All Figures

$\begin{figure} \par\includegraphics[width=3.8cm,height=10.7cm,clip]{1147fg01.eps... ...clip]{1147fg02.eps}\includegraphics[width=5.5cm,clip]{1147fg03.eps} \end{figure}$ Figure 1: Left and Middle: HST and ESO H $\alpha$ +[N II] images. The white bar in the ESO image corresponds to the gap between the 2 CCD of the mosaic camera SUSI2. Right: sketch of Mz 3, showing the various nebular components discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1147fg04.eps} \end{figure}$ Figure 2: Echelle long-slit location display over Mz 3. CTIO slit positions are indicated by black lines, whereas white ones indicate ESO slit positions.
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In the text

$\begin{figure} \par\includegraphics[width=2.6cm,height=10cm,clip]{1147fg05.eps}\includegraphics[width=4cm,height=10cm,clip]{1147fg06.eps} \end{figure}$ Figure 3: The [N II] ESO spectrum along the nebular symmetry axis ( $\rm PA=5^\circ$ ), shown with two different contrasts. The association of velocity features with the different nebular components is indicated. Each frame is 100'' along y axis. Left and right frame are 275 and 430 km s^-1, respectively, along xaxis (both frames have the same scale). Northern side is at the top.
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In the text

$\begin{figure} \par\includegraphics[width=2.8cm,height=6.5cm,clip]{1147fg07.eps}\includegraphics[width=2.8cm,height=6.5cm,clip]{1147fg08.eps} \end{figure}$ Figure 4: Left: the H $\alpha$ +[N II] HST image of the lobes of Mz 3. Right: adopted model.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1147fg09.eps}\par\includegraphics[width=8.8cm,clip]{1147fg10.eps} \end{figure}$ Figure 5: Top: the ESO [N II] echelle spectra. Frames correspond, from left to right, to PA from $-40^\circ$ to $+65^\circ$ in increments of $15^\circ$ and no offset. Bottom: the same spectra with the spatio-kinematical model of the lobes superimposed. Model lines have been artificially broadened to facilitate the display and to improve the S/N ratio. The main velocity deviations from this Hubble-like flow model are indicated by arrows. Note: each frame is 50'' tall and 200 km s^-1 wide. Northern side is up.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1147fg11.eps} \end{figure}$ Figure 6: Mz 3 STIS central region data fitted to gaussians ( $\Box$ ) and lobes model ( $\times$ ).
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{1147fg12.eps}\hspace*{5mm} \includegraphics[width=2.3cm,clip]{1147fg13.eps} \end{figure}$ Figure 7: Left: the H $\alpha$ +[N II] ESO image of Mz 3. Right: the best-fitting model for the columns.
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{1147fg14.eps}\par\includegraphics[width=10.2cm,clip]{1147fg15.eps} \end{figure}$ Figure 8: Top: the CTIO [N II] echelle spectra. Frames correspond to $\rm PA=0^\circ$ and offsets from -8'' (E) to +8'' (W) from left to right, in increments of 2''. Bottom: the same spectra with the spatio-kinematical model of the columns superimposed. Model lines have been artificially broadened with displaying purposes. Note: each frame is 120'' tall and 275 km s^-1 wide. Northern side is up.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1147fg16.eps}\hspace*{4mm} \includegraphics[width=8cm,clip]{1147fg17.eps} \end{figure}$ Figure 9: Left: the H $\alpha$ +[N II] ESO image of Mz 3. Right: the best-fitting model for the rays.
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{1147fg18.eps}\par\includegraphics[width=10.2cm,clip]{1147fg19.eps} \end{figure}$ Figure 10: Top: the CTIO [N II] echelle spectra. Frames correspond to $\rm PA=0^\circ$ and offsets from -8'' (E) to +8'' (W) from left to right, in increments of 2''. Bottom: the model of the rays superimposed to the CTIO spectra. As in previous cases, model lines have been broadened to improve the S/N ratio and get better displaying results. Note: Each frame is 100'' tall and 480 km s^-1 wide. Northern side is up.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1147fg20.eps}\includegraphics[width=8cm,clip]{1147fg21.eps} \end{figure}$ Figure 11: Left: the H $\alpha$ +[N II] ESO image of Mz 3. Right: the adopted model for the chakram.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1147fg22.eps}\par\includegraphics[width=8.8cm,clip]{1147fg23.eps} \end{figure}$ Figure 12: Top: the ESO [N II] echelle spectra. Frames correspond, from left to right