Multifrequency studies of seven 3CR radio sources - 1. The observations

Details Multifrequency studies of seven 3CR radio sources - 1. The observations Multifrequency studies of seven 3CR radio sources - 1. The observations

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.186..293b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 186, p. 293-296 (1979)

Mathematics

Logic

30

Scientific paper

In order to study the variation in spectrum and polarization across double radio sources, seven sources have been mapped at 2.7 and 15 GHz with the Cambridge 5-km telescope (Ryle 1972). In addition, the One-Mile Telescope (Elsmore, Kenderdine & Ryle 1966) has been used to make maps at 1.4 GHz which have more interferometer spacings and greater dynamic ranges than those by Macdonald, Kenderdine & Neville (1968, hereinafter MKN). Polarization maps of the sources have also been made for the first time with the One-Mile Telescope at 1.4 GHz.
The results, which allow various source models to be explored in detail, will be discussed in a subsequent paper.
The morphological information for each source is summarized in Table 1. Each source is subdivided into several components, usually following a clear distinction between the compact and extended features visible on the 2.7-GHz maps.
The details of Table 1 are as follows:
(1) The 3CR number of the source. (2) The individual components of each source. (3) The observing frequency. (4), (5) The 1950.0 coordinates of each component. (6) The angular extents of the component. When the component is barely resolved, the values are the half-power widths of a Gaussian source which would produce the observed broadening of the beam. For 3C 219, 3C 382 and 3C 430, results are presented for typical sections only of the bridge regions. (7) The position angles of the components, if well defined. (8) The flux density from each component, representing the Stokes' parameter I at 2.7 GHz and I - Q or I + Q at 15 GHz. The total flux densities at 1.4 GHz were obtained by integrating over the I maps while those at 2.7 GHz were derived from the maximum amplitudes observed on the shortest interferometer spacings, corrected from I - Q to I using the integrated polarization values in (11) and (12).

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