MULTIWAVELENGTH OBSERVATIONS OF 3C 454.3. I. THE AGILE 2007 NOVEMBER CAMPAIGN ON THE "CRAZY DIAMOND"

被引：71

作者：

Vercellone, S. ^{[1
]}

Chen, A. W. ^{[1
,2
]}

Vittorini, V. ^{[3
]}

Giuliani, A. ^{[1
]}

D'Ammando, F. ^{[3
,4
]}

Tavani, M. ^{[3
,4
]}

Donnarumma, I. ^{[3
]}

Pucella, G. ^{[3
]}

Raiteri, C. M. ^{[5
]}

Villata, M. ^{[5
]}

Chen, W. P. ^{[6
]}

Tosti, G.

Impiombato, D. ^{[7
]}

Romano, P. ^{[8
]}

Belfiore, A. ^{[9
]}

De Luca, A. ^{[1
,9
,10
]}

Novara, G. ^{[11
]}

Senziani, F. ^{[1
,9
]}

Bazzano, A. ^{[3
]}

Fiocchi, M. T. ^{[3
]}

Ubertini, P. ^{[3
]}

Ferrari, A. ^{[2
,12
]}

Argan, A. ^{[3
]}

Barbiellini, G.

Boffelli, F. ^{[10
,11
]}

Bulgarelli, A.

Caraveo, P. ^{[1
]}

Cattaneo, P. W. ^{[10
]}

Cocco, V. ^{[3
]}

Costa, E. ^{[3
]}

Del Monte, E. ^{[3
]}

De Paris, G. ^{[3
]}

Di Cocco, G. ^{[13
]}

Evangelista, Y. ^{[3
]}

Feroci, M. ^{[3
]}

Fiorini, M. ^{[1
]}

Fornari, F. ^{[1
]}

Froysland, T. ^{[3
,14
]}

Fuschino, F. ^{[13
]}

Galli, M. ^{[15
]}

Gianotti, F. ^{[13
]}

Labanti, C. ^{[13
]}

Lapshov, I. ^{[3
]}

Lazzarotto, F. ^{[3
]}

Lipari, P. ^{[16
]}

Longo, F. ^{[17
,18
]}

Marisaldi, M. ^{[13
]}

Mereghetti, S. ^{[1
]}

Morselli, A. ^{[14
]}

Pellizzoni, A. ^{[1
]}

机构：

[1] Ist Astrofis Spaziale & Fis Cosm Milano, Ist Nazl Astrofis, I-20133 Milan, Italy

[2] Consorzio Interuniv Fis Spaziale Torino, I-10133 Turin, Italy

[3] Ist Astrofis Spaziale & Fis Cosm Roma, Ist Nazl Astrofis, I-00133 Rome, Italy

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

[5] Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy

[6] Natl Cent Univ, Ist Astron, Chungli, Taiwan

[7] Univ Perugia, Dip Fis, I-06123 Perugia, Italy

[8] Consorzio Interuniv Fis Spaziale Palermo, I-90146 Palermo, Italy

[9] Ist Univ Super, I-27100 Pavia, Italy

[10] Ist Nazl Fis Nucl, I-27100 Pavia, Italy

[11] Univ Pavia, Dip Fis Nucl & Teor, I-27100 Pavia, Italy

[12] Univ Turin, Dip Fis, I-10125 Turin, Italy

[13] Ist Astrofis Spaziale & Fis Cosm Bologna, Ist Nazl Astrofis, I-40129 Bologna, Italy

[14] Ist Nazl Fis Nucl Roma Tor Vergata, I-00133 Rome, Italy

[15] Ente Nuovo Tecnol Energia & Ambiente Bologna, I-40129 Bologna, Italy

[16] Ist Nazl Fis Nucl Roma La Sapienza, I-00185 Rome, Italy

[17] Ist Nazl Fis Nucl, I-34127 Trieste, Italy

[18] Dip Fis, I-34127 Trieste, Italy

[19] Ente Nuovo Tecnol Energia & Ambiente Roma, I-00044 Frascati, Italy

[20] Sci Data Ctr, Agenzia Spaziale Italiana, I-00044 Rome, Italy

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

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 690卷 / 01期

关键词：

galaxies: active; galaxies: jets; quasars: general; quasars: individual (3C 454.3); radiation mechanisms: non-thermal; GAMMA-RAY SOURCES; BL-LAC OBJECTS; BLAZAR; 3C-454.3; INFRARED OBSERVATIONS; QUASAR; EGRET DETECTION; SPACE MISSION; TELESCOPE; RADIATION; OUTBURST;

D O I：

10.1088/0004-637X/690/1/1018

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on a multiwavelength observation of the blazar 3C 454.3 (which we dubbed crazy diamond) carried out on November 2007 by means of the astrophysical satellites AGILE, International Gamma-Ray Astrophysics Laboratory (INTEGRAL), Swift, the Whole Earth Blazar Telescope (WEBT) Consortium, and the optical-NIR telescope Rapid EyeMount (REM). Thanks to the wide field of view of the AGILE satellite and its prompt alert dissemination to other observatories, we obtained a long (three weeks), almost continuous. gamma-ray coverage of the blazar 3C 454.3 across 14 decades of energy. This broadband monitoring allows us to study in great detail light curves, correlations, time lags, and spectral energy distributions (SEDs) during different physical states. Gamma-ray data were collected during an AGILE pointing toward the Cygnus Region. Target of Opportunity (ToO) observations were performed to follow up the gamma-ray observations in the soft and hard X-ray energy bands. Optical data were acquired continuously by means of a preplanned WEBT campaign and through an REM ToO repointing. 3C 454.3 is detected at a similar to 19 sigma level during the three-week observing period, with an average flux above 100 MeV of F-E>100MeV = (170 +/- 13) x 10-8 photons cm-2 s-1. The gamma-ray spectrum can be fitted with a single power law with photon index Gamma(GRID) = 1.73 +/- 0.16 between 100 MeV and 1 GeV. We detect significant day-by-day variability of the gamma-ray emission during our observations, and we can exclude that the fluxes are constant at the 99.6% (similar to 2.9s) level. The source was detected typically around 40 deg off-axis, and it was substantially off-axis in the field of view of the AGILE hard X-ray imager. However, a five-day long ToO observation by INTEGRAL detected 3C 454.3 at an average flux of about F20-200 keV = 1.49 x 10(-3) photons cm(-2) s(-1)with an average photon index of Gamma(IBIS) = 1.75 +/- 0.24 between 20-200 keV. Swift also detected 3C 454.3 with a flux in the 0.3-10 keV energy band in the range (1.23-1.40) x 10(-2) photons cm(-2) s(-1) and a photon index in the range Gamma(XRT) = 1.56-1.73. In the optical band, both WEBT and REM show an extremely variable behavior in the R band. A correlation analysis based on the entire data set is consistent with no time lags between the gamma-ray and the optical flux variations. Our simultaneous multifrequency observations strongly indicate that the dominant emission mechanism between 30 MeV and 30 GeV is dominated by inverse Compton scattering of relativistic electrons in the jet on the external photons from the broad line region.

引用

页码：1018 / 1030

页数：13

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