24 results on '"W. Max-Moerbeck"'
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2. Multiwavelength study of the gravitationally lensed blazar QSO B0218+357 between 2016 and 2020
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V A Acciari, S Ansoldi, L A Antonelli, A Arbet Engels, M Artero, K Asano, D Baack, A Babić, A Baquero, U Barres de Almeida, J A Barrio, I Batković, J Becerra González, W Bednarek, L Bellizzi, E Bernardini, M Bernardos, A Berti, J Besenrieder, W Bhattacharyya, C Bigongiari, A Biland, O Blanch, G Bonnoli, Ž Bošnjak, G Busetto, R Carosi, G Ceribella, M Cerruti, Y Chai, A Chilingarian, S Cikota, S M Colak, E Colombo, J L Contreras, J Cortina, S Covino, G D’Amico, V D’Elia, P Da Vela, F Dazzi, A De Angelis, B De Lotto, M Delfino, J Delgado, C Delgado Mendez, D Depaoli, F Di Pierro, L Di Venere, E Do Souto Espiñeira, D Dominis Prester, A Donini, D Dorner, M Doro, D Elsaesser, V Fallah Ramazani, A Fattorini, G Ferrara, M V Fonseca, L Font, C Fruck, S Fukami, R J García López, M Garczarczyk, S Gasparyan, M Gaug, N Giglietto, F Giordano, P Gliwny, N Godinović, J G Green, D Green, D Hadasch, A Hahn, L Heckmann, J Herrera, J Hoang, D Hrupec, M Hütten, T Inada, S Inoue, K Ishio, Y Iwamura, I Jiménez, J Jormanainen, L Jouvin, Y Kajiwara, M Karjalainen, D Kerszberg, Y Kobayashi, H Kubo, J Kushida, A Lamastra, D Lelas, F Leone, E Lindfors, S Lombardi, F Longo, R López-Coto, M López-Moya, A López-Oramas, S Loporchio, B Machado de Oliveira Fraga, C Maggio, P Majumdar, M Makariev, M Mallamaci, G Maneva, M Manganaro, K Mannheim, L Maraschi, M Mariotti, M Martínez, D Mazin, S Menchiari, S Mender, S Mićanović, D Miceli, T Miener, M Minev, J M Miranda, R Mirzoyan, E Molina, A Moralejo, D Morcuende, V Moreno, E Moretti, V Neustroev, C Nigro, K Nilsson, K Nishijima, K Noda, S Nozaki, Y Ohtani, T Oka, J Otero-Santos, S Paiano, M Palatiello, D Paneque, R Paoletti, J M Paredes, L Pavletić, P Peñil, C Perennes, M Persic, P G Prada Moroni, E Prandini, C Priyadarshi, I Puljak, W Rhode, M Ribó, J Rico, C Righi, A Rugliancich, L Saha, N Sahakyan, T Saito, S Sakurai, K Satalecka, F G Saturni, B Schleicher, K Schmidt, T Schweizer, J Sitarek, I Šnidarić, D Sobczynska, A Spolon, A Stamerra, D Strom, M Strzys, Y Suda, T Surić, M Takahashi, F Tavecchio, P Temnikov, T Terzić, M Teshima, L Tosti, S Truzzi, A Tutone, S Ubach, J van Scherpenberg, G Vanzo, M Vazquez Acosta, S Ventura, V Verguilov, C F Vigorito, V Vitale, I Vovk, M Will, C Wunderlich, D Zarić, F de Palma, F D’Ammando, A Barnacka, D K Sahu, M Hodges, T Hovatta, S Kiehlmann, W Max-Moerbeck, A C S Readhead, R Reeves, T J Pearson, A Lähteenmäki, I Björklund, M Tornikoski, J Tammi, S Suutarinen, K Hada, and K Niinuma
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- 2021
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3. Investigating the multiwavelength behaviour of the flat spectrum radio quasar CTA 102 during 2013–2017
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F D’Ammando, C M Raiteri, M Villata, J A Acosta-Pulido, I Agudo, A A Arkharov, R Bachev, G V Baida, E Benítez, G A Borman, W Boschin, V Bozhilov, M S Butuzova, P Calcidese, M I Carnerero, D Carosati, C Casadio, N Castro-Segura, W-P Chen, G Damljanovic, A Di Paola, J Echevarría, N V Efimova, Sh A Ehgamberdiev, C Espinosa, A Fuentes, A Giunta, J L Gómez, T S Grishina, M A Gurwell, D Hiriart, H Jermak, B Jordan, S G Jorstad, M Joshi, G N Kimeridze, E N Kopatskaya, K Kuratov, O M Kurtanidze, S O Kurtanidze, A Lähteenmäki, V M Larionov, E G Larionova, L V Larionova, C Lázaro, C S Lin, M P Malmrose, A P Marscher, K Matsumoto, B McBreen, R Michel, B Mihov, M Minev, D O Mirzaqulov, S N Molina, J W Moody, D A Morozova, S V Nazarov, A A Nikiforova, M G Nikolashvili, J M Ohlert, N Okhmat, E Ovcharov, F Pinna, T A Polakis, C Protasio, T Pursimo, F J Redondo-Lorenzo, N Rizzi, G Rodriguez-Coira, K Sadakane, A C Sadun, M R Samal, S S Savchenko, E Semkov, L Sigua, B A Skiff, L Slavcheva-Mihova, P S Smith, I A Steele, A Strigachev, J Tammi, C Thum, M Tornikoski, Yu V Troitskaya, I S Troitsky, A A Vasilyev, O Vince, T Hovatta, S Kiehlmann, W Max-Moerbeck, A C S Readhead, R Reeves, T J Pearson, T Mufakharov, Yu V Sotnikova, and M G Mingaliev
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- 2019
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4. The presence of interstellar scintillation in the 15 GHz interday variability of 1158 OVRO-monitored blazars
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J Y Koay, D L Jauncey, T Hovatta, S Kiehlmann, H E Bignall, W Max-Moerbeck, T J Pearson, A C S Readhead, R Reeves, C Reynolds, and H Vedantham
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- 2019
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5. New Tests of Milli-lensing in the Blazar PKS 1413 + 135
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A. L. Peirson, I. Liodakis, A. C. S Readhead, M. L. Lister, E. S. Perlman, M. F. Aller, R. D. Blandford, K. J. B. Grainge, D. A. Green, M. A. Gurwell, M. W. Hodges, T. Hovatta, S. Kiehlmann, A. Lähteenmäki, W. Max-Moerbeck, T. Mcaloone, S. O’Neill, V. Pavlidou, T. J. Pearson, V. Ravi, R. A. Reeves, P. F. Scott, G. B. Taylor, D. J. Titterington, M. Tornikoski, H. K. Vedantham, P. N. Wilkinson, D. T. Williams, and J. A. Zensus
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- 2022
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6. Multiwavelength cross-correlations and flaring activity in bright blazars
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I Liodakis, R W Romani, A V Filippenko, S Kiehlmann, W Max-Moerbeck, A C S Readhead, and W Zheng
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- 2018
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7. The Unanticipated Phenomenology of the Blazar PKS 2131-021: A Unique Supermassive Black Hole Binary Candidate
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S. O’Neill, S. Kiehlmann, A. C. S. Readhead, M. F. Aller, R. D. Blandford, I. Liodakis, M. L. Lister, P. Mróz, C. P. O’Dea, T. J. Pearson, V. Ravi, M. Vallisneri, K. A. Cleary, M. J. Graham, K. J. B. Grainge, M. W. Hodges, T. Hovatta, A. Lähteenmäki, J. W. Lamb, T. J. W. Lazio, W. Max-Moerbeck, V. Pavlidou, T. A. Prince, R. A. Reeves, M. Tornikoski, P. Vergara de la Parra, J. A. Zensus, California Institute of Technology, University of Crete, University of Michigan, Ann Arbor, Stanford University, University of Turku, Purdue University, University of Warsaw, University of Manitoba, Jet Propulsion Laboratory, University of Manchester, Metsähovi Radio Observatory, Department of Electronics and Nanoengineering, Universidad de Chile, Universidad de Concepción, Max Planck Institute for Radio Astronomy, Aalto-yliopisto, and Aalto University
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Space and Planetary Science ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
Most large galaxies host supermassive black holes in their nuclei and are subject to mergers, which can produce a supermassive black hole binary (SMBHB), and hence periodic signatures due to orbital motion. We report unique periodic radio flux density variations in the blazar PKS~2131$-$021, which strongly suggest an SMBHB with an orbital separation of $\sim 0.001-0.01$ pc. Our 45.1-year radio light curve shows two epochs of strong sinusoidal variation with the same period and phase to within $, Comment: 24 pages, 13 figure, 3 Tables, accepted for publication in APJL
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- 2022
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8. Cherenkov Telescope Array : the World’s largest VHE gamma-ray observatory
