VLBI limits on the proper motion of the ‘core’ of the superluminal quasar 3C345

Bartel, N.; Herring, T. A.; Ratner, M. I.; Shapiro, I. I.; Corey, B. E.

doi:10.1038/319733a0

Cited by 101 publications

(58 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Finding stationary components in 15 sources (the 13 of our sample, 3C 345, Bartel et al 1986; and 1038+528 A, Marcaide et al 1994) would strongly support the standard model for AGNs (Blandford & Königl 1979). On the contrary, finding that some have no stationary components might reveal phenomena unthought.…”

Section: Added a New Sourcementioning

confidence: 67%

Absolute kinematics of radio source components in the complete S5 polar cap sample

Ros

Marcaide

Guirado

2001

A&A

View full text Add to dashboard Cite

Abstract. We observed the thirteen extragalactic radio sources of the S5 polar cap sample at 8.4 GHz with the Very Long Baseline Array, on 1997.93 and 1999.41. We present the maps from those two epochs and briefly discuss the morphological changes experimented by some of the radio sources in the 1.4 yr elapsed. These results correspond to the first two epochs at 8.4 GHz of a program directed to study the absolute kinematics of the radio source components of the members of the sample by means of phase delay astrometry at 8.4, 15 and 43 GHz.

show abstract

Section: Added a New Sourcementioning

confidence: 67%

Absolute kinematics of radio source components in the complete S5 polar cap sample

Ros

Marcaide

Guirado

2001

A&A

View full text Add to dashboard Cite

show abstract

“…We conservatively adopt the same error for the 13 and 4 cm data. Given that the core (C1) has a flat-spectrum in centimeter bands (Zhang et al 1994;Cotton et al 1997), it is expected that the core position r c (ν) is a power-law function of frequency (r c ∝ν −1/ k , e.g., Bartel et al 1986;Lobanov 1998). Since we have only three data points, it is not possible to perform a fit with the function r c =A + Bν −1/k , leaving A, B, and k as free parameters.…”

Section: Discussionmentioning

confidence: 99%

Alma Science Verification Data: Millimeter Continuum Polarimetry of the Bright Radio Quasar 3c 286

Nagai

Nakanishi

Paladino

et al. 2016

ApJ

View full text Add to dashboard Cite

We present full-polarization observations of the compact, steep-spectrum radio quasar 3C286 made with the Atacama Large Millimeter and Submillimeter Array (ALMA) at 1.3mm. These are the first full-polarization ALMA observations, which were obtained in the framework of Science Verification. A bright core and a southwest component are detected in the total intensity image, similar to previous centimeter images. Polarized emission is also detected toward both components. The fractional polarization of the core is about 17%; this is higher than the fractional polarization at centimeter wavelengths, suggesting that the magnetic field is even more ordered in the millimeter radio core than it is further downstream in the jet. The observed polarization position angle (or electric vector position angle (EVPA)) in the core is ∼39• , which confirms the trend that the EVPA slowly increases from centimeter to millimeter wavelengths. With the aid of multi-frequency VLBI observations, we argue that this EVPA change is associated with the frequency-dependent core position. We also report a serendipitous detection of a sub-mJy source in the field of view, which is likely to be a submillimeter galaxy.

show abstract

“…The uncertainty of the di †erential position of the supernova phase center is caused by only the di †erential parts of the above errors in the correlator model, which, over only D170A on the sky, are much smaller. In total, the errors in the correlator model contribute not more than 10 kas to the uncertainty of a di †erential position determination of any Ðducial point in the brightness distribution of SN 1993J (see Bartel et al 1986 for an estimate of such errors for the close pair of quasars 3C 345 and NRAO 512 at the same frequency). .…”

Section: T He Degree Of Circularity In the Imagesmentioning

confidence: 99%

SN 1993J VLBI. I. The Center of the Explosion and a Limit on Anisotropic Expansion

Bietenholz

Bartel

Rupen

2001

ApJ

Self Cite

View full text Add to dashboard Cite

Phase-referenced VLBI observations of supernova 1993J at 24 epochs, from 50 days after shock breakout to the present, allowed us to determine the coordinates of the explosion center relative to the quasistationary core of the host galaxy M81 with an accuracy of 45 kas and to determine the nominal proper motion of the geometric center of the radio shell with an accuracy of 9 kas yr~1. The uncertainties correspond to 160 AU for the position and 160 km s~1 for the proper motion at the distance of the source of 3.63 Mpc. After correcting for the expected galactic proper motion of the supernova around the core of M81 using H I rotation curves, we obtain a peculiar proper motion of the radio shell center of only 320^160 km s~1 to the south, which limits any possible one-sided expansion of the shell. We also Ðnd that the shell is highly circular, the outer contours in fact being circular to within 3%. Combining our proper-motion values with the degree of circular symmetry, we Ðnd that the expansion of the shock front from the explosion center is isotropic to within 5.5% in the plane of the sky. This is a more fundamental result on isotropic expansion than can be derived from the circularity of the images alone. The brightness of the radio shell, however, varies along the ridge and systematically changes with time. The degree of isotropy in the expansion of the shock front contrasts with the asymmetries and polarization found in optical spectral lines. Asymmetric density distributions in the ejecta, or more likely in the circumstellar medium, are favored to reconcile the radio and optical results. We see no sign of any disklike density distribution of the circumstellar material, with the average axis ratio of the radio shell of SN 1993J being less than 1.04.

show abstract

VLBI limits on the proper motion of the ‘core’ of the superluminal quasar 3C345

Cited by 101 publications

References 44 publications

Absolute kinematics of radio source components in the complete S5 polar cap sample

Absolute kinematics of radio source components in the complete S5 polar cap sample

Alma Science Verification Data: Millimeter Continuum Polarimetry of the Bright Radio Quasar 3c 286

SN 1993J VLBI. I. The Center of the Explosion and a Limit on Anisotropic Expansion

Contact Info

Product

Resources

About