AGN jets under the microscope: A divide?

Karouzos, Marios; Britzen, S.; Witzel, A.; Zensus, J. A.; Eckart, A.

doi:10.1002/asna.201211685

Cited by 4 publications

(7 citation statements)

References 61 publications

(77 reference statements)

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“…Several well-studied AGN have been found to show nonballistic motions in their jets, which are interpreted in terms of a helical or precessing jet (e.g. Steffen et al 1995;Abraham 1999;Britzen et al 2009;Liu et al 2010;Kudryavtseva et al 2011a;Karouzos et al 2012a). The projected positions of individual components on the plane of the sky can be directly used for fitting of analytical models and can therefore usually constrain both the opening angle of the precession cone, the initial time and angle of ejection of each jet component, and given enough data, the periodicity of the jet precession and consequently of the binary black hole system.…”

Section: Agn Jet Kinematicsmentioning

confidence: 99%

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A spinning supermassive black hole binary model consistent with VLBI observations of the S5 1928+738 jet

Kun

Gabányi

Karouzos

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Very Long Baseline Interferometry (VLBI) allows for high-resolution and highsensitivity observations of relativistic jets, that can reveal periodicities of several years in their structure. We perform an analysis of long-term VLBI data of the quasar S5 1928+738 in terms of a geometric model of a helical structure projected onto the plane of the sky. We monitor the direction of the jet axis through its inclination and position angles. We decompose the variation of the inclination of the inner 2 milliarcseconds of the jet of S5 1928+738 into a periodic term with amplitude of ∼ 0.89 • and a linear decreasing trend with rate of ∼ 0.05 • yr −1 . We also decompose the variation of the position angle into a periodic term with amplitude of ∼ 3.39 • and a linear increasing trend with rate of ∼ 0.24 • yr −1 . We interpret the periodic components as arising from the orbital motion of a binary black hole inspiraling at the jet base and derive corrected values of the mass ratio and separation from the accumulated 18 years of VLBI data. Then we identify the linear trends in the variations as due to the slow reorientation of the spin of the jet emitter black hole induced by the spin-orbit precession and we determine the precession period T SO = 4852 ± 646 yr of the more massive black hole, acting as the jet emitter. Our study provides indications, for the first time from VLBI jet kinematics, for the spinning nature of the jet-emitting black hole.

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Section: Agn Jet Kinematicsmentioning

confidence: 99%

“…The jet ridge line of AGN jets can be used to identify jets with strong variations of their curvature along the jet axis. Karouzos et al (2012a), using a simple geometrical model of a helical jet, showed that a helically structured or a precessing jet can give rise to the curvature observed in many AGN jets.…”

Section: Agn Jet Morphologymentioning

confidence: 99%

A spinning supermassive black hole binary model consistent with VLBI observations of the S5 1928+738 jet

Kun

Gabányi

Karouzos

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Jet bendings or non-linear morphologies are very common in BL Lacs (e.g. Karouzos et al 2012). Jorstad et al (2005) suggest that the first bending in 3C 66A jet occurs smoothly from 1.2 mas up to 3 mas.…”

Section: Morphologymentioning

confidence: 99%

Multi-Epoch Multi-Frequency Vlbi Study of the Parsec-Scale Jet in the Blazar 3c 66a

Zhao

Chen

Shen

et al. 2015

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We present the observational results of the γ-ray blazar, 3C 66A, at 2. 3, 8.4, and 22 GHz at 4 epochs during 2004-05 with the VLBA. The resulting images show an overall core-jet structure extending roughly to the south with two intermediate breaks occurring in the region near the core. By model-fitting to the visibility data, the northmost component, which is also the brightest, is identified as the core according to its relatively flat spectrum and its compactness. As combined with some previous results to investigate the proper motions of the jet components, it is found the kinematics of 3C 66A is quite complicated with components of inward and outward, subluminal and superluminal motions all detected in the radio structure. The superluminal motions indicate strong Doppler boosting exists in the jet. The apparent inward motions of the innermost components last for at least 10 years and could not be caused by new-born components. The possible reason could be non-stationarity of the core due to opacity change.

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“…Britzen et al 2001;Tateyama et al 2002;Britzen et al 2005bBritzen et al , 2010; Fractional variability amplitude Fvar for jet components C0, C1, Ca, C2, C4, C8 as function of time in 3-year bins Karouzos et al 2012a)…”

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confidence: 99%

Flaring radio lanterns along the ridge line: long-term oscillatory motion in the jet of S5 1803+784

Kun

Karouzos

Gabányi

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of 30 very long baseline interferometric observations of the BL Lac object S5 1803+784 (z = 0.679), obtained between mean observational time 1994.67 and 2012.91 at observational frequency 15 GHz. The long-term behaviour of the jet ridge line reveals the jet experiences an oscillatory motion superposed on its helical jet kinematics on a time-scale of about 6 years. The excess variance of the positional variability indicates the jet components being farther from the VLBI core have larger amplitude in their position variations. The fractional variability amplitude shows slight changes in 3-year bins of the component's position. The temporal variability in the Doppler boosting of the ridge line results in jet regions behaving as flaring "radio lanterns". We offer a qualitative scenario leading to the oscillation of the jet ridge line, that utilizes the orbital motion of the jet emitter black hole due to a binary black hole companion. A correlation analysis implies composite origin of the flux variability of the jet components, emerging due to possibly both the evolving jet-structure and its intrinsic variability.

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AGN jets under the microscope: A divide?

Cited by 4 publications

References 61 publications

A spinning supermassive black hole binary model consistent with VLBI observations of the S5 1928+738 jet

A spinning supermassive black hole binary model consistent with VLBI observations of the S5 1928+738 jet

Multi-Epoch Multi-Frequency Vlbi Study of the Parsec-Scale Jet in the Blazar 3c 66a

Flaring radio lanterns along the ridge line: long-term oscillatory motion in the jet of S5 1803+784

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