Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007
| Autor: | V. M. Larionov, S. G. Jorstad, A. P. Marscher, C. M. Raiteri, M. Villata, I. Agudo, M. F. Aller, A. A. Arkharov, I. M. Asfandiyarov, U. Bach, R. Bachev, A. Berdyugin, M. Böttcher, C. S. Buemi, P. Calcidese, D. Carosati, P. Charlot, W.-P. Chen, A. Di Paola, M. Dolci, S. Dogru, V. T. Doroshenko, Yu. S. Efimov, A. Erdem, A. Frasca, L. Fuhrmann, P. Giommi, L. Glowienka, A. C. Gupta, M. A. Gurwell, V. A. Hagen-Thorn, W.-S. Hsiao, M. A. Ibrahimov, B. Jordan, M. Kamada, T. S. Konstantinova, E. N. Kopatskaya, Y. Y. Kovalev, Y. A. Kovalev, O. M. Kurtanidze, A. Lähteenmäki, L. Lanteri, L. V. Larionova, P. Leto, P. Le Campion, C.-U. Lee, E. Lindfors, E. Marilli, I. McHardy, M. G. Mingaliev, S. V. Nazarov, E. Nieppola, K. Nilsson, J. Ohlert, M. Pasanen, D. Porter, T. Pursimo, J. A. Ros, K. Sadakane, A. C. Sadun, S. G. Sergeev, N. Smith, A. Strigachev, N. Sumitomo, L. O. Takalo, K. Tanaka, C. Trigilio, G. Umana, H. Ungerechts, A. Volvach, W. Yuan |
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| Přispěvatelé: | INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS) |
| Jazyk: | angličtina |
| Rok vydání: | 2008 |
| Předmět: |
Brightness
Photon [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] Astrophysics::High Energy Astrophysical Phenomena galaxies: active [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] quasars: general 0103 physical sciences Radiative transfer quasars: individual: 3C 279 010303 astronomy & astrophysics Physics 010308 nuclear & particles physics Linear polarization Astrophysics (astro-ph) Compton scattering Spectral density Astronomy and Astrophysics Light curve Polarization (waves) Space and Planetary Science |
| Zdroj: | Larionov, V M, Jorstad, S G, Marscher, A P, Raiteri, C M, Villata, M, Agudo, I, Aller, M F, Arkharov, A A, Asfandiyarov, I M, Bach, U, Bachev, R, Berdyugin, A, Böttcher, M, Buemi, C S, Calcidese, P, Carosati, D, Charlot, P, Chen, W-P, Di Paola, A, Dolci, M, Dogru, S, Doroshenko, V T, Efimov, Y S, Erdem, A, Frasca, A, Fuhrman, L, Giommi, P, Glowienka, L & ... 2008, ' Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007 ', Astronomy & Astrophysics, vol. 492, no. 2, pp. 389-400 . https://doi.org/10.1051/0004-6361:200810937 Astronomy and Astrophysics-A&A Astronomy and Astrophysics-A&A, EDP Sciences, 2008, 492 (2), pp.389-400. ⟨10.1051/0004-6361:200810937⟩ |
| ISSN: | 0004-6361 |
| Popis: | We present radio-to-optical data taken by the WEBT, supplemented by VLBA and RXTE observations, of 3C 279. Our goal is to use this extensive database to draw inferences regarding the physics of the relativistic jet. We assemble multifrequency light curves with data from 30 ground-based observatories and the space-based instruments, along with linear polarization vs. time in the optical R band. In addition, we present a sequence of 22 images (with polarization vectors) at 43 GHz at resolution 0.15 milliarcsec, obtained with the VLBA. We analyse the light curves and polarization, as well as the spectral energy distributions at different epochs, corresponding to different brightness states. The IR-optical-UV continuum spectrum of the variable component corresponds to a power law with a constant slope of -1.6, while in the 2.4-10 keV X-ray band it varies in slope from -1.1 to -1.6. The steepest X-ray spectrum occurs at a flux minimum. During a decline in flux from maximum in late 2006, the optical and 43 GHz core polarization vectors rotate by ~300 degrees. The continuum spectrum agrees with steady injection of relativistic electrons with a power-law energy distribution of slope -3.2 that is steepened to -4.2 at high energies by radiative losses. The X-ray emission at flux minimum comes most likely from a new component that starts in an upstream section of the jet where inverse Compton scattering of seed photons from outside the jet is important. The rotation of the polarization vector implies that the jet contains a helical magnetic field that extends ~20 pc past the 43 GHz core. 12 pages, aa.cls style; accepted for publication in A&A |
| Databáze: | OpenAIRE |
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