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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

A peculiar multiwavelength flare in the blazar 3C 454.3

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Gupta, Alok C. [1, 2] ; Mangalam, Arun [3] ; Wiita, Paul J. [4, 5] ; Kushwaha, P. [6] ; Gaur, H. [1] ; Zhang, H. [7] ; Gu, M. F. [1] ; Liao, M. [1, 8] ; Dewangan, G. C. [9] ; Ho, L. C. [10, 11] ; Mohan, P. [12] ; Umeura, M. [13] ; Sasada, M. [14] ; Volvach, A. E. [15, 16] ; Agarwal, A. [2] ; Aller, M. F. [17] ; Aller, H. D. [17] ; Bachev, R. [18, 19] ; Lahteenmaki, A. [20] ; Semkov, E. [18, 19] ; Strigachev, A. [18, 19] ; Tornikoski, M. [20] ; Volvach, L. N. [15, 16]
Total Authors: 23
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[1] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030 - Peoples R China
[2] Aryabhatta Res Inst Observat Sci ARIES, Manora Peak 263002, Nainital - India
[3] Indian Inst Astrophys, Sarjapur Rd, Bangalore 560034, Karnataka - India
[4] Coll New Jersey, Dept Phys, POB 7718, Ewing, NJ 08628 - USA
[5] SLAC, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 - USA
[6] Univ Sao Paulo, Dept Astron IAG USP, BR-05508090 Sao Paulo - Brazil
[7] Ohio Univ, Dept Phys & Astron, Astrophys Inst, Athens, OH 45701 - USA
[8] Univ Chinese Acad Sci, 19A Yuquanlu, Beijing 100049 - Peoples R China
[9] Inter Univ Ctr Astron & Astrophys IUCAA, Post Bag 4, Pune 411007, Maharashtra - India
[10] Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Lu 5, Beijing 100871 - Peoples R China
[11] Peking Univ, Dept Astron, Yi He Yuan Lu 5, Beijing 100871 - Peoples R China
[12] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030 - Peoples R China
[13] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Kagamiyama 1-3-1, Higashihiroshima 7398526 - Japan
[14] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502 - Japan
[15] Crimean Astrophys Observ, Radio Astron Lab, UA-98688 Katsiveli, Crimea - Ukraine
[16] Taras Shevchenko Natl Univ Kyiv, 4 Academician Glushkov Ave, UA-03127 Kiev - Ukraine
[17] Univ Michigan, Astron Dept, 311 West Hall, Ann Arbor, MI 48109 - USA
[18] Bulgarian Acad Sci, Inst Astron, 72 Tsarigradsko Shosse Blvd, BU-1784 Sofia - Bulgaria
[19] Bulgarian Acad Sci, Natl Astron Observ, 72 Tsarigradsko Shosse Blvd, BU-1784 Sofia - Bulgaria
[20] Aalto Univ, Metsahovi Radio Observ, POB 11000, FI-00076 Aalto - Finland
Total Affiliations: 20
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 472, n. 1, p. 788-798, NOV 2017.
Web of Science Citations: 8

The blazar 3C 454.3 exhibited a strong flare seen in gamma-rays, X-rays and optical/near-infrared bands during 2009 December 3-12. Emission in the V and J bands rose more gradually than did the gamma-rays and soft X-rays, though all peaked at nearly the same time. Optical polarization measurements showed dramatic changes during the flare, with a strong anticorrelation between optical flux and degree of polarization (which rose from similar to 3 to similar to 20 per cent) during the declining phase of the flare. The flare was accompanied by large rapid swings in polarization angle of similar to 170.. This combination of behaviours appears to be unique. We have cm-band radio data during the same period but they show no correlation with variations at higher frequencies. Such peculiar behaviour may be explained using jet models incorporating fully relativistic effects with a dominant source region moving along a helical path or by a shock-in-jet model incorporating three-dimensional radiation transfer if there is a dominant helical magnetic field. We find that spectral energy distributions at different times during the flare can be fit using modified one-zone models where only the magnetic field strength and particle break frequencies and normalizations need change. An optical spectrum taken at nearly the same time provides an estimate for the central black hole mass of similar to 2.3 x 10(9) M-circle dot. We also consider two weaker flares seen during the similar to 200 d span over which multiband data are available. In one of them, the V and J bands appear to lead the gamma-ray and X-ray bands by a few days; in the other, all variations are simultaneous. (AU)

FAPESP's process: 15/13933-0 - Probing relativistic jets and high energy emission through Multi-wavelength observation analysis
Grantee:Pankaj Kushwaha
Support type: Scholarships in Brazil - Post-Doctorate