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Roberta Zanin, H. Abdalla, H. Abe, S. Abe, A. Abusleme, F. Acero, A. Acharyya, V. Acin Portella, K. Ackley, R. Adam, C. Adams, S.S. Adhikari, I. Aguado Ruesga, I. Agudo, R. Aguilera, A. Aguirre Santaella, F. Aharonian, A. Alberdi, R. Alfaro, J. Alfaro, C. Alispach, R. Aloisio, R. Alves Batista, J.P. Amans, L. Amati, E. Amato, L. Ambrogi, G. Ambrosi, M. Ambrosio, R. Ammendola, J. Anderson, M. Anduze, E.O. Anguner, L.A. Antonelli, V. Antonuccio, P. Antoranz, R. Anutarawiramkul, J. Aragunde Gutierrez, C. Aramo, A. Araudo, M. Araya, A. Arbet Engels, C. Arcaro, V. Arendt, C. Armand, T. Armstrong, F. Arqueros, L. Arrabito, B. Arsioli, M. Artero, K. Asano, Y. Ascasibar, J. Aschersleben, M. Ashley, P. Attina, P. Aubert, C. B. Singh, D. Baack, A. Babic, M. Backes, V. Baena, S. Bajtlik, A. Baktash, C. Balazs, M. Balbo, O. Ballester, J. Ballet, B. Balmaverde, A. Bamba, R. Bandiera, A. Baquero Larriva, P. Barai, C. Barbier, V. Barbosa Martins, M. Barcelo, M. Barkov, M. Barnard, L. Baroncelli, U. Barres de Almeida, J.A. Barrio, D. Bastieri, P.I. Batista, I. Batkovic, C. Bauer, R. Bautista González, J. Baxter, U. Becciani, J. Becerra González, Y. Becherini, G. Beck, J. Becker Tjus, W. Bednarek, A. Belfiore, L. Bellizzi, R. Belmont, W. Benbow, D. Berge, E. Bernardini, M.I. Bernardos, K. Bernlöhr, A. Berti, M. Berton, B. Bertucci, V. Beshley, N. Bhatt, S. Bhattacharyya, W. Bhattacharyya, B. Y. Bi, G. Bicknell, N. Biederbeck, C. Bigongiari, A. Biland, R. Bird, E. Bissaldi, J. Biteau, M. Bitossi, O. Blanch, M. Blank, J. Blazek, J. Bobin, C. Boccato, F. Bocchino, C. Boehm, M. Bohacova, C. Boisson, J. Boix, J.P. Bolle, J. Bolmont, G. Bonanno, C. Bonavolontà, L. Bonneau Arbeletche, G. Bonnoli, P. Bordas, J. Borkowski, R. Bose, D. Bose, Z. Bosnjak, E. Bottacini, Markus Böttcher, M.T. Botticella, C. Boutonnet, F. Bouyjou, V. Bozhilov, E. Bozzo, L. Brahimi, C. Braiding, S. Brau Nogue, S. Breen, J. Bregeon, M. Breuhaus, A. Brill, W. Brisken, E. Brocato, A.M. Brown, K. Brügge, P. Brun, F. Brun, L. Brunetti, G. Brunetti, P. Bruno, A. Bruno, A. Bruzzese, N. Bucciantini, J. H. Buckley, R. Bühler, A. Bulgarelli, T. Bulik, M. Bünning, M. Bunse, M. Burton, A. Burtovoi, M. Buscemi, S. Buschjager, G. Busetto, J. Buss, K. Byrum, A. Caccianiga, F. Cadoux, A. Calanducci, C. Calderon, J. Calvo Tovar, R. A. Cameron, P. Campana, R. Canestrari, F. Cangemi, B. Cantlay, M. Capalbi, M. Capasso, M. Cappi, A. Caproni, R. Capuzzo Dolcetta, P. Caraveo, V. Cárdenas, L. Cardiel, M. Cardillo, C. Carlile, S. Caroff, R. Carosi, A. Carosi, E. Carquin, M. Carrere, J.M. Casandjian, S. Casanova, F. Cassol, F. Catalani, O. Catalano, D. Cauz, A. Ceccanti, C. Celestino Silva, K. Cerny, M. Cerruti, E. Chabanne, P. Chadwick, Y. Chai, P. Chambery, C. Champion, S. Chaty, A. Chen, K. Cheng, M. Chernyakova, G. Chiaro, A. Chiavassa, M. Chikawa, V.R. Chitnis, J. Chudoba, L. Chytka, S. Cikota, A. Circiello, P. Clark, M. Colak, E. Colombo, S. Colonges, A. Comastri, A. Compagnino, V. Conforti, E. Congiu, R. Coniglione, J. Conrad, F. Conte, J.L. Contreras, P. Coppi, R. Cornat, J. Coronado Blazquez, J. Cortina, A. Costa, H. Costantini, G. Cotter, B. Courty, S. Covino, S. Crestan, P. Cristofari, R. Crocker, J. Croston, K. Cubuk, O. Cuevas, X. Cui, G. Cusumano, S. Cutini, G. D'Amico, F. D'Ammando, P. D'Avanzo, P. Da Vela, M. Dadina, S. Dai, M. Dalchenko, M. Dall'Ora, M.K. Daniel, J. Dauguet, I. Davids, J. Davies, B. Dawson, A. De Angelis, A.E. de Araujo Carvalho, M. de Bony de Lavergne, G. De Cesare, F. de Frondat, I. de la Calle, E. de Gouveia Dal Pino, B. De Lotto, A. De Luca, D. De Martino, M. de Naurois, E. de Ona Wilhelmi, F. De Palma Persio, N. De Simone, V. de Souza Valle, E. Delagnes, G. Deleglise Reznicek, C. Delgado, A.G. Delgado Giler, J. Delgado Mengual Valle, Domenico Della Volpe, D. Depaoli, J. Devin, T. Di Girolamo, C. Di Giulio Pierro, L. Di Venere, C. Díaz, C. Dib, S. Diebold, S. Digel, A. Djannati Atai, J. Djuvsland, A. Dmytriiev, K. Docher, A. Domínguez, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, Rita Cassia dos Anjos, J.L. Dournaux, T. Downes, G. Drake, H. Drass, D. Dravins, C. Duangchan, A. Duara, G. Dubus, L. Ducci, C. Duffy, D. Dumora, K. Dundas Mora, A. Durkalec, V.V. Dwarkadas, J. Ebr, C. Eckner, J. Eder, E. Edy, K. Egberts, S. Einecke, C. Eleftheriadis, D. Elsässer, G. Emery, D. Emmanoulopoulos, J.P. Ernenwein, M. Errando, P. Escarate, J. Escudero, C. Espinoza, S. Ettori, A. Eungwanichayapant, P. Evans, C. Evoli, M. Fairbairn, D. Falceta Goncalves, A. Falcone, V. Fallah Ramazanı, R. Falomo, K. Farakos, G. Fasola, A. Fattorini, Y. Favre, R. Fedora, E. Fedorova, K. Feijen, Q. Feng, G. Ferrand, G. Ferrara, O. Ferreira, M. Fesquet, E. Fiandrini, A. Fiasson, M. Filipovic, D. Fink, J.P. Finley, V. Fioretti, D.F.G. Fiorillo, M. Fiorini, S. Flis, H. Flores, L. Foffano, C. Fohr, M.V. Fonseca, L. Font, G. Fontaine, O. Fornieri, P. Fortin, L. Fortson, N. Fouque, B. Fraga, A. Franceschini, F.J. Franco, L. Freixas Coromina, L. Fresnillo, D. Fugazza, Y. Fujita, S. Fukami, Y. Fukazawa, D. Fulla, S. Funk, A. Furniss, S. Gabici, D. Gaggero, G. Galanti, P. Galdemard, Y. A. Gallant, D. Galloway, S. Gallozzi, V. Gammaldi, R. Garcia, L. E. García-Muñoz, E. Garcia Lopez, F. Gargano, C. Gargano, S. Garozzo, D. Gascon, T. Gasparetto, D. Gasparrini, H. Gasparyan, M. Gaug, N. Geffroy, A. Gent, S. Germani, A. Ghalumyan, A. Ghedina, G. Ghirlanda, F. Gianotti, S. Giarrusso, M. Giarrusso, G. Giavitto, B. Giebels, N. Giglietto, V. Gika, F. Gillardo, R. Gimenes, F. Giordano, E. Giro, M. Giroletti, Andrea Giuliani, M. Gjaja, J.F. Glicenstein, P. Gliwny, H. Goksu, P. Goldoni, J.L. Gomez, M.M. Gonzalez, Juan Manuel Gonzalez, K.S. Gothe, D. Gotz Coelho, T. Grabarczyk, R. Graciani, P. Grandi, G. Grasseau, D. Grasso, D. Green, J. Green, T. Greenshaw, P. Grespan, A. Grillo, M.H. Grondin, J. Grube, V. Guarino, B. Guest, O. Gueta, M. Günduz, S. Gunji, G. Gyuk, J. Hackfeld, D. Hadasch, L. Hagge, A. Hahn, J.E. Hajlaoui, A. Halim, P. Hamal, W. Hanlon, Y. Harada, M.J. Hardcastle, M. Harvey Collado, T. Haubold, A. Haupt, M. Havelka, K. Hayashi, M. Hayashida, H. He, L. Heckmann, M. Heller, F. Henault, Gilles Henri, G. Hermann, S. Hernández Cadena, J. Herrera Llorente, O. Hervet, J. Hinton, A. Hiramatsu, K. Hirotani, B. Hnatyk, R. Hnatyk, J.K. Hoang, D. H.H. Hoffmann, C. Hoischen, J. Holder, M. Holler, B. Hona, D. Horan, Dieter Horns, P. Horvath, J. Houles, M. Hrabovsky, D. Hrupec, Y. Huang, J.‑M. Huet, G. Hughes, G. Hull, T.B. Humensky, M. Hütten, M. Iarlori, J.M. Illa, R. Imazawa, T. Inada, F. Incardona, A. Ingallinera, S. Inoue, T. Inoue, Y. Inoue, F. Iocco, K. Ioka, M. Ionica, S. Iovenitti, A. Iriarte, K. Ishio, W. Ishizaki, Y. Iwamura, J. Jacquemier, M. Jacquemont, M. Jamrozy, P. Janecek, F. Jankowsky, A. JardinBlicq, C. Jarnot, P. Jean Martínez, L. Jocou, N. Jordana, M. Josselin, I. JungRichardt, F.J.P.A. Junqueira, C. Juramy Gilles, P. Kaaret, L.H.S. Kadowaki, M. Kagaya, R. Kankanyan, D. Kantzas, V. Karas, A. Karastergiou, S. Karkar, J. Kasperek, H. Katagiri, J. Kataoka, K. Katarzynski, S. Katsuda, N. Kawanaka, D. Kazanas, D. Kerszberg, B. Khélifi, M.C. Kherlakian, T.P. Kian, D.B. Kieda, T. Kihm, S. Kim, S. Kisaka, R. Kissmann, R. Kleijwegt, G. Kluge, W. Kluźniak, J. Knapp, A. Kobakhidze, Y. Kobayashi, B. Koch, J. Kocot, K. Kohri, N. Komin, A. Kong, K. Kosack, F. Krack, M. Krause, F. Krennrich, H. Kubo, V. N. Kudryavtsev, S. Kunwar, J. Kushida, P. Kushwaha, Barbera Parola, G. La Rosa, R. Lahmann, A. Lamastra, M. Landoni, D. Landriu, R.G. Lang, J. Lapington, P. Laporte, P. Lason, J. Lasuik, J. Lazendic Galloway, T. Le Flour, P. Le Sidaner, S. Leach, S.H. Lee, W.H. Lee, S. Lee Oliveira, A. Lemiere, M. Lemoine Goumard, J.P. Lenain, F. Leone, V. Leray, G. Leto, F. Leuschner, R. Lindemann, E. Lindfors, L. Linhoff, I. Liodakis, A. Lipniacka, M. Lobo, Thomas Lohse, S. Lombardi, A. Lopez, M. Lopez, R. Lopez Coto, F. Louis, M. Louys, F. Lucarelli, H. Ludwig Boudi, P.L. Luque Escamilla, M.C. Maccarone, E. Mach, A.J. Maciejewski, J. Mackey, P. Maeght, C. Maggio, G. Maier, P. Majumdar, M. Makariev, M. Mallamaci, R. Malta Nunes de Almeida, D. Malyshev, D. Mandat, G. Maneva, M. Manganaro, P. Manigot, K. Mannheim, N. Maragos, D. Marano, M. Marconi, A. Marcowith, M. Marculewicz, B. Marcun, J. Marin, N. Marinello, P. Marinos, S. Markoff, P. Marquez, G. Marsella, J. M. Martin, P. G. Martin, M. Martinez, G. Martinez, O. Martinez, H. Martinez Huerta, C. Marty, R. Marx, N. Masetti, P. Massimino, H. Matsumoto, N. Matthews, G. Maurin, W. Max Moerbeck, N. Maxted, M.N. Mazziotta, S.M. Mazzola, J.D. Mbarubucyeye, L. Mc Comb, I. McHardy, S. McKeague, S. McMuldroch, E. Medina, D. Medina Miranda, A. Melandri, C. Melioli, D. Melkumyan, S. Menchiari, S. Mereghetti, G. Merino Arevalo, E. Mestre, J.L. Meunier, T. Meures, S. Micanovic, M. Miceli, M. Michailidis, J. Michalowski, T. Miener, I. Mievre, J. D. Miller, T. Mineo, M. Minev, J.M. Miranda, A. Mitchell, T. Mizuno, B. A. Mode, R. Moderski, L. Mohrmann, E. Molinari, T. Montaruli, I. Monteiro, C. Moore, A. Moralejo, D. Morcuende Parrilla, E. Moretti, K. Mori, P. Moriarty, K. Morik, P. Morris, A. Morselli, K. Mosshammer, R. Mukherjee, J. Muller, C. Mundell, J. Mundet, T. Murach, A. Muraczewski, H. Muraishi, I. Musella, A. Musumarra, A. Nagai, S. Nagataki, T. Naito, T. Nakamori, K. Nakashima, K. Nakayama, N. Nakhjiri, G. Naletto, D. Naumann, L. Nava, M.A. Nawaz, H. Ndiyavala, D. Neise, L. Nellen, R. Nemmen, N. Neyroud, K. Ngernphat, T. Nguyen Trung, L. Nicastro, L. Nickel, J. Niemiec, D. Nieto, C. Nigro, M. Nikołajuk, D. Ninci, K. Noda, Y. Nogami, S. Nolan, R. P. Norris, D. Nosek, M. Nöthe, V. Novotny, S. Nozaki, F. Nunio, P. O'Brien, K. Obara, Y. Ohira, M. Ohishi, S. Ohm, T. Oka, N. Okazaki, A. Okumura, C. Oliver, G. Olivera, B. Olmi, M. Orienti, R. Orito, M. Orlandini, E. Orlando, J.P. Osborne, M. Ostrowski, N. Otte, E. Ovcharov, E. Owen, I. Oya, A. Ozieblo, M. Padovani, A. Pagliaro, A. Paizis, M. Palatiello, M. Palatka, E. Palazzi, J.