Relativistic outflow drives<i>γ</i>-ray emission in 3C 345

Schinzel, F. K.; Lobanov, A. P.; Taylor, G. B.; Jorstad, S. G.; Marscher, A. P.; Zensus, J. A.

doi:10.1051/0004-6361/201117705

Cited by 87 publications

(105 citation statements)

References 46 publications

Supporting

Mentioning

101

Contrasting

Order By: Relevance

“…To derive the kinematics of the source, we fit polynomials to the observed x-and y-positions of the fitted components. We follow the procedure presented in e.g., Homan et al (2001) and Schinzel et al (2012), using firstand second-order polynomials if the components was detected in more than ten epochs (the latter can only be applied to the long-term monitoring of the source at 15 GHz and 43 GHz):…”

Section: Calculation Of Kinematic Parametersmentioning

confidence: 99%

“…These observations provide a tool to test several jet models and to probe how variations within the first few parsecs contribute to the high-energy emission. The brightness temperature, T b , can be used to derive estimates of the dominant energyloss mechanism and the evolution of intrinsic properties, such as the jet speed, the particle density, and the magnetic field (e.g., Kadler et al 2004;Schinzel et al 2012).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Catching the radio flare in CTA 102

Fromm¹,

Ros²,

Perucho³

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

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 on 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 multifrequency multiepoch Very Long Baseline Array (VLBA) observations of the blazar CTA 102 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 CTA 102 (Paper I). Methods. In this paper we study the kinematics of CTA 102 at several frequencies using VLBI observations. From the modeled jet features we derived estimates for the evolution of the physical parameters, such as the particle density and the magnetic field. Furthermore, we combined 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 t ej = 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.

show abstract

Section: Calculation Of Kinematic Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Catching the radio flare in CTA 102

Fromm¹,

Ros²,

Perucho³

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Kovalev et al 2009;Pushkarev et al 2010;Leon-Ravares et al 2011;Schinzel et al 2012;Wehrle et al 2012;Kutkin et al 2014). In this scenarios, we could determine the properties of jet through observing the electromagnetic spectrum.…”

Section: Introductionmentioning

confidence: 97%

Modelling the multi-wavelength emission of flat-spectrum radio quasar 3C 279

Zheng

Yang

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We employ a length-dependent conical jet model for the jet structure and emission properties of flat spectrum radio quasar 3C 279 in the steady state. In the model, ultrarelativistic leptons are injected at the base of jet and propagate along the jet structure, non-thermal photons are produced by both synchrotron emission and inverse Comtpon scattering off synchrotron photons and external soft photons at each segment of jet. We derive the total energy spectra contribution through integrating every segment. We apply the model to the quasi-simultaneous multi-wavelength observed data of two quiescent epoches. Using the observed radio data of source, we determine the length of jet L ∼ 100 pc, and magnetic field B 0 ∼ 0.1 − 1 G at the base of jet. Assuming a steady geometry of the jet structure and suitable physical parameters, we reproduce the multi-wavelength spectra during two quiescent observed epoches, respectively. Our results show that the initial γ-ray emission site takes place at ∼ 0.5 pc from black hole.

show abstract

“…We further discuss studies of the γ-ray production beyond the radio core. Schinzel et al (2012) found from the VLBA, optical and γ-ray monitoring of the quasar 3C 345 that γ-ray emission from 0.1-300 GeV is driven by relativistic outflows of the jet and is produced in a region of the jet that extends up to ∼ 23 pc. The γ-ray emission is proposed to arise from SSC.…”

Section: Location Of γ-Ray Emission In the Jetmentioning

confidence: 99%

“…Series of quasi-stationary knots and knots moving downstream the jet are often identified from the VLBA monitoring of blazars. The first stationary component from the radio core is located at submilliarcsecond scales which translates to a sub-parsec distance for nearby RGs 3C 390.3, 3C 120, BL Lacertae and M 87, and FSRQs 3C 273 and 3C 345.3 (e.g., Arshakian et al 2010;León-Tavares et al 2010;Cohen et al 2014;Cheung et al 2007;Jorstad et al 2005;Schinzel et al 2012). This stationary component appears to be a common feature in blazars and it is likely to be a standing recollimation shock (RCS), which is evident from HD/MHD simulations of jets (e.g., Gomez et al 1995;Krause & Gamenzid 2001).…”

mentioning

confidence: 99%

The central pc-scale region in blazars: insights from multi-band observations

Arshakian

Chavushyan

2013

Proc. IAU

View full text Add to dashboard Cite

Abstract. The empirical relations in the black hole-accretion disk-relativistic jet system and physical processes behind these relations are still poorly understood, partly because they operate close to the black hole within the central light year. Very long baseline array (VLBA) provides unparalleled resolution at 15 GHz with which to observe the jet components at submilliarcsecond scales, corresponding to sub-pc-scales for local blazars. We discuss the jet inner structure of blazars, location and radiation mechanisms operating in the innermost parsec-scale region of blazars, and evidence for jet-excited broad-line region (BLR) ouflowing downstream the jet. Outflowing BLR can provide necessary conditions for production of high energy emission along the jet between the base of the jet and the BLR and far beyond the BLR as evidenced by recent observations. Flat spectrum quasars and low synchrotron peaked sources are the most likely objects to host the outfllowing BLR. From the γ-ray absorption arguments, we propose that the jet-excited region of the outflowing BLR in quasars is small and/or gas filling factor is low, and that the orientation and opening angle of the outflowing BLR can lead to relevant γ-ray absorption features observed in quasars.

show abstract

Relativistic outflow drivesγ-ray emission in 3C 345

Cited by 87 publications

References 46 publications

Catching the radio flare in CTA 102

Catching the radio flare in CTA 102

Modelling the multi-wavelength emission of flat-spectrum radio quasar 3C 279

The central pc-scale region in blazars: insights from multi-band observations

Contact Info

Product

Resources

About