All Figures

$\begin{figure} \par\includegraphics[width=16cm,clip]{1894fig1.ps} \end{figure}$ Figure 1: The central portion (FoV: $6 \times 6$ arcsec; North is up and East to the left) of images in the Ks filter of the three selected quasars ( left: 0045-3337; middle: 0101-337; right: 0113-283). At the redshift of the objects, these correspond to rest frame V or R-bands. In all frames the target is indicated by the arrow.
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In the text

$\begin{figure} \par\includegraphics[width=5.45cm,clip]{1894fig2.ps} \end{figure}$ Figure 2: Contour plot of the K band image of Q 0045-3337 (North is up and East to the left). The QSO is the bright compact source 1.2 arcsec South of the more extended, K= 17.6, foreground galaxy. The image of the quasar is slightly elongated along the direction perpendicular to the QSO-galaxy pair. The circle represents the Einstein ring centered on the companion galaxy for a point source of mass $M = 1 \times 10^{11}~M_\odot$ (see text).
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{1894fig3.ps} \end{figure}$ Figure 3: The observed radial brightness profiles of the QSO 0113-283 (filled squares), superimposed on the fitted model (solid line) consisting of the PSF (dotted line) and an elliptical galaxy convolved with its PSF (dashed line). The associated errors are a combination of the statistical photometry in each bin and of the uncertainty on the background level (that is dominant at the faintest fluxes).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{1894fig4.ps} \end{figure}$ Figure 4: The evolution of radio loud quasar host luminosity compared with that expected for massive ellipticals (at M^*, M^*-1 and M^*-2; solid, dotted and dashed line) undergoing passive stellar evolution (Bressan Granato & Silva 1998). The new detected host galaxy at $z \sim 2.5$ (asterisk) is compared with the data for samples of lower redshift RLQ presented in Falomo et al. (2004). Each point is plotted at the mean redshift of the considered sample while the error bar represents the $1\sigma$ dispersion of the mean except for the new detection where the uncertainty of the measurement is given.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{1894fig1.ps} \end{figure}$	Figure 1: The central portion (FoV: $6 \times 6$ arcsec; North is up and East to the left) of images in the Ks filter of the three selected quasars ( left: 0045-3337; middle: 0101-337; right: 0113-283). At the redshift of the objects, these correspond to rest frame V or R-bands. In all frames the target is indicated by the arrow.
Open with DEXTER