‑L. Panazol, D. Paneque, S. Panny, Francesca Romana Pantaleo, M. Panter, M. Paolillo, A. Papitto, A. Paravac, J.M. Paredes, G. Pareschi, N. Parmiggiani, R.D. Parsons, P. Paśko, S. R. Patel, B. Patricelli, L. Pavletic, S. Pavy, A. Peer, M. Pecimotika, M.G. Pellegriti, P. Peñil Del Campo, A. Pepato, S. Perard, C. Perennes, M. Peresano, A. Perez Aguilera, J. Perez Romero, M.A. Perez Torres, M. Persic, P. O. Petrucci, O. Petruk, B. Peyaud, K. Pfrang, E. Pian, P. Piatteli, E. Pietropaolo, R. Pillera, D. Pimentel, F. Pintore, C. Pio Garcia, G. Pirola, F. Piron, S. Pita, M. Pohl, V. Poireau, A. Pollo, M. Polo, C. Pongkitivanichkul, J. Porthault, J. Powell, D. Pozo, R.R. Prado, E. Prandini, J. Prast, K. Pressard, G. Principe, N. Produit, D. Prokhorov, H. Prokoph, H. Przybilski, E. Pueschel, G. Pühlhofer, I. Puljak, M.L. Pumo, M. Punch, F. Queiroz, J. Quinn, A. Quirrenbach, P.J. Rajda, R. Rando, S. Razzaque, S. Recchia, P. Reichherzer, O. Reimer, A. Reisenegger, Q. Remy, M. Renaud, T. Reposeur, B. Reville, J.M. Reymond, J. Reynolds, D. Ribeiro, M. Ribo, G. Richards, J. Rico, F. Rieger, L. Riitano, M. Riquelme, D. Riquelme, S. Rivoire, V. Rizi, E. Roache, M. Roche, J. Rodriguez, G. Rodriguez Fernandez, J.C. Rodriguez Ramirez, J.J. Rodriguez Vazquez, G. Rojas, P. Romano, G. Romeo Lobato, C. Romoli, M. Roncadelli, J. Rosado, A. Rosales de Leon, G. Rowell, A. Rugliancich, J.E. Ruiz del Mazo, C. Rulten, C. Russell, F. Russo Hatlen, S. Safi Harb, L. Saha, V. Sahakian, S. Sailer, T. Saito, N. Sakaki, S. Sakurai, G. Salina, H. Salzmann, D. Sanchez, H. Sandaker, A. Sandoval, P. Sangiorgi, M. Sanguillon, H. Sano, M. Santander, A. Santangelo, R. Santos Lima, A. Sanuy, L. Sapozhnikov, T. Saric, S. Sarkar, H. Sasaki, N. Sasaki, Y. Sato, F.G. Saturni, M. Sawada, J. Schaefer, A. Scherer, J. Scherpenberg, P. Schipani, B. Schleicher, J. Schmoll, M. Schneider, H. Schoorlemmer, P. Schovanek, F. Schussler, B. Schwab, U. Schwanke, J. Schwarz, E. Sciacca, S. Scuderi, M. Seglar Arroyo, I. Seitenzahl, D. Semikoz, O. Sergijenko, J.E. Serna Franco, Karol Seweryn, V. Sguera, A. Shalchi, R.Y. Shang, P. Sharma, L. Sidoli, J. Sieiro, H. Siejkowski, A. Sillanpaa, B.B. Singh, K.K. Singh, A. Sinha, C. Siqueira, J. Sitarek, P. Sizun, V. Sliusar, D. Sobczynska, R.W. Sobrinho, H. Sol, G. Sottile, H. Spackman, S. Spencer, G. Spengler, D. Spiga, W. Springer, A. Stamerra, S. Stanic, R. Starling, Ł. Stawarz, Stanislav Stefanik, C. Stegmann, A. Steiner, S. Steinmassl, C. Stella, R. Sternberger, M. Sterzel, C. Stevens, B. Stevenson, T. Stolarczyk, G. Stratta, U. Straumann, J. Striskovic, M. Strzys, R. Stuik, M. Suchenek, Y. Sunada, Tiina Suomijarvi, T. Suric, H. Suzuki, P. Swierk, T. Szepieniec, K. Tachihara, G. Tagliaferri, H. Tajima, N. Tajima, D. Tak, H. Takahashi, M. Takahashi, J. Takata, R. Takeishi, T. Tam, M. Tanaka, T. Tanaka, S. Tanaka, M. Tavani, F. Tavecchio, T. Tavernier, A. Russ Taylor, L.A. Tejedor, P. Temnikov, K. Terauchi, J.C. Terrazas, R. Terrier, T. Terzic, M. Teshima, D. Thibaut, F. Thocquenne, W. Tian, L. Tibaldo, A. Tiengo, M. Tluczykont, C.J. Todero Peixoto, K. Toma, L. Tomankova, J. Tomastik, M. Tornikoski, D.F. Torres, E. Torresi, G. Tosti, L. Tosti, N. Tothill, F. Toussenel, G. Tovmassian, C. Trichard, M. Trifoglio, A. Trois, S. Truzzi, A. Tsiahina, B. Turk, A. Tutone, Y. Uchiyama, P. Utayarat, L. Vaclavek, M. Vacula, V. Vagelli, F. Vagnetti, J.A. Valdivia, M. Valentino, A. Valio, B. Vallage, P. Vallania Quispe, A.M. van den Berg, W. van Driel, C. van Eldik, C. van Rensburg, Brian van Soelen, J. Vandenbroucke, G. Vasileiadis, V. Vassiliev, M. Vazquez Acosta, M. Vecchi, A. Vega, J. Veh, P. Veitch, C. Venter, S. Ventura, S. Vercellone, V. Verguilov, G. Verna, S. Vernetto, V. Verzi, G.P. Vettolani, C. Veyssiere, I. Viale, A. Viana, N. Viaux, J. Vignatti, C.F. Vigorito, J. Villanueva, V. Vitale, V. Vittorini, V. Vodeb, N. Vogel, V. Voisin, S. Vorobiov, M. Vrastil, T. Vuillaume, S.J. Wagner, P. Wagner, K. Wakazono, S.P. Wakely, M. Ward, D. Warren, J. Watson, M. Wechakama, P. Wegner, A. Weinstein, C. Weniger, F. Werner, H. Wetteskind, M. L. White, A. Wierzcholska, S. Wiesand, R. Wijers, M. Wilkinson, M. Will, J. Williams, T. J. Williamson, A. Wolter, Y.W. Wong, M. Wood, T. Yamamoto, H. Yamamoto, Y. Yamane, R. Yamazaki, S. Yanagita, L. Yang, S. Yoo, T. Yoshida, T. Yoshikoshi, P. Yu, A. Yusafzai, Michael Zacharias, B. Zaldivar, L. Zampieri, R. Zanin, R. Zanmar Sanchez, D. Zaric, M. Zavrtanik, D. Zavrtanik, Andrzej Zdziarski, A. Zech, H. Zechlin, A. Zenin, A. Zerwekh, K. Ziętara, A. Zink, J. Ziolkowski, M. Zivec, A. Zmija, Współautorami artykułu są członkowie CTA Observatory, CTA Consortium i LST Collaboration w liczbie 1139, Astronomy, Research unit Nuclear & Hadron Physics, and Research unit Astroparticle Physics
- Subjects
Physics ,Observatory ,Gamma ray ,Astronomy - Abstract
Very-high Energy (VHE) gamma-ray astroparticle physics is a relatively young field, and observations over the past decade have surprisingly revealed almost two hundred VHE emitters which appear to act as cosmic particle accelerators. These sources are an important component of the Universe, influencing the evolution of stars and galaxies. At the same time, they also act as a probe of physics in the most extreme environments known - such as in supernova explosions, and around or after the merging of black holes and neutron stars. However, the existing experiments have provided exciting glimpses, but often falling short of supplying the full answer. A deeper understanding of the TeV sky requires a significant improvement in sensitivity at TeV energies, a wider energy coverage from tens of GeV to hundreds of TeV and a much better angular and energy resolution with respect to the currently running facilities. The next generation gamma-ray observatory, the Cherenkov Telescope Array Observatory (CTAO), is the answer to this need. In this talk I will present this upcoming observatory from its design to the construction, and its potential science exploitation. CTAO will allow the entire astronomical community to explore a new discovery space that will likely lead to paradigm-changing breakthroughs. In particular, CTA has an unprecedented sensitivity to short (sub-minute) timescale phenomena, placing it as a key instrument in the future of multi-messenger and multi-wavelength time domain astronomy. I will conclude the talk presenting the first scientific results obtained by the LST-1, the prototype of one CTAO telescope type - the Large-Sized Telescope, that is currently under commission., PoS: Proceedings of Science, 395, ISSN:1824-8039, Proceedings of 37th International Cosmic Ray Conference (ICRC2021)
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- 2022
9. Why Have Many of the Brightest Radio-loud Blazars Not Been Detected in Gamma-Rays by Fermi?
- Author
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M. L. Lister, M. F. Aller, H. D. Aller, T. Hovatta, W. Max-Moerbeck, A. C. S. Readhead, J. L. Richards, E. Ros, Aalto-yliopisto, and Aalto University
- Subjects
Astrofísica ,Active galactic nucleus ,media_common.quotation_subject ,Astrophysics::High Energy Astrophysical Phenomena ,jets [galaxies] ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,general [gamma-ray burst] ,7. Clean energy ,01 natural sciences ,law.invention ,symbols.namesake ,law ,0103 physical sciences ,Blazar ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,general [quasars] ,010308 nuclear & particles physics ,Scattering ,Spectral density ,Astronomy and Astrophysics ,galaxies [radio continuum] ,Synchrotron ,13. Climate action ,Space and Planetary Science ,Sky ,active [galaxies] ,Astronomia ,symbols ,Doppler effect ,Fermi Gamma-ray Space Telescope - Abstract
We use the complete MOJAVE 1.5 Jy sample of active galactic nuclei (AGNs) to examine the gamma-ray detection statistics of the brightest radio-loud blazars in the northern sky. We find that 23% of these AGNs were not detected above 0.1 GeV by the Fermi-LAT during the four-year 3FGL catalog period partly because of an instrumental selection effect and partly due to their lower Doppler boosting factors. Blazars with synchrotron peaks in their spectral energy distributions located below 10^(13.4) Hz also tend to have high-energy peaks that lie below the 0.1 GeV threshold of the LAT, and are thus less likely to be detected by Fermi. The non-detected AGNs in the 1.5 Jy sample also have significantly lower 15 GHz radio modulation indices and apparent jet speeds, indicating that they have lower than average Doppler factors. Since the effective amount of relativistic Doppler boosting is enhanced in gamma-rays (particularly in the case of external inverse-Compton scattering), this makes them less likely to appear in the 3FGL catalog. Based on their observed properties, we have identified several bright radio-selected blazars that are strong candidates for future detection by Fermi.
