Показать сокращенную информацию
dc.contributor.author | Larionov V.M. | |
dc.contributor.author | Jorstad S.G. | |
dc.contributor.author | Marscher A.P. | |
dc.contributor.author | Villata M. | |
dc.contributor.author | Raiteri C.M. | |
dc.contributor.author | Smith P.S. | |
dc.contributor.author | Agudo I. | |
dc.contributor.author | Savchenko S.S. | |
dc.contributor.author | Morozova D.A. | |
dc.contributor.author | Acosta-Pulido J.A. | |
dc.contributor.author | Aller M.F. | |
dc.contributor.author | Aller H.D. | |
dc.contributor.author | Andreeva T.S. | |
dc.contributor.author | Arkharov A.A. | |
dc.contributor.author | Bachev R. | |
dc.contributor.author | Bonnoli G. | |
dc.contributor.author | Borman G.A. | |
dc.contributor.author | Bozhilov V. | |
dc.contributor.author | Calcidese P. | |
dc.contributor.author | Carnerero M.I. | |
dc.contributor.author | Carosati D. | |
dc.contributor.author | Casadio C. | |
dc.contributor.author | Chen W.P. | |
dc.contributor.author | Damljanovic G. | |
dc.contributor.author | Dementyev A.V. | |
dc.contributor.author | Di Paola A. | |
dc.contributor.author | Frasca A. | |
dc.contributor.author | Fuentes A. | |
dc.contributor.author | Gómez J.L. | |
dc.contributor.author | Gónzalez-Morales P. | |
dc.contributor.author | Giunta A. | |
dc.contributor.author | Grishina T.S. | |
dc.contributor.author | Gurwell M.A. | |
dc.contributor.author | Hagen-Thorn V.A. | |
dc.contributor.author | Hovatta T. | |
dc.contributor.author | Ibryamov S. | |
dc.contributor.author | Joshi M. | |
dc.contributor.author | Kiehlmann S. | |
dc.contributor.author | Kim J.Y. | |
dc.contributor.author | Kimeridze G.N. | |
dc.contributor.author | Kopatskaya E.N. | |
dc.contributor.author | Kovalev Y.A. | |
dc.contributor.author | Kovalev Y.Y. | |
dc.contributor.author | Kurtanidze O.M. | |
dc.contributor.author | Kurtanidze S.O. | |
dc.contributor.author | Lähteenmäki A. | |
dc.contributor.author | Lázaro C. | |
dc.contributor.author | Larionova L.V. | |
dc.contributor.author | Larionova E.G. | |
dc.contributor.author | Leto G. | |
dc.contributor.author | Marchini A. | |
dc.contributor.author | Matsumoto K. | |
dc.contributor.author | Mihov B. | |
dc.contributor.author | Minev M. | |
dc.contributor.author | Mingaliev M.G. | |
dc.contributor.author | Mirzaqulov D. | |
dc.contributor.author | Muñoz Dimitrova R.V. | |
dc.contributor.author | Myserlis I. | |
dc.contributor.author | Nikiforova A.A. | |
dc.contributor.author | Nikolashvili M.G. | |
dc.contributor.author | Nizhelsky N.A. | |
dc.contributor.author | Ovcharov E. | |
dc.contributor.author | Pressburger L.D. | |
dc.contributor.author | Rakhimov I.A. | |
dc.contributor.author | Righini S. | |
dc.contributor.author | Rizzi N. | |
dc.contributor.author | Sadakane K. | |
dc.contributor.author | Sadun A.C. | |
dc.contributor.author | Samal M.R. | |
dc.contributor.author | Sanchez R.Z. | |
dc.contributor.author | Semkov E. | |
dc.contributor.author | Sergeev S.G. | |
dc.contributor.author | Sigua L.A. | |
dc.contributor.author | Slavcheva-Mihova L. | |
dc.contributor.author | Sola P. | |
dc.contributor.author | Sotnikova Y.V. | |
dc.contributor.author | Strigachev A. | |
dc.contributor.author | Thum C. | |
dc.contributor.author | Traianou E. | |
dc.contributor.author | Troitskaya Y.V. | |
dc.contributor.author | Troitsky I.S. | |
dc.contributor.author | Tsybulev P.G. | |
dc.contributor.author | Vasilyev A.A. | |
dc.contributor.author | Vince O. | |
dc.contributor.author | Weaver Z.R. | |
dc.contributor.author | Williamson K.E. | |
dc.contributor.author | Zhekanis G.V. | |
dc.date.accessioned | 2021-02-24T20:33:35Z | |
dc.date.available | 2021-02-24T20:33:35Z | |
dc.date.issued | 2020 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | https://dspace.kpfu.ru/xmlui/handle/net/160899 | |
dc.description.abstract | © 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. | |
dc.relation.ispartofseries | Monthly Notices of the Royal Astronomical Society | |
dc.subject | 3C 279 | |
dc.subject | Active | |
dc.subject | Galaxies | |
dc.subject | Individual | |
dc.subject | Methods | |
dc.subject | Observational | |
dc.subject | Photometric | |
dc.subject | Polarimetric | |
dc.subject | Quasars | |
dc.subject | Spectroscopic | |
dc.subject | Techniques | |
dc.subject | Techniques | |
dc.subject | Techniques | |
dc.title | Multiwavelength behaviour of the blazar 3C 279: Decade-long study from γ -ray to radio | |
dc.type | Article | |
dc.relation.ispartofseries-issue | 3 | |
dc.collection | Публикации сотрудников КФУ | |
dc.relation.startpage | 3829 | |
dc.source.id | SCOPUS00358711-2020-3-SID85084541346 |