All Figures

$\begin{figure} \par\includegraphics[height=6.4cm,width=8.5cm,clip]{0481fg01.eps}\end{figure}$ Figure 1: Part of the FORS1 field of view around HE 1434-1600. Five galaxies with measured redshifts are indicated by horizontal arrows. They all have redshifts very similar to that of the quasar, $z\sim 0.144$ (see Sect. 5). North is up and East is left, as all other figures in this paper.
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In the text

$\begin{figure} \par\includegraphics[width=4.25cm,clip]{0481fg02.ps}\includegraph... ...cm}\includegraphics[width=4.25cm,clip]{0481fg04.ps}\hspace*{2.2cm}} \end{figure}$ Figure 2: Deconvolved images of the host galaxy alone, with the quasar removed. The position of the quasar is indicated by the cross. The intensity scale is different in each image, as well as the angular resolutions. While the J-band image appears smooth, both R images show structure about 2 $^{\prime \prime }$ away from the center of the host galaxy.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.25cm,clip]{0481fg05.ps}\end{figure}$ Figure 3: NVSS image centered on the position of HE 1434-1600. The field of view is 30 $^\prime$ $\times$ 30 $^\prime$ , and the beam size in this 1.4 GHz map is 45 $^{\prime \prime }$ . The central "hot spot'' corresponds to HE 1434-1600. Two lobes also extend over 5-6 $^\prime$ to the north and south of the quasar.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0481fg06.ps}\end{figure}$ Figure 4: Slit orientations represented in overlay on the deconvolved R-band image of the host, after removal of the quasar. The companion galaxy G1 is also visible on this image. Slit 1 corresponds to the data taken in April 2000, and slit 2 corresponds to the May 2002 data. In each case the slit width is 1 $^{\prime \prime }$ . A, B and C are the three regions we used to extract the spectra (see Sect. 3). The total size of this image is about the size of the central hot-spot in the radio map of Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=3.8cm,clip]{0481fg07.ps}\hspace*{2mm} \includegraphics[width=3.85cm,clip]{0481fg08.ps}\end{figure}$ Figure 5: Extracted intensity profiles along slit1 and slit 2 of the host galaxy, as defined in Fig. 4. Each profile is obtained by spatially integrating the deconvolved R-band image across the 2 slits, after removal of the quasar. Obvious structures with a typical size of 1 kpc do appear 2 $^{\prime \prime }$ away from the quasar.
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In the text

$\begin{figure} \par\includegraphics[height=9.9cm,width=13.7cm,clip]{0481fg09.ps}\end{figure}$ Figure 6: 1D spectra of the quasar and the host galaxy after deconvolution. The spectrum of the host is integrated over 6 $^{\prime \prime }$ . All spectra are displayed in the rest frame, for the two slit orientations. The quasar spectra are shown in the two upper panels, while the spectra of the host galaxy alone, are shown in the two lower ones. Note the different flux scales.
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In the text

$\begin{figure} \includegraphics[height=9.8cm,width=13.6cm,clip]{0481fg10.ps}\end{figure}$ Figure 7: Deconvolved spectra of host galaxy, for the three regions A, B, C, defined in Fig. 4. The size of the central aperture (B) is 2 $^{\prime \prime }$ , while apertures A and C, that correspond to the external parts of the galaxy, are 4 $^{\prime \prime }$ wide.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0481fg11.ps}\end{figure}$ Figure 8: Diagnostic diagram from Veilleux & Osterbrock 1987, where the measurements for different regions of the host of HE 1434-1600 have been overplotted. Four points are available, for apertures A, B, C of slit 1 and for slit 2. They are represented as crosses with associated 1 $\sigma$ error box. Open symbols, following Veilleux & Osterbrock (1987), represent typical H II regions. Black symbols are active galaxies. All measurements of Veilleux & Osterbrock include the nucleus and the host of the objects.
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In the text

$\begin{figure} \par\includegraphics[height=4.8cm,width=8.2cm,clip]{0481fg12.ps}\end{figure}$ Figure 9: Integrated spectrum of companion galaxy G1 (see Fig. 4). One strong absorption feature is detected: the sodium Na I (5896 Å) line. All other absorptions are tellurics (labeled "A'' on the figure). The emission lines visible here are extended emissions of the host of HE 1434-1600, that are contaminating the spectrum of G1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0481fg13.ps}\end{figure}$ Figure 10: Flux calibrated spectra of 4 neighbours of HE 1434-1600. All show clear H ${\alpha }$ and [N II] emissions. G2 and G3 show the [O III] and H ${\beta }$ emission lines as well.
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In the text

$\begin{figure} \par\includegraphics[height=4.8cm,width=7.8cm,clip]{0481fg14.ps}\end{figure}$ Figure 11: Correlation function of the two extracted regions of the host's spectrum (see text) along slit 1. Only the spectral regions with no emission lines are considered, i.e., from 5246 Å to 5706 Å, in the rest frame. The centroid of the correlation peak is located at 0.03 $\pm$ 0.1 pixels, which translates into v=2 $\pm$ $10~{\rm km~s}^{-1}$ , hence confirming that the stars in the host are not affected by any circular motion.
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In the text

$\begin{figure} \par\includegraphics[width=4.05cm,clip]{0481fg15.ps}\hspace*{2mm} \includegraphics[width=4.05cm,clip]{0481fg16.ps}\end{figure}$ Figure 12: Spatial profile of the [O III] emission line for slit 1 and slit 2 prior to any host/nucleus decomposition. The dip in intensity profile through slit 1, 3 $^{\prime \prime }$ away from the quasar, and the two "hot spots'' of Fig. 13 are already visible in this raw undeconvolved intensity profile.
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In the text

