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FLARING BEHAVIOR OF THE QUASAR 3C 454.3 ACROSS THE ELECTROMAGNETIC SPECTRUM

S. G. JorstadAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaAlan P. MarscherInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston MA 02215, USAV. M. LarionovIsaac Newton Institute of Chile, St. Petersburg Branch, St. Petersburg, RussiaI. AgudoInstituto de Astrofísica de Andalucía,CSIC,Apartado 3004,18080,Granada,SpainPaul S. SmithSteward Observatory, University of Arizona, Tucson, AZ 85721-0065, USAMark GurwellHarvard-Smithsonian Center for Astrophysics, 60 Garden St. Cambridge, MA,02138, USAA. LähteenmäkiMetsähovi Radio Observatory, Helsinki University of Technology TKK, Metsähovintie 114, FIN-02540 Kylmälä, FinlandM. TornikoskiMetsähovi Radio Observatory, Helsinki University of Technology TKK, Metsähovintie 114, FIN-02540 Kylmälä, FinlandA. MarkowitzCenter for Astrophysics and Space Sciences, University of California, San Diego, M.C. 0424, La Jolla, CA, 92093-0424, USAArkadi A. ArkharovMain (Pulkovo) Astronomical Observatory of RAS, Pulkovskoye shosse, 60, 196140, St. Petersburg, RussiaD. BlinovAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaRitaban ChatterjeeInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston MA 02215, USAFrancesca D’ArcangeloInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston MA 02215, USAAbe FalconeDeptartment of Astronomy & Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USAJosé L. GómezInstituto de Astrofísica de Andalucía,CSIC,Apartado 3004,18080,Granada,SpainV. A. Hagen‐ThornAstronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaBrendan JordanSchool of Cosmic Physics, Dublin Institute of Advances Studies, Republic of IrelandGivi N. KimeridzeAbastumani Astrophysical Observatory, Mt Kanobili, Abastumani, Georgia ,T. S. KonstantinovaAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaE. N. KopatskayaAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaO. M. KurtanidzeAbastumani Astrophysical Observatory, Mt Kanobili, Abastumani, Georgia ,Е. Г. ЛарионоваAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaL. V. LarionovaAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaI. M. McHardyDepartment of Physics & Astronomy, University of Southampton, Southampton SO17 1BJ, UKDaria A. MelnichukAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaMar Roca-SogorbInstituto de Astrofísica de Andalucía,CSIC,Apartado 3004,18080,Granada,SpainGary D. SchmidtSteward Observatory, University of Arizona, Tucson, AZ 85721-0065, USAB. A. SkiffLowell Observatory, Flagstaff, AZ 86001, USABrian TaylorInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USAClemens ThumInstitut de Radio Astronomie Millimétrique, 300 Rue de la Piscine, 38406 St. Martin d’Hères, FranceI. S. TroitskyAstronomical Institute, St Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St Petersburg, RussiaH. WiesemeyerInstituto de Radio Astronomía Milimétrica, Avenida Divina Pastora, 7, Local 20, E-18012 Granada, Spain

2010en

ABI

Annotatsiya

We analyze the behavior of the parsec-scale jet of the quasar 3C~454.3 during pronounced flaring activity in 2005-2008. Three major disturbances propagated down the jet along different trajectories with Lorentz factors $\Gamma>$10. The disturbances show a clear connection with millimeter-wave outbursts, in 2005 May/June, 2007 July, and 2007 December. High-amplitude optical events in the $R$-band light curve precede peaks of the millimeter-wave outbursts by 15-50 days. Each optical outburst is accompanied by an increase in X-ray activity. We associate the optical outbursts with propagation of the superluminal knots and derive the location of sites of energy dissipation in the form of radiation. The most prominent and long-lasting of these, in 2005 May, occurred closer to the black hole, while the outbursts with a shorter duration in 2005 Autumn and in 2007 might be connected with the passage of a disturbance through the millimeter-wave core of the jet. The optical outbursts, which coincide with the passage of superluminal radio knots through the core, are accompanied by systematic rotation of the position angle of optical linear polarization. Such rotation appears to be a common feature during the early stages of flares in blazars. We find correlations between optical variations and those at X-ray and $\gamma$-ray energies. We conclude that the emergence of a superluminal knot from the core yields a series of optical and high-energy outbursts, and that the mm-wave core lies at the end of the jet's acceleration and collimation zone.

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DOI: 10.1088/0004-637x/715/1/362

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