- Published
- 2015
10. The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies
- Author
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MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, Italy), M. Asensio(Universidad Complutense, Spain), M. Backes(Technische Universität Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, München, Germany), J. A. Barrio(Universidad Complutense, Spain), W. Bednarek(University of Łódź, Poland), K. Berger(Inst. de Astrofísica de Canarias, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, Spain), R. K. Bock(Max-Planck-Institut für Physik, München, Germany), A. Boller(ETH Zurich, Switzerland), S. Bonnefoy(Universidad Complutense, Spain), G. Bonnoli(INAF National Institute for Astrophysics, Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, München, Germany), T. Bretz(Universität Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), A. Carosi(INAF National Institute for Astrophysics, Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. L. Contreras(Universidad Complutense, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, Spain), L. Cossio(Università di Udine, and INFN Trieste, Italy), S. Covino(INAF National Institute for Astrophysics, Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, Italy), F. Dazzi(Università di Udine, and INFN Trieste, Italy), A. De Angelis(Università di Udine, and INFN Trieste, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), M. Doert(Technische Universität Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Dorner(Universität Würzburg, Germany), M. Doro(Universitat Autònoma de Barcelona, Spain), D. Eisenacher(Universität Würzburg, Germany), D. Elsaesser(Universität Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), M. V. Fonseca(Universidad Complutense, Spain), L. Font(Universitat Autònoma de Barcelona, Spain), C. Fruck(Max-Planck-Institut für Physik, München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, Spain), M. Gaug(Universitat Autònoma de Barcelona, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. Hose(Max-Planck-Institut für Physik, München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), F. Jankowski(Deutsches Elektronen-Synchrotron), V. Kadenius(Tuorla Observatory, University of Turku, Finland), S. Klepser(IFAE, Edifici Cn., Campus UAB, Spain), M. L. Knoetig(Max-Planck-Institut für Physik, München, Germany), T. Krähenbühl(ETH Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, Italy), N. Lewandowska(Universität Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, Finland), S. Lombardi(INAF National Institute for Astrophysics, Rome, Italy), M. López(Universidad Complutense, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, Spain), E. Lorenz(Max-Planck-Institut für Physik, München, Germany), I. Lozano(Universidad Complutense, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, Italy), K. Mannheim(Universität Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, Spain), J. Masbou(Università di Padova and INFN Padova, Italy), D. Mazin(Max-Planck-Institut für Physik, München, Germany), M. Meucci(Università di Siena, and INFN Pisa, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Max-Planck-Institut für Physik, München, Germany), A. Niedzwiecki(University of Łódź, Poland), D. Nieto(Universidad Complutense, Spain), K. Nilsson(Tuorla Observatory, University of Turku, Finland), N. Nowak(Max-Planck-Institut für Physik, München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, Italy), D. Paneque(Max-Planck-Institut für Physik, München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, Italy), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, Italy), M. Persic(Università di Udine, and INFN Trieste, Italy), M. Pilia(Università dell'Insubria, Como, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, Italy), E. Prandini(Università di Padova and INFN Padova, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, Spain), R. Reinthal(Tuorla Observatory, University of Turku, Finland), W. Rhode(Technische Universität Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, Barcelona, Spain), S. Rügamer(Universität Würzburg, Germany), A. Saggion(Università di Padova and INFN Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), T. Y. Saito(Max-Planck-Institut für Physik, München, Germany), M. Salvati(INAF National Institute for Astrophysics, Rome, Italy), K. Satalecka(Universidad Complutense, Spain), V. Scalzotto(Università di Padova and INFN Padova, Italy), V. Scapin(Universidad Complutense, Spain), C. Schultz(Università di Padova and INFN Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Sobczynska(University of Łódź, Poland), F. Spanier(Universität Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, Spain), A. Stamerra(Università di Siena, and INFN Pisa, Italy), B. Steinke(Max-Planck-Institut für Physik, München, Germany), J. Storz(Universität Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), L. Takalo(Tuorla Observatory, University of Turku, Finland), H. Takami(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), F. Tavecchio(INAF National Institute for Astrophysics, Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, München, Germany), O. Tibolla(Universität Würzburg, Germany), D. F. Torres(ICREA, Barcelona, Spain), T. Toyama(Max-Planck-Institut für Physik, München, Germany), A. Treves(Università dell'Insubria, Como, Italy), M. Uellenbeck(Technische Universität Dortmund, Germany), P. Vogler(ETH Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, München, Germany), Q. Weitzel(ETH Zurich, Switzerland), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), The MAGIC Collaboration(Università di Trieste, and INFN Trieste, Italy), F. Longo(Università di Trieste, and INFN Trieste, Italy), F. Lucarelli(Agenzia Spaziale Italiana), C. Pittori(Agenzia Spaziale Italiana), S. Vercellone(INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy), for the AGILE team(Università di Padova and INFN Padova, Italy), D. Bastieri(Università di Padova and INFN Padova, Italy), C. Sbarra(INFN Padova, Italy), for the Fermi-LAT Collaboration(Max-Planck-Institut für Radioastronomie, Germany), E. Angelakis(Max-Planck-Institut für Radioastronomie, Germany), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Germany), I. Nestoras(Max-Planck-Institut für Radioastronomie, Germany), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Germany), A. Sievers(Instituto de Radio Astronoma Milimétrica, Spain), J. A. Zensus(Max-Planck-Institut für Radioastronomie, Germany), for the F-GAMMA program(Crimean Astrophysical Observatory, Ukraine), K. A. Antonyuk(Crimean Astrophysical Observatory, Ukraine), W. Baumgartner(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), A. Berduygin(Tuorla Observatory, University of Turku, Finland), M. Carini(Department of Physics and Astronomy, Western Kentucky University, USA), K. Cook(Department of Physics and Astronomy, Western Kentucky University, USA), N. Gehrels(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Kadler(Universität Würzburg, Germany), Yu. A. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), Y. Y. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), F. Krauss(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), H. A. Krimm(Universities Space Research Association, Columbia, MD 21044, USA), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory, Finland), M. L. Lister(Department of Physics, Purdue University, USA), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), M. Pasanen(Tuorla Observatory, University of Turku, Finland), A. B. Pushkarev(Pulkovo Observatory, St. Petersburg, Russia), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), J. L. Richards(Department of Physics, Purdue University, USA), J. Sainio(Tuorla Observatory, University of Turku, Finland), D. N. Shakhovskoy(Crimean Astrophysical Observatory, Ukraine), K. V. Sokolovsky(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), M. Tornikoski(Aalto University Metsähovi Radio Observatory, Finland), J. Tueller(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Weidinger(Theoretische Physik IV, Ruhr-Universität Bochum, Germany), J. Wilms(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), INAF-Cagliari Astronomical Observatory, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Università degli Studi di Udine - University of Udine [Italie], Universita degli studi di Napoli 'Parthenope' [Napoli], Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Vecteurs - Infections tropicales et méditerranéennes (VITROME), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées (IRBA), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), DAAA, ONERA, Université Paris Saclay (COmUE) [Meudon], ONERA-Université Paris-Saclay, University of Bath [Bath], Waves and Solitons LLC, 918 W. Windsong Dr., Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, E., Leonardo, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, D., Nieto, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, M., Pilia, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, S., Rügamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, S., Vercellone, D., Bastieri, C., Sbarra, E., Angelaki, L., Fuhrmann, I., Nestora, T. P., Krichbaum, A., Siever, J. A., Zensu, K. A., Antonyuk, W., Baumgartner, A., Berduygin, M., Carini, K., Cook, N., Gehrel, M., Kadler, Kovalev, Y. u. A., Y. Y., Kovalev, F., Krau, H. A., Krimm, A., Lähteenmäki, M. L., Lister, W., Max Moerbeck, M., Pasanen, A. B., Pushkarev, A. C. S., Readhead, J. L., Richard, J., Sainio, D. N., Shakhovskoy, K. V., Sokolovsky, M., Tornikoski, J., Tueller, M., Weidinger, J., Wilms, UAM. Departamento de Física Teórica, Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées [Brétigny-sur-Orge] (IRBA), Universitat Autònoma de Barcelona [Barcelona] (UAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Helmholtz-Gemeinschaft, National Institute for Nuclear Physics (INFN), National Academy of Sciences of Armenia, The Netherlands Institute for Radio Astronomy (ASTRON), 7990-AA Dwingeloo, Netherlands, Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), INAF-OAB, and DAAA, ONERA, Université Paris Saclay [Meudon]
- Subjects
galaxies [Gamma rays] ,Radiation mechanisms: non-thermal ,Flux ,Astrophysics ,01 natural sciences ,LARGE-AREA TELESCOPE ,law.invention ,law ,[PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex] ,BL Lacertae objects: individual: 1ES 2344+514 ,MAGIC (telescope) ,010303 astronomy & astrophysics ,galaxies: active ,BL Lacerae objects: individual: 1ES 2344+514 ,gamma rays: galaxies ,X-rays: individuals: 1ES 2344+514 ,radiation mechanisms: non-thermal ,ComputingMilieux_MISCELLANEOUS ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,astro-ph.HE ,ACTIVE GALACTIC NUCLEI ,BL-LACERTAE OBJECTS ,GAMMA-RAY EMISSION ,SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS ,SELF-COMPTON MODEL ,X-RAY ,LAC OBJECTS ,RELATIVISTIC JETS ,MARKARIAN 501 ,Gamma ray ,non-thermal [radiation mechanisms] ,active [galaxies] ,astro-ph.CO ,Spectral energy distribution ,Electrónica ,Física nuclear ,Electricidad ,Astrophysics - High Energy Astrophysical Phenomena ,Flare ,Astrophysics - Cosmology and Nongalactic Astrophysics ,[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Astrophysics::High Energy Astrophysical Phenomena ,education ,FOS: Physical sciences ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,0103 physical sciences ,galaxie [gamma rays] ,010308 nuclear & particles physics ,Física ,Astronomy and Astrophysics ,Light curve ,individual: 1ES 2344+514 [BL Lacertae objects] ,[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA] ,galaxies [gamma-rays] ,Space and Planetary Science ,ddc:520 ,individuals: 1ES 2344+514 [X-rays] ,Fermi Gamma-ray Space Telescope - Abstract
Astronomy and Astrophysics 556 (2013): A67 reproduced with permission from Astronomy and Astrophysics, Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states. Aims.We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods.The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Metsähovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign, The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The AGILE Mission is funded by the Italian Space Agency (ASI), with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A.Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged
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- 2013
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11. Near real-time astrometry for spacecraft navigation with the VLBA: A demonstration with the Mars Reconnaissance Orbiter and Odyssey
- Author
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Walter Brisken, Jonathan D. Romney, and W. Max-Moerbeck
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Spacecraft ,business.industry ,media_common.quotation_subject ,FOS: Physical sciences ,Astronomy and Astrophysics ,Quasar ,Astrometry ,Mars Exploration Program ,Ephemeris ,law.invention ,Orbiter ,Space and Planetary Science ,law ,Sky ,business ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Geology ,Remote sensing ,media_common - Abstract
We present a demonstration of near real-time spacecraft astrometry with the VLBA. We detect the X-band downlink signal from Mars Reconnaissance Orbiter and Odyssey with the VLBA and transmit the data over the internet for correlation at the VLBA correlator in near real-time. Quasars near Mars in the plane of the sky are used as position references. In the demonstration we were able to obtain initial position measurements within about 15 minutes of the start of the observation. The measured positions differ from the projected ephemerides by a few milliarcseconds, and the repeatability of the measurement is better than 0.3 milliarcseconds as determined from measurements from multiple scans. We demonstrate that robust and repeatable offsets are obtained even when removing half of the antennas. These observations demonstrate the feasibility of astrometry with the VLBA with a low latency and sub-milliarcsecond repeatability., 10 pages, 2 figures and 5 tables. Accepted for publication in PASP
- Published
- 2015
12. The 2009 multiwavelength campaign on Mrk 421: Variability and correlation studies
- Author
