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Published August 1995 | Published
Journal Article Open

The First Caltech-Jodrell Bank VLBI Survey. III. VLBI and MERLIN Observations at 5 GHz and VLA Observations at 1.4 GHz


We present the 5 GHz results from the first Caltech-Jodrell Bank (CJ1) VLBI survey. The 1.6 GHz maps were presented in two separate papers (Polatidis et al. 1995; Thakkar et al. 1995). These three papers complete the first stage of this program to map at both 1.6 and 5 GHz all objects accessible to Mark II VLBI in the complete sample of 135 objects with 1.3 > S_(5 GHz) ≥ 0.7 Jy, δ(1950) ≥ 35°, and |b| > 10°. The combination of the CJ1 sample with the Pearson-Readhead (PR) sample provides a complete, flux density-limited sample of 200 objects with S_(5 GHz) ≥ 0.7 Jy, δ(1950) ≥35°, and |b| > 10° for which all of the objects accessible to Mark II VLBI have been mapped at both 5 GHz(129 objects) and 1.6 GHz(132 objects). In addition to the 5 GHz VLBI maps, we present in this paper 5 GHz MERLIN observations of 20 objects and 1.4 GHz VLA observations of 92 objects in the combined CJ1 + PR sample. The VLA maps, together with L- band (1.3-1.7 GHz) maps available in the literature, provide a complete set of VLA maps for the combined CJ1 + PR sample. Finally, we present the radio spectra of the objects in the CJ1 sample. The combined CJ1 + PR VLBI surveys provide a sample which is large enough for a number of important astrophysical and cosmological studies. These will be presented in further papers in this series.

Additional Information

© 1995 The American Astronomical Society. Received 1994 November 28; accepted 1995 January 26. We thank the staffs of the observatories in the European and the US VLBI networks and the staff of the JPL/Caltech Block 2 correlator for their assistance during the CJl survey. We also thank R. C. Vermeulen and G. B. Taylor for their help with fringe-fitting and automatic mapping and G. B. Taylor and D. R. Henstock for observing six objects for us. A. G. P. acknowledges the receipt of a British Council Fellowship for the year 1991. The work at the California Institute of Technology was supported by the National Science Foundation (grants AST-8814554 and AST-9117100). The VLA and VLBA are instruments of the National Radio Astronomy Observatory, which is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation.

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