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Raiteri, C M; Villata, M; Larionov, V M; Jorstad, S G; Marscher, A P; Weaver, Z R; Acosta-Pulido, J A; Agudo, I; Andreeva, T; Arkharov, A; Bachev, R; Benítez, E; Berton, M; Björklund, I; Borman, G A; Bozhilov, V; Carnerero, M I; Carosati, D; Casadio, C; Chen, W P; Damljanovic, G; D’Ammando, F; Escudero, J; Fuentes, A; Giroletti, M; Grishina, T S; Gupta, A C; Hagen-Thorn, V A; Hart, M; Hiriart, D; Hou, W-J; Ivanov, D; Kim, J-Y; Kimeridze, G N; Konstantopoulou, C; Kopatskaya, E N; Kurtanidze, O M; Kurtanidze, S O; Lähteenmäki, A; Larionova, E G; Larionova, L V; Marchili, N; Markovic, G; Minev, M; Morozova, D A; Myserlis, I; Nakamura, M; Nikiforova, A A; Nikolashvili, M G; Otero-Santos, J; Ovcharov, E; Pursimo, T; Rahimov, I; Righini, S; Sakamoto, T; Savchenko, S S; Semkov, E H; Shakhovskoy, D; Sigua, L A; Stojanovic, M; Strigachev, A; Thum, C; Tornikoski, M; Traianou, E; Troitskaya, Y V; Troitskiy, I S; Tsai, A; Valcheva, A; Vasilyev, A A; Vince, O; Zaharieva, E
Monthly notices of the Royal Astronomical Society, 07/2021, Volume: 504, Issue: 4Journal Article
ABSTRACT Among active galactic nuclei, blazars show extreme variability properties. We here investigate the case of the BL Lac object S4 0954+65 with data acquired in 2019–2020 by the Transiting Exoplanet Survey Satellite (TESS) and by the Whole Earth Blazar Telescope (WEBT) Collaboration. The 2-min cadence optical light curves provided by TESS during three observing sectors of nearly 1 month each allow us to study the fast variability in great detail. We identify several characteristic short-term time-scales, ranging from a few hours to a few days. However, these are not persistent, as they differ in the various TESS sectors. The long-term photometric and polarimetric optical and radio monitoring undertaken by the WEBT brings significant additional information, revealing that (i) in the optical, long-term flux changes are almost achromatic, while the short-term ones are strongly chromatic; (ii) the radio flux variations at 37 GHz follow those in the optical with a delay of about 3 weeks; (iii) the range of variation of the polarization degree and angle is much larger in the optical than in the radio band, but the mean polarization angles are similar; (iv) the optical long-term variability is characterized by a quasi-periodicity of about 1 month. We explain the source behaviour in terms of a rotating inhomogeneous helical jet, whose pitch angle can change in time.
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