Evidence for a clumpy disc-wind in the star-forming Seyfert 2 galaxy MCG–03–58–007
- Author
-
Matzeu, G A, primary, Braito, V, additional, Reeves, J N, additional, Severgnini, P, additional, Ballo, L, additional, Caccianiga, A, additional, Campana, S, additional, Cicone, C, additional, Della Ceca, R, additional, Parker, M L, additional, Santos-Lleó, M, additional, and Schartel, N, additional
- Published
- 2018
- Full Text
- View/download PDF
186. A new powerful and highly variable disc wind in an AGN–star-forming galaxy, the case of MCG-03-58-007
- Author
-
Braito, V, primary, Reeves, J N, additional, Matzeu, G A, additional, Severgnini, P, additional, Ballo, L, additional, Caccianiga, A, additional, Campana, S, additional, Cicone, C, additional, Della Ceca, R, additional, and Turner, T J, additional
- Published
- 2018
- Full Text
- View/download PDF
187. Swift data hint at a binary supermassive black hole candidate at sub-parsec separation
- Author
-
Severgnini, P, primary, Cicone, C, additional, Della Ceca, R, additional, Braito, V, additional, Caccianiga, A, additional, Ballo, L, additional, Campana, S, additional, Moretti, A, additional, La Parola, V, additional, Vignali, C, additional, Zaino, A, additional, Matzeu, G A, additional, and Landoni, M, additional
- Published
- 2018
- Full Text
- View/download PDF
188. A catalog of X-ray measurements of selected samples of active galaxies and nuclei
- Author
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Della Ceca, R, Palumbo, G. G. C, Persic, M, Boldt, E. A, Marshall, E. E, and De Zotti, G
- Subjects
Astronomy - Abstract
X-ray fluxes or upper limits in the 2-10 keV energy band from the HEAO 1 A-2 experiment are given for well-defined samples of QSOs and of Seyfert galaxies of types 1, 1.5 and 2, and for a list of BL Lac objects (334 sources in total). All on-orbit X-ray measurements of these objects published between 1976 and 1986 from other experiments have also been cataloged.
- Published
- 1990
- Full Text
- View/download PDF
189. The BeppoSAX program on X-ray weak Seyfert 2 galaxies
- Author
-
Salvati, M., Maiolino, R., Bassani, L., Dadina, M., Della Ceca, R., Matt, G., Risaliti, G., and Zamorani, G.
- Published
- 1999
- Full Text
- View/download PDF
190. AGNs with discordant optical and X-ray classification are not a physical family: diverse origin in two AGNs
- Author
-
National Science Foundation (US), Alfred P. Sloan Foundation, Agenzia Spaziale Italiana, European Commission, Ministerio de Economía y Competitividad (España), Fundações de Amparo à Pesquisa (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Department of Energy (US), National Aeronautics and Space Administration (US), Higher Education Funding Council for England, Max Planck Institute for Astrophysics, Japan Science and Technology Agency, Ordovás-Pascual, I., Mateos, Silvia, Carrera, Francisco J., Wiersema, Klass, Barcons, Xavier, Braito, V., Caccianiga, A., Moro, A. del, Della Ceca, R., Severgnini, P., National Science Foundation (US), Alfred P. Sloan Foundation, Agenzia Spaziale Italiana, European Commission, Ministerio de Economía y Competitividad (España), Fundações de Amparo à Pesquisa (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Department of Energy (US), National Aeronautics and Space Administration (US), Higher Education Funding Council for England, Max Planck Institute for Astrophysics, Japan Science and Technology Agency, Ordovás-Pascual, I., Mateos, Silvia, Carrera, Francisco J., Wiersema, Klass, Barcons, Xavier, Braito, V., Caccianiga, A., Moro, A. del, Della Ceca, R., and Severgnini, P.
- Abstract
Approximately 3-17 per cent of active galactic nuclei (AGNs) without detected rest-frame UV/optical broad emission lines (type-2 AGN) do not show absorption in X-rays. The physical origin behind the apparently discordant optical/X-ray properties is not fully understood. Our study aims at providing insight into this issue by conducting a detailed analysis of the nuclear dust extinction and X-ray absorption properties of two AGNs with low X-ray absorption and with high optical extinction, for which a rich set of high-quality spectroscopic data is available from XMM-Newton archive data in X-rays and XSHOOTER proprietary data at UV-to-NIR wavelengths. In order to unveil the apparent mismatch, we have determined the AV/NH and both the supermassive black hole and the host galaxy masses. We find that the mismatch is caused in one case by an abnormally high dust-to-gas ratio that makes the UV/optical emission to appear more obscured than in the X-rays. For the other object, we find that the dust-to-gas ratio is similar to the Galactic one but the AGN is hosted by a very massive galaxy so that the broad emission lines and the nuclear continuum are swamped by the star light and difficult to detect.
