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dc.contributor.authorRani, B.
dc.contributor.authorBöttcher, M.
dc.contributor.authorKrichbaum, T.P.
dc.contributor.authorFuhrmann, L.
dc.contributor.authorLott, B.
dc.date.accessioned2015-03-23T12:32:56Z
dc.date.available2015-03-23T12:32:56Z
dc.date.issued2013
dc.identifier.citationRani, B. et al. 2013. Radio to gamma-ray variability study of blazar S5 0716+714. Astronomy & astrophysics, 552: Article no A11. [https://doi.org/10.1051/0004-6361/201321058]en_US
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746 (Online)
dc.identifier.urihttp://hdl.handle.net/10394/13608
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201321058
dc.description.abstractWe 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. 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.en_US
dc.language.isoenen_US
dc.publisherEDP Sciencesen_US
dc.subjectGalaxies: activeen_US
dc.subjectBL Lacertae objects: individual: S5 0716+714en_US
dc.subjectgamma rays: galaxiesen_US
dc.subjectX-rays: galaxiesen_US
dc.subjectradio continuum: galaxiesen_US
dc.titleRadio to gamma-ray variability study of blazar S5 0716+714en_US
dc.typeArticleen_US
dc.contributor.researchID24420530 - Böttcher, Markus


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