Volume 472, Number 3, September IV 2007
|Page(s)||763 - 771|
|Published online||10 May 2007|
A multi-epoch VLBI survey of the kinematics of CJF sources*
I. Model-fit parameters and maps
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: email@example.com
2 ASTRON, Netherlands Foundation for Research in Astronomy, Oude Hoogeveensedijk 4, PO Box 2, 7990 AA Dwingeloo, The Netherlands
3 Landessternwarte, Königstuhl, 69117 Heidelberg, Germany
4 Kavli Institute of particle Astrophysics and Cosmology, Menlo Park, CA 94025, USA
5 National Radio Astronomy Observatory, Socorro, NM 87801, USA
6 Joint Institute for VLBI in Europe, Oude Hoogeveensedijk 4, PO Box 2, 7991 PD Dwingeloo, The Netherlands
7 California Institute of Technology, Department of Astronomy, 105-24, Pasadena, CA 91125, USA
8 University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire SK11 9 DL, UK
Accepted: 2 May 2007
Context.This is the first of a series of papers presenting VLBI observations of the 293 Caltech-Jodrell Bank Flat-Spectrum (hereafter CJF) sources and their analysis.
Aims.One of the major goals of the CJF is to make a statistical study of the apparent velocities of the sources.
Methods.We have conducted global VLBI and VLBA observations at 5 GHz since 1990, accumulating thirteen separate observing campaigns.
Results.We present here an overview of the observations, give details of the data reduction and present the source parameters resulting from a model-fitting procedure. For every source at every observing epoch, an image is shown, built up by restoring the model-fitted components, convolved with the clean beam, into the residual image, which was made by Fourier transforming the visibility data after first subtracting the model-fitted components in the uv-plane. Overplotted we show symbols to represent the model components.
Conclusions.We have produced VLBI images of all but 5 of the 293 sources in the complete CJF sample at several epochs and investigated the kinematics of 266 AGN.
Key words: techniques: interferometric / surveys / galaxies: active / radio continuum: galaxies
© ESO, 2007
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