E-viri
Recenzirano
Odprti dostop
-
Ahnen, M M; Ansoldi, A A; Antonelli, L L; Arcaro, A A; Babic, A.; Banerjee, B; Bangale, P; Barres de Almeida, D A; Barrio, A J; Becerra González, J G; Bednarek, W; Bernardini, E; Berti, A A; Biasuzzi, B; Biland, A A; Blanch, B; Bonnefoy, Serge; Bonnoli, G G; Carosi, R R; Carosi, A A; Chatterjee, A A; Colin, P; Colombo, E; Contreras, L J; Cortina, J J; Covino, S; Cumani, P; da Vela, D V; Dazzi, D F; de Angelis, D A; de Lotto, D L; de Oña Wilhelmi, E.; Pierro, D F; Doert, D M; Domínguez, D A; Dominis Prester, D; Dorner, D; Doro, D M; Einecke, S; Glawion, D G; Elsaesser, D; Engelkemeier, M M; Fallah Ramazani, F F; Fernández-Barral, A.; Fidalgo, D F; Fonseca, M F; Font, F F; Fruck, F F; Galindo, D G; López, L R; Garczarczyk, M G; Gaug, M G; Giammaria, P G; Godinovic, N G; Gora, D G; Griffiths, S G; Guberman, D G; Hadasch, D; Hahn, A A; Hassan, T.; Hayashida, M M; Herrera, J J; Hose, J J; Hrupec, D; Hughes, G G; Ishio, I; Konno, K; Kubo, K; Kushida, J J; Kuveždic, D.; Lelas, D L; Lindfors, L L; Lombardi, L L; Longo, F F; López, M M; Maggio, M M; Majumdar, M M; Makariev, M M; Maneva, M G; Manganaro, M M; Mannheim, M M; Maraschi, M M; Mariotti, M M; Martínez, M M; Mazin, D M; Menzel, M M; Minev, M M; Mirzoyan, M R; Moralejo, M M; Moreno, M M; Moretti, E.; Neustroev, N V; Niedzwiecki, N A; Nievas Rosillo, N R; Nilsson, N; Ninci, N; Nishijima, N; Noda, N; Nogués, N L; Paiano, P
Monthly notices of the Royal Astronomical Society, 2017Journal Article
The microquasar V404 Cygni underwent a series of outbursts in 2015, June 15-31, during which its flux in hard X-rays (20-40 keV) reached about 40 times the Crab Nebula flux. Because of the exceptional interest of the flaring activity from this source, observations at several wavelengths were conducted. The MAGIC telescopes, triggered by the INTEGRAL alerts, followed-up the flaring source for several nights during the period June 18-27, for more than 10 hours. One hour of observation was conducted simultaneously to a giant 22 GHz radio flare and a hint of signal at GeV energies seen by Fermi-LAT. The MAGIC observations did not show significant emission in any of the analysed time intervals. The derived flux upper limit, in the energy range 200–1250 GeV, is 4.8×10$^{−12}$ ph cm$^{−2}$ s$^{−1}$. We estimate the gamma-ray opacity during the flaring period, which along with our non-detection, points to an inefficient acceleration in the V404 Cyg jets if VHE emitter is located further than 1 × 10$^{10}$ cm from the compact object.
