THE IMPORTANCE OF JET BENDING IN GAMMA-RAY AGNs—REVISITED

Graham, P. J.; Tingay, S. J.

doi:10.1088/0004-637x/784/2/159

Cited by 3 publications

(3 citation statements)

References 74 publications

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“…They suggested that the observed polarization behavior may be the result of the jet bending. Jet bending has been observed in a number of AGNs (e.g., Graham & Tingay 2014). In this scenario, an oblique shock could be formed due to the interaction of the jet with the external medium.…”

Section: On the Acceleration Mechanismmentioning

confidence: 99%

On the injection of relativistic electrons in the jet of 3C 279

Yan

Dai

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The acceleration of electrons in 3C 279 is investigated through analyzing the injected electron energy distribution (EED) in a time-dependent synchrotron self-Compton + external Compton emission model. In this model, it is assumed that relativistic electrons are continuously injected into the emission region, and the injected EED [Q ′ e (γ ′ )] follows a single power-law form with low-and high-energy cutoffs γ ′ min and γ ′ max , respectively, and the spectral index n, i.e, Q ′ e (γ ′ ) ∝ γ ′−n . This model is applied to 14 quasi-simultaneous spectral energy distributions (SEDs) of 3C 279. The Markov Chain Monte Carlo fitting technique is performed to obtain the best-fitting parameters and the uncertainties on the parameters. The results show that the injected EED is well constrained in each state. The value of n is in the range of 2.5 to 3.8, which is larger than that expected by the classic non-relativistic shock acceleration. However, the large value of n can be explained by the relativistic oblique shock acceleration. The flaring activity seems to be related to an increased acceleration efficiency, reflected in an increased γ ′ min and electron injection power.

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Section: On the Acceleration Mechanismmentioning

confidence: 99%

On the injection of relativistic electrons in the jet of 3C 279

Yan

Dai

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The comparison of the jet position angle (PA) on parsec and kiloparsec scales does not suggest the presence of strong viewing angle changes; indeed, Graham & Tingay (2014) report a jet PA of ϕ = 139…”

Section: Radiomentioning

confidence: 99%

Restarting activity in the nucleus of PBC J2333.9-2343

Hernández-García¹,

Panessa²,

Giroletti³

et al. 2017

A&A

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Context. The giant radio galaxy PBC J2333.9-2343 shows different characteristics at different wavebands that are difficult to explain within the actual generic schemes of unification of active galactic nuclei (AGN). It is therefore a good candidate host for different phases of nuclear activity. Aims. We aim at disentangling the nature of this AGN by using simultaneous multiwavelength data. Methods. We obtained data in 2015 from the Very Long Baseline Array (VLBA), the San Pedro Mártir telescope, and the XMMNewton observatories. This allows the study of the nuclear parts of the galaxy through its morphology and spectra and the analysis of the spectral energy distribution (SED). We also reanalysed previously-presented optical data from the San Pedro Mártir telescope from 2009 to provide a homogeneous comparison. Results. At X-ray frequencies the source is unabsorbed. The optical spectra are of a type 1.9 AGN, both in 2009 and 2015, although showing a broader component in 2015. The VLBA radio images show an inverted spectrum with a self-absorbed, optically thick compact core (α c = 0.40, where S ν ∝ ν +α ) and a steep-spectrum, optically thin jet (α j,8−15 = −0.5). The SED resembles that of typical blazars and is best represented by an external Compton (EC) model with a viewing angle of approximately 3-6• . The apparent size of the large-scale structure of PBC J2333.9-2343 must correspond to an intrinsic deprojected value of approximately 7 Mpc for θ v < 10• , and to >13 Mpc for θ v < 5• , a value much larger than the biggest giant radio galaxy known, which is 4.5 Mpc. Conclusions. The above arguments suggest that PBC J2333.9-2343 has undergone a new episode of nuclear activity and that the direction of the new jet has changed in the plane of the sky and is now pointing towards us. This changes this source from a radio galaxy to a blazar, a very exceptional case of restarting activity.

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“…(Jorstad et al 2001). This paper is the third a series of VLBI observations of southern gamma-ray sources: paper I (Tingay et al 1996) contained first-epoch VLBI images of PKS 0208−512, PKS 0521−365, and PKS 0537−441, and paper II (Tingay et al 1998) included VLBI images of an additional six southern sources and investigated the suggestion that jet bending played an important role in gamma-ray sources-a topic revisited more recently by Graham & Tingay (2014).…”

Section: Introductionmentioning

confidence: 99%

VLBI Observations of Southern Gamma-Ray Sources. III

Edwards

Ojha

Dodson

et al. 2018

Publ. Astron. Soc. Aust.

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We report the results of Long Baseline Array observations made in 2001 of ten southern sources proposed by Mattox et al. as counterparts to EGRET >100 MeV gamma-ray sources. Source structures are compared with published data where available and possible superluminal motions identified in several cases. The associations are examined in the light of Fermi observations, indicating that the confirmed counterparts tend to have radio properties consistent with other identifications, including flat radio spectral index, high brightness temperature, greater radio variability, and higher core dominance.

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THE IMPORTANCE OF JET BENDING IN GAMMA-RAY AGNs—REVISITED

Cited by 3 publications

References 74 publications

On the injection of relativistic electrons in the jet of 3C 279

On the injection of relativistic electrons in the jet of 3C 279

Restarting activity in the nucleus of PBC J2333.9-2343

VLBI Observations of Southern Gamma-Ray Sources. III

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