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Correlated multi–wave band variability in the blazar 3C 279 from 1996 to 2007

Correlated multi–wave band variability in the blazar 3C 279 from 1996 to 2007
Correlated multi–wave band variability in the blazar 3C 279 from 1996 to 2007
We present the results of extensive multi-wave band monitoring of the blazar 3C 279 between 1996 and 2007 at X-ray energies (2-10 keV), optical R band, and 14.5 GHz, as well as imaging with the Very Long Baseline Array (VLBA) at 43 GHz. In all bands the power spectral density corresponds to "red noise" that can be fit by a single power law over the sampled timescales. Variations in flux at all three wave bands are significantly correlated. The time delay between high- and low-frequency bands changes substantially on timescales of years. A major multifrequency flare in 2001 coincided with a swing of the jet toward a more southerly direction, and in general the X-ray flux is modulated by changes in the position angle of the jet near the core. The flux density in the core at 43 GHz—increases in which indicate the appearance of new superluminal knots—are significantly correlated with the X-ray flux. We decompose the X-ray and optical light curves into individual flares, finding that X-ray leads optical variations (XO) in six flares, the reverse (OX) occurs in three flares, and there is essentially zero lag in four flares. Upon comparing theoretical expectations with the data, we conclude that (1) XO flares can be explained by gradual acceleration of radiating electrons to the highest energies, (2) OX flares can result from either light-travel delays of the seed photons (synchrotron self-Compton scattering) or gradients in maximum electron energy behind shock fronts, and (3) events with similar X-ray and optical radiative energy output originate well upstream of the 43 GHz core, while those in which the optical radiative output dominates occur at or downstream of the core.
galaxies: jets, quasars: individual (3C 279), radiation mechanisms: non-thermal, radio continuum: galaxies, x-rays: galaxies
0004-637X
79
Chatterjee, Ritaban
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Jorstad, Svetlana G.
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Marscher, Alan P.
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Oh, Haruki
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McHardy, Ian M.
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Aller, Margo F.
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Aller, Hugh D.
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Balonek, Thomas J.
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Miller, H. Richard
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Ryle, Wesley T.
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Tosti, Gino
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Kurtanidze, Omar
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Nikolashvili, Maria
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Larionov, Valeri M.
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Hagen‐Thorn, Vladimir A.
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Chatterjee, Ritaban
04c1a235-6ebe-473f-a344-64bd1a13dfab
Jorstad, Svetlana G.
44452806-4721-48d9-bc9a-1b3046b78546
Marscher, Alan P.
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Oh, Haruki
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McHardy, Ian M.
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Aller, Margo F.
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Aller, Hugh D.
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Balonek, Thomas J.
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Miller, H. Richard
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Ryle, Wesley T.
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Tosti, Gino
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Kurtanidze, Omar
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Nikolashvili, Maria
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Larionov, Valeri M.
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Hagen‐Thorn, Vladimir A.
de031442-fef7-4a17-be25-7d193056b4ac

Chatterjee, Ritaban, Jorstad, Svetlana G., Marscher, Alan P., Oh, Haruki, McHardy, Ian M., Aller, Margo F., Aller, Hugh D., Balonek, Thomas J., Miller, H. Richard, Ryle, Wesley T., Tosti, Gino, Kurtanidze, Omar, Nikolashvili, Maria, Larionov, Valeri M. and Hagen‐Thorn, Vladimir A. (2008) Correlated multi–wave band variability in the blazar 3C 279 from 1996 to 2007. The Astrophysical Journal, 689 (1), 79. (doi:10.1086/592598).

Record type: Article

Abstract

We present the results of extensive multi-wave band monitoring of the blazar 3C 279 between 1996 and 2007 at X-ray energies (2-10 keV), optical R band, and 14.5 GHz, as well as imaging with the Very Long Baseline Array (VLBA) at 43 GHz. In all bands the power spectral density corresponds to "red noise" that can be fit by a single power law over the sampled timescales. Variations in flux at all three wave bands are significantly correlated. The time delay between high- and low-frequency bands changes substantially on timescales of years. A major multifrequency flare in 2001 coincided with a swing of the jet toward a more southerly direction, and in general the X-ray flux is modulated by changes in the position angle of the jet near the core. The flux density in the core at 43 GHz—increases in which indicate the appearance of new superluminal knots—are significantly correlated with the X-ray flux. We decompose the X-ray and optical light curves into individual flares, finding that X-ray leads optical variations (XO) in six flares, the reverse (OX) occurs in three flares, and there is essentially zero lag in four flares. Upon comparing theoretical expectations with the data, we conclude that (1) XO flares can be explained by gradual acceleration of radiating electrons to the highest energies, (2) OX flares can result from either light-travel delays of the seed photons (synchrotron self-Compton scattering) or gradients in maximum electron energy behind shock fronts, and (3) events with similar X-ray and optical radiative energy output originate well upstream of the 43 GHz core, while those in which the optical radiative output dominates occur at or downstream of the core.

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More information

Published date: 10 December 2008
Keywords: galaxies: jets, quasars: individual (3C 279), radiation mechanisms: non-thermal, radio continuum: galaxies, x-rays: galaxies

Identifiers

Local EPrints ID: 144671
URI: https://eprints.soton.ac.uk/id/eprint/144671
ISSN: 0004-637X
PURE UUID: ea5e2812-e7b8-401e-91cd-95d0ff89bdb2

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Date deposited: 26 May 2010 15:52
Last modified: 18 Jul 2017 23:08

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Contributors

Author: Ritaban Chatterjee
Author: Svetlana G. Jorstad
Author: Alan P. Marscher
Author: Haruki Oh
Author: Ian M. McHardy
Author: Margo F. Aller
Author: Hugh D. Aller
Author: Thomas J. Balonek
Author: H. Richard Miller
Author: Wesley T. Ryle
Author: Gino Tosti
Author: Omar Kurtanidze
Author: Maria Nikolashvili
Author: Valeri M. Larionov
Author: Vladimir A. Hagen‐Thorn

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