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

被引：169

作者：

Jorstad, Svetlana G. ^{[1
,2
]}

Marscher, Alan P. ^{[1
]}

Larionov, Valeri M. ^{[2
,3
]}

Agudo, Ivan ^{[4
]}

Smith, Paul S. ^{[5
]}

Gurwell, Mark ^{[6
]}

Lahteenmaki, Anne ^{[7
]}

Tornikoski, Merja ^{[7
]}

Markowitz, Alex ^{[8
]}

Arkharov, Arkadi A. ^{[9
]}

Blinov, Dmitry A. ^{[2
]}

Chatterjee, Ritaban ^{[1
]}

D'Arcangelo, Francesca D. ^{[1
]}

Falcone, Abe D. ^{[10
]}

Gomez, Jose L.

Hagen-Thorn, Vladimir A. ^{[2
,3
]}

Jordan, Brendan ^{[11
]}

Kimeridze, Givi N. ^{[12
]}

Konstantinova, Tatiana S. ^{[2
]}

Kopatskaya, Evgenia N. ^{[2
]}

Kurtanidze, Omar ^{[12
]}

Larionova, Elena G. ^{[2
]}

Larionova, Liudmilla V. ^{[2
]}

McHardy, Ian M. ^{[13
]}

Melnichuk, Daria A. ^{[2
]}

Roca-Sogorb, Mar ^{[4
]}

Schmidt, Gary D. ^{[5
]}

Skiff, Brian ^{[14
]}

Taylor, Brian ^{[1
,14
]}

Thum, Clemens ^{[15
]}

Troitsky, Ivan S. ^{[2
]}

Wiesemeyer, Helmut ^{[16
]}

机构：

[1] Boston Univ, Inst Astrophys Res, Boston, MA 02115 USA

[2] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia

[3] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia

[4] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[5] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[6] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[7] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland

[8] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA

[9] Russian Acad Sci, Main Pulkovo Astron Observ, St Petersburg 196140, Russia

[10] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[11] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland

[12] Abastumani Astrophys Observ, Mt Kanobili, Abastumani, Georgia

[13] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England

[14] Lowell Observ, Flagstaff, AZ 86001 USA

[15] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France

[16] IRAM, E-18012 Granada, Spain

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 715卷 / 01期

基金：

美国国家科学基金会; 芬兰科学院; 英国科学技术设施理事会;

关键词：

galaxies: active; galaxies: jets; polarization; quasars: individual (3C 454.3); X-rays: galaxies; ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC RADIO-SOURCES; GAMMA-RAY FLARE; BL-LACERTAE; POLARIMETRIC OBSERVATIONS; POLARIZATION VARIABILITY; HIGH-FREQUENCIES; WEBT CAMPAIGNS; XMM-NEWTON; INNER JET;

D O I：

10.1088/0004-637X/715/1/362

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyze the behavior of the parsec-scale jet of the quasar 3C 454.3 during pronounced flaring 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 millimeter-wave core lies at the end of the jet's acceleration and collimation zone. We infer that the X-ray emission is produced via inverse Compton scattering by relativistic electrons of photons both from within the jet (synchrotron self-Compton) and external to the jet (external Compton, or EC); which one dominates depends on the physical parameters of the jet. A broken power-law model of the gamma-ray spectrum reflects a steepening of the synchrotron emission spectrum from near-IR to soft UV wavelengths. We propose that the gamma-ray emission is dominated by the EC mechanism, with the sheath of the jet supplying seed photons for gamma-ray events that occur near the millimeter-wave core.

引用

页码：362 / 384

页数：23

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