All Figures

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[clip]{1591_f1.eps}}\end{figure}$ Figure 1: Broad band image in the wavelength range $4500 < \lambda < 8000$ Å of the QSO at the position (0, 0) and the galaxy G4 at (-6.5, -1.5) as indicated. Each spaxel represents a spectrum and the field of view is $8\hbox {$^{\prime \prime }$ }\times 8\hbox {$^{\prime \prime }$ }$ . North is up and east is left. Coordinates are relative to the QSO position.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{1591_f2.ps}}\end{figure}$ Figure 2: Spectrum of PHL 1226 created by co-adding 20 spaxels. The flux levels are relative since the QSO is located at the edge of the field of view. Broad emission lines from H $\gamma$ and H $\beta$ at z=0.404 can be seen at 6100 Å and 6820 Å, respectively.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip,angle=90]{1591_f3.ps}}\end{figure}$ Figure 3: Spectrum of the galaxy created by co-addition of 112 spaxels. Any emission line present in the galaxy has been smeared out because many spaxels do not contribute to the line emission as shown in Sect. 3.1. The seemingly strong [S II] lines are partly caused by errors in sky subtraction.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip,angle=90]{1591_f4.ps}}\end{figure}$ Figure 4: Zoom in of the spectrum in Fig. 6 in the region around [N II], H $\alpha$ , and [S II]. This plot shows the effect of correcting for the telluric absorption feature around 7600 Å. The lower spectrum (thin line) is the uncorrected spectrum, and the gray line is the model of the telluric feature created from the QSO spectrum. The upper spectrum (thick line) has been corrected for the absorption feature and offset by $+3\times 10^{-17}$ erg cm^-2 s^-1 Å^-1 for clarity.
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In the text

$\begin{figure} \par\resizebox{5cm}{!}{\includegraphics[clip]{1591_f5.ps}}\hspace... ...hspace*{6mm} \resizebox{5cm}{!}{\includegraphics[clip]{1591_f10.ps}}\end{figure}$ Figure 5: Emission line images of various emission lines where the continuum has been subtracted using images using adjacent wavelengths. For comparison a broad band image is included in the lower right hand panel. Smoothed contours of 2, 4, 6,... $\sigma$ levels are overlayed. The solid black line represent the 4 $\sigma$ level.
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In the text

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[angle=90,clip]{1591_f11.ps}}\end{figure}$ Figure 6: Spectrum of the galaxy created by co-adding 15 spaxels that appeared to be associated with the bright line emission region. Emission lines listed in Table 2 are indicated.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{1591_f12.ps}}\end{figure}$ Figure 7: The gray scale image shows the intensity of the H $\alpha$ emission line. Relative velocities in km s^-1 inferred from H $\alpha$ emission lines are shown as contours. Grey contours (orange in the electronic edition) are positive velocities, and black (blue) contours are negative. Only regions showing H $\alpha$ emission have been included for clarity. In comparison, the relative velocity difference of absorption in the sub-DLA cloud is +180 km s^-1 towards the QSO sight-line.
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In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[clip]{1591_f1.eps}}\end{figure}$	Figure 1: Broad band image in the wavelength range $4500 < \lambda < 8000$ Å of the QSO at the position (0, 0) and the galaxy G4 at (-6.5, -1.5) as indicated. Each spaxel represents a spectrum and the field of view is $8\hbox {$^{\prime \prime }$ }\times 8\hbox {$^{\prime \prime }$ }$ . North is up and east is left. Coordinates are relative to the QSO position.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{1591_f2.ps}}\end{figure}$	Figure 2: Spectrum of PHL 1226 created by co-adding 20 spaxels. The flux levels are relative since the QSO is located at the edge of the field of view. Broad emission lines from H $\gamma$ and H $\beta$ at z=0.404 can be seen at 6100 Å and 6820 Å, respectively.
Open with DEXTER

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip,angle=90]{1591_f3.ps}}\end{figure}$	Figure 3: Spectrum of the galaxy created by co-addition of 112 spaxels. Any emission line present in the galaxy has been smeared out because many spaxels do not contribute to the line emission as shown in Sect. 3.1. The seemingly strong [S II] lines are partly caused by errors in sky subtraction.
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$\begin{figure} \par\resizebox{5cm}{!}{\includegraphics[clip]{1591_f5.ps}}\hspace... ...hspace*{6mm} \resizebox{5cm}{!}{\includegraphics[clip]{1591_f10.ps}}\end{figure}$	Figure 5: Emission line images of various emission lines where the continuum has been subtracted using images using adjacent wavelengths. For comparison a broad band image is included in the lower right hand panel. Smoothed contours of 2, 4, 6,... $\sigma$ levels are overlayed. The solid black line represent the 4 $\sigma$ level.
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$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[angle=90,clip]{1591_f11.ps}}\end{figure}$	Figure 6: Spectrum of the galaxy created by co-adding 15 spaxels that appeared to be associated with the bright line emission region. Emission lines listed in Table 2 are indicated.
Open with DEXTER