All Figures

$\begin{figure} \par\includegraphics[height=20.5cm,width=14.6cm,clip]{6410_f1.ps}\end{figure}$ Figure 1: QSO spectra extracted with a 3 $^{\prime \prime }$ radial aperture. No correction for Galactic reddening is applied. Metal absorption lines associated with the DLA systems are indicated. For those QSOs with multiple DLA lines only the DLA lines and their redshifts are indicated. Line identifications written below the spectra are QSO emission lines.
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In the text

$\begin{figure} \par\includegraphics[height=19.9cm,width=12.5cm,clip]{6410_f2.ps}\end{figure}$ Figure 2: Left panels: narrow-band images of the QSOs with overlayed contours of narrow-band images centered on the Ly $\alpha$ wavelengths of the DLAs. The images are 8 $^{\prime \prime }$ square. Contour levels correspond to 2, 3, 4 $\sigma$ levels above the background noise. Middle panels: the reverse, where the contours are arbitrary apart from the central one that shows the QSO seeing FWHM. Right hand panels: spectra of candidate emission line objects created from co-adding spectra from spaxels associated with the emission line candidates. The width of the grey bars over the emission lines correspond to the wavelength ranges of the narrow band images. The lines below the spectra show the background sky noise spectra determined from background spaxels. See the online version for plots of the remaining candidates.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6410_f3.ps}\end{figure}$ Figure 3: Line fluxes of Ly $\alpha$ emission objects as function of redshift, where square symbols represent already confirmed objects and triangles the candidates. The solid and dashed lines correspond to Ly $\alpha$ luminosities of 10⁴² and 10⁴³ erg s^-1, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6410_f4.ps}\end{figure}$ Figure 4: Velocity differences between the Ly $\alpha$ emission lines and DLA redshifts as a function of the Ly $\alpha$ luminosity. An average error bar for the Ly $\alpha$ emission candidates is shown in the lower right corner.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6410_f5.ps}\end{figure}$ Figure 5: Velocity differences between the Ly $\alpha$ emission lines and DLA redshifts as a function of the impact parameter.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6410_f6.ps}\end{figure}$ Figure 6: Angular impact parameter vs. redshift. The solid line corresponds to the size-luminosity relation for an L_B^* galaxy (Chen & Lanzetta 2003), while the dotted and dashed lines correspond to galaxies with B band luminosities $L_B=10\%L_B^*$ and $L_B=1\%L_B^*$ , respectively. Squares are objects from the literature and triangles the candidates from this survey.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{6410_f7.ps}\end{figure}$ Figure 7: Column density of neutral hydrogen as a function of impact parameters for the candidates and previously confirmed objects. The symbols are similar to the previous figures. The solid and dashed lines are fits to the power-law relation $b/b^*=(N/N^*)^{\beta }$ for the candidates and confirmed objects, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{6410_f8.ps}\end{figure}$ Figure 8: Column density of neutral hydrogen as a function of impact parameter for the candidates and previously confirmed objects. The solid and dashed lines show the fit to the exponential relation $\mbox{$N(H {\sc i})$ }= \mbox{$N(H {\sc i})$ }_0 \exp (-b/h)$ for the candidates and confirmed objects, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6410_f9.ps}\end{figure}$ Figure 9: Cumulative distribution of Si metallicities of the six good emission line candidates compared to the remaining part of the sample. The probability that the two distributions are similar is 38% estimated from a Kolmogorov-Smirnov test.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{6410_f10.ps}\end{figure}$ Figure 10: DLA metallicities as a function of the impact parameters, where symbols shapes have similar meanings as in the previous figures. The dotted line shows a fit to all the objects excluding the limits. This line has a gradient of -0.024 $\pm$ 0.015 dex kpc^-1. Data for the confirmed objects are either [Si/H] of [Zn/H] taken from Møller et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[height=19.9cm,width=12.5cm,clip]{6410f2.2.ps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[height=19.9cm,width=12.5cm,clip]{6410f2.3.ps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[height=19.9cm,width=12.5cm,clip]{6410f2.4.ps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6410f2.5.ps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[height=20.5cm,width=14.6cm,clip]{6410_f1.ps}\end{figure}$	Figure 1: QSO spectra extracted with a 3 $^{\prime \prime }$ radial aperture. No correction for Galactic reddening is applied. Metal absorption lines associated with the DLA systems are indicated. For those QSOs with multiple DLA lines only the DLA lines and their redshifts are indicated. Line identifications written below the spectra are QSO emission lines.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6410_f3.ps}\end{figure}$	Figure 3: Line fluxes of Ly $\alpha$ emission objects as function of redshift, where square symbols represent already confirmed objects and triangles the candidates. The solid and dashed lines correspond to Ly $\alpha$ luminosities of 10⁴² and 10⁴³ erg s^-1, respectively.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6410_f4.ps}\end{figure}$	Figure 4: Velocity differences between the Ly $\alpha$ emission lines and DLA redshifts as a function of the Ly $\alpha$ luminosity. An average error bar for the Ly $\alpha$ emission candidates is shown in the lower right corner.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6410_f5.ps}\end{figure}$	Figure 5: Velocity differences between the Ly $\alpha$ emission lines and DLA redshifts as a function of the impact parameter.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6410_f6.ps}\end{figure}$	Figure 6: Angular impact parameter vs. redshift. The solid line corresponds to the size-luminosity relation for an L_B^* galaxy (Chen & Lanzetta 2003), while the dotted and dashed lines correspond to galaxies with B band luminosities $L_B=10\%L_B^$ and $L_B=1\%L_B^$ , respectively. Squares are objects from the literature and triangles the candidates from this survey.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{6410_f7.ps}\end{figure}$	Figure 7: Column density of neutral hydrogen as a function of impact parameters for the candidates and previously confirmed objects. The symbols are similar to the previous figures. The solid and dashed lines are fits to the power-law relation $b/b^=(N/N^)^{\beta }$ for the candidates and confirmed objects, respectively.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{6410_f8.ps}\end{figure}$	Figure 8: Column density of neutral hydrogen as a function of impact parameter for the candidates and previously confirmed objects. The solid and dashed lines show the fit to the exponential relation $\mbox{$N(H {\sc i})$ }= \mbox{$N(H {\sc i})$ }_0 \exp (-b/h)$ for the candidates and confirmed objects, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6410_f9.ps}\end{figure}$	Figure 9: Cumulative distribution of Si metallicities of the six good emission line candidates compared to the remaining part of the sample. The probability that the two distributions are similar is 38% estimated from a Kolmogorov-Smirnov test.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{6410_f10.ps}\end{figure}$	Figure 10: DLA metallicities as a function of the impact parameters, where symbols shapes have similar meanings as in the previous figures. The dotted line shows a fit to all the objects excluding the limits. This line has a gradient of -0.024 $\pm$ 0.015 dex kpc^-1. Data for the confirmed objects are either [Si/H] of [Zn/H] taken from Møller et al. (2004).
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$\begin{figure} \par\includegraphics[height=19.9cm,width=12.5cm,clip]{6410f2.2.ps} \end{figure}$	Figure 2: continued.
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