Peculiar variations in the structure of the quasar 3C454.3

Pauliny-Toth, I. I. K.; Porcas, R. W.; Zensus, J. A.; Kellermann, K. I.; Wu, Shuisheng; Nicolson, G. D.; Mantovani, F.

doi:10.1038/328778a0

Cited by 47 publications

(45 citation statements)

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“…We confirm the results concerning the general VLBI structure of 2251+158 by Pauliny-Toth et al (1987). The source shows a core-jet structure with a jet extending about 10 mas from the core oriented along an overall position angle of ∼−50 • .…”

Section: Results Of the Vlbi Analysissupporting

confidence: 78%

“…Recent investigations (e.g., Bartel et al 2012;Ransom et al 2012) of VLBI observations at 8.4 GHz to estimate the stability of the "core" component of 2251+158 as reference point for GRAVITY Probe B revealed that the core is stationary within 1σ upper limits on its proper motion of 39 µas yr −1 , for the period [2002][2003][2004][2005]. We want to stress that for this source the determination of the core position is problematic, as discussed already by Pauliny-Toth et al (1987).…”

Section: Results Of the Vlbi Analysismentioning

confidence: 99%

“…Based on the observations and findings reported by Pauliny-Toth et al (1984, 1987, after a major radio flare in 1981 the components close to the core remained at similar core distances for some time -not showing the typical apparent superluminal motion expected for this kind of object and thus appearing to be stationary. These structural changes, as reported by Pauliny-Toth et al, do not appear to fit easily into the scheme of relativistic jet models.…”

Section: Peculiar Kinematicsmentioning

confidence: 99%

“…The polarimetry at 43 GHz has been studied by e.g., Kemball et al (1996). A detailed early study of component motion in the parsec-scale jet of this source has been performed by Pauliny-Toth et al (1987). Qian et al (2007) showed that the long-term radio-variability at 4.8 and 8 GHz can be explained by a binary black hole model.…”

Section: Introductionmentioning

confidence: 99%

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2251+158 (3C 454.3): detection of an arc-like structure on parsec scales

Britzen

Qian

Witzel

et al. 2013

A&A

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Context. 2251+158 (3C 454.3) is a well-studied quasar with rather unusual properties. It is among the most variable and brightest gamma-ray emitting active galactic nucleus (AGN) in the sky observed by Fermi. The multi-wavelength flux density emission of this source is peculiar, and so is the very long baseline interferometry (VLBI) structure. While it is usually assumed that the jet and jet-components in a given AGN show more or less the same properties (e.g., apparent velocities and paths) with time, we demonstrate here that unusual morphologies (arc-like structure) can occur as temporal phenomena. We also show that the kinematic properties of jet components change from slow to fast apparent motion. Aims. We present the detection of an arc around the core region. To understand the physical nature of this and other peculiar kinematic properties of the parsec-scale jet of 2251+158 we performed detailed radio-interferometric studies of this prototypical AGN. Methods. We (re-)analyzed 32 Very Long Baseline Array (VLBA) observations covering 16 years in time (between 1995.57 and 2011.48), observed at 15 GHz from the Monitoring Of Jets in Active galactic nuclei with VLBA Experiments (MOJAVE/2 cm) survey and derived the parameters of the observed VLBI structure. Three 43 GHz VLBA observations from 2001.22, 2005.38, and 2005.76 have been reprocessed. We fitted the components of the VLBI structure with Gaussian components. We studied the properties of light-curves obtained in the radio (4.8, 8.0, and 14.5 GHz) and optical regime (R-band), and studied the correlations between the flaring properties and the VLBI structure of the source. Results. We report the detection of an arc-like structure around the core of an AGN. This ring-structure becomes visible in VLBI maps around 1996. It expands with an apparent proper motion between 0.12 ± 0.01 mas yr −1 and 0.19 ± 0.01 mas yr −1 (corresponding to 5.4 ± 0.3c to 9.0 ± 0.4c) and dominates the parsec-scale structure for about 14 years. In addition, we report a significant change in the kinematic properties of jet components close to the core. A phase of slow apparent radial motion (directed away from the core) of two inner jet components (A and B) and no component ejection after a major radio-flare in 1995 is atypical for AGN. This phase is followed by a more typical behaviour in which the same components separate with higher apparent speeds from the core and two new components appear to be ejected from the central region. Conclusions. We observe significant changes in the morphological and kinematic properties of the parsec-scale jet. Taken together, it is tempting to see a causal connection between the different phenomena. We briefly suggest and discuss several possible physical scenarios to explain the observed phenomena. The kinematic changes as well as the changes in the flaring characteristics could be explained geometrically because of a change in the angle to the line of sight towards the observer assuming a helical structure of the jet. Another possible expl...

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Section: Results Of the Vlbi Analysissupporting

confidence: 78%

Section: Results Of the Vlbi Analysismentioning

confidence: 99%

Section: Peculiar Kinematicsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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2251+158 (3C 454.3): detection of an arc-like structure on parsec scales

Britzen

Qian

Witzel

et al. 2013

A&A

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“…It is a strong γ-ray and X-ray source (Hartman et al 1993). It has been observed extensively at lower resolutions (Pauliny-Toth et al 1987) and at 43 GHz (Kemball et al 1996). The mas structure is a typical core-jet structure with the extended jet in PA ∼ −65 • (Padrielli et al 1986).…”

Section: Cta 102mentioning

confidence: 99%

50 μas resolution VLBI images of AGN's at λ3 mm

Rantakyrö

Bååth

Backer

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. We present 15 images from the global mm-VLBI sessions in 1990 April at 100 GHz and 1993 April at 86 GHz. These observations probe the central engines of the 16 observed AGN's with up to 50 µas resolution. Among other sources previously observed with λ3 mm VLBI we present the first λ3 mm maps of 0735+178, 0748+126, 1055+018, 2145+067, and CTA 102, in total we have been able to image 13 out of the 16 observed sources. 6 out of the 13 imaged sources observed exhibit curvature and rapid structural changes, although the low dynamic range in two thirds of the maps limits the detection of weak features. Most of the sources have unresolved cores even at this high resolution. There is substantial evidence that the observed sources can be grouped into two general groups: A misaligned population with parsec scale jets in the form of low pitch helices and an aligned population with straight jets with small changes in PA due to intrinsic bends.

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Observing Blazars with VLBI

Porcas

2004

The Role of VLBI in Astrophysics, Astrometry and Geodesy

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Peculiar variations in the structure of the quasar 3C454.3

Cited by 47 publications

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2251+158 (3C 454.3): detection of an arc-like structure on parsec scales

2251+158 (3C 454.3): detection of an arc-like structure on parsec scales

50 μas resolution VLBI images of AGN's at λ3 mm

Observing Blazars with VLBI

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