All Figures

$\begin{figure} \par\includegraphics[width=12.3cm,clip]{5318f1.ps} \end{figure}$ Figure 1: Extended Ly $\alpha$ emission line regions at the QSO redshifts. The left hand panels show 8 $^{\prime \prime }$ $\times$ 8 $^{\prime \prime }$ narrow-band images created using a simple on-band minus off-band image technique. The centers of the QSOs are placed at the coordinates (0, 0). All images are interpolated representations with pixel sizes of 0 $.\!\!^{\prime\prime}$ 2 with the orientation north up and east left. The bright objects (Q1425+606 and Q1759+7539) have strong residuals within the central 1 $^{\prime \prime }$ . The Right hand panels show the spectra of the extended narrow Ly $\alpha$ emission (thin line) compared with the QSO spectra scaled down by a factor of 40 (thick line). The spectrum of Q1802+5616 was only scaled down by a factor of 3. No extended emission is found from Q1802+5616 and Q1347+112. Where found, the Ly $\alpha$ emission lines from the EELRs are clearly narrower than the broad QSO lines.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5318f2.ps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5318f3.ps} \end{figure}$ Figure 2: Similar to Fig. 1, but using an alternative QSO subtraction method, where the PSF is modeled as a function of wavelength. The image still shows strong residuals close to the QSO center. Compared to the spectrum in Fig. 1, the one-dimensional spectrum of the EELR is more noisy.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5318f4.ps} \end{figure}$ Figure 3: Maps of properties for the Ly $\alpha$ emission nebula around Q1425+606. Upper left panel: map of the Ly $\alpha$ emission velocity offset relative to the QSO redshift. Upper right panel: map of the integrated flux from each spaxel with smoothed velocity contours overlaid. White fields correspond to spaxels where the Ly $\alpha$ emission line could not be recognised visually, which therefore warps the velocity contours close to the QSO center at (0, 0) where residuals are present. Lower left panel: map of the Ly $\alpha$ FWHM corrected for the instrument resolution. The lower right panel shows the radial profiles of the velocity component (solid line, left side axis) and Ly $\alpha$ surface flux density (dashed line, right axis) starting from the center of the QSO along a direction with PA = 135 $^{\circ }$ east of north. A fit of the radial surface brightness profile by an exponential function gives a scale length of $\sim$ 2 $.\!\!^{\prime\prime}$ 5 (20 kpc). (This figure is available in color in electronic form.)
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5318f5.ps} \end{figure}$ Figure 4: Maps of the Ly $\alpha$ emission nebula surrounding Q1759+7539. The panels are similar to those described in Fig. 3. Profiles in the lower right panel are derived at PA = 225 $^{\circ }$ east of north. A fit of an exponential function to the radial surface brightness profile gives a scale length of $\sim$ 1 $.\!\!^{\prime\prime}$ 4 corresponding to 10 kpc at the QSO redshift. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5318f6.ps} \end{figure}$ Figure 5: Luminosities in the EELRs as a function of the integrated luminosities for the QSO broad Ly $\alpha$ lines. The IFS results are indicated by stars, where the filled star represents the one core-dominated RLQ, and the outlined stars the four RQQs. Squares represent the emission line nebulae surrounding 18 lobe-dominated RLQs from the sample in H91b. Arrows indicate upper limits for objects where no extended Ly $\alpha$ emission was found.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5318f7.ps} \end{figure}$ Figure 6: Extended Ly $\alpha$ emission line luminosities as a function of the predicted quasar luminosities at the rest-frame 912 Å. There is no significant correlation between the EELR luminosities and the nuclear ionising luminosities.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5318f8.ps} \end{figure}$ Figure 7: Integrated luminosities from the QSOs broad Ly $\alpha$ lines as a function of the ionising flux calculated at 912 Å.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5318f9.ps} \end{figure}$ Figure 8: Total Ly $\alpha$ luminosity from the nebulae as a function of the maximum projected sizes. Symbol shapes are as in the other figures and arrows indicate upper limits.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5318f2.ps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{5318f3.ps} \end{figure}$	Figure 2: Similar to Fig. 1, but using an alternative QSO subtraction method, where the PSF is modeled as a function of wavelength. The image still shows strong residuals close to the QSO center. Compared to the spectrum in Fig. 1, the one-dimensional spectrum of the EELR is more noisy.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5318f7.ps} \end{figure}$	Figure 6: Extended Ly $\alpha$ emission line luminosities as a function of the predicted quasar luminosities at the rest-frame 912 Å. There is no significant correlation between the EELR luminosities and the nuclear ionising luminosities.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5318f8.ps} \end{figure}$	Figure 7: Integrated luminosities from the QSOs broad Ly $\alpha$ lines as a function of the ionising flux calculated at 912 Å.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5318f9.ps} \end{figure}$	Figure 8: Total Ly $\alpha$ luminosity from the nebulae as a function of the maximum projected sizes. Symbol shapes are as in the other figures and arrows indicate upper limits.
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