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Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007. / 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.; Di Paola, A.; Dolci, M.; Dogru, S.; Doroshenko, V. T.; Efimov, Yu S.; Erdem, A.; Frasca, A.; Fuhrmann, L.; Giommi, P.; Glowienka, L.; Gupta, A. C.; Gurwell, M. A.; Hagen-Thorn, V. A.; Hsiao, W. S.; Ibrahimov, M. A.; Jordan, B.; Kamada, M.; Konstantinova, T. S.; Kopatskaya, E. N.; Kovalev, Y. Y.; Kovalev, Y. A.; Kurtanidze, O. M.; Lähteenmäki, A.; Lanteri, L.; Larionova, L. V.; Leto, P.; Le Campion, P.; Lindfors, E.; Marilli, E.; McHardy, I.; Mingaliev, M. G.; Nazarov, S. V.; Nieppola, E.; Nilsson, K.; Ohlert, J.; Pasanen, M.; Porter, D.; Pursimo, T.; Ros, J. A.; Sadakane, K.; Sadun, A. C.; Sergeev, S. G.; Smith, N.; Strigachev, A.; Sumitomo, N.; Takalo, L. O.; Tanaka, K.; Trigilio, C.; Umana, G.; Ungerechts, H.; Volvach, A.

в: Astronomy and Astrophysics, Том 492, № 2, 12.2008, стр. 389-400.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Larionov, VM, Jorstad, SG, Marscher, AP, Raiteri, CM, Villata, M, Agudo, I, Aller, MF, Arkharov, AA, Asfandiyarov, IM, Bach, U, Bachev, R, Berdyugin, A, Böttcher, M, Buemi, CS, Calcidese, P, Carosati, D, Charlot, P, Di Paola, A, Dolci, M, Dogru, S, Doroshenko, VT, Efimov, YS, Erdem, A, Frasca, A, Fuhrmann, L, Giommi, P, Glowienka, L, Gupta, AC, Gurwell, MA, Hagen-Thorn, VA, Hsiao, WS, Ibrahimov, MA, Jordan, B, Kamada, M, Konstantinova, TS, Kopatskaya, EN, Kovalev, YY, Kovalev, YA, Kurtanidze, OM, Lähteenmäki, A, Lanteri, L, Larionova, LV, Leto, P, Le Campion, P, Lindfors, E, Marilli, E, McHardy, I, Mingaliev, MG, Nazarov, SV, Nieppola, E, Nilsson, K, Ohlert, J, Pasanen, M, Porter, D, Pursimo, T, Ros, JA, Sadakane, K, Sadun, AC, Sergeev, SG, Smith, N, Strigachev, A, Sumitomo, N, Takalo, LO, Tanaka, K, Trigilio, C, Umana, G, Ungerechts, H & Volvach, A 2008, 'Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007', Astronomy and Astrophysics, Том. 492, № 2, стр. 389-400. https://doi.org/10.1051/0004-6361:200810937

APA

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., Di Paola, A., Dolci, M., ... Volvach, A. (2008). Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007. Astronomy and Astrophysics, 492(2), 389-400. https://doi.org/10.1051/0004-6361:200810937

Vancouver

Larionov VM, Jorstad SG, Marscher AP, Raiteri CM, Villata M, Agudo I и пр. Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007. Astronomy and Astrophysics. 2008 Дек.;492(2):389-400. https://doi.org/10.1051/0004-6361:200810937

Author

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. ; Di Paola, A. ; Dolci, M. ; Dogru, S. ; Doroshenko, V. T. ; Efimov, Yu S. ; Erdem, A. ; Frasca, A. ; Fuhrmann, L. ; Giommi, P. ; Glowienka, L. ; Gupta, A. C. ; Gurwell, M. A. ; Hagen-Thorn, V. A. ; Hsiao, W. S. ; Ibrahimov, M. A. ; Jordan, B. ; Kamada, M. ; Konstantinova, T. S. ; Kopatskaya, E. N. ; Kovalev, Y. Y. ; Kovalev, Y. A. ; Kurtanidze, O. M. ; Lähteenmäki, A. ; Lanteri, L. ; Larionova, L. V. ; Leto, P. ; Le Campion, P. ; Lindfors, E. ; Marilli, E. ; McHardy, I. ; Mingaliev, M. G. ; Nazarov, S. V. ; Nieppola, E. ; Nilsson, K. ; Ohlert, J. ; Pasanen, M. ; Porter, D. ; Pursimo, T. ; Ros, J. A. ; Sadakane, K. ; Sadun, A. C. ; Sergeev, S. G. ; Smith, N. ; Strigachev, A. ; Sumitomo, N. ; Takalo, L. O. ; Tanaka, K. ; Trigilio, C. ; Umana, G. ; Ungerechts, H. ; Volvach, A. / Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007. в: Astronomy and Astrophysics. 2008 ; Том 492, № 2. стр. 389-400.

