Submilliarcsecond astrometry via VLBI. I - Relative position of the radio sources 3C 345 and NRAO 512

Shapiro, I. I.; Wittels, J. J.; Counselman, C. C.; Robertson, D. S.; Whitney, A. R.; Hinteregger, H. F.; Knight, C. A.; Rogers, A. E. E.; Clark, T. A.; Hutton, Laura; Niell, A. E.

doi:10.1086/112565

Cited by 69 publications

(54 citation statements)

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“…Figure 5 shows the uncertainties in the relative α and δ for the 24 pairs as a function of their separations. This behaviour is roughly linear, as predicted by the empirical formulae given by Shapiro et al (1979) and corroborated by simulations of astrometric VLBA observations performed by Pradel et al (2006). This linearity is more clearly seen in Fig.…”

Section: Resultssupporting

confidence: 84%

“…6, which shows the uncertainties of the estimates of the separations as a function of such separations. However, our astrometric uncertainties are ∼10 times smaller than those predicted by Shapiro et al (1979) and those estimated by Pradel, Charlot & Lestrade (2006) from their simulations, for typical declinations of the S5 polar cap sample sources. This improvement in precision is probably due to the fact that we have analysed the 13 sources simultaneously, instead of using the usual two-source (target/reference) scheme.…”

Section: Resultscontrasting

confidence: 60%

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

Martí-Vidal¹,

Marcaide²,

Guirado³

et al. 2007

A&A

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We report on the first wide-field, high-precision astrometric analysis of the 13 extragalactic radio sources of the complete S5 polar cap sample at 15.4 GHz. We describe new algorithms developed to enable the use of differenced phase delays in wide-field astrometric observations and discuss the impact of using differenced phase delays on the precision of the wide-field astrometric analysis. From this global fit, we obtained estimates of the relative source positions with precisions ranging from 14 to 200 µas at 15.4 GHz, depending on the angular separation of the sources (from ∼1.6 to ∼20.8 degrees). These precisions are ∼10 times higher than the achievable precisions using the phase-reference mapping technique.

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Section: Resultssupporting

confidence: 84%

Section: Resultscontrasting

confidence: 60%

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

Martí-Vidal¹,

Marcaide²,

Guirado³

et al. 2007

A&A

View full text Add to dashboard Cite

show abstract

“…Send offprint requests to: E. Ros, e-mail: ros@mpifr-bonn.mpg.de (BL 1803+784) to this pair, and extended the phaseconnection technique (Shapiro et al 1979) to separations of 6. • 8 from observations at 8.4 GHz.…”

Section: Added a New Sourcementioning

confidence: 99%

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

Ros

Marcaide

Guirado

2001

A&A

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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.

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“…Fundamentally, phase referencing (PR; Shapiro et al, 1979;Alef, 1988) uses the fringes of the calibrator to estimate the antenna based complex gains. These gains are time interpolated to the target observations resulting in calibrated target visibilities.…”

Section: Phase Referencingmentioning

confidence: 99%

KVN Phase Referencing Observations of the Virgo Cluster

Tremou¹,

Chung²,

Sohn³

2015

Publications of The Korean Astronomical Society

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By probing nuclear regions and the overall properties of AGN hosts as a function of their environments, we aim to observationally examine how AGN activities are related to their surroundings. We have selected a representative sample of AGN hosts in the Virgo cluster. The selected galaxies are located in a range of density regions showing various morphologies in 1.4 GHz continuum emission. High-resolution observations with the Korean VLBI Network (KVN) allow us to access the inner region of the AGN without suffering from dust extinction and synchrotron self-absorption. Since a number of our targets are too weak to be detected at K-band (22 GHz) within their coherence time, we applied phase referencing to calibrate fast atmospheric phase fluctuations.

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Submilliarcsecond astrometry via VLBI. I - Relative position of the radio sources 3C 345 and NRAO 512

Cited by 69 publications

References 0 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

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

KVN Phase Referencing Observations of the Virgo Cluster

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