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	Figure 1: Chandra images of 0156-252, 0406-244, 0828+193, 2036-254 and 2048-272, showing the 0.2-6 keV X-ray images in colorscales, and the 4.7 GHz VLA radio contours in yellow (from Carilli et al. 1997; Pentericci et al. 2000a). The Chandra images have been smoothed using a Gaussian kernel of width 2 ( FWHM). Radio contours are mJy beam-1.
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In the text

Figure 2: Monochromatic X-ray luminosity versus radio luminosity. The four detected cores from our sample are indicated by filled stars. Their X-ray luminosities were corrected for galactic absorption only. Narrow line AGN from the FIRST/ROSAT sample of Brinkmann et al. (2000) are indicated by circles. The dashed line indicates the correlation for radio-loud quasars of Brinkmann et al. (2000). Open stars indicate several low (Cygnus A at z=0.06) and high redshift (1138-262 at z=2.16, B0902+343 at z=3.395, 4C41.17 at z=3.798) radio galaxies from the literature (see Carilli et al. 2002; Scharf et al. 2003; Fabian et al. 2002, and references therein). The X-ray luminosities of these sources were all corrected for intrinsic absorption.

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In the text

	Figure 3: Spectrum of the core of 0156-252, fitted with a power-law spectrum modified by absorption at the source.
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In the text

Figure 4: Synchrotron model predictions. We indicate the observed radio, optical and X-ray flux densities for all components that have a positive X-ray detection. Solid lines represent synchrotron spectra constructed using the 4.7 GHz radio to X-ray spectral index, . Dotted lines indicate spectra constructed using a radio spectral index, . For each component, the data and models were offset for clearer visibility of the results. The multiplicative factors for 0156-252 NE, 0156-252 SW, 0406-244 SE, 2036-254 SE and 2048-272 NE were 1.1, 1.4, 0.03, 0.001, 0.0003, respectively.

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In the text

	Figure 5: HST/WFPC2 F555W image of 0156-252 with 4.7 GHz VLA radio contours superimposed. We have detected extended UV line emission (most likely C  Å) at the position of the NE lobe (box region). An elongated feature in the extended emission resembles a bow-shock that follows the radio lobe (arrow).
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In the text

	Figure 6: X-ray image of the field around 0156-252 . The image was smoothed by a Gaussian (10 FWHM), after replacing the X-ray counts due to the radio source and point sources in the field by a Poissonian background. A large region of diffuse emission (indicated by the dashed ellipse) is found just northeast to the radio galaxy (indicated by its radio contours).
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In the text

Figure 7: Left: stacked image of the five HzRG fields, after subtraction of point sources. Indicated are the annuli from which a radial surface brightness profile was extracted. The innermost circle encompasses the total extent of the largest radio source in the sample. Counts inside this region due to the radio sources have been replaced by the background, estimated from the large, dashed annular region. Right: stacked image smoothed by a 10 ( FWHM) Gaussian. Scales run from below (white) to above (black) the mean. The background region and the maximum size of the radio sources are indicated. The distinct peaks in this summed image are not traced back to significant features in any of the individual images.

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In the text

	Figure 8: Radial surface brightness profile extracted from the stackedimage shown in Fig. 7.
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In the text

Figure 9: The positions of serendipitous X-ray sources with flux  erg cm-2 s-1 in the five HzRG fields combined. Different symbols indicate the sources in the 5 individual fields. The five images are aligned so that the radio sources (indicated by large diamond) all coincide with the position of 0156-252, and rotated to maximize the overlapping areas of the different pointings (indicated by dotted circles). The full circle indicates an area of 1 Mpc in radius around the radio source.

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In the text