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MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Mu\ noz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Longo(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(6,32,*), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS collaboration(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), (Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. Archambault(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. H. Buckley(Department of Physics, Washington University, St. Louis, MO 63130, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), J. D. Eisch(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(DESY, Platanenallee 6, 15738 Zeuthen, Germany), Q. Feng(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), H. Fleischhack(Deutsches Elektronen-Synchrotron), P. Fortin(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), G. Hughes(Deutsches Elektronen-Synchrotron), T. B. Humensky(Physics Department, Columbia University, New York, NY 10027, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), Y. Khassen(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), F. Krennrich(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), S. Kumar(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), G. Maier(Deutsches Elektronen-Synchrotron), S. McArthur(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), N. Park(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), K. Ragan(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. C. Rovero(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), G. H. Sembroski(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. V. Tucci(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. Weinstein(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), R. Welsing(Deutsches Elektronen-Synchrotron), A. Wilhelm(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), W. P. Chen(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), B. Jordan(School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, 2, Ireland), E. Koptelova(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), B. McBreen(University College Dublin, Belfield, Dublin 4, Ireland), V. M. Larionov(Isaac Newton Institute of Chile, St. Petersburg Branch, St. Petersburg, Russia), C. S. Lin(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), E. Angelakis(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Capalbi(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), A. Carrami\ nana(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), L. Carrasco(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), P. Cassaro(INAF Istituto di Radioastronomia, Sezione di Noto, Contrada Renna Bassa, 96017 Noto), A. Cesarini(Department of Physics, University of Trento, I38050, Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), T. Hovatta(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), H. A. Krimm(Astro Space Center of the Lebedev Physical Institute, 117997 Moscow, Russia), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. W. Moody(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), G. Maccaferri(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), Y. Mori(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), I. Nestoras(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), A. Orlati(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), C. Pace(Indiana University, Department of Astronomy, Swain Hall West 319, Bloomington, IN 47405-7105, USA), R. Pearson(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), M. Perri(INAF National Institute for Astrophysics, I-00136 Rome, Italy), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. L. Richards(Department of Physics, Purdue University, 525 Northwestern Ave, West Lafayette, IN 47907), A. C. Sadun(Department of Physics, University of Colorado, Denver, CO 80220, USA), T. Sakamoto(Department of Physics and Mathematics, College of Science and 952 Engineering, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuoku, Sagamihara-shi Kanagawa 252-5258, Japan), J. Tammi(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), Y. Yatsu(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), A. Zook(Department of Physics and Astronomy, Pomona College, Claremont CA 91711-6312, USA), Aleksić, J, Ansoldi, Stefano, Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bock, R. K., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Carreto Fidalgo, D., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., Delgado Mendez, C., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Farina, E., Ferenc, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Hadamek, A., Hadasch, D., Herrero, A., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Knoetig, M. L., Krause, J., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Longo, Francesco, Lombardi, S., López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Meucci, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nowak, N., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Partini, S., Persic, M., Prada, F., Prada Moroni, P. G., Prandini, E., Preziuso, S., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguezgarcia, J., Rügamer, S., Saggion, A., Saito, K., Salvati, M., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Sun, S., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Wagner, R. M., Zandanel, F., Zanin, R., Archambault, S., Behera, B., Beilicke, M., Benbow, W., Bird, R., Buckley, J. H., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Collins Hughes, E., Cui, W., Dumm, J., Eisch, J. D., Falcone, A., Federici, S., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Furniss, A., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Hanna, D., Holder, J., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krawczynski, H., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Mukherjee, R., Ong, R. A., Otte, A. N., Park, N., Pichel, A., Pohl, M., Popkow, A., Prokoph, H., Quinn, J., Ragan, K., Rajotte, J., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Theiling, M., Tucci, J. V., Tyler, J., Varlotta, A., Wakely, S. P., Weekes, T. C., Weinstein, A., Welsing, R., Wilhelm, A., Williams, D. A., Zitzer, B., Villata, M., Raiteri, C., Aller, H. D., Aller, M. F., Chen, W. P., Jordan, B., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Mcbreen, B., Larionov, V. M., Lin, C. S., Nikolashvili, M. G., Angelakis, E., Capalbi, M., Carramiñana, A., Carrasco, L., Cassaro, P., Cesarini, A., Fuhrmann, L., Giroletti, M., Hovatta, T., Krichbaum, T. P., Krimm, H. A., Max Moerbeck, W., Moody, J. W., Maccaferri, G., Mori, Y., Nestoras, I., Orlati, A., Pace, C., Pearson, R., Perri, M., Readhead, A. C. S., Richards, J. L., Sadun, A. C., Sakamoto, T., Tammi, J., Tornikoski, M., Yatsu, Y., Zook, A., Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Universitat de Barcelona
- Subjects
Astrofísica ,Brightness ,Ciencias Físicas ,blazars ,Astrophysics ,telescope ,x-ray variability ,01 natural sciences ,Spectral line ,BL Lacertae objects ,individual ,Mrk 421 ,purl.org/becyt/ford/1 [https] ,Raigs gamma ,emission ,MAGIC (telescope) ,010303 astronomy & astrophysics ,Physics ,astro-ph.HE ,High Energy Astrophysical Phenomena (astro-ph.HE) ,individual: Mrk 421 [BL Lacertae objects] ,Galaxies: BL Lacertae objects: individual: Markarian 421 ,Spectral energy distribution ,Electrónica ,Electricidad ,Astrophysics - High Energy Astrophysical Phenomena ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,power spectra ,BL Lacertae object ,tev photons ,0103 physical sciences ,Nucli galàctic actiu ,bl lacertae objects: individual: mrk 421 ,Blazar ,Astronomy and Astrophysics ,Space and Planetary Science ,Active galactic nuclei ,010308 nuclear & particles physics ,light curves ,Gamma rays ,Institut für Physik und Astronomie ,purl.org/becyt/ford/1.3 [https] ,Light curve ,Galaxies ,Galàxies ,Astronomía ,Crab Nebula ,optical variability ,active galactic nuclei ,Galàxies actives ,Active galaxies ,markarian-421 ,ddc:520 - Abstract
We performed a 4.5-month multi-instrument campaign (from radio to VHE gamma rays) on Mrk421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical/UV and X-rays extending over the duration of the campaign. The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multi-wavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk421 during non-flaring activity. Such a temporally extended X-ray/VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies., Comment: Accepted for publication in A&A, 18 pages, 14 figures (v2 has a small modification in the acknowledgments, and also corrects a typo in the field "author" in the metadata)
- Published
- 2015
- Full Text
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13. 15 GHz Monitoring of Gamma-ray Blazars with the OVRO 40 Meter Telescope in Support of Fermi
- Author
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J. L. Richards, W. Max-Moerbeck, V. Pavlidou, T. J. Pearson, A. C. S. Readhead, M. A. Stevenson, S. E. Healey, R. W. Romani, M. S. Shaw, L. Fuhrmann, E. Angelakis, J. A. Zensus, K. Grainge, G. B. Taylor, J. D. Scargle, A. Comastri, L. Angelini, M. Cappi, Comastri, Andrea, Cappi, Massimo, and Angelini, L.
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,Gamma ray ,FOS: Physical sciences ,020206 networking & telecommunications ,02 engineering and technology ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Light curve ,Monitoring program ,law.invention ,Telescope ,Spitzer Space Telescope ,law ,0202 electrical engineering, electronic engineering, information engineering ,020201 artificial intelligence & image processing ,Blazar ,Noise (radio) ,Astrophysics::Galaxy Astrophysics ,Fermi Gamma-ray Space Telescope ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present results from the first two years of our fast-cadence 15 GHz gamma-ray blazar monitoring program, part of the F-GAMMA radio monitoring project. Our sample includes the 1158 blazars north of -20 degrees declination from the Candidate Gamma-Ray Blazar Survey (CGRaBS), which encompasses a significant fraction of the extragalactic sources detected by the Fermi Gamma-ray Space Telescope. We introduce a novel likelihood analysis for computing a time series variability amplitude statistic that separates intrinsic variability from measurement noise and produces a quantitative error estimate. We use this method to characterize our radio light curves. We also present results indicating a statistically significant correlation between simultaneous average 15 GHz radio flux density and gamma-ray photon flux., 5 pages, 7 figures; 2009 Fermi Symposium; eConf Proceedings C091122
- Published
- 2009
14. Fermi/large area telescope discovery of gamma-ray emission from a relativistic jet in the narrow-line quasar pmn j0948+0022
- Author
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A. A. Abdo, M. Ackermann, M. Ajello, M. Axelsson, L. Baldini, J. Ballet, G. Barbiellini, D. Bastieri, M. Battelino, B. M. Baughman, K. Bechtol, R. Bellazzini, E. D. Bloom, E. Bonamente, A. W. Borgland, J. Bregeon, A. Brez, M. Brigida, P. Bruel, G. A. Caliandro, R. A. Cameron, P. A. Caraveo, J. M. Casandjian, E. Cavazzuti, C. Cecchi, A. Chekhtman, C. C. Cheung, J. Chiang, S. Ciprini, R. Claus, J. Cohen Tanugi, W. Collmar, J. Conrad, L. Costamante, C. D. Dermer, A. d. Angelis, F. d. Palma, S. W. Digel, E. D. E. Silva, P. S. Drell, R. Dubois, D. Dumora, C. Farnier, C. Favuzzi, W. B. Focke, L. Foschini, M. Frailis, L. Fuhrmann, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, N. Gehrels, S. Germani, B. Giebels, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, I. A. Grenier, M. H. Grondin, J. E. Grove, L. Guillemot, S. Guiriec, Y. Hanabata, A. K. Harding, R. C. Hartman, M. Hayashida, E. Hays, R. E. Hughes, G. Johannesson, A. S. Johnson, R. P. Johnson, W. N. Johnson, T. Kamae, H. Katagiri, J. Kataoka, M. Kerr, J. Knodlseder, F. Kuehn, M. Kuss, J. Lande, L. Latronico, M. Lemoine Goumard, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, A. Makeev, W. Max Moerbeck, M. N. Mazziotta, W. McConville, J. E. McEnery, C. Meurer, P. F. Michelson, W. Mitthumsiri, T. Mizuno, C. Monte, M. E. Monzani, A. Morselli, I. V. Moskalenko, S. Murgia, P. L. Nolan, J. P. Norris, E. Nuss, T. Ohsugi, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, J. H. Panetta, D. Parent, V. Pavlidou, T. J. Pearson, M. Pepe, M. Pesce Rollins, F. Piron, T. A. Porter, S. Raino, R. Rando, M. Razzano, A. Readhead, A. Reimer, O. Reimer, T. Reposeur, J. L. Richards, S. Ritz, A. Y. Rodriguez, R. W. Romani, F. Ryde, H. F. W. Sadrozinski, R. Sambruna, D. Sanchez, A. Sander, P. M. S. Parkinson, J. D. Scargle, T. L. Schalk, C. Sgro, D. A. Smith, G. Spandre, P. Spinelli, J. L. Starck, M. Stevenson, M. S. Strickman, D. J. Suson, G. Tagliaferri, H. Takahashi, T. Tanaka, J. G. Thayer, D. J. Thompson, L. Tibaldo, O. Tibolla, D. F. Torres, G. Tosti, A. Tramacere, Y. Uchiyama, T. L. Usher, N. Vilchez, V. Vitale, A. P. Waite, B. L. Winer, K. S. Wood, T. Ylinen, J. A. Zensus, M. Ziegler, G. Ghisellini, L. Maraschi, F. Tavecchio, E. Angelakis, LONGO, FRANCESCO, Abdo, A. A., Ackermann, M., Ajello, M., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Battelino, M., Baughman, B. M., Bechtol, K., Bellazzini, R., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Collmar, W., Conrad, J., Costamante, L., Dermer, C. D., Angelis, A. d., Palma, F. d., Digel, S. W., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Focke, W. B., Foschini, L., Frailis, M., Fuhrmann, L., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Giebels, B., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Hanabata, Y., Harding, A. K., Hartman, R. C., Hayashida, M., Hays, E., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knodlseder, J., Kuehn, F., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Max Moerbeck, W., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pavlidou, V., Pearson, T. J., Pepe, M., Pesce Rollins, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Razzano, M., Readhead, A., Reimer, A., Reimer, O., Reposeur, T., Richards, J. L., Ritz, S., Rodriguez, A. Y., Romani, R. W., Ryde, F., Sadrozinski, H. F. W., Sambruna, R., Sanchez, D., Sander, A., Parkinson, P. M. S., Scargle, J. D., Schalk, T. L., Sgro, C., Smith, D. A., Spandre, G., Spinelli, P., Starck, J. L., Stevenson, M., Strickman, M. S., Suson, D. J., Tagliaferri, G., Takahashi, H., Tanaka, T., Thayer, J. G., Thompson, D. J., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Usher, T. L., Vilchez, N., Vitale, V., Waite, A. P., Winer, B. L., Wood, K. S., Ylinen, T., Zensus, J. A., Ziegler, M., Ghisellini, G., Maraschi, L., Tavecchio, F., and Angelakis, E.
