All Figures

	Figure 1: Surface brightness profile (SBP) of the quasar B3 0740+380C (solid circles) together with the SBP of the field stars scaled to the quasar intensity peak (points). The solid line shows the mean of the stars' SBPs, and the dashed line shows the mean PSF derived from fitting a Moffat function.
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In the text

	Figure 2: Probability density functions for exponent  obtained from fits to simulated elliptical and disk galaxies.
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In the text

Figure 3: Contour maps and surface brightness profiles of the quasars with detected extension. In each panel a) is the contour map (left) and surface brightness (right) of the original image, and b) is the contour map (left) and surface brigthness (right) of the HG image. The solid line in a) shows the mean PSF scaled to the quasar intensity peak. The distances between small marks are 2 (for objects observed with OMEGA), and 1.2 (for objects observed with WHIRCAM). The size of the contour maps is 16 16 for all the images. First contour level is at 2 per pixel, with a separation of 0.5 mag between successive contours.

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In the text

	Figure 3: continued.
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In the text

	Figure 3: continued.
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In the text

	Figure 3: continued.
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In the text

Figure 4: K-band magnitude distribution with redshift for the HGs of radio quasars: circles for the B3-VLA (solid for new data and open for Paper I data), diamonds for Lehnert et al. (1992), open squares for Taylor et al. (1996), asterisks for Kotilainen et al. (1998), stars for Kotilainen & Falomo (2000), triangles for Falomo et al. (2001) and solid squares for Kukula et al. (2001). The typical error of the magnitudes for the different samples is presented in the upper-left panel. The shaded region shows the parameter space occupied by radio galaxies of different samples (see text); the dashed line is the distribution of the mean values. The solid concave lines show the expected evolution of an elliptical galaxy with different formation redshifts ( , 4.5, 2.5, 1.5, 1.0 and 0.7, from right to left). The convex lines show the expected evolution of an galaxy with an ongoing burst with different formation redshifts ( , 1.5, 1.0 and 0.7, from right to left). The near straight solid line shows the expected magnitudes for a galaxy without evolution.

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In the text

	Figure 5: Distribution of the radio power at 1460 MHz against the redshift. The solid symbols are the HGs for the B3-VLA quasars; the open symbols are the HGs from the literature.
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In the text

	Figure 6: Distribution of the radio power at 1460 MHz against the absolute magnitude of the HGs. The solid symbols are the HGs for the B3-VLA quasars; the open symbols are the HGs from the literature.
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In the text

	Figure 7: Distribution of the K-band absolute magnitudes of the HGs against the absolute magnitude of the central source. The solid symbols are the HGs for the B3-VLA quasars; the open symbols are the HGs from the literature.
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In the text

	Figure 8: Distribution of the K-band apparent magnitudes of the HGs against the apparent magnitude of the central source. The solid symbols are the HGs for the B3-VLA quasars; the open symbols are the HGs from the literature.
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In the text

	Figure 9: Distribution of the effective surface brightness profile against the effective radius. The solid symbols are the HGs for the B3-VLA quasars; the open symbols are the HGs from the literature. The solid line show the best linear regression fit to the unbiased data. The dashed lines show the exclusion region for detection for the B3-VLA subsample.
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In the text

	Figure 10: Distribution of the radio power at 1460 MHz against the absolute magnitude of the nuclear source. The solid symbols are the HGs for the B3-VLA quasars; the open symbols are the HGs from the literature.
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In the text