BibTeX

@article{3e7ff696c23543f589bb3993a928d1aa,
title = "Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007",
abstract = "Context. The quasar 3C 279 is among the most extreme blazars in terms of luminosity and variability of flux at all wavebands. Its variations in flux and polarization are quite complex and therefore require intensive monitoring observations at multiple wavebands to characterise and interpret the observed changes.Aims. In this paper, we present radio-to-optical data taken by the WEBT, supplemented by our 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.Methods. We assemble multifrequency light curves with data from 30 ground-based observatories and the space-based instruments SWIFT (UVOT) and RXTE, 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.Results. We find that 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°.Conclusions. 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.",
keywords = "Galaxies: active, Quasars: general, Quasars: individual: 3C 279",
author = "Larionov, {V. M.} and Jorstad, {S. G.} and Marscher, {A. P.} and Raiteri, {C. M.} and M. Villata and I. Agudo and Aller, {M. F.} and Arkharov, {A. A.} and Asfandiyarov, {I. M.} and U. Bach and R. Bachev and A. Berdyugin and M. B{\"o}ttcher and Buemi, {C. S.} and P. Calcidese and D. Carosati and P. Charlot and {Di Paola}, A. and M. Dolci and S. Dogru and Doroshenko, {V. T.} and Efimov, {Yu S.} and A. Erdem and A. Frasca and L. Fuhrmann and P. Giommi and L. Glowienka and Gupta, {A. C.} and Gurwell, {M. A.} and Hagen-Thorn, {V. A.} and Hsiao, {W. S.} and Ibrahimov, {M. A.} and B. Jordan and M. Kamada and Konstantinova, {T. S.} and Kopatskaya, {E. N.} and Kovalev, {Y. Y.} and Kovalev, {Y. A.} and Kurtanidze, {O. M.} and A. L{\"a}hteenm{\"a}ki and L. Lanteri and Larionova, {L. V.} and P. Leto and {Le Campion}, P. and E. Lindfors and E. Marilli and I. McHardy and Mingaliev, {M. G.} and Nazarov, {S. V.} and E. Nieppola and K. Nilsson and J. Ohlert and M. Pasanen and D. Porter and T. Pursimo and Ros, {J. A.} and K. Sadakane and Sadun, {A. C.} and Sergeev, {S. G.} and N. Smith and A. Strigachev and N. Sumitomo and Takalo, {L. O.} and K. Tanaka and C. Trigilio and G. Umana and H. Ungerechts and A. Volvach",
year = "2008",
month = dec,
doi = "10.1051/0004-6361:200810937",
language = "English",
volume = "492",
pages = "389--400",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "2",

}

RIS

TY - JOUR

T1 - Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007

AU - Larionov, V. M.

AU - Jorstad, S. G.

AU - Marscher, A. P.

AU - Raiteri, C. M.

AU - Villata, M.

AU - Agudo, I.

AU - Aller, M. F.

AU - Arkharov, A. A.

AU - Asfandiyarov, I. M.

AU - Bach, U.

AU - Bachev, R.

AU - Berdyugin, A.

AU - Böttcher, M.

AU - Buemi, C. S.

AU - Calcidese, P.

AU - Carosati, D.

AU - Charlot, P.

AU - Di Paola, A.

AU - Dolci, M.

AU - Dogru, S.

AU - Doroshenko, V. T.

AU - Efimov, Yu S.

AU - Erdem, A.

AU - Frasca, A.

AU - Fuhrmann, L.

AU - Giommi, P.

AU - Glowienka, L.

AU - Gupta, A. C.

AU - Gurwell, M. A.

AU - Hagen-Thorn, V. A.

AU - Hsiao, W. S.

AU - Ibrahimov, M. A.

AU - Jordan, B.

AU - Kamada, M.

AU - Konstantinova, T. S.

AU - Kopatskaya, E. N.

AU - Kovalev, Y. Y.

AU - Kovalev, Y. A.

AU - Kurtanidze, O. M.

AU - Lähteenmäki, A.

AU - Lanteri, L.

AU - Larionova, L. V.

AU - Leto, P.

AU - Le Campion, P.

AU - Lindfors, E.

AU - Marilli, E.

AU - McHardy, I.

AU - Mingaliev, M. G.

AU - Nazarov, S. V.

AU - Nieppola, E.

AU - Nilsson, K.

AU - Ohlert, J.

AU - Pasanen, M.

AU - Porter, D.

AU - Pursimo, T.

AU - Ros, J. A.

AU - Sadakane, K.

AU - Sadun, A. C.

AU - Sergeev, S. G.

AU - Smith, N.

AU - Strigachev, A.

AU - Sumitomo, N.

AU - Takalo, L. O.

AU - Tanaka, K.

AU - Trigilio, C.

AU - Umana, G.

AU - Ungerechts, H.

AU - Volvach, A.

PY - 2008/12

Y1 - 2008/12

N2 - Context. The quasar 3C 279 is among the most extreme blazars in terms of luminosity and variability of flux at all wavebands. Its variations in flux and polarization are quite complex and therefore require intensive monitoring observations at multiple wavebands to characterise and interpret the observed changes.Aims. In this paper, we present radio-to-optical data taken by the WEBT, supplemented by our 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.Methods. We assemble multifrequency light curves with data from 30 ground-based observatories and the space-based instruments SWIFT (UVOT) and RXTE, 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.Results. We find that 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°.Conclusions. 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.

AB - Context. The quasar 3C 279 is among the most extreme blazars in terms of luminosity and variability of flux at all wavebands. Its variations in flux and polarization are quite complex and therefore require intensive monitoring observations at multiple wavebands to characterise and interpret the observed changes.Aims. In this paper, we present radio-to-optical data taken by the WEBT, supplemented by our 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.Methods. We assemble multifrequency light curves with data from 30 ground-based observatories and the space-based instruments SWIFT (UVOT) and RXTE, 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.Results. We find that 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°.Conclusions. 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.

KW - Galaxies: active

KW - Quasars: general

KW - Quasars: individual: 3C 279

UR - http://www.scopus.com/inward/record.url?scp=57349142380&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:200810937

DO - 10.1051/0004-6361:200810937

M3 - Article

AN - SCOPUS:57349142380

VL - 492

SP - 389

EP - 400

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

IS - 2

ER -

ID: 88376865