The sample is defined as follows:
Part 1: 233 sources with (hereafter on the Baars et al. 1977 scale) within the B(1950) sky coordinates: , and , . Sky area of 0.4414 sr.
Part 2: 109 sources with
, . Sky area of 0.0906 sr.
Part 3: 31 sources with
, . Sky area of 0.0550 sr.
All the sources have . Hereafter these parts are referred to as Subsample 1, 2, and 3, respectively.
For all the sample sources their two independent measurements of 1.4 GHz flux density resulting from the Green Bank surveys GB/GB2 (Maslowski 1972; Machalski 1978a) and 83GB (Condon & Broderick 1985; the relevant catalogue by White & Becker 1992) were compared with the measured VLA flux density (cf. Introduction). That comparison allowed to select either confused sources requiring flux correction or heavily resolved sources for further reobservations with lower resolution. Some of the confused sources appeared to be two different ones but still satisfying the criteria of the sample. Recently D-array and B-array maps for several of the sample sources have become available from the large VLA 1.4-GHz sky surveys: FIRST by Becker et al. (1995) and Condon et al. (1996). These were also used to check the effects of resolution in our data.
For many of the sources, additional 1.4 GHz fluxes were also available from
observations with the Effelsberg 100 m telescope
(Kühr et al. 1981) and
Arecibo 300 m telescope (Owen et al. 1983); some fluxes for compact
available from measurements with the WSRT and Cambridge One-mile (OMT)
telescopes. All collected 1.4 GHz flux densities, corrected for confusion if
necessary, were then used to compute the weighted mean flux density at this
and its error, , with the standard formulae
The mean 1.4-GHz flux density was used to verify completeness of the sample.
In order to satisfy the conditions given in Sect. 2.1, 12 sources from
Paper I and 20 sources observed in Papers IV and V have been excluded from the
sample. They are listed in
Table 1 (click here) with information about the cause of exclusion. In turn, 15
sources have been added to the sample because they were underestimated in
the finding surveys due to a large flux density error but their mean 1.4-GHz
flux density calculated from all available observations
(cf. Sect. 2.2) satisfied the selection criterion. These additional sources are indicated by a diamond mark preceding the source name in Table A3 (click here). Due to the above corrections, we estimate that now the sample is about 99 per cent complete for sources with , about 97 per cent complete for sources with , and about 95 per cent complete for sources with
. The completeness is evaluated using the method of Dixon & Kraus (1968).
|0738+336||2 sources||0728+364||2 sources||1202+488||cluster|
|0908+340||2 sources||0846+377||2 sources||1204+483||2 sources|
|0913+471||0851+363||2 sources||1205+500||2 sources|
|0914+502||0902+480||2 sources||1225+498||2 sources|
|1135+464||2 sources||0954+490||2 sources||1401+350||cluster||a)|
|1317+362||2 sources||0955+492||3 sources||1533+345||cluster|
|1442+363||2 sources||1124+488||cluster||1648+350||2 sources|
|1615+352||part of 1615+351?|
|a) given in Machalski & Condon (1990).|