Exceptional outburst of the blazar CTA 102 in 2012: the GASP-WEBT campaign and its extension

被引：51

作者：

Larionov, V. M. ^{[1
,2
]}

Villata, M. ^{[3
]}

Raiteri, C. M. ^{[3
]}

Jorstad, S. G. ^{[1
,4
]}

Marscher, A. P. ^{[4
]}

Agudo, I. ^{[5
]}

Smith, P. S. ^{[6
]}

Acosta-Pulido, J. A. ^{[7
,8
]}

Arevalo, M. J. ^{[7
,8
]}

Arkharov, A. A. ^{[2
]}

Bachev, R. ^{[9
]}

Blinov, D. A. ^{[1
,10
,11
,12
]}

Borisov, G. ^{[9
,13
]}

Borman, G. A. ^{[14
]}

Bozhilov, V. ^{[15
]}

Bueno, A. ^{[7
,8
]}

Carnerero, M. I. ^{[3
,7
,8
]}

Carosati, D. ^{[16
,17
]}

Casadio, C. ^{[5
]}

Chen, W. P. ^{[18
]}

Clemens, D. P. ^{[4
]}

Di Paola, A. ^{[19
]}

Ehgamberdiev, Sh. A. ^{[20
]}

Gomez, J. L. ^{[5
]}

Gonzalez-Morales, P. A. ^{[7
,8
]}

Grinon-Marin, A. ^{[7
,8
]}

Grishina, T. S. ^{[1
]}

Hagen-Thorn, V. A. ^{[1
]}

Ibryamov, S. ^{[9
]}

Itoh, R. ^{[21
]}

Joshi, M. ^{[4
]}

Kopatskaya, E. N. ^{[1
]}

Koptelova, E. ^{[18
]}

Lazaro, C. ^{[7
,8
]}

Larionova, E. G. ^{[1
]}

Larionova, L. V. ^{[1
]}

Manilla-Robles, A. ^{[7
,8
]}

Metodieva, Y. ^{[15
]}

Milanova, Yu. V. ^{[1
]}

Mirzaqulov, D. O. ^{[20
]}

Molina, S. N. ^{[5
]}

Morozova, D. A. ^{[1
]}

Nazarov, S. V. ^{[14
]}

Ovcharov, E. ^{[15
]}

Peneva, S. ^{[9
]}

Ros, J. A. ^{[22
]}

Sadun, A. C. ^{[23
]}

Savchenko, S. S. ^{[1
]}

Semkov, E. ^{[9
]}

Sergeev, S. G. ^{[14
]}

机构：

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

[2] Pulkovo Observ, St Petersburg 196140, Russia

[3] Osservatorio Astrofis Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy

[4] Boston Univ, Inst Astrophys Res, Boston, MA 22015 USA

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

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

[7] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain

[8] Univ La Laguna, Dept Astrofis, Tenerife, Spain

[9] Bulgarian Acad Sci, Inst Astron, BG-1784 Sofia, Bulgaria

[10] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece

[11] Univ Crete, Inst Plasma Phys, GR-71003 Iraklion, Greece

[12] IESL, Fdn Res & Technol Hellas, GR-7110 Iraklion, Greece

[13] Armagh Observ, Armagh, North Ireland

[14] Crimean Astrophys Observ, Po Nauchny 298409, Russia

[15] Univ Sofia, Fac Phys, Dept Astron, BG-1164 Sofia, Bulgaria

[16] EPT Observ, E-38780 Tijarafe, La Palma, Spain

[17] TNG Fdn Galileo Galilei, INAF, E-38712 La Palma, Spain

[18] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan

[19] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[20] Ulugh Beg Astron Inst, Maidanak Observ, Tashkent, Uzbekistan

[21] Hiroshima Univ, Dept Phys Sci, Hiroshima 730, Japan

[22] Agrupacio Astron Sabadell, Barcelona, Spain

[23] Univ Colorado, Dept Phys, Denver, CO 80217 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 461卷 / 03期

基金：

芬兰科学院; 美国国家科学基金会;

关键词：

methods: observational; techniques: photometric; techniques: polarimetric; galaxies: active; quasars: individual: CTA 102; LARGE-AREA TELESCOPE; STELLAR RADIO-SOURCES; GAMMA-RAY FLARE; 3C; 454.3; BL LACERTAE; EMISSION-LINE; VARIABILITY; FERMI; POLARIZATION; JET;

D O I：

10.1093/mnras/stw1516

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

After several years of quiescence, the blazar CTA 102 underwent an exceptional outburst in 2012 September-October. The flare was tracked from gamma-ray to near-infrared (NIR) frequencies, including Fermi and Swift data as well as photometric and polarimetric data from several observatories. An intensive Glast-Agile support programme of the Whole Earth Blazar Telescope (GASP-WEBT) collaboration campaign in optical and NIR bands, with an addition of previously unpublished archival data and extension through fall 2015, allows comparison of this outburst with the previous activity period of this blazar in 2004-2005. We find remarkable similarity between the optical and gamma-ray behaviour of CTA 102 during the outburst, with a time lag between the two light curves of approximate to 1 h, indicative of cospatiality of the optical and gamma-ray emission regions. The relation between the gamma-ray and optical fluxes is consistent with the synchrotron self-Compton (SSC) mechanism, with a quadratic dependence of the SSC gamma -ray flux on the synchrotron optical flux evident in the post-outburst stage. However, the gamma -ray/optical relationship is linear during the outburst; we attribute this to changes in the Doppler factor. A strong harder-when-brighter spectral dependence is seen both the in gamma-ray and optical non-thermal emission. This hardening can be explained by convexity of the UV-NIR spectrum that moves to higher frequencies owing to an increased Doppler shift as the viewing angle decreases during the outburst stage. The overall pattern of Stokes parameter variations agrees with a model of a radiating blob or shock wave that moves along a helical path down the jet.

引用

页码：3047 / 3056

页数：10

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