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Rani, B.; Krichbaum, T. P.; Fuhrmann, L.; Böttcher, M.; Lott, B.; Aller, H. D.; Aller, M. F.; Angelakis, E.; Bach, U.; Bastieri, D.; Falcone, A. D.; Fukazawa, Y.; Gabanyi, K. E.; Gupta, A. C.; Gurwell, M.; Itoh, R.; Kawabata, K. S.; Krips, M.; Lähteenmäki, A. A.; Liu, X.; Marchili, N.; Max-Moerbeck, W.; Nestoras, I.; Nieppola, E.; Quintana-Lacaci, G.; Readhead, A. C. S.; Richards, J. L.; Sasada, M.; Sievers, A.; Sokolovsky, K.; Stroh, M.; Tammi, J.; Tornikoski, M.; Uemura, M.; Ungerechts, H.; Urano, T.; Zensus, J. A.
Astronomy and astrophysics (Berlin), 04/2013, Letnik: 552Journal Article
We present the results of a series of radio, optical, X-ray, and γ-ray observations of the BL Lac object S50716+714 carried out between April 2007 and January 2011. The multifrequency observations were obtained using several ground- and space-based facilities. The intense optical monitoring of the source reveals faster repetitive variations superimposed on a long-term variability trend on a time scale of ~350 days. Episodes of fast variability recur on time scales of ~60−70 days. The intense and simultaneous activity at optical and γ-ray frequencies favors the synchrotron self-Compton mechanism for the production of the high-energy emission. Two major low-peaking radio flares were observed during this high optical/γ-ray activity period. The radio flares are characterized by a rising and a decaying stage and agrees with the formation of a shock and its evolution. We found that the evolution of the radio flares requires a geometrical variation in addition to intrinsic variations of the source. Different estimates yield robust and self-consistent lower limits of δ ≥ 20 and equipartition magnetic field Beq ≥ 0.36 G. Causality arguments constrain the size of emission region θ ≤ 0.004 mas. We found a significant correlation between flux variations at radio frequencies with those at optical and γ-rays. Theoptical/GeV flux variations lead the radio variability by ~65 days. The longer time delays between low-peaking radio outbursts and optical flares imply that optical flares are the precursors of radio ones. An orphan X-ray flare challenges the simple, one-zone emission models, rendering them too simple. Here we also describe the spectral energy distribution modeling of the source from simultaneous data taken through different activity periods.
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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