Multiwavelength behaviour of the blazar 3C 279: Decade-long study from γ -ray to radio

Ibryamov S.; Nizhelsky N.A.; Mirzaqulov D.; Hovatta T.; Gómez J.L.; Sadakane K.; Calcidese P.; Carnerero M.I.; Bachev R.; Thum C.; Strigachev A.; Weaver Z.R.; Agudo I.; Lähteenmäki A.; Gurwell M.A.; Kovalev Y.Y.; Mingaliev M.G.; Rizzi N.; Zhekanis G.V.; Borman G.A.; Di Paola A.; Morozova D.A.; Savchenko S.S.; Kovalev Y.A.; Sola P.; Casadio C.; Aller M.F.; Troitsky I.S.; Aller H.D.; Gónzalez-Morales P.; Fuentes A.; Kurtanidze O.M.; Acosta-Pulido J.A.; Sotnikova Y.V.; Matsumoto K.; Larionova E.G.; Vince O.; Giunta A.; Rakhimov I.A.; Ovcharov E.; Kurtanidze S.O.; Nikolashvili M.G.; Samal M.R.; Muñoz Dimitrova R.V.; Kopatskaya E.N.; Semkov E.; Marchini A.; Marscher A.P.; Damljanovic G.; Sergeev S.G.; Bonnoli G.; Joshi M.; Dementyev A.V.; Raiteri C.M.; Mihov B.; Lázaro C.; Frasca A.; Chen W.P.; Slavcheva-Mihova L.; Leto G.; Sigua L.A.; Tsybulev P.G.; Williamson K.E.; Villata M.; Hagen-Thorn V.A.; Arkharov A.A.; Kim J.Y.; Jorstad S.G.; Minev M.; Troitskaya Y.V.; Sanchez R.Z.; Traianou E.; Nikiforova A.A.; Vasilyev A.A.; Kimeridze G.N.; Pressburger L.D.; Grishina T.S.; Bozhilov V.; Sadun A.C.; Larionova L.V.; Myserlis I.; Kiehlmann S.; Larionov V.M.; Righini S.; Smith P.S.; Carosati D.; Andreeva T.S.

Multiwavelength behaviour of the blazar 3C 279: Decade-long study from γ -ray to radio

Larionov V.M.; Jorstad S.G.; Marscher A.P.; Villata M.; Raiteri C.M.; Smith P.S.; Agudo I.; Savchenko S.S.; Morozova D.A.; Acosta-Pulido J.A.; Aller M.F.; Aller H.D.; Andreeva T.S.; Arkharov A.A.; Bachev R.; Bonnoli G.; Borman G.A.; Bozhilov V.; Calcidese P.; Carnerero M.I.; Carosati D.; Casadio C.; Chen W.P.; Damljanovic G.; Dementyev A.V.; Di Paola A.; Frasca A.; Fuentes A.; Gómez J.L.; Gónzalez-Morales P.; Giunta A.; Grishina T.S.; Gurwell M.A.; Hagen-Thorn V.A.; Hovatta T.; Ibryamov S.; Joshi M.; Kiehlmann S.; Kim J.Y.; Kimeridze G.N.; Kopatskaya E.N.; Kovalev Y.A.; Kovalev Y.Y.; Kurtanidze O.M.; Kurtanidze S.O.; Lähteenmäki A.; Lázaro C.; Larionova L.V.; Larionova E.G.; Leto G.; Marchini A.; Matsumoto K.; Mihov B.; Minev M.; Mingaliev M.G.; Mirzaqulov D.; Muñoz Dimitrova R.V.; Myserlis I.; Nikiforova A.A.; Nikolashvili M.G.; Nizhelsky N.A.; Ovcharov E.; Pressburger L.D.; Rakhimov I.A.; Righini S.; Rizzi N.; Sadakane K.; Sadun A.C.; Samal M.R.; Sanchez R.Z.; Semkov E.; Sergeev S.G.; Sigua L.A.; Slavcheva-Mihova L.; Sola P.; Sotnikova Y.V.; Strigachev A.; Thum C.; Traianou E.; Troitskaya Y.V.; Troitsky I.S.; Tsybulev P.G.; Vasilyev A.A.; Vince O.; Weaver Z.R.; Williamson K.E.; Zhekanis G.V.

URI: https://dspace.kpfu.ru/xmlui/handle/net/160899

Дата: 2020

Аннотации:

© 2020 The Author(s). We report the results of decade-long (2008-2018) γ -ray to 1 GHz radio monitoring of the blazar 3C 279, including GASP/WEBT, Fermi and Swift data, as well as polarimetric and spectroscopic data. The X-ray and γ -ray light curves correlate well, with no delay ≳ 3 h, implying general cospatiality of the emission regions. The γ -ray-optical flux-flux relation changes with activity state, ranging from a linear to amore complex dependence. The behaviour of the Stokes parameters at optical and radio wavelengths, including 43 GHz Very Long Baseline Array images, supports either a predominantly helical magnetic field or motion of the radiating plasma along a spiral path. Apparent speeds of emission knots range from 10 to 37c, with the highest values requiring bulk Lorentz factors close to those needed to explain γ -ray variability on very short time-scales. The MgII emission line flux in the 'blue' and 'red' wings correlates with the optical synchrotron continuum flux density, possibly providing a variable source of seed photons for inverse Compton scattering. In the radio bands, we find progressive delays of the most prominent light-curve maxima with decreasing frequency, as expected from the frequency dependence of the τ= 1 surface of synchrotron self-absorption. The global maximum in the 86 GHz light curve becomes less prominent at lower frequencies, while a local maximum, appearing in 2014, strengthens toward decreasing frequencies, becoming pronounced at ∼5 GHz. These tendencies suggest different Doppler boosting of stratified radio-emitting zones in the jet.

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