The Caltech-Jodrell Bank VLBI Survey

Details The Caltech-Jodrell Bank VLBI Survey The Caltech-Jodrell Bank VLBI Survey

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...18111303x&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #113.03D; Bulletin of the American Astronomical Society, Vol. 24, p.1300

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The Caltech--Jodrell Bank (CJ) sample includes all 135 extragalatic sources in the S4 (Pauliny-Toth et al., 1978, A.J., 83, 451) and S5 (K{u}hr et al., 1981, A.J., 86, 854) surveys with 0.7 Jy <= S(5GHz) <= 1.3 Jy, delta >= 35(deg) , and |b| >= 10(deg) ; which, combined with the Pearson--Readhead sample (1988, Ap.J., 328, 114) of 65 sources brighter than 1.3 Jy in the same sky region, provides a complete flux-limited sample of 200 sources. In the past three years we developed and successfully implemented the ``VLBI-SNAPSHOT'' technique. This technique can provide thermal noise limited images of the compact radio sources brighter than ~ 300 mJy with a global VLBI array of more than 13 stations and three 20--30 minutes scans in the MK II format. This new technique has increased the observation efficiency by an order of magnitude and hence made the Calthch--Jodrell Bank VLBI survey possible. In the survey, all sources in the CJ sample with a compact emission region brighter than 300 mJy at 5 GHz were mapped at both 1.6 GHz and 5 GHz, and 27 sources in the PR sample not previously mapped at 1.6 GHz were mapped at this frequency. In addition to the VLBI observations, 92 of the 200 sources were observed with VLA at 1.4 GHz so as to obtain a collection of quasi-uniform maps with dynamic range > 1000:1, and the sources with structures between 0.05 and 2 arcsec were observed with MERLIN at 5 GHz. This is the largest sample ever imaged at all milliarcsecond, subarcsecond and arcsecond scales. The main objectives of this study are: (1) to classify these objects, based on radio morphologies on all scales, radio spectral index, optical identification; Such a classification is an essential pre-requisite to understanding the physics and evolution of the radio loud active galaxies; it is also an important observational foundation for testing various ``Unified Schemes''. (2) to make interesting statistical tests by class, such as cosmological evolution; (3) to reveal the relationships between different classes, if any; and (4) to study the physics of individual objects of interest.

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