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Continuum (design consultancy) ,Fermi satellite ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Gamma rays: observations ,01 natural sciences ,High Energy Gamma-ray Astronomy ,law.invention ,Telescope ,Spitzer Space Telescope ,law ,0103 physical sciences ,Galaxies: active ,Blazar ,010303 astronomy & astrophysics ,Quasars ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Quasar ,Active Galactic Nuclei ,Black hole ,13. Climate action ,Space and Planetary Science ,Spectral energy distribution ,Fermi Gamma-ray Space Telescope - Abstract
We report the discovery by the Large Area Telescope (LAT) onboard the Fermi Gamma-Ray Space Telescope of high-energy. gamma-ray emission from the peculiar quasar PMN J0948+0022 (z = 0.5846). The optical spectrum of this object exhibits rather narrow H beta (FWHM(H beta) similar to 1500 km s(-1)), weak forbidden lines, and is therefore classified as a narrow-line type I quasar. This class of objects is thought to have relatively small black hole mass and to accrete at a high Eddington ratio. The radio loudness and variability of the compact radio core indicate the presence of a relativistic jet. Quasi-simultaneous radio/optical/X-ray and gamma-ray observations are presented. Both radio and gamma-ray emissions (observed over five months) are strongly variable. The simultaneous optical and X-ray data from Swift show a blue continuum attributed to the accretion disk and a hard X-ray spectrum attributed to the jet. The resulting broadband spectral energy distribution (SED) and, in particular, the gamma-ray spectrum measured by Fermi are similar to those of more powerful Flat-Spectrum Radio Quasars (FSRQs). A comparison of the radio and gamma-ray characteristics of PMN J0948+0022 with the other blazars detected by LAT shows that this source has a relatively low radio and gamma-ray power with respect to other FSRQs. The physical parameters obtained from modeling the SED also fall at the low power end of the FSRQ parameter region discussed in Celotti & Ghisellini. We suggest that the similarity of the SED of PMN J0948+0022 to that of more massive and more powerful quasars can be understood in a scenario in which the SED properties depend on the Eddington ratio rather than on the absolute power.
- Published
- 2009
15. MOJAVE. XVII. Jet Kinematics and Parent Population Properties of Relativistically Beamed Radio-loud Blazars.
- Author
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M. L. Lister, D. C. Homan, T. Hovatta, K. I. Kellermann, S. Kiehlmann, Y. Y. Kovalev, W. Max-Moerbeck, A. B. Pushkarev, A. C. S. Readhead, E. Ros, and T. Savolainen
- Subjects
RADIO galaxies ,LOUDNESS ,ACTIVE galactic nuclei ,KINEMATICS ,MONTE Carlo method ,PARAMETERS (Statistics) - Abstract
We present results from a parsec-scale jet kinematics study of 409 bright radio-loud active galactic nuclei (AGNs) based on 15 GHz Very Long Baseline Array (VLBA) data obtained between 1994 August 31 and 2016 December 26 as part of the 2 cm VLBA survey and Monitoring Of Jets in Active galactic nuclei with VLBA Experiments (MOJAVE) programs. We tracked 1744 individual bright features in 382 jets over at least 5 epochs. A majority (59%) of the best-sampled jet features showed evidence of accelerated motion at the >3σ level. Although most features within a jet typically have speeds within ∼40% of a characteristic median value, we identified 55 features in 42 jets that had unusually slow pattern speeds, nearly all of which lie within 4 pc (100 pc deprojected) of the core feature. Our results, combined with other speeds from the literature, indicate a strong correlation between apparent jet speed and synchrotron peak frequency, with the highest jet speeds being found only in low-peaked AGNs. Using Monte Carlo simulations, we find best-fit parent population parameters for a complete sample of 174 quasars above 1.5 Jy at 15 GHz. Acceptable fits are found with a jet population that has a simple unbeamed power-law luminosity function incorporating pure luminosity evolution and a power-law Lorentz factor distribution ranging from 1.25 to 50 with slope −1.4 ± 0.2. The parent jets of the brightest radio quasars have a space density of 261 ± 19 Gpc
−3 and unbeamed 15 GHz luminosities above ∼1024.5 W Hz−1 , consistent with FR II class radio galaxies. [ABSTRACT FROM AUTHOR]- Published
- 2019
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16. The Peculiar Light Curve of J1415+1320: A Case Study in Extreme Scattering Events.
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H. K. Vedantham, A. C. S. Readhead, T. Hovatta, L. V. E. Koopmans, T. J. Pearson, R. D. Blandford, M. A. Gurwell, A. Lähteenmäki, W. Max-Moerbeck, V. Pavlidou, V. Ravi, R. A. Reeves, J. L. Richards, M. Tornikoski, and J. A. Zensus
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LIGHT curves ,PECULIAR stars ,SCATTERING (Physics) ,GRAVITATIONAL lenses ,STELLAR parallax ,EXTRAGALACTIC distances - Abstract
The radio light curve of J1415+1320 (PKS 1413+135) shows time-symmetric and recurring U-shaped features across the centimeter-wave and millimeter-wave bands. The symmetry of these features points to lensing by an intervening object as the cause. U-shaped events in radio light curves in the centimeter-wave band have previously been attributed to Extreme scattering events (ESE). ESEs are thought to be the result of lensing by compact plasma structures in the Galactic interstellar medium, but the precise nature of these plasma structures remains unknown. Since the strength of a plasma lens evolves with wavelength λ as , the presence of correlated variations at over a wide wavelength range casts doubt on the canonical ESE interpretation for J1415+1320. In this paper, we critically examine the evidence for plasma lensing in J1415+1320. We compute limits on the lensing strength and the associated free–free opacity of the putative plasma lenses. We compare the observed and model ESE light curves, and also derive a lower limit on the lens distance based on the effects of parallax due to the Earth’s orbit around the Sun. We conclude that plasma lensing is not a viable interpretation for J1415+1320's light curves and that symmetric U-shaped features in the radio light curves of extragalactic sources do not present prima facie evidence for ESEs. The methodology presented here is generic enough to be applicable to any plasma-lensing candidate. [ABSTRACT FROM AUTHOR]
- Published
- 2017
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17. Symmetric Achromatic Variability in Active Galaxies: A Powerful New Gravitational Lensing Probe?
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H. K. Vedantham, A. C. S. Readhead, T. Hovatta, T. J. Pearson, R. D. Blandford, M. A. Gurwell, A. Lähteenmäki, W. Max-Moerbeck, V. Pavlidou, V. Ravi, R. A. Reeves, J. L. Richards, M. Tornikoski, and J. A. Zensus
- Subjects
ACTIVE galaxies ,ACHROMATISM ,GRAVITATIONAL lenses ,LIGHT curves ,BLACK holes ,INTERPLANETARY medium - Abstract
We report the discovery of a rare new form of long-term radio variability in the light curves of active galaxies (AG)—symmetric achromatic variability (SAV)—a pair of opposed and strongly skewed peaks in the radio flux density observed over a broad frequency range. We propose that SAV arises through gravitational milli-lensing when relativistically moving features in AG jets move through gravitational lensing caustics created by subhalo condensates or black holes located within intervening galaxies. The lower end of this mass range has been inaccessible with previous gravitational lensing techniques. This new interpretation of some AG variability can easily be tested and if it passes these tests, will enable a new and powerful probe of cosmological matter distribution on these intermediate-mass scales, as well as provide, for the first time, micro-arcsecond resolution of the nuclei of AG—a factor of 30–100 greater resolution than is possible with ground-based millimeter very-long-baseline interferometry. [ABSTRACT FROM AUTHOR]
- Published
- 2017
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18. A SEARCH FOR SUB-SECOND RADIO VARIABILITY PREDICTED TO ARISE TOWARD 3C 84 FROM INTERGALACTIC DISPERSION.
