VLBI Space Observatory Programme Observation of the Quasar PKS 2215+020: A New Laboratory for Core‐Jet Physics at<i>z</i> = 3.572

Lobanov, A. P.; Gurvits, L. I.; Frey, S.; Schilizzi, R. T.; Kawaguchi, Noriyuki; Pauliny-Toth, I. I. K.

doi:10.1086/318391

Cited by 19 publications

(31 citation statements)

References 20 publications

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“…2. Our results are very similar to those of Lobanov et al (2001) who employed the same model for this source at 1.6 GHz.…”

Section: Discussionsupporting

confidence: 89%

“…Our 5‐GHz image has a similar resolution to the Lobanov et al (2001) image but is less sensitive to the extended jet emission; hence, our image has a similar but sparser intensity distribution. We also detect the particularly bright region, where the jet changes direction from east to north‐east on the plane of the sky.…”

Section: Resultsmentioning

confidence: 83%

“…Drinkwater et al (1997) found an emission redshift of 3.572 for this quasar. Lobanov et al (2001) present a 1.6‐GHz VSOP Space‐VLBI image of this source showing the jet extending to almost 80 mas (∼600 pc) with a particularly bright section between 45 and 60 mas. The extent of this jet is ∼4 times greater than in any other parsec‐scale jet observed for quasars with z > 3.…”

Section: Resultsmentioning

confidence: 99%

“…From the observed brightness temperatures of the individual jet components, we can investigate the assumption of adiabatic expansion following Marscher (1990), Lobanov et al (2001) and Pushkarev, Kovalev & Lobanov (2008), who model the individual jet components as independent relativistic shocks with adiabatic energy losses dominating the radio emission. Note that this description of the outer jet differs from the N ∝ r −2 , B ∝ r −1 case describing the compact inner jet region, which is not adiabatic.…”

Section: Discussionmentioning

confidence: 99%

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Multifrequency polarization properties of 10 quasars on decaparsec scales at z > 3

O’Sullivan¹,

Gabuzda²,

Gurvits³

2011

Monthly Notices of the Royal Astronomical Society

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Global very long baseline interferometry (VLBI) (European VLBI Network + Very Long Baseline Array) polarization observations at 5 and 8.4 GHz of 10 high-redshift (z > 3) quasars are presented. The core and jet brightness temperatures are found through modelling the self-calibrated uv data with Gaussian components, which provide reliable estimates of the flux density and the size of the individual components. The observed high core brightness temperatures (median T-b,T- core = 4 x 10(11) K) are consistent with Doppler-boosted emission from a relativistic jet orientated close to the line of sight. This can also explain the dramatic jet bends observed for some of our sources since small intrinsic bends can be significantly amplified due to projection effects in a highly beamed relativistic jet. We also model-fit the polarized emission and, by taking the minimum angle separation between the model-fitted polarization angles at 5 and 8.4 GHz, we calculate the minimum inferred Faraday rotation measure (RMmin) for each component. We also calculate the minimum intrinsic RM in the rest frame of the active galactic nuclei (AGN) [RMminintr = RMmin(1 + z)(2)], first subtracting the integrated (presumed foreground) RM in those cases where we felt we could do this reliably. The resulting mean core vertical bar RMminintr vertical bar is 5580 rad m(-2), with a standard deviation of 3390 rad m(-2), for four high-z quasars for which we believe we could reliably remove the foreground RM. We find relatively steep core and jet spectral index values, with a median core spectral index of -0.3 and a median jet spectral index of -1.0. Comparing our results with RM observations of more nearby AGN at similar emitted frequencies does not provide any significant evidence for dependence of the quasar nuclear environment with redshift. However, more accurate RM and spectral information for a larger sample of sources would be required before making any conclusive statements about the environment of quasar jets in the early universe

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“…2. Our results are very similar to those of Lobanov et al (2001) who employed the same model for this source at 1.6 GHz.…”

Section: Discussionsupporting

confidence: 89%

Section: Resultsmentioning

confidence: 83%

Section: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

See 2 more Smart Citations

Multifrequency polarization properties of 10 quasars on decaparsec scales at z > 3

O’Sullivan¹,

Gabuzda²,

Gurvits³

2011

Monthly Notices of the Royal Astronomical Society

Self Cite

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“…Therefore, a $ R 0 (B in =B ext ) 1=2 (Beskin 1997;Lobanov et al 2001). For the BH-disk system produced by the NS-NS merger, B in $ 10 12 10 13 G, B ext $ 10 À6 G, and R 0 $ 10 6 cm, we get a $ 10 15 10 16 cm.…”

Section: Model Assumptions and Parameter Valuesmentioning

confidence: 91%

Optical Afterglows from Cylindrical Jets of Short Gamma‐Ray Bursts

Wang

Cheng

Tam

2005

ApJ

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Observations of extragalactic radio jets and young stellar jets show that the jets are cylindrical; i.e., they maintain a nearly constant cross section on large scales. It has been suggested that the afterglow behaviors of some long-duration gamma-ray bursts (GRBs) are consistent with the cylindrical jet model of GRBs. Here we study the afterglow emission of cylindrical jets from short-duration GRBs. For the usual conical jet geometry, it is argued that, because of the low fluence of short GRBs, the prospects of detecting the optical afterglow 10 hr after the burst are not promising. However, in the present work we find that if the jets are cylindrical, the chance for detecting the optical afterglow will be increased, even if the burst occurs in a low-density (n $ 10 À3 cm À3 ) medium. Since the jets are expected to not be well collimated initially and the time when they change from conical to cylindrical is not exactly known, we discuss two cases for the afterglow of cylindrical jets: the jets becoming cylindrical (1) after the gamma-ray-emitting phase and (2) before the gamma-ray-emitting phase. In both cases, the light-curve behaviors, especially the peak time, are sensitive to the cross section radius of the cylindrical jet. In the former case we find that for viewing angles less than $0.03 rad relative to the jet axis, typical short GRBs have a late-time R-band afterglow with a maximum apparent magnitude of m R P 23, given that the efficiency for producing gamma rays and the shock microphysical parameters of the afterglow are the same in short and long bursts. For the latter case the optical afterglows can always be readily detected with m R < 23 at 10 hr after the burst. Comparison between model light curves and observational upper limits of the optical afterglow flux of a few short GRBs are also made.

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Space VLBI

Frey¹

2004

The Role of VLBI in Astrophysics, Astrometry and Geodesy

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VLBI Space Observatory Programme Observation of the Quasar PKS 2215+020: A New Laboratory for Core‐Jet Physics atz = 3.572

Cited by 19 publications

References 20 publications

Multifrequency polarization properties of 10 quasars on decaparsec scales at z > 3

Multifrequency polarization properties of 10 quasars on decaparsec scales at z > 3

Optical Afterglows from Cylindrical Jets of Short Gamma‐Ray Bursts

Space VLBI

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