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Catching the radio flare in CTA 102. II. VLBI kinematic analysis

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Catching the radio flare in CTA 102. II. VLBI kinematic analysis

dc.contributor.author	Fromm, Christian M.
dc.contributor.author	Ros Ibarra, Eduardo
dc.contributor.author	Perucho Pla, Manuel
dc.contributor.author	Savolainen, Tuomas
dc.contributor.author	Mimica, Petar
dc.contributor.author	Kadler, Matthias
dc.contributor.author	Lobanov, A.P.
dc.contributor.author	Lister, Matthiew L.
dc.contributor.author	Kovalev, Yuri Y.
dc.contributor.author	Zensus, J. Anton
dc.date.accessioned	2017-07-04T15:37:17Z
dc.date.available	2017-07-04T15:37:17Z
dc.date.issued	2013
dc.identifier.citation	Fromm, Christian M. Ros Ibarra, Eduardo Perucho Pla, Manuel Savolainen, Tuomas Mimica, Petar Kadler, Matthias Lobanov, A.P. Lister, M. L. Kovalev, Y. Y. Zensus, J. Anton 2013 Catching the radio flare in CTA 102. II. VLBI kinematic analysis Astronomy and Astrophysics 551 A32 1 30
dc.identifier.uri	http://hdl.handle.net/10550/59339
dc.description.abstract	Context. Very Long Baseline Interferometry (VLBI) observations can resolve the radio structure of Active Galactic Nuclei (AGN) and provide estimates of the structural and kinematic characteristics at parsec-scales in their jets. The changes in the kinematics of the observed jet features can be used to study the physical conditions in the innermost regions of these sources. We performed multi-frequency multi-epoch Very Long Baseline Array (VLBA) observations of the blazar CTA102 during its 2006 radio flare, the strongest ever reported for this source. These observations provide an excellent opportunity to investigate the evolution of the physical properties of blazars, especially during these flaring events Aims. We want to study the kinematic changes in the source during the strong radio outburst in April 2006 and test the assumption of a shock-shock interaction. This assumption is based on the analysis and modeling of the single dish observations of CTA102 (Paper I). Methods. In this paper we study the kinematics of CTA102 at several frequencies using VLBI observations. From the modeled jet features we derive estimates on the evolution of the physical parameters, such as the particle density and the magnetic field. Furthermore, we combine our observations during the 2006 flare with long-term VLBA monitoring of the source at 15 GHz and 43 GHz. Results. We cross-identified seven features throughout our entire multifrequency observations and find evidence of two possible recollimation shocks around 0.1 mas (deprojected 18 pc at a viewing angle ϑ = 2.6°) and 6.0 mas (deprojected 1 kpc) from the core. The 43 GHz observations reveal a feature ejected at epoch tej = 2005.9 ± 0.2, which could be connected to the 2006 April radio flare. Furthermore, this feature might be associated with the traveling component involved in the possible shock-shock interaction, which gives rise to the observed double peak structure in the single-dish light curves reported in Paper I.
dc.language.iso	eng
dc.relation.ispartof	Astronomy and Astrophysics, 2013, vol. 551, num. A32, p. 1-30
dc.subject	Astrofísica
dc.subject	Astronomia
dc.title	Catching the radio flare in CTA 102. II. VLBI kinematic analysis
dc.type	journal article	es_ES
dc.date.updated	2017-07-04T15:37:18Z
dc.identifier.doi	10.1051/0004-6361/201219913
dc.identifier.idgrec	085591
dc.rights.accessRights	open access	es_ES