- Author
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C. A. Hales, W. Max-Moerbeck, D. A. Roshi, and M. P. Rupen
- Subjects
- *
LIGHT sources , *ELECTROMAGNETIC waves , *SPECTRUM analysis , *HELIOSPHERE , *SOLAR corona - Abstract
We empirically evaluate the scheme proposed by Lieu & Duan in which the light curve of a time-steady radio source is predicted to exhibit increased variability on a characteristic timescale set by the sightline’s electron column density. Application to extragalactic sources is of significant appeal, as it would enable a unique and reliable probe of cosmic baryons. We examine temporal power spectra for 3C 84, observed at 1.7 GHz with the Karl G. Jansky Very Large Array and the Robert C. Byrd Green Bank Telescope. These data constrain the ratio between standard deviation and mean intensity for 3C 84 to less than 0.05% at temporal frequencies ranging between 0.1 and 200 Hz. This limit is 3 orders of magnitude below the variability predicted by Lieu & Duan and is in accord with theoretical arguments presented by Hirata & McQuinn rebutting electron density dependence. We identify other spectral features in the data consistent with the slow solar wind, a coronal mass ejection, and the ionosphere. [ABSTRACT FROM AUTHOR]
- Published
- 2016
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19. The ordinary life of the gamma-ray emitting narrow-line Seyfert 1 galaxy PKS 1502+036
- Author
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D'Ammando, F., Orienti, M., Giroletti, M., Dallacasa, D., Hovatta, T., Drake, A. J., Max-Moerbeck, W., Readhead, A. C. S., Richards, J. L., Doi, Akihiro, F. D'Ammando, M. Orienti, A. Doi, M. Giroletti, D. Dallacasa, T. Hovatta, A. J. Drake, W. Max-Moerbeck, A. C. S. Readhead, and J. L. Richards
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,galaxies: active ,FOS: Physical sciences ,Owens Valley Radio Observatory ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Luminosity ,law.invention ,Telescope ,law ,galaxies: individual: PKS 1502+036 ,0103 physical sciences ,Blazar ,010303 astronomy & astrophysics ,Very Long Baseline Array ,Astrophysics::Galaxy Astrophysics ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Superluminal motion ,gamma-rays: general ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Quasar ,Galaxy ,galaxies: Seyfert ,Galaxies: active, Galaxies: individual: PKS 1502+036, Galaxies: nuclei, Galaxies: Seyfert, Gamma-rays: general ,Space and Planetary Science ,galaxies: nuclei ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We report on multifrequency observations of the gamma-ray emitting narrow-line Seyfert 1 galaxy PKS 1502+036 performed from radio to gamma-rays during 2008 August-2012 November by Fermi-LAT, Swift (XRT and UVOT), OVRO, VLBA, and VLA. No significant variability has been observed in gamma-rays, with 0.1-100 GeV flux that ranged between (3-7)x10^-8 ph/cm^2/s using 3-month time bins. The photon index of the LAT spectrum (Gamma=2.60+/-0.06) and the apparent isotropic gamma-ray luminosity, L(0.1-100 GeV)= 7.8x10^45 erg/s, over 51 months are typical of a flat spectrum radio quasar. The radio spectral variability and the one-sided structure, in addition to the observed gamma-ray luminosity, suggest a relativistic jet with a high Doppler factor. In contrast to SBS 0846+513, the VLBA at 15 GHz did not observe superluminal motion for PKS 1502+036. Despite having the optical characteristics typical of a narrow-line Seyfert 1 galaxy, radio and gamma-ray properties of PKS 1502+036 are found to be similar to those of a blazar at the low end of the black hole mass distribution for blazars. This is in agreement with what has been found in the case of the other gamma-ray emitting narrow-line Seyfert 1 SBS 0846+513., Comment: 11 pages, 9 figures, 6 tables. MNRAS in press - Minor editing changes
- Published
- 2013
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20. Magic Constraints on γ-ray Emission from Cygnus X-3
- Author
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Aleksic, J, Antonelli, La, Antoranz, P, Backes, M, Baixeras, C, Barrio, Ja, Bastieri, Denis, Gonzalez, Jb, Bednarek, W, Berdyugin, A, Berger, K, Bernardini, E, Biland, A, Blanch, O, Bock, Rk, Boller, A, Bonnoli, G, Bordas, P, Tridon, Db, BOSCH RAMON, V, Bose, D, Braun, I, Bretz, T, Britzger, D, Camara, M, Carmona, E, Carosi, A, Colin, P, Contreras, Jl, Cortina, J, Costado, Mt, Covino, S, Dazzi, F, DE ANGELIS, A, DEL POZO EDC, DE LOTTO, B, DE MARIA, M, DE SABATA, F, Mendez, Cd, Doert, M, Dominguez, A, Prester, Dd, Dorner, D, Doro, Michele, Elsaesser, D, Errando, M, Ferenc, D, Fonseca, Mv, Font, L, Lopez, Rjg, Garczarczyk, M, Gaug, M, Godinovic, N, Goebel, F, Hadasch, D, Herrero, A, Hildebrand, D, HOHNE MONCH, D, Hose, J, Hrupec, D, Hsu, Cc, Jogler, T, Klepser, S, Krahenbuhl, T, Kranich, D, LA BARBERA, A, Laille, A, Leonardo, E, Lindfors, E, Lombardi, S, Longo, F, Lopez, M, Lorenz, E, Majumdar, P, Maneva, G, Mankuzhiyil, N, Mannheim, K, Maraschi, L, Mariotti, Mose', Martinez, M, Mazin, D, Meucci, M, Miranda, Jm, Mirzoyan, R, Miyamoto, H, Moldon, J, Moles, M, Moralejo, A, Nieto, D, Nilsson, K, Ninkovic, J, Orito, R, Oya, I, Paiano, S, Paoletti, R, Paredes, Jm, Partini, S, Pasanen, M, Pascoli, Donatella, Pauss, F, Pegna, Rg, PEREZ TORRES MA, Persic, M, Peruzzo, L, Prada, F, Prandini, Elisa, Puchades, N, Puljak, I, Reichardt, I, Rhode, W, Ribo, M, Rico, J, Rissi, M, Rugamer, S, Saggion, Antonio, Saito, K, Saito, Ty, Salvati, M, SANCHEZ CONDE, M, Satalecka, K, Scalzotto, VILLI MARIO, Scapin, V, Schultz, C, Schweizer, T, Shayduk, M, Shore, Sn, SIERPOWSKA BARTOSIK, A, Sillanpaa, A, Sitarek, J, Sobczynska, D, Spanier, F, Spiro, S, Stamerra, A, Steinke, B, Struebig, Jc, Suric, T, Takalo, L, Tavecchio, F, Temnikov, P, Terzic, T, Tescaro, D, Teshima, M, Torres, Df, Vankov, H, Wagner, Rm, Weitzel, Q, Zabalza, V, Zandanel, F, Zanin, R, Bulgarelli, A, MAX MOERBECK, W, Piano, G, Pooley, G, Readhead, Acs, Richards, Jl, Sabatini, S, Striani, E, Tavani, M, Trushkin, S., J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, J. A., Barrio, D., Bastieri, J. B., Gonzalez, W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, D., Britzger, M., Camara, E., Carmona, A., Carosi, P., Colin, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, F., Dazzi, A. D., Angeli, E. D. C., Del Pozo, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, M., Doert, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J. G., Lopez, M., Garczarczyk, M., Gaug, N., Godinovic, F., Goebel, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, C. C., Hsu, T., Jogler, S., Klepser, T., Krahenbuhl, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, R., Orito, I., Oya, S., Paiano, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, W., Rhode, M., Ribo, J., Rico, M., Rissi, S., Rugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, R., Zanin, A., Bulgarelli, W., Max Moerbeck, G., Piano, G., Pooley, A. C. S., Readhead, J. L., Richard, S., Sabatini, E., Striani, M., Tavani, and S., Trushkin
- Subjects
Photon ,HIGH-ENERGY EMISSION ,MICROQUASAR GRS 1915+105 ,X-RAY ,RELATIVISTIC JET ,CYG X-3 ,RADIO OUTBURST ,CRAB-NEBULA ,BINARY ,TELESCOPE ,PULSAR ,Astrophysics ,01 natural sciences ,law.invention ,Raigs gamma ,law ,Observacions astronòmiques ,010303 astronomy & astrophysics ,Estels binaris de raigs X ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Very High Energy Gamma-ray Astronomy ,MAGIC telescope ,Black Holes ,Gamma ray ,X-ray binaries ,Electrónica ,Física nuclear ,Radio frequency ,Electricidad ,Astrophysics - High Energy Astrophysical Phenomena ,Astronomical observations ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Compact star ,Radiation ,gamma ray astronomy ,Cosmic rays ,IMAGING CHERENKOV DETECTOR ,Telescope ,0103 physical sciences ,acceleration of particles ,binaries: general ,gamma rays: observations ,X-rays: bina- ries — X-rays: individual (Cygnus X-3) ,Cherenkov radiation ,Astrophysics::Galaxy Astrophysics ,010308 nuclear & particles physics ,Gamma rays ,Magic (programming) ,Astronomy ,Astronomy and Astrophysics ,Space and Planetary Science - Abstract
Cygnus X-3 is a microquasar consisting of an accreting compact object orbiting around a Wolf-Rayet star. It has been detected at radio frequencies and up to high-energy gamma rays (above 100 MeV). However, many models also predict a very high energy (VHE) emission (above hundreds of GeV) when the source displays relativistic persistent jets or transient ejections. Therefore, detecting such emission would improve the understanding of the jet physics. The imaging atmospheric Cherenkov telescope MAGIC observed Cygnus X-3 for about 70 hours between 2006 March and 2009 August in different X-ray/radio spectral states and also during a period of enhanced gamma-ray emission. MAGIC found no evidence for a VHE signal from the direction of the microquasar. An upper limit to the integral flux for energies higher than 250 GeV has been set to 2.2 x 10-12 photons cm-2 s-1 (95% confidence level). This is the best limit so far to the VHE emission from this source. The non-detection of a VHE signal during the period of activity in the high-energy band sheds light on the location of the possible VHE radiation favoring the emission from the innermost region of the jets, where absorption is significant. The current and future generations of Cherenkov telescopes may detect a signal under precise spectral conditions., 14 pages, 11 figures, This manuscript has been accepted by ApJ (2010)
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- 2010
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21. Modulated high-energy gamma-ray emission from the microquasar Cygnus X-3