$\begin{figure} \par\includegraphics[width=5.45cm,clip]{0481fg17.ps}\includegraph... ...21.ps}\hspace*{3mm} \includegraphics[width=5.45cm,clip]{0481fg22.ps}\end{figure}$ Figure 13: Top: zoom on the [O III] (5007 Å) emission line in slit 1 ( left), in slit 2 ( middle). The H ${\alpha }$ emission lines is displayed on the right panel. The spatial direction is horizontal and the wavelength direction vertical. Both the quasar spectrum and the continuum of the host galaxy have been subtracted. The sharp structures in the very center (central kpc) of the galaxy corresponds to oversubtraction of the quasar. The gas motion is striking in slit 1, while the stars are not showing any motion in this same slit position. No gas velocity field is detected for slit 2. Bottom: Corresponding intensity profiles.
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In the text

$\begin{figure} \includegraphics[width=8cm,clip]{0481fg23.ps}\hspace*{6mm} \includegraphics[width=8cm,clip]{0481fg24.ps}\end{figure}$ Figure 14: Left: velocity curves obtained for the [O III] doublet and for the H ${\alpha }$ emission line. Right: mean velocity curve. The data points are the mean of the two [O III] measurement and of the H ${\alpha }$ measurement. The error bars correspond to the dispersion between the three curves of the left panel. Our best fit model is overplotted. With a central mass fixed to 3.6 $\times$ $10^{8}~M_{\odot}$ , the $\chi ^2$ of the fit is acceptable only for model with mass components unrealistically concentrated near the nucleus (see text).
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In the text

$\begin{figure} \par\includegraphics[height=6.4cm,width=8.5cm,clip]{0481fg01.eps}\end{figure}$	Figure 1: Part of the FORS1 field of view around HE 1434-1600. Five galaxies with measured redshifts are indicated by horizontal arrows. They all have redshifts very similar to that of the quasar, $z\sim 0.144$ (see Sect. 5). North is up and East is left, as all other figures in this paper.
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$\begin{figure} \par\includegraphics[width=4.25cm,clip]{0481fg02.ps}\includegraph... ...cm}\includegraphics[width=4.25cm,clip]{0481fg04.ps}\hspace*{2.2cm}} \end{figure}$	Figure 2: Deconvolved images of the host galaxy alone, with the quasar removed. The position of the quasar is indicated by the cross. The intensity scale is different in each image, as well as the angular resolutions. While the J-band image appears smooth, both R images show structure about 2 $^{\prime \prime }$ away from the center of the host galaxy.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.25cm,clip]{0481fg05.ps}\end{figure}$	Figure 3: NVSS image centered on the position of HE 1434-1600. The field of view is 30 $^\prime$ $\times$ 30 $^\prime$ , and the beam size in this 1.4 GHz map is 45 $^{\prime \prime }$ . The central "hot spot'' corresponds to HE 1434-1600. Two lobes also extend over 5-6 $^\prime$ to the north and south of the quasar.
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$\begin{figure} \par\includegraphics[width=3.8cm,clip]{0481fg07.ps}\hspace*{2mm} \includegraphics[width=3.85cm,clip]{0481fg08.ps}\end{figure}$	Figure 5: Extracted intensity profiles along slit1 and slit 2 of the host galaxy, as defined in Fig. 4. Each profile is obtained by spatially integrating the deconvolved R-band image across the 2 slits, after removal of the quasar. Obvious structures with a typical size of 1 kpc do appear 2 $^{\prime \prime }$ away from the quasar.
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$\begin{figure} \par\includegraphics[height=9.9cm,width=13.7cm,clip]{0481fg09.ps}\end{figure}$	Figure 6: 1D spectra of the quasar and the host galaxy after deconvolution. The spectrum of the host is integrated over 6 $^{\prime \prime }$ . All spectra are displayed in the rest frame, for the two slit orientations. The quasar spectra are shown in the two upper panels, while the spectra of the host galaxy alone, are shown in the two lower ones. Note the different flux scales.
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$\begin{figure} \includegraphics[height=9.8cm,width=13.6cm,clip]{0481fg10.ps}\end{figure}$	Figure 7: Deconvolved spectra of host galaxy, for the three regions A, B, C, defined in Fig. 4. The size of the central aperture (B) is 2 $^{\prime \prime }$ , while apertures A and C, that correspond to the external parts of the galaxy, are 4 $^{\prime \prime }$ wide.
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$\begin{figure} \par\includegraphics[height=4.8cm,width=8.2cm,clip]{0481fg12.ps}\end{figure}$	Figure 9: Integrated spectrum of companion galaxy G1 (see Fig. 4). One strong absorption feature is detected: the sodium Na I (5896 Å) line. All other absorptions are tellurics (labeled "A'' on the figure). The emission lines visible here are extended emissions of the host of HE 1434-1600, that are contaminating the spectrum of G1.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0481fg13.ps}\end{figure}$	Figure 10: Flux calibrated spectra of 4 neighbours of HE 1434-1600. All show clear H ${\alpha }$ and [N II] emissions. G2 and G3 show the [O III] and H ${\beta }$ emission lines as well.
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$\begin{figure} \par\includegraphics[width=4.05cm,clip]{0481fg15.ps}\hspace*{2mm} \includegraphics[width=4.05cm,clip]{0481fg16.ps}\end{figure}$	Figure 12: Spatial profile of the [O III] emission line for slit 1 and slit 2 prior to any host/nucleus decomposition. The dip in intensity profile through slit 1, 3 $^{\prime \prime }$ away from the quasar, and the two "hot spots'' of Fig. 13 are already visible in this raw undeconvolved intensity profile.
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