The structure and emission model of the relativistic jet in the quasar 3C279 inferred from radio to high-energy γ-ray observations in 2008-2010

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/100843

Title:	The structure and emission model of the relativistic jet in the quasar 3C279 inferred from radio to high-energy γ-ray observations in 2008-2010
Authors:	陳文屏;Hayashida, M.;Madejski, G. M.;Nalewajko, K.;Sikora, M.;Wehrle, A. E.;Ogle, P.;Collmar, W.;Larsson, S.;Fukazawa, Y.;Itoh, R.;Chiang, J.;Stawarz, Ł.;Blandford, R. D.;Richards, J. L.;Max-Moerbeck, W.;Readhead, A.;Buehler, R.;Cavazzuti, E.;Ciprini, S.;Gehrels, N.;Reimer, A.;Szostek, A.;Tanaka, T.;Tosti, G.;Uchiyama, Y.;Kawabata, K. S.;Kino, M.;Sakimoto, K.;Sasada, M.;Sato, S.;Uemura, M.;Yamanaka, M.;Greiner, J.;Kruehler, T.;Rossi, A.;Macquart, J. P.;Bock, D. C.-J.;Villata, M.;Raiteri, C. M.;Agudo, I.;Aller, H. D.;Aller, M. F.;Arkharov, A. A.;Bach, U.;Benítez, E.;Berdyugin, A.;Blinov, D. A.;Blumenthal, K.;Böttcher, M.;Buemi, C. S.;Carosati, D.;Chen, W. P.;Paola, A. Di;Dolci, M.;Efimova, N. V.;Forné, E.;Gómez, J. L.;Gurwell, M. A.;Heidt, J.;Hiriart, D.;Jordan, B.;Jorstad, S. G.;Joshi, M.;Kimeridze, G.;Konstantinova, T. S.;Kopatskaya, E. N.;Koptelova, E.;Kurtanidze, O. M.;Lähteenmäki, A.;Lamerato, A.;Larionov, V. M.;Larionova, E. G.;Larionova, L. V.;Leto, P.;Lindfors, E.;Marscher, A. P.;McHardy, I. M.;Molina, S. N.;Morozova, D. A.;Nikolashvili, M. G.;Nilsson, K.;Reinthal, R.;Roustazadeh, P.;Sakamoto, T.;Sigua, L. A.;Sillanpää, A.;Takalo, L.;Tammi, J.;Taylor, B.;Tornikoski, M.;Trigilio, C.;Troitsky, I. S.;Umana, G.
Contributors:	理學院天文研究所
Keywords:	Astronomy;Band spectra;Banded structure;Broadband;Earth, ocean, space;Emission;Emission analysis;Exact sciences and technology;Flares;galaxies: active;galaxies: jets;gamma rays: galaxies;Quasars;quasars: individual (3C 279);radiation mechanisms: non-thermal;Synchrotrons;X-rays: galaxies
Date:	2012-08-01
Issue Date:	2026-04-21 14:16:02 (UTC+8)
Publisher:	IOP Publishing Ltd.;Bristol: IOP
Abstract:	摘要： We present time-resolved broadband observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma -ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears to be delayed with respect to the gamma -ray emission by about 10 days. X-ray observations reveal a pair of "isolated" flares separated by ~90 days, with only weak gamma -ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the gamma -ray flare, while the peak appears in the millimeter (mm)/submillimeter (sub-mm) band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broadband spectra during the gamma -ray flaring event by a shift of its location from ~1 pc to ~4 pc from the central black hole. On the other hand, if the gamma -ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission. 出版者： Bristol: IOP 出版日期： 2012-08-01 出處： The Astrophysical journal, 2012-08, Vol.754 (2), p.114-22 資源來源： Institute of Physics Journals 版權： 2015 INIST-CNRS 識別號： ISSN: 0004-637X 識別號： ISSN: 1538-4357 識別號： EISSN: 1538-4357 識別號： DOI: 10.1088/0004-637X/754/2/114 識別號： CODEN: ASJOAB
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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