Multiwavelength behaviour of the blazar 3C 279: decade-long study from γ-ray to radio
V. M. LarionovAstronomical Institute, St.-Petersburg State University, 198504, St. Petersburg, RussiaSvetlana G. JorstadAstronomical Institute, St.-Petersburg State University, 198504, St. Petersburg, RussiaAlan P. MarscherInstitute for Astrophysical Research, Boston University, MA, USAM. VillataINAF, Osservatorio Astrofisico di Torino, Turin, ItalyC. M. RaiteriINAF, Osservatorio Astrofisico di Torino, Turin, ItalyPaul S. SmithSteward Observatory, University of Arizona, Tucson, AZ 85721, USAI. AgudoInstituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, E–18008 Granada, SpainС. С. СавченкоD. A. MorozovaJ. A. Acosta‐PulidoDepartamento de Astrofisica, Universidad de La Laguna, La Laguna, Tenerife, SpainM. F. AllerDepartment of Astronomy, University of Michigan, 323 West Hall, Ann Arbor, MI 48109-1107, USAH. D. AllerDepartment of Astronomy, University of Michigan, 323 West Hall, Ann Arbor, MI 48109-1107, USAT. S. AndreevaInstitute of Applied Astronomy, Russian Academy of Sciences, Kutuzov emb. 10, 191187 St. Petersburg, RussiaA. A. ArkharovPulkovo Observatory, 196140, St.-Petersburg, RussiaR. BachevInstitute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaG. BonnoliAstronomical Observatory, Department of Physical Sciences, Earth and Environment – University of Siena, Via Roma 56, I-53100 Siena, ItalyГ. А. БорманCrimean Astrophysical Observatory, 298409, Nauchnyi, Crimea, RussiaV. BozhilovDepartment of Astronomy, Faculty of Physics, Sofia University, Sofia, BulgariaP. CalcideseOsservatorio Astronomico della Regione Autonoma Valle d’Aosta, I-11020 Nus, ItalyM. I. CarnereroINAF, Osservatorio Astrofisico di Torino, Turin, ItalyD. CarosatiEPT Observatories, Tijarafe, La Palma, SpainC. CasadioMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyW-P ChenGraduate Institute of Astronomy, National Central University, Jhongli City, Taoyuan County 32001, TaiwanG. DamljanovićAstronomical Observatory, Volgina 7, 11060 Belgrade, SerbiaA. V. DementyevA. Di PaolaINAF, Osservatorio Astronomico di Roma, Rome, ItalyA. FrascaINAF – Osservatorio Astrofisico di Catania, via S. Sofia, 78, I-95123 Catania, ItalyAntonio FuentesInstituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, E–18008 Granada, SpainJosé L. GómezInstituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, E–18008 Granada, SpainP. A. González-MoralesDepartamento de Astrofisica, Universidad de La Laguna, La Laguna, Tenerife, SpainA. GiuntaASI Italian Space Agency, Rome, ItalyT. S. GrishinaMark GurwellCenter for Astrophysics, Harvard and Smithsonian, 60 Garden Street, Cambrige, MA 02138 USAV. A. Hagen‐ThornT. HovattaFinnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, FinlandS. IbryamovDepartment of Physics and Astronomy, University of Shumen, 9700 Shumen, BulgariaM. JoshiInstitute for Astrophysical Research, Boston University, MA, USAS. KiehlmannCalifornia Institute of Technology, 1216 E California Blvd, Pasadena, CA 91125, USAJ-Y KimMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyG. N. KimeridzeAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaE. N. KopatskayaYu. A. KovalevAstro Space Center of Lebedev Physical Institute, Profsoyuznaya St. 84/32, 117997 Moscow, RussiaY. Y. KovalevAstro Space Center of Lebedev Physical Institute, Profsoyuznaya St. 84/32, 117997 Moscow, RussiaO. M. KurtanidzeAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaS. O. KurtanidzeAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaA. LähteenmäkiDepartment of Electronics and Nanoengineering, Aalto University, FI-00076 Aalto, FinlandC. LázaroDepartamento de Astrofisica, Universidad de La Laguna, La Laguna, Tenerife, SpainL. V. LarionovaЕ. Г. ЛарионоваG. LetoINAF – Osservatorio Astrofisico di Catania, via S. Sofia, 78, I-95123 Catania, ItalyAlessandro MarchiniAstronomical Observatory, Department of Physical Sciences, Earth and Environment – University of Siena, Via Roma 56, I-53100 Siena, ItalyKatsura MatsumotoAstronomical Institute, Osaka Kyoiku University, Osaka 582-8582, JapanB. MihovInstitute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaM. MinevDepartment of Astronomy, Faculty of Physics, Sofia University, Sofia, BulgariaМ. Г. МингалиевKazan Federal University, 18 Kremlyovskaya St., Kazan 420008, RussiaD. O. MirzaqulovUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Astronomical street 33, Tashkent 100052, UzbekistanR. V. Muñoz DimitrovaInstitute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaI. MyserlisMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyA. A. NikiforovaAstronomical Institute, St.-Petersburg State University, 198504, St. Petersburg, RussiaM. G. NikolashviliAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaN. A. NizhelskySpecial Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, RussiaE. OvcharovDepartment of Astronomy, Faculty of Physics, Sofia University, Sofia, BulgariaLeeya PressburgerInstitute for Astrophysical Research, Boston University, MA, USAI. A. RakhimovInstitute of Applied Astronomy, Russian Academy of Sciences, Kutuzov emb. 10, 191187 St. Petersburg, RussiaS. RighiniINAF, Istituto di Radioastronomia, via Piero Gobetti 93/2, I-40129 Bologna, ItalyN. RizziKunihiko SadakaneAstronomical Institute, Osaka Kyoiku University, Osaka 582-8582, JapanA. C. SadunDepartment of Physics, University of Colorado, Denver, CO, USAM. R. SamalGraduate Institute of Astronomy, National Central University, Jhongli City, Taoyuan County 32001, TaiwanR. Zanmar SánchezINAF – Osservatorio Astrofisico di Catania, via S. Sofia, 78, I-95123 Catania, ItalyE. SemkovInstitute of Astronomy, Bulgarian Academy of Sciences, Sofia, BulgariaС. Г. СергеевCrimean Astrophysical Observatory, 298409, Nauchnyi, Crimea, RussiaL. A. SiguaAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaL. Slavcheva‐MihovaInstitute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaPoc SolaInstituto de Astrofisica de Canarias (IAC), La Laguna, Tenerife, SpainYu. V. SotnikovaSpecial Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, RussiaA. StrigachevInstitute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaC. ThumInstituto de Radio Astronomía Millimétrica, Avenida Divina Pastora, 7, Local 20, E-18012 Granada, SpainEfthalia TraianouMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyYu. V. TroitskayaI. S. TroitskyП. Г. ЦыбулевSpecial Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, RussiaA. A. VasilyevO. VinceAstronomical Observatory, Volgina 7, 11060 Belgrade, SerbiaZ. R. WeaverInstitute for Astrophysical Research, Boston University, MA, USAKaren E. WilliamsonInstitute for Astrophysical Research, Boston University, MA, USAГ. В. ЖеканисSpecial Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz 369167, Russia
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ABSTRACT 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 $\gtrsim 3$ h, implying general cospatiality of the emission regions. The γ-ray–optical flux–flux relation changes with activity state, ranging from a linear to a more 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 Mg ii 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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