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Astron. Astrophys. 345, 769-777 (1999)

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2. Sample selection

The sample we choose for this study consists of:

1) the sample selected from the 3CR and the Peacock & Wall (1981; PW) catalogues (Fanti et al. 1995), and

2) nine sources extracted from the B3 VLA sample (Vigotti et al. 1989).

1) The 3CR/PW sample (38 sources) was established on the basis of the well-known criteria: linear size [FORMULA] 15 kpc, spectral index [FORMULA] 0.5 and a limit in radio power P [FORMULA] W/Hz at 178 MHz for the 3CR, or P [FORMULA] W/Hz at 2.7 GHz for the PW. High resolution structure information is available for these sources from the literature. In the framework of this project we observed at 230 GHz the 17 sources for which the flux densities at this frequency were not available from literature.

2) The second complete sample of CSS sources was selected from the "strong" section of the B3 VLA catalogue ([FORMULA] 0.8 Jy) according to the following definitions: [FORMULA] up to 10 GHz, and a size of [FORMULA] 15 kpc. Sources with [FORMULA] have also been included if their spectrum is steeper than [FORMULA] at [FORMULA] GHz. These are Giga-Hertz-peaked spectrum (GPS) candidate sources. This sample contains 83 objects. The sample has been recently observed with the VLA at 5 and 8.4 GHz, with resolutions of [FORMULA]. Additional observations with VLBI arrays are planned. Only about 60% of these sources have at the moment either a photometric or a spectroscopic redshift, therefore we limited the list to the objects which could be observed at 230 GHz to the latter. Due to scheduling constraints we only observed 9 sources of the B3 VLA sample.

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© European Southern Observatory (ESO) 1999

Online publication: April 28, 1999