The radio delay of the exceptional 3C 454.3 outburst -: Follow-up WEBT observations in 2005-2006

被引：71

作者：

Villata, M. ^{[1
]}

Raiteri, C. M. ^{[1
]}

Aller, M. F. ^{[2
]}

Bach, U. ^{[1
,3
]}

Ibrahimov, M. A. ^{[4
]}

Kovalev, Y. Y. ^{[3
,5
,6
]}

Kurtanidze, O. M. ^{[7
,8
,9
]}

Larionov, V. M. ^{[10
,11
]}

Lee, C. -U. ^{[12
]}

Leto, P. ^{[13
]}

Lahteenmaki, A. ^{[14
]}

Nilsson, K. ^{[15
]}

Pursimo, T. ^{[16
]}

Ros, J. A. ^{[17
]}

Sumitomo, N. ^{[18
]}

Volvach, A. ^{[19
]}

Aller, H. D. ^{[2
]}

Arai, A. ^{[18
]}

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

Coloma, J. M. ^{[17
]}

Doroshenko, V. T. ^{[21
]}

Efimov, Yu. S. ^{[22
]}

Fuhrmann, L. ^{[1
,3
,23
]}

Hagen-Thorn, V. A. ^{[10
,11
]}

Kamada, M. ^{[18
]}

Katsuura, M. ^{[18
]}

Konstantinova, T. ^{[10
]}

Kopatskaya, E. ^{[10
]}

Kotaka, D. ^{[18
]}

Kovalev, Yu. A. ^{[5
]}

Kurosaki, M. ^{[18
]}

Lanteri, L. ^{[1
]}

Larionova, L. ^{[10
]}

Mingaliev, M. G. ^{[24
]}

Mizoguchi, S. ^{[18
]}

Nakamura, K. ^{[18
]}

Nikolashvili, M. G. ^{[7
]}

Nishiyama, S. ^{[18
]}

Sadakane, K. ^{[18
]}

Sergeev, S. G. ^{[22
]}

Sigua, L. A. ^{[7
]}

Sillanpaa, A. ^{[15
]}

Smart, R. L. ^{[1
]}

Takalo, L. O. ^{[15
]}

Tanaka, K. ^{[18
]}

Tornikoski, M. ^{[14
]}

Trigilio, C. ^{[20
]}

Umana, G. ^{[20
]}

机构：

[1] Osserv Astron Torino, INAF, Turin, Italy

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

[3] Max Planck Inst Radioastron, Bonn, Germany

[4] Acad Sci Uzbek, Ulugh Beg Astron Inst, Tashkent, Uzbekistan

[5] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117924, Russia

[6] Natl Radio Astron Observ, Green Bank, WV USA

[7] Abastumani Astrophys Observ, Abastumani, Georgia

[8] Astrophys Inst Potsdam, Potsdam, Germany

[9] Landessternwarte Heidelberg Konigstuhl, Heidelberg, Germany

[10] St Petersburg State Univ, Astron Inst, St Petersburg 198904, Russia

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

[12] Korea Astron & Space Sci Inst, Taejon, South Korea

[13] INAF, Ist Radioastron, Sez Noto, Noto, Italy

[14] Aalto Univ, Metsahovi Radio Observ, Helsinki, Finland

[15] Tuorla Observ, Piikkio, Finland

[16] Roque de los Muchachos Astron Observ, Brena Baja, Isla De La Palm, Spain

[17] Agrupacio Astron Sabadell, Sabadell, Spain

[18] Osaka Kyoiku Univ, Astron Inst, Osaka, Japan

[19] Crimean Astrophys Observ, Radio Astron Lab, Crimea, Ukraine

[20] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy

[21] Moscow MV Lomonosov State Univ, Moscow, Russia

[22] Univ Perugia, Dipartimento Fis, I-06100 Perugia, Italy

[23] Univ Perugia, Osservatorio Astron, I-06100 Perugia, Italy

[24] Special Astrophys Observ, Zelenchukskaya, Karachaevo Cher, Russia

来源：

ASTRONOMY & ASTROPHYSICS | 2007年 / 464卷 / 02期

关键词：

galaxies : active; galaxies : quasars : general; galaxies : quasars : individual : 3C 454.3; galaxies : jets;

D O I：

10.1051/0004-6361:20066958

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. In spring 2005 the blazar 3C 454.3 was observed in an unprecedented bright state from the near-IR to the hard X-ray frequencies. A mm outburst peaked in June-July 2005, and it was followed by a flux increase at high radio frequencies. Aims. In this paper we report on multifrequency monitoring by the WEBT aimed at following the further evolution of the outburst in detail. In particular, we investigate the expected correlation and time delays between the optical and radio emissions in order to derive information on the variability mechanisms and jet structure. Methods. A comparison among the light curves at different frequencies is performed by means of visual inspection and discrete correlation function, and the results are interpreted with a simple model taking into account Doppler factor variations of geometric origin. Results. The high-frequency radio light curves show a huge outburst starting during the dimming phase of the optical one and lasting more than 1 year. The first phase is characterized by a slow flux increase, while in early 2006 a major flare is observed. The lower-frequency radio light curves show a progressively delayed and fainter event, which disappears below 8 GHz. We suggest that the radio major peak is not physically connected with the spring 2005 optical one, but it is actually correlated with a minor optical flare observed in October-November 2005. This interpretation involves both an intrinsic and a geometric mechanism. The former is represented by disturbances travelling down the emitting jet, the latter being due to the curved-jet motion, with the consequent differential changes of viewing angles of the di. erent emitting regions.

引用

页码：L5 / L9

页数：5

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