PKS 1510−089: A Head‐on View of a Relativistic Jet

Homan, D. C.; Wardle, J. F. C.; Cheung, C. C.; Roberts, D. H.; Attridge, J. M.

doi:10.1086/343894

Cited by 44 publications

(50 citation statements)

References 32 publications

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“…The maximum rotation rate of the polarization angle would correspond to the minimum of θ. Similar geometry -albeit on larger scales -has been observed in another blazar, PKS 1510-089 (Homan et al 2002). Nonetheless, in both scenarios, the coherent polarization event is produced by a density pattern co-moving along the jet, and therefore, it is possible to estimate the distance traveled by the emitting material during the flare ∆r event ; this in turn allows us to constrain the distance of the dissipation region from the black hole r event ∆r event ∼ 10 19 (∆t event /20 days) (Γ jet /15) 2 cm , which is ∼ 5 orders of magnitude larger than the gravitational radius of the black hole in 3C 279.…”

Section: Gamma-ray Flare With a Change Of Optical Polarizationsupporting

confidence: 75%

The picture of relativistic jet from Fermi-LAT and multi-band observations of blazar 3C 279

Hayashida¹,

Madejski²

2010

Proc. IAU

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Abstract. Strong and variable radiation detected over all accessible energy bands in blazar arises from a relativistic, Doppler-boosted jet pointing close to our line of sight. Flat Spectrum Radio Quasar 3C 279 was one of the brightest γ-ray blazars in the sky at the time of the discovery with EGRET. Since the successful launch of the Fermi Gamma-ray Space telescope in 2008, we have organized extensive multi-band observational campaign of 3C 279 from radio to γ-ray bands, also including optical polarimetric observations. The uninterrupted monitoring in the γ-ray band by Fermi-LAT together with the multi-band data provide us with new insights of the relativistic jet of blazar. Here, we present the results of the first-year multi-band campaign of 3C 279 including the discovery of a γ-ray flare event associated with a dramatic change of the optical polarization -as well as a discovery of an "orphan" X-ray flare, unassociated with prominent outbursts in other bands.

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Section: Gamma-ray Flare With a Change Of Optical Polarizationsupporting

confidence: 75%

The picture of relativistic jet from Fermi-LAT and multi-band observations of blazar 3C 279

Hayashida¹,

Madejski²

2010

Proc. IAU

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“…This would require, as is being proposed here for most of these sources, that the jet and counter-jet are both at large viewing angles instead of being viewed endon as proposed by [30]. In this scenario there is also evidence that the jets in PKS 1510 -089 switch on and off, as is required to explain intrinsic one-sidedness.…”

Section: Relative Strengths Of the Boosted And Un-boosted Radiationmentioning

confidence: 68%

“…As noted above, this is because most of these sources would have been detected even without this small amount of boosted radiation from the jet, and their distribution of orientations must then be close to random. In particular, we note that the outer jet in PKS 1510-089 has been found, in the CR model, to be directed at an angle of between 12˚ -24˚ from the line-of-sight [30]. This means that its radiation would not be significantly boosted.…”

Section: Relative Strengths Of the Boosted And Un-boosted Radiationmentioning

confidence: 71%

“…It is worth noting that this model, where the jets turn on and off and are closer to the plane of the sky, would then easily explain why [30] found no evidence for a counter-jet in PKS 1510 -089 by simply interpreting the arcsec jet, lying ~180˚ from the milliarcsec jet, as the counter-jet. This would require, as is being proposed here for most of these sources, that the jet and counter-jet are both at large viewing angles instead of being viewed endon as proposed by [30].…”

Section: Relative Strengths Of the Boosted And Un-boosted Radiationmentioning

confidence: 95%

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Doppler Boosting May Have Played No Significant Role in the Finding Surveys of Radio-Loud Quasars

Bell¹

2012

IJAA

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There appears to be a fundamental problem facing Active Galactic Nuclei (AGN) jet models that require highly relativistic ejection speeds and small jet viewing angles to explain the large apparent superluminal motions seen in so many of the radio-loud quasars with high redshift. When the data are looked at closely it is found that, assuming the core component is unboosted, only a small percentage of the observed radio frequency flux density from these sources can be Doppler boosted. If the core component is boosted the percentage of boosted to unboosted flux will be higher but will still be far from the 90 percent required for Doppler boosting to have played a significant role. Without a highly directed, Doppler boosted component that dominates the observed flux, radio sources found in low-frequency finding surveys cannot be preferentially selected with small jet viewing angles. The distribution of jet orientations will then follow the sini curve associated with a random distribution, where only a very few sources (~1%) will have the small viewing angles (<8˚) required to explain apparent superluminal motions v app > 10c, and this makes it difficult to explain how around 33% of the radio-loud AGNs with high redshift can exhibit such highly superluminal motions. When the boosted component is the dominant one it can be argued that in a flux limited sample only those members with small viewing angles would be picked up while those with larger viewing angles (the un-boosted ones) would be missed. However, this is not the case when the boosted component is small and a new model to explain the high apparent superluminal motions may be needed if the redshifts of high-redshift quasars are to remain entirely cosmological.

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“…The Lorentz factors (and Doppler factors) thus derived are of the order of ten for general samples of AGNs (Vermeulen & Cohen 1994), but may be higher for AGNs showing prominent gamma-ray emission (e.g. Homan et al 2002Homan et al , 2003. The range of Lorentz factors prevalent at the time of gamma-ray emission, which presumably occurs before the emission region becomes visible at radio frequencies, is not known, but is likely higher than ten, if the bulk kinetic energy of the jets is the energy reservoir for the particle acceleration (see, e.g., Georganopoulos & Kazanas 2003).…”

Section: Introductionmentioning

confidence: 98%

The impact of thermal gas in AGN jets on the low-frequency emission

Siewert

Pohl

Schlickeiser

2004

A&A

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Abstract.We study the effect of non-relativistic, thermal matter in the jets of active galaxies (AGN) on the low-frequency non-thermal emission and the variability thereof. In matter-dominated jets, sizable quantities of gas should exist, in particular in the compression zones near the collision fronts that are an implicit ingredient of Fermi-type particle acceleration scenarios. Non-relativistic thermal gas in AGN jets noticably contributes to the optical depth at radio to infrared frequencies, and much less to the emission, with an efficiency that is strongly temperature-dependent. The observable flux of low-frequency emission is thus modulated by the temperature evolution of the thermal gas, and it can therefore display very complicated variability. For a particular particle energisation scenario we calculate the temperature evolution of the thermal plasma as well as the radiation transport of low-frequency emission, and thus derive simulated light curves at different frequencies and their typical correlation properties.

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PKS 1510−089: A Head‐on View of a Relativistic Jet

Cited by 44 publications

References 32 publications

The picture of relativistic jet from Fermi-LAT and multi-band observations of blazar 3C 279

The picture of relativistic jet from Fermi-LAT and multi-band observations of blazar 3C 279

Doppler Boosting May Have Played No Significant Role in the Finding Surveys of Radio-Loud Quasars

The impact of thermal gas in AGN jets on the low-frequency emission

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