All data reduction for this study used the NOD2 software package (Haslam
1974), modified for the Parkes telescope data. The automatic two-dimensional
elliptical Gaussian-fitting algorithms implemented in the NOD2 package were used to
search for sources and to determine source positions, flux densities and extension. A
planar base level was fitted to the region of every source detected in the survey
and the position and flux intensity of the discrete sources were then determined.
Sources were catalogued if their fitted Gaussian flux intensity was at least 5
times the rms. noise level (
) in the image (Table 1 (click here)) or seen in at least
two different frequency images but not weaker than 
. The validity of
each source was then checked by inspecting the images and, for those regions
in which there were clearly more than one discrete source, multi-source Gaussian
fitting was used to model the extended emitting region.