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Abdo, Aa, Ackermann, M, Ajello, M, Axelsson, M, Baldini, Luca, Ballet, J, Barbiellini, G, Bastieri, D, Baughman, Bm, Bechtol, K, Bellazzini, R, Berenji, B, Blandford, Rd, Bloom, Ed, Bonamente, E, Borgland, Aw, Brez, A, Brigida, M, Bruel, P, Burnett, Th, Buson, S, Caliandro, Ga, Cameron, Ra, Caraveo, Pa, Casandjian, Jm, Cecchi, C, Celik, O, Chaty, S, Cheung, Cc, Chiang, J, Ciprini, S, Claus, R, Cohen Tanugi, J, Cominsky, Lr, Conrad, J, Corbel, S, Corbet, R, Dermer, Cd, de Palma, F, Digel, Sw, Silva, Ede, Drell, Ps, Dubois, R, Dubus, G, Dumora, D, Farnier, C, Favuzzi, C, Fegan, Sj, Focke, Wb, Fortin, P, Frailis, M, Fusco, P, Gargano, F, Gehrels, N, Germani, S, Giavitto, G, Giebels, B, Giglietto, N, Giordano, F, Glanzman, T, Godfrey, G, Grenier, Ia, Grondin, Mh, Grove, Je, Guillemot, L, Guiriec, S, Hanabata, Y, Harding, Ak, Hayashida, M, Hays, E, Hill, Ab, Hjalmarsdotter, L, Horan, D, Hughes, Re, Jackson, Ms, Johannesson, G, Johnson, As, Johnson, Tj, Johnson, Wn, Kamae, T, Katagiri, H, Kawai, N, Kerr, M, Knodlseder, J, Kocian, Ml, Koerding, E, Kuss, M, Lande, J, Latronico, L, Lemoine Goumard, M, Longo, F, Loparco, F, Lott, B, Lovellette, Mn, Lubrano, P, Madejski, Gm, Makeev, A, Marchand, L, Marelli, M, Max Moerbeck, W, Mazziotta, Mn, Mccoll, N, Mcenery, Je, Meurer, C, Michelson, Pf, Migliari, S, Mitthumsiri, W, Mizuno, T, Monte, C, Monzani, Me, Morselli, A, Moskalenko, Iv, Murgia, S, Nolan, Pl, Norris, Jp, Nuss, E, Ohsugi, T, Omodei, N, Ong, Ra, Ormes, Jf, Paneque, D, Parent, D, Pelassa, V, Pepe, M, Pesce Rollins, M, Piron, F, Pooley, G, Porter, Ta, Pottschmidt, K, Raino, S, Rando, R, Ray, Ps, Razzano, Massimiliano, Rea, N, Readhead, A, Reimer, A, Reimer, O, Richards, Jl, Rochester, Ls, Rodriguez, J, Rodriguez, Ay, Romani, Rw, Ryde, F, Sadrozinski, Hfw, Sander, A, Parkinson, Pms, Sgro, C, Siskind, Ej, Smith, Da, Smith, Pd, Spinelli, P, Starck, Jl, Stevenson, M, Strickman, Ms, Suson, Dj, Takahashi, H, Tanaka, T, Thayer, Jb, Thompson, Dj, Tibaldo, L, Tomsick, Ja, Torres, Df, Tosti, G, Tramacere, A, Uchiyama, Y, Usher, Tl, Vasileiou, V, Vilchez, N, Vitale, V, Waite, Ap, Wang, P, Wilms, J, Winer, Bl, Wood, Ks, Ylinen, T, Ziegler, M., High Energy Astrophys. & Astropart. Phys (API, FNWI), A. A., Abdo, M., Ackermann, M., Ajello, M., Axelsson, L., Baldini, J., Ballet, G., Barbiellini, D., Bastieri, B. M., Baughman, K., Bechtol, R., Bellazzini, B., Berenji, R. D., Blandford, E. D., Bloom, E., Bonamente, A. W., Borgland, A., Brez, M., Brigida, P., Bruel, T. H., Burnett, S., Buson, G. A., Caliandro, R. A., Cameron, P. A., Caraveo, J. M., Casandjian, C., Cecchi, O., Celik, S., Chaty, C. C., Cheung, J., Chiang, S., Ciprini, R., Clau, J., Cohen Tanugi, L. R., Cominsky, J., Conrad, S., Corbel, R., Corbet, C. D., Dermer, F. d., Palma, S. W., Digel, E. D. E., Silva, P. S., Drell, R., Duboi, G., Dubu, D., Dumora, C., Farnier, C., Favuzzi, S. J., Fegan, W. B., Focke, P., Fortin, M., Fraili, P., Fusco, F., Gargano, N., Gehrel, S., Germani, G., Giavitto, B., Giebel, N., Giglietto, F., Giordano, T., Glanzman, G., Godfrey, I. A., Grenier, M. H., Grondin, J. E., Grove, L., Guillemot, S., Guiriec, Y., Hanabata, A. K., Harding, M., Hayashida, E., Hay, A. B., Hill, L., Hjalmarsdotter, D., Horan, R. E., Hughe, M. S., Jackson, G., Johannesson, A. S., Johnson, T. J., Johnson, W. N., Johnson, T., Kamae, H., Katagiri, N., Kawai, M., Kerr, J., Knodlseder, M. L., Kocian, E., Koerding, M., Ku, J., Lande, L., Latronico, M., Lemoine Goumard, Longo, Francesco, F., Loparco, B., Lott, M. N., Lovellette, P., Lubrano, G. M., Madejski, A., Makeev, L., Marchand, M., Marelli, W., Max Moerbeck, M. N., Mazziotta, N., Mccoll, J. E., Mcenery, C., Meurer, P. F., Michelson, S., Migliari, W., Mitthumsiri, T., Mizuno, C., Monte, M. E., Monzani, A., Morselli, I. V., Moskalenko, S., Murgia, P. L., Nolan, J. P., Norri, E., Nu, T., Ohsugi, N., Omodei, R. A., Ong, J. F., Orme, D., Paneque, D., Parent, V., Pelassa, M., Pepe, M., Pesce Rollin, F., Piron, G., Pooley, T. A., Porter, K., Pottschmidt, S., Raino, R., Rando, P. S., Ray, M., Razzano, N., Rea, A., Readhead, A., Reimer, O., Reimer, J. L., Richard, L. S., Rochester, J., Rodriguez, A. Y., Rodriguez, R. W., Romani, F., Ryde, H. F. W., Sadrozinski, A., Sander, P. M. S., Parkinson, C., Sgro, E. J., Siskind, D. A., Smith, P. D., Smith, P., Spinelli, J. L., Starck, M., Stevenson, M. S., Strickman, D. J., Suson, H., Takahashi, T., Tanaka, J. B., Thayer, D. J., Thompson, L., Tibaldo, J. A., Tomsick, D. F., Torre, G., Tosti, A., Tramacere, Y., Uchiyama, T. L., Usher, V., Vasileiou, N., Vilchez, V., Vitale, A. P., Waite, P., Wang, J., Wilm, B. L., Winer, K. S., Wood, T., Ylinen, M., Ziegler, 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), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
- Subjects
Physics ,[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Multidisciplinary ,Black Holes ,010308 nuclear & particles physics ,[SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Astrophysics::High Energy Astrophysical Phenomena ,X-ray binary ,Gamma ray ,Astronomy ,Cosmic ray ,Quasar ,Fermi satellite ,Astrophysics ,01 natural sciences ,High Energy Gamma-ray Astronomy ,Neutron star ,Relativistic beaming ,Astrophysical jet ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Fermi Gamma-ray Space Telescope - Abstract
Microquasar Spotted Microquasars are binary star systems where a normal star sheds matter onto a neutron star or a black hole, generating x-ray radiation and jets of material moving at relativistic speeds. Microquasars have proved difficult to detect in high-energy gamma rays (> 100 megaelectron volts). Using the Fermi Large Area Telescope, Abdo et al. (p. 1512 , published online 26 November; see the Perspective by Bignami ) now report the detection of variable gamma-ray emission from the microquasar Cygnus X-3. The gamma-ray flux is modulated at the orbital period of Cygnus X-3, and its variation is correlated with the radio emission originating from the microquasar's relativistic jets.
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- 2009
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22. Assigning Degrees of Stochasticity to Blazar Light Curves in the Radio Band Using Complex Networks.
- Author
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Acosta-Tripailao B, Max-Moerbeck W, Pastén D, and Moya PS
- Abstract
We focus on characterizing the high-energy emission mechanisms of blazars by analyzing the variability in the radio band of the light curves of more than a thousand sources. We are interested in assigning complexity parameters to these sources, modeling the time series of the light curves with the method of the Horizontal Visibility Graph (HVG), which allows us to obtain properties from degree distributions, such as a characteristic exponent to describe its stochasticity and the Kullback-Leibler Divergence (KLD), presenting a new perspective to the methods commonly used to study Active Galactic Nuclei (AGN). We contrast these parameters with the excess variance, which is an astronomical measurement of variability in light curves; at the same time, we use the spectral classification of the sources. While it is not possible to find significant correlations with the excess variance, the degree distributions extracted from the network are detecting differences related to the spectral classification of blazars. These differences suggest a chaotic behavior in the time series for the BL Lac sources and a correlated stochastic behavior in the time series for the FSRQ sources. Our results show that complex networks may be a valuable alternative tool to study AGNs according to the variability of their energy output.
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- 2022
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23. Birth of a relativistic outflow in the unusual γ-ray transient Swift J164449.3+573451.
- Author
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Zauderer BA, Berger E, Soderberg AM, Loeb A, Narayan R, Frail DA, Petitpas GR, Brunthaler A, Chornock R, Carpenter JM, Pooley GG, Mooley K, Kulkarni SR, Margutti R, Fox DB, Nakar E, Patel NA, Volgenau NH, Culverhouse TL, Bietenholz MF, Rupen MP, Max-Moerbeck W, Readhead AC, Richards J, Shepherd M, Storm S, and Hull CL
- Abstract
Active galactic nuclei, which are powered by long-term accretion onto central supermassive black holes, produce relativistic jets with lifetimes of at least one million years, and the observation of the birth of such a jet is therefore unlikely. Transient accretion onto a supermassive black hole, for example through the tidal disruption of a stray star, thus offers a rare opportunity to study the birth of a relativistic jet. On 25 March 2011, an unusual transient source (Swift J164449.3+573451) was found, potentially representing such an accretion event. Here we report observations spanning centimetre to millimetre wavelengths and covering the first month of evolution of a luminous radio transient associated with Swift J164449.3+573451. The radio transient coincides with the nucleus of an inactive galaxy. We conclude that we are seeing a newly formed relativistic outflow, launched by transient accretion onto a million-solar-mass black hole. A relativistic outflow is not predicted in this situation, but we show that the tidal disruption of a star naturally explains the observed high-energy properties and radio luminosity and the inferred rate of such events. The weaker beaming in the radio-frequency spectrum relative to γ-rays or X-rays suggests that radio searches may uncover similar events out to redshifts of z ≈ 6.
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- 2011
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24. Modulated high-energy gamma-ray emission from the microquasar Cygnus X-3.
- Author
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Abdo AA, Ackermann M, Ajello M, Axelsson M, Baldini L, Ballet J, Barbiellini G, Bastieri D, Baughman BM, Bechtol K, Bellazzini R, Berenji B, Blandford RD, Bloom ED, Bonamente E, Borgland AW, Brez A, Brigida M, Bruel P, Burnett TH, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Casandjian JM, Cecchi C, Celik O, Chaty S, Cheung CC, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Cominsky LR, Conrad J, Corbel S, Corbet R, Dermer CD, de Palma F, Digel SW, do Couto e Silva E, Drell PS, Dubois R, Dubus G, Dumora D, Farnier C, Favuzzi C, Fegan SJ, Focke WB, Fortin P, Frailis M, Fusco P, Gargano F, Gehrels N, Germani S, Giavitto G, Giebels B, Giglietto N, Giordano F, Glanzman T, Godfrey G, Grenier IA, Grondin MH, Grove JE, Guillemot L, Guiriec S, Hanabata Y, Harding AK, Hayashida M, Hays E, Hill AB, Hjalmarsdotter L, Horan D, Hughes RE, Jackson MS, Jóhannesson G, Johnson AS, Johnson TJ, Johnson WN, Kamae T, Katagiri H, Kawai N, Kerr M, Knödlseder J, Kocian ML, Koerding E, Kuss M, Lande J, Latronico L, Lemoine-Goumard M, Longo F, Loparco F, Lott B, Lovellette MN, Lubrano P, Madejski GM, Makeev A, Marchand L, Marelli M, Max-Moerbeck W, Mazziotta MN, McColl N, McEnery JE, Meurer C, Michelson PF, Migliari S, Mitthumsiri W, Mizuno T, Monte C, Monzani ME, Morselli A, Moskalenko IV, Murgia S, Nolan PL, Norris JP, Nuss E, Ohsugi T, Omodei N, Ong RA, Ormes JF, Paneque D, Parent D, Pelassa V, Pepe M, Pesce-Rollins M, Piron F, Pooley G, Porter TA, Pottschmidt K, Rainò S, Rando R, Ray PS, Razzano M, Rea N, Readhead A, Reimer A, Reimer O, Richards JL, Rochester LS, Rodriguez J, Rodriguez AY, Romani RW, Ryde F, Sadrozinski HF, Sander A, Saz Parkinson PM, Sgrò C, Siskind EJ, Smith DA, Smith PD, Spinelli P, Starck JL, Stevenson M, Strickman MS, Suson DJ, Takahashi H, Tanaka T, Thayer JB, Thompson DJ, Tibaldo L, Tomsick JA, Torres DF, Tosti G, Tramacere A, Uchiyama Y, Usher TL, Vasileiou V, Vilchez N, Vitale V, Waite AP, Wang P, Wilms J, Winer BL, Wood KS, Ylinen T, and Ziegler M
- Abstract
Microquasars are accreting black holes or neutron stars in binary systems with associated relativistic jets. Despite their frequent outburst activity, they have never been unambiguously detected emitting high-energy gamma rays. The Fermi Large Area Telescope (LAT) has detected a variable high-energy source coinciding with the position of the x-ray binary and microquasar Cygnus X-3. Its identification with Cygnus X-3 is secured by the detection of its orbital period in gamma rays, as well as the correlation of the LAT flux with radio emission from the relativistic jets of Cygnus X-3. The gamma-ray emission probably originates from within the binary system, opening new areas in which to study the formation of relativistic jets.
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- 2009
- Full Text
- View/download PDF
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