THE 2009 DECEMBER GAMMA-RAY FLARE OF 3C 454.3: THE MULTIFREQUENCY CAMPAIGN

被引：48

作者：

Pacciani, L. ^{[1
]}

Vittorini, V. ^{[1
,2
]}

Tavani, M. ^{[1
,2
]}

Fiocchi, M. T. ^{[1
]}

Vercellone, S. ^{[3
]}

D'Ammando, F. ^{[3
]}

Sakamoto, T. ^{[4
,5
]}

Pian, E. ^{[6
,7
]}

Raiteri, C. M. ^{[8
]}

Villata, M. ^{[8
]}

Sasada, M. ^{[9
]}

Itoh, R. ^{[9
]}

Yamanaka, M. ^{[9
,10
]}

Uemura, M. ^{[10
]}

Striani, E. ^{[2
,11
]}

Fugazza, D. ^{[12
]}

Tiengo, A. ^{[13
]}

Krimm, H. A. ^{[4
,14
]}

Stroh, M. C. ^{[15
]}

Falcone, A. D. ^{[15
]}

Curran, P. A. ^{[16
]}

Sadun, A. C. ^{[17
]}

Lahteenmaki, A. ^{[18
]}

Tornikoski, M. ^{[18
]}

Aller, H. D. ^{[19
]}

Aller, M. F. ^{[19
]}

Lin, C. S. ^{[20
]}

Larionov, V. M. ^{[21
,22
,23
]}

Leto, P. ^{[24
]}

Takalo, L. O. ^{[25
]}

Berdyugin, A. ^{[25
]}

Gurwell, M. A. ^{[26
]}

Bulgarelli, A. ^{[27
]}

Chen, A. W. ^{[13
,28
]}

Donnarumma, I. ^{[1
]}

Giuliani, A. ^{[13
]}

Longo, F. ^{[29
,30
]}

Pucella, G. ^{[31
]}

Argan, A. ^{[1
]}

Barbiellini, G. ^{[29
,30
]}

Caraveo, P. ^{[13
]}

Cattaneo, P. W.

Costa, E. ^{[1
]}

De Paris, G. ^{[1
]}

Del Monte, E. ^{[1
]}

Di Cocco, G. ^{[27
]}

Evangelista, Y. ^{[1
]}

Ferrari, A. ^{[32
]}

Feroci, M. ^{[1
]}

Fiorini, M. ^{[13
]}

机构：

[1] INAF IASF Roma, I-00133 Rome, Italy

[2] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy

[3] INAF IASF Palermo, I-90146 Palermo, Italy

[4] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA

[5] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA

[6] INAF OATS, I-34143 Trieste, Italy

[7] SNS, I-56126 Pisa, Italy

[8] OATO INAF, I-10025 Pino Torinese, To, Italy

[9] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan

[10] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan

[11] INFN Roma Tor Vergata, I-00133 Rome, Italy

[12] OAB INAF, I-20121 Milan, Italy

[13] INAF IASF Milano, I-20133 Milan, Italy

[14] Univ Space Res Assoc, Columbia, MD 21044 USA

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

[16] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[17] Univ Colorado, Denver, CO 80202 USA

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

[19] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[20] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan

[21] St Petersburg State Univ, Astron Inst, St Petersburg, Russia

[22] Pulkovo Observ, St Petersburg, Russia

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

[24] Osserv Astrofis Catania, INAF, Catania, Italy

[25] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland

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

[27] INAF IASF Bologna, I-40129 Bologna, Italy

[28] CIFS Torino, I-10133 Turin, Italy

[29] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[30] INFN Trieste, I-34127 Trieste, Italy

[31] ENEA Frascati, I-00044 Rome, Italy

[32] Univ Turin, Dip Fis, Turin, Italy

[33] ENEA Bologna, I-40129 Bologna, Italy

[34] INFN Roma La Sapienza, I-00185 Rome, Italy

[35] INAF OAC, I-09012 Capoterra, Italy

[36] Univ Insubria, Dip Fis, I-22100 Como, Italy

[37] ASI Sci Data Ctr, I-00044 Rome, Italy

[38] Agenzia Spaziale Italiana, I-00198 Rome, Italy

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 716卷 / 02期

关键词：

galaxies: active; galaxies: individual (3C 454.3); quasars: general; radiation mechanisms: non-thermal; MULTIWAVELENGTH OBSERVATIONS; TIMING EXPLORER; CRAZY-DIAMOND; BLAZAR MODEL; WEBT; TELESCOPE; OUTBURST; CALIBRATION; 3C-454.3; RADIO;

D O I：

10.1088/2041-8205/716/2/L170

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

During the month of 2009 December, the blazar 3C 454.3 became the brightest gamma-ray source in the sky, reaching a peak flux F similar to 2000 x 10(-8) photons cm(-2) s(-1) for E > 100 MeV. Starting in 2009 November intensive multifrequency campaigns monitored the 3C 454 gamma-ray outburst. Here, we report on the results of a two-month campaign involving AGILE, INTEGRAL, Swift/XRT, Swift/BAT, and Rossi XTE for the high-energy observations and Swift/UVOT, KANATA, Goddard Robotic Telescope, and REM for the near-IR/optical/UV data. GASP/WEBT provided radio and additional optical data. We detected a long-term active emission phase lasting similar to 1 month at all wavelengths: in the gamma-ray band, peak emission was reached on 2009 December 2-3. Remarkably, this gamma-ray super-flare was not accompanied by correspondingly intense emission in the optical/UV band that reached a level substantially lower than the previous observations in 2007-2008. The lack of strong simultaneous optical brightening during the super-flare and the determination of the broadband spectral evolution severely constrain the theoretical modeling. We find that the pre- and post-flare broadband behavior can be explained by a one-zone model involving synchrotron self-Compton plus external Compton emission from an accretion disk and a broad-line region. However, the spectra of the 2009 December 2-3 super-flare and of the secondary peak emission on 2009 December 9 cannot be satisfactorily modeled by a simple one-zone model. An additional particle component is most likely active during these states.

引用

页码：L170 / L175

页数：6

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