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

dc.contributor.authorLARIONOV, V. M.
dc.contributor.authorJORSTAD, S. G.
dc.contributor.authorMARSCHER, A. P.
hal.structure.identifierINAF - Osservatorio Astrofisico di Torino [OATo]
dc.contributor.authorRAITERI, C. M.
hal.structure.identifierINAF - Osservatorio Astrofisico di Torino [OATo]
dc.contributor.authorVILLATA, M.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCHARLOT, P.
dc.date.issued2008
dc.identifier.issn0004-6361
dc.description.abstractEnWe 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.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enResults of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361:200810937
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv0810.4261
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page389-400
bordeaux.volume492
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-00402924
hal.version1
hal.popularnon
hal.audienceInternationale
dc.subject.esgalaxies: active
dc.subject.esquasars: general
dc.subject.esquasars: individual: 3C 279
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00402924v1
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