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1 Introduction

Multiwaveband studies of Active Galactic Nuclei (AGN) have become an essential part in understanding these objects. Indeed, our knowledge of this group of objects is not complete until the relation between their (e.g.) optical, radio and X-ray emission is clear. Moreover, part of the study of AGN concentrates on the importance of "unified schemes'' in explaining the appearance of these objects. Tests for these schemes are more efficient when different characteristics in different wavebands have to be explained.

For these reasons we started a few years ago the study of a complete sample of radio sources with the idea of building an homogeneous database that could allow a comprehensive investigation of various aspects and open questions connected with AGNs. For this study we have used the southern part of the so-called 2-Jy sample (Wall & Peacock 1985) with selection criteria $S_{2.7\, {\rm GHz}}> 2$ Jy, $\delta<+10^\circ$ and z<0.7. This sample includes 88 radio sources (radio galaxies and quasars) of many different classes, i.e. Fanaroff-Riley (Fanaroff & Riley 1974) types I and II, core/halo, Compact Steep Spectrum (CSS) and flat spectrum sources. For all these objects we have now collected optical spectra and polarimetry (Tadhunter et al. 1997; Tadhunter et al. 1998), X-ray data (Siebert et al. 1996; Padovani et al. 1999; Trussoni et al. 1999) and radio data. The latter comprise images (VLA and ATCA, Morganti et al. 1993) and high resolution core flux density measurements (Morganti et al. 1997a).

A number of interesting results have been already obtained from this database (see Morganti & Tadhunter 1997; Morganti et al. 1997a; Tadhunter et al. 1997; Tadhunter et al. 1998 and ref. therein). However, together with the results some new questions have arisen which would benefit from higher quality data than available at present. In particular, for a number of sources the radio maps available are not good enough for a proper morphological classification and to derive other important parameters.

  \begin{figure}{\psfig{figure=ds1732f1.eps,angle=0,width=8.8cm} }
\end{figure} Figure 1: Image of 0039-44 at 3-cm (full resolution) with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 0.26 ratio). The contour levels are: $0.5 \times -1$, 1, 2, 4, 8, 16, 32, 64, 128, 256 mJy beam-1. The peak flux is 289.0 mJy beam-1. The synthesized beam of the observations is marked in the low left corner. The cross indicates the position (from di Serego et al. 1994) of the optical galaxy

In order to improve the available radio images we have carried out new observations, for a number of radio galaxies in the sample, using either the VLA or the ATCA, according to the declination of the sources. This work can be, therefore, considered as a follow-up and completion of the radio study of this sample presented in Morganti et al. (1993). In this paper we present the new total intensity and polarisation radio images obtained for 14 radio galaxies. The objects selected are very different in morphology: among them there are both small double-lobed and large objects that needed a better radio image for a proper classification. These images will be mainly used for follow up work where radio-optical comparison will be done.

Throughout this paper we assume that H0 = 50 km s-1 Mpc-1 and q0=0.


 


 
Table 1: General characteristics
Object   z $\alpha^{4.8\, {\rm GHz}}_{2.3\, {\rm GHz}}$ $\log P_{{\rm tot}}^{6\, {\rm cm}}$ LAS LLS
        W Hz-1 arcsec kpc
             
0034-01 3C 15 0.073 0.79 25.59 42 80
0035-02 3C 17 0.220 0.72 26.81 38 181
0039-44   0.346 0.93 26.93 9.5 62
0043-42   0.116 0.87 26.28 160 460
0117-15 3C 38 0.565 0.90 27.54 14 120
0409-75   0.693 0.86 28.18 9 85
0442-28 OF-271 0.147 0.93 26.38 105 367
0453-20 OF-289 0.035 0.73 25.00 27 26
0625-53   0.054 1.17 25.40 90 130
1602+01 3C 327.1 0.462 1.07 27.21 19 147
1938-15 OV-164 0.452 0.82 27.47 6.5 50
1954-55   0.060 0.78 25.58 360 576
2058-28   0.038 0.74 25.11 600 628
2314+03 3C 459 0.220 0.97 26.54 10 48
             



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