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3C 454.3的多波长观测。III。AGILE对“疯狂钻石”的18个月监测

Multiwavelength observations of 3C 454.3. III. Eighteen months of AGILE monitoring of the "Crazy Diamond"

S. Vercellone, F. D'Ammando, V. Vittorini, I. Donnarumma, G. Pucella, M. Tavani, A. Ferrari, C. M. Raiteri, M. Villata, P. Romano, H. Krimm, A. Tiengo, A. W. Ch… 展开作者

S. Vercellone, F. D'Ammando, V. Vittorini, I. Donnarumma, G. Pucella, M. Tavani, A. Ferrari, C. M. Raiteri, M. Villata, P. Romano, H. Krimm, A. Tiengo, A. W. Chen, G. Giovannini, T. Venturi, M. Giroletti, Y. Y. Kovalev, K. Sokolovsky, A. B. Pushkarev, M. L. Lister, A. Argan, G. Barbiellini, A. Bulgarelli, P. Caraveo, P. W. Cattaneo, V. Cocco, E. Costa, E. Del Monte, G. De Paris, G. Di Cocco, Y. Evangelista, M. Feroci, M. Fiorini, F. Fornari, T. Froysland, F. Fuschino, M. Galli, F. Gianotti, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, F. Longo, A. Giuliani, M. Marisaldi, S. Mereghetti, A. Morselli, A. Pellizzoni, L. Pacciani, F. Perotti, G. Piano, P. Picozza, M. Pilia, M. Prest, M. Rapisarda, A. Rappoldi, S. Sabatini, P. Soffitta, E. Striani, M. Trifoglio, A. Trois, E. Vallazza, A. Zambra, D. Zanello, C. Pittori, F. Verrecchia, P. Santolamazza, P. Giommi, S. Colafrancesco, L. Salotti, I. Agudo, H. D. Aller, M. F. Aller, A. A. Arkharov, U. Bach, R. Bachev, P. Beltrame, E. Benitez, M. Boettcher, C. S. Buemi, P. Calcidese, D. Capezzali, D. Carosati, W. P. Chen, D. Da Rio, A. Di Paola, M. Dolci, D. Dultzin, E. Forne, J. L. Gomez, M. A. Gurwell, V. A. Hagen-Thorn, A. Halkola, J. Heidt, D. Hiriart, T. Hovatta, H. Y. Hsiao, S. G. Jorstad, G. Kimeridze, T. S. Konstantinova, E. N. Kopatskaya, E. Koptelova, O. Kurtanidze, A. Lahteenmaki, V. M. Larionov, P. Leto, R. Ligustri, E. Lindfors, J. M. Lopez, A. P. Marscher, R. Mujica, M. Nikolashvili, K. Nilsson

备注：
Accepted for publication in ApJ. Adapted Abstract. 17 pages, 19 Figures, 5 Tables
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摘要：

我们报告了2007年7月至2009年1月对耀变体3C 454.3（疯狂钻石）进行的18个月的多波长观测。我们展示了2008年5月至6月、2008年7月至8月和2008年10月至2009年1月进行的AGILE活动的结果。在2008年5月至2009年1月期间，源的平均通量变化很大，从2008年5月至6月的平均γ射线通量F（E> 100 MeV）> 200 E-8 ph/cm 2/s到2008年10月至2009年1月的F（E> 100 MeV）~ 80 E-8 ph/cm 2/s。100 MeV和1 GeV之间的平均伽马射线谱可以用简单的幂律拟合（Gamma_GRID ~ 2.0 to 2.2）。在20-60 keV能带中，只能使用Super-AGILE导出3-sigma上限。在2007年7月至8月和2008年5月至6月期间，RXTE分别测量了F（3-20 keV）= 8.4E-11 erg/cm 2/s和F（3-20 keV）=4.5E-11 erg/cm 2/s的通量，以及恒定光子指数Gamma_PCA=1.65。在所有AGILE活动期间进行了Swift/XRT观测，获得F（2-10 keV）=（0.9-7.5）E-11 erg/cm 2/s和光子指数Gamma_XRT=1.33-2.04。BAT测得的平均通量约为5 mCrab。GASP-WEBT在整个2007-2008年期间从无线电到光学监测3C 454.3。光学通量和伽马射线通量之间的相关性分析显示τ =-0.4天的时滞。对15 GHz和43 GHz VLBI核心射电通量观测结果的分析表明，核心射电通量有增加的趋势，与较高频率的数据呈反相关。模拟的SED，以及在不同的能量带的长期光变曲线的行为，使我们能够比较在不同的发射状态下的喷流特性，并研究喷流的几何特性的时间跨度超过一年。

英文摘要：

We report on 18 months of multiwavelength observations of the blazar 3C 454.3 (Crazy Diamond) carried out in July 2007-January 2009. We show the results of the AGILE campaigns which took place on May-June 2008, July-August 2008, and October 2008-January 2009. During the May 2008-January 2009 period, the source average flux was highly variable, from an average gamma-ray flux F(E>100MeV) > 200E-8 ph/cm2/s in May-June 2008, to F(E>100MeV)~80E-8 ph/cm2/s in October 2008-January 2009. The average gamma-ray spectrum between 100 MeV and 1 GeV can be fit by a simple power law (Gamma_GRID ~ 2.0 to 2.2). Only 3-sigma upper limits can be derived in the 20-60 keV energy band with Super-AGILE. During July-August 2007 and May-June 2008, RXTE measured a flux of F(3-20 keV)= 8.4E-11 erg/cm2/s, and F(3-20 keV)=4.5E-11 erg/cm2/s, respectively and a constant photon index Gamma_PCA=1.65. Swift/XRT observations were carried out during all AGILE campaigns, obtaining a F(2-10 keV)=(0.9-7.5)E-11 erg/cm2/s and a photon index Gamma_XRT=1.33-2.04. BAT measured an average flux of ~5 mCrab. GASP-WEBT monitored 3C 454.3 during the whole 2007-2008 period from the radio to the optical. A correlation analysis between the optical and the gamma-ray fluxes shows a time lag of tau=-0.4 days. An analysis of 15 GHz and 43 GHz VLBI core radio flux observations shows an increasing trend of the core radio flux, anti- correlated with the higher frequency data. The modeling SEDs, and the behavior of the long-term light curves in different energy bands, allow us to compare the jet properties during different emission states, and to study the geometrical properties of the jet on a time-span longer than one year.

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