Radio to gamma-ray variability study of blazar S5 0716+714

B. Rani, T. P. Krichbaum, L. Fuhrmann, M. Böttcher, B. Lott, H. D. Aller, M. F. Aller, E. Angelakis, U. Bach, D. Bastieri, A. D. Falcone, Y. Fukazawa, K. E. Gabanyi, A. C. Gupta, M. Gurwell, R. Itoh, K. S. Kawabata, M. Krips, A. A. Lähteenmäki, X. LiuN. Marchili, W. Max-Moerbeck, I. Nestoras, E. Nieppola, G. Quintana-Lacaci, A. C.S. Readhead, J. L. Richards, M. Sasada, A. Sievers, K. Sokolovsky, M. Stroh, J. Tammi, M. Tornikoski, M. Uemura, H. Ungerechts, T. Urano, J. A. Zensus

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66 Scopus citations

Abstract

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 λ ≥ 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. The optical/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.

Original languageEnglish (US)
Article numberA11
JournalAstronomy and Astrophysics
Volume552
DOIs
StatePublished - 2013

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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