- Published
- 2017
191. AGN Diagnostic Plot in the WISE and 3XMM Era: the Role of Variability
- Author
-
Zaino, Alessandra, Severgnini, P., Vignali, C., Della Ceca, R., and Ballo, L.
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,active galactic nuclei ,AGN - Abstract
An efficient diagnostic method to find local (z
- Published
- 2016
- Full Text
- View/download PDF
192. Comparison of the optical and X-ray obscuration in AGN
- Author
-
Ordovás-Pascual, I., Mateos, Silvia, Carrera, Francisco J., Wiersema, Klass, Caccianiga, A., Severgnini, P., Della Ceca, R., Ballo, Lucía, and Moretti, A.
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Resumen del trabajo presentado al XXIX XMM-Newton SSC consortium meeting, celebrado en Madrid (España) del 14 al 15 de marzo de 2016., To provide insight into the apparent mismatch between the optical and X-ray absorption properties observed in 10-30 % of Active Galactic Nuclei (AGN), we have conducted a detailed study of two X-ray unabsorbed AGN with a type-2 optical spectroscopic classification. In addition to high quality X-ray spectroscopic observations, that we used to determine both the AGN luminosities and absorption, we have a VLT/XSHOOTER UV-to-near-IR high resolution spectrum for each object, that we used to determine the AGN intrinsic emision corrected for both contamination from the AGN hosts and extinction. Thanks to the high quality data available for these two intriguing sources, we unveil the origin of the mismatch. The most likely explanation is that both objects have an intrinsically high dust-to-gas ratio. In addition, we are conducting an statistical analysis of the optical obscuration and X-ray absorption properties of 159 Type-1 AGN drawn from BUXS to determine the distribution of dust-to-gas ratios in AGN over a broad range of luminosities and redshifts.
- Published
- 2016
193. VII. The third XMM-Newton serendipitous source catalogue
- Author
-
Rosen, Simon, Webb, N. A., Watson, M. G., Ballet, J., Braito, V., Carrera, Francisco J., Ceballos, María Teresa, Coriat, M., Della Ceca, R., Denkinson, G., Esquej, Pilar, Farrell, S. A., Freyberg, M. J., Grisé, F., Guillout, P., Heil, L., Koliopanos, F., Law-Green, D., Lamer, Georg, Lin, D., Martino, R., Michel, L., Motch, C., Nebot Gómez-Morán, A., Page, C. G., Page, K., Page, M. J., Pakull, M. W., Pye, J. P., Read, A. M., Rodriguez, P., Sakano, M., Saxton, R. D., Schwope, A., Scott, A. E., Sturm, R., Traulsen, I., Yershov, V., Zolotukhin, I., European Commission, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), and Ministero dell'Istruzione, dell'Università e della Ricerca
- Subjects
general [X-rays] ,miscellaneous [Astronomical databases] ,Surveys ,Catalogues - Abstract
[Context]: Thanks to the large collecting area (3 × ∼1500 cm at 1.5 keV) and wide field of view (30′ across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of up to several hundred X-ray sources, most of which are newly discovered objects. Since XMM-Newton has now been in orbit for more than 15 yr, hundreds of thousands of sources have been detected. [Aims]: Recently, many improvements in the XMM-Newton data reduction algorithms have been made. These include enhanced source characterisation and reduced spurious source detections, refined astrometric precision of sources, greater net sensitivity for source detection, and the extraction of spectra and time series for fainter sources, both with better signal-to-noise. Thanks to these enhancements, the quality of the catalogue products has been much improved over earlier catalogues. Furthermore, almost 50% more observations are in the public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science Centre to produce a much larger and better quality X-ray source catalogue. [Methods]: The XMM-Newton Survey Science Centre has developed a pipeline to reduce the XMM-Newton data automatically. Using the latest version of this pipeline, along with better calibration, a new version of the catalogue has been produced, using XMM-Newton X-ray observations made public on or before 2013 December 31. Manual screening of all of the X-ray detections ensures the highest data quality. This catalogue is known as 3XMM. [Results]: In the latest release of the 3XMM catalogue, 3XMM-DR5, there are 565 962 X-ray detections comprising 396 910 unique X-ray sources. Spectra and lightcurves are provided for the 133 000 brightest sources. For all detections, the positions on the sky, a measure of the quality of the detection, and an evaluation of the X-ray variability is provided, along with the fluxes and count rates in 7 X-ray energy bands, the total 0.2-12 keV band counts, and four hardness ratios. With the aim of identifying the detections, a cross correlation with 228 catalogues of sources detected in all wavebands is also provided for each X-ray detection. [Conclusions]: 3XMM-DR5 is the largest X-ray source catalogue ever produced. Thanks to the large array of data products associated with each detection and each source, it is an excellent resource for finding new and extreme objects. F.J.C. acknowledges financial support by the Spanish Ministry of Economy and Competitiveness through grant AYA2012-31447, which is partly funded by the FEDER programme, and grant AYA2015-64346-C2-1-P. M.T.C. acknowledges financial support from the Spanish Ministry of Science and Innovation through grant AYA2010-21490-C02-1. The Italian team acknowledges financial support during the years from the Ministero dell’Istruzione, dell’Universita’ e della Ricerca (MIUR), from the Agenzia Spaziale Italiana (ASI) and from the Istituto Nazionale di Astrofisica (INAF).
- Published
- 2016
194. On the relation between X-ray absorption and optical extinction in AGN
- Author
-
Ordovás-Pascual, I., Mateos, S., Carrera, F. J., Wiersema, K., Caccianiga, A., Della Ceca, R., Severgnini, P., Moretti, A., Lucia Ballo, Alfred P. Sloan Foundation, National Science Foundation (US), Department of Energy (US), Japan Society for the Promotion of Science, National Aeronautics and Space Administration (US), European Commission, Higher Education Funding Council for England, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministerio de Economía y Competitividad (España), and Max Planck Society
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Active Galactic Nuclei ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Trabajo presentado al XII Scientific Meeting of the Spanish Astronomical Society (SEA), celebrado en Bilbao del 18 al 22 de julio de 2016., According to the Unified Model of Active Galactic Nuclei (AGN), an X-ray unabsorbed AGN should appear as unobscured in the optical (Type-1) and viceversa (Type-2). However, there is an important fraction (10-30%) of AGN whose optical and X-ray classifications do not match. To provide insight into the origin of such apparent discrepancies, we have conducted two analyses: 1) a detailed study of the UV-to-near-IR emission of two X-ray unabsorbed Type-2 AGN drawn from the Bright Ultra-Hard XMM-Newton Survey (BUXS); 2) a statistical analysis of the optical obscuration and X-ray absorption properties of 159 Type-1 AGN drawn from BUXS to determine the distribution of dust-to-gas ratios in AGN over a broad range of luminosities and redshifts. In our works we have also determined the impact of contamination from the AGN hosts in the optical classification of AGNs. Our studies are already provided very exciting results such as the detection of objects with extreme dust-to-gas ratios, between 300-10000 times below the Galactic dust-to-gas ratio., IO-P and FJC acknowledge financial support through grant AYA2015-64346-C2-1-P (MINECO/FEDER). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The STARLIGHT project is supported by the Brazilian agencies CNPq, CAPES and FAPESP and by the France-Brazil CAPES/Cofecub program.
- Published
- 2016
195. The XMM-Newton serendipitous survey
- Author
-
Rosen, Simon, Webb, N. A., Watson, M. G., Ballet, J., Braito, V., Carrera, Francisco J., Ceballos, María Teresa, Coriat, M., Della Ceca, R., Denkinson, G., Esquej, Pilar, Farrell, S. A., Freyberg, M. J., Grisé, F., Guillout, P., Heil, L., Koliopanos, F., Law-Green, D., Lamer, Georg, Lin, D., Martino, R., Michel, L., Motch, C., Nebot Gómez-Morán, A., Page, C. G., Page, K., Page, M. J., Pakull, M. W., Pye, J. P., Read, A. M., Rodriguez, P., Sakano, M., Saxton, R. D., Schwope, A., Scott, A. E., Sturm, R., Traulsen, I., Yershov, V., Zolotukhin, I., European Commission, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), and Ministero dell'Istruzione, dell'Università e della Ricerca
- Subjects
Astronomical databases: miscellaneous ,Surveys ,X-rays: general ,Catalogues - Abstract
[Context]: Thanks to the large collecting area (3 × ∼1500 cm at 1.5 keV) and wide field of view (30′ across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of up to several hundred X-ray sources, most of which are newly discovered objects. Since XMM-Newton has now been in orbit for more than 15 yr, hundreds of thousands of sources have been detected. [Aims]: Recently, many improvements in the XMM-Newton data reduction algorithms have been made. These include enhanced source characterisation and reduced spurious source detections, refined astrometric precision of sources, greater net sensitivity for source detection, and the extraction of spectra and time series for fainter sources, both with better signal-to-noise. Thanks to these enhancements, the quality of the catalogue products has been much improved over earlier catalogues. Furthermore, almost 50% more observations are in the public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science Centre to produce a much larger and better quality X-ray source catalogue. [Methods]: The XMM-Newton Survey Science Centre has developed a pipeline to reduce the XMM-Newton data automatically. Using the latest version of this pipeline, along with better calibration, a new version of the catalogue has been produced, using XMM-Newton X-ray observations made public on or before 2013 December 31. Manual screening of all of the X-ray detections ensures the highest data quality. This catalogue is known as 3XMM. [Results]: In the latest release of the 3XMM catalogue, 3XMM-DR5, there are 565 962 X-ray detections comprising 396 910 unique X-ray sources. Spectra and lightcurves are provided for the 133 000 brightest sources. For all detections, the positions on the sky, a measure of the quality of the detection, and an evaluation of the X-ray variability is provided, along with the fluxes and count rates in 7 X-ray energy bands, the total 0.2-12 keV band counts, and four hardness ratios. With the aim of identifying the detections, a cross correlation with 228 catalogues of sources detected in all wavebands is also provided for each X-ray detection. [Conclusions]: 3XMM-DR5 is the largest X-ray source catalogue ever produced. Thanks to the large array of data products associated with each detection and each source, it is an excellent resource for finding new and extreme objects., F.J.C. acknowledges financial support by the Spanish Ministry of Economy and Competitiveness through grant AYA2012-31447, which is partly funded by the FEDER programme, and grant AYA2015-64346-C2-1-P. M.T.C. acknowledges financial support from the Spanish Ministry of Science and Innovation through grant AYA2010-21490-C02-1. The Italian team acknowledges financial support during the years from the Ministero dell’Istruzione, dell’Universita’ e della Ricerca (MIUR), from the Agenzia Spaziale Italiana (ASI) and from the Istituto Nazionale di Astrofisica (INAF).
- Published
- 2016
196. XMM–Newton and NuSTAR joint observations of Mrk 915: a deep look into the X-ray properties★
- Author
-
Ballo, L., primary, Severgnini, P., additional, Della Ceca, R., additional, Braito, V., additional, Campana, S., additional, Moretti, A., additional, Vignali, C., additional, and Zaino, A., additional
- Published
- 2017
- Full Text
- View/download PDF
197. AGN with discordant optical and X-ray classification are not a physical family: Diverse origin in two AGN
- Author
-
Ordovás-Pascual, I., primary, Mateos, S., additional, Carrera, F. J., additional, Wiersema, K., additional, Barcons, X., additional, Braito, V., additional, Caccianiga, A., additional, Del Moro, A., additional, Della Ceca, R., additional, and Severgnini, P., additional
- Published
- 2017
- Full Text
- View/download PDF
198. Revisiting the relationship between 6 ��m and 2-10 keV continuum luminosities of AGN
- Author
-
Mateos, S., Carrera, F. J., Alonso-Herrero, A., Rovilos, E., Hern��n-Caballero, A., Barcons, X., Blain, A., Caccianiga, A., Della Ceca, R., and Severgnini, P.
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::Solar and Stellar Astrophysics ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We have determined the relation between the AGN luminosities at rest-frame 6 ��m associated to the dusty torus emission and at 2-10 keV energies using a complete, X-ray flux limited sample of 232 AGN drawn from the Bright Ultra-hard XMM-Newton Survey. The objects have intrinsic X-ray luminosities between 10^42 and 10^46 erg/s and redshifts from 0.05 to 2.8. The rest-frame 6 ��m luminosities were computed using data from the Wide-Field Infrared Survey Explorer and are based on a spectral energy distribution decomposition into AGN and galaxy emission. The best-fit relationship for the full sample is consistent with being linear, L_6 ��m $\propto$ L_2-10 keV^0.99$\pm$0.032, with intrinsic scatter, ~0.35 dex in log L_6 ��m. The L_6 ��m/L_2-10 keV luminosity ratio is largely independent on the line-of-sight X-ray absorption. Assuming a constant X-ray bolometric correction, the fraction of AGN bolometric luminosity reprocessed in the mid-IR decreases weakly, if at all, with the AGN luminosity, a finding at odds with simple receding torus models. Type 2 AGN have redder mid-IR continua at rest-frame wavelengths, Accepted for publication in MNRAS. 24 pages, 10 figures and 5 tables. This version includes minor changes to the text and Table 2 in response to comments from the referee
- Published
- 2015
- Full Text
- View/download PDF
199. X-ray properties of z > 4 blazars.
- Author
-
Ighina, L, Caccianiga, A, Moretti, A, Belladitta, S, Della Ceca, R, Ballo, L, and Dallacasa, D
- Subjects
SPECTRAL energy distribution ,COSMIC rays ,COSMIC background radiation ,X-rays ,GAMMA ray bursts ,ASTRONOMICAL surveys ,STELLAR luminosity function - Abstract
We present the X-ray analysis of the largest flux-limited complete sample of blazar candidates at z > 4 selected from the Cosmic Lens All Sky Survey (CLASS). After obtaining a nearly complete (24/25) X-ray coverage of the sample (from Swift-XRT, XMM–Newton , and Chandra), we analysed the spectra in order to identify the bona fide blazars. We classified the sources based on the shape of their Spectral Energy Distributions and, in particular, on the flatness of the X-ray emission and its intensity compared to the optical one. We then compared these high-z blazars with a blazar sample selected at lower redshifts (|$\bar{z}\sim 1$|). We found a significant difference in the X-ray-to-radio luminosity ratios, with the CLASS blazars having a mean ratio 2.4 ± 0.5 times larger than low-z blazars. We tentatively interpret this evolution as due to the interaction of the electrons of the jet with the Cosmic Microwave Background photons, which is expected to boost the observed X-ray emission at high redshifts. Such a dependence has been already observed in highly radio loud AGNs in the recent literature. This is the first time it is observed using a statistically complete radio flux limited sample of blazars. We have then evaluated whether this effect could explain the differences in the cosmological evolution recently found between radio and X-ray selected samples of blazars. We found that the simple version of this model is not able to solve the tension between the two evolutionary results. [ABSTRACT FROM AUTHOR]
- Published
- 2019
- Full Text
- View/download PDF
200. The space density of z > 4 blazars.
- Author
-
Caccianiga, A, Moretti, A, Belladitta, S, Della Ceca, R, Antón, S, Ballo, L, Cicone, C, Dallacasa, D, Gargiulo, A, Ighina, L, Marchã, M J, and Severgnini, P
- Subjects
REDSHIFT ,BL Lacertae objects ,DENSITY ,SPACE ,ACTIVE galactic nuclei - Abstract
High-redshift blazars are an important class of active galactic nuclei (AGN) that can provide an independent estimate of the supermassive black hole mass function in high-redshift radio-loud AGN without the bias due to absorption along the line of sight. Using the Cosmic Lens All Sky Survey (CLASS), we built a complete radio flux-limited sample of high-redshift (z > 4) blazars suitable for statistical studies. By combining dedicated optical observations and the SDSS spectroscopic database, we obtained a sample of 26 blazar candidates with a spectroscopic redshift above 4. On the basis of their radio spectrum, we distinguish between blazars and QSO with a Gigahertz Peaked Spectrum (GPS) like spectrum. Out of the 18 confirmed blazars 14 constitute a completely identified, flux-limited sample down to a magnitude of 21 (AB). Using this complete sample, we derive a space density of blazars with 4 < z < 5.5 of ρ = 0.13 |$^{+0.05}_{-0.03}$| Gpc
−3 . This is the first actual estimate of the blazar space density in this range of redshift. This value is in good agreement with the extrapolation of the luminosity function and cosmological evolution based on a sample of flat-spectrum radio quasars selected at lower redshifts and it is consistent with a cosmological evolution peaking at z ∼ 2 similar to radio-quiet QSO. We do not confirm, instead, the presence of a peak at z ∼ 4 in the space density evolution, recently suggested using an X-ray selected sample of blazars. It is possible that this extreme peak of the evolution is present only among the most luminous blazars. [ABSTRACT FROM AUTHOR]- Published
- 2019
- Full Text
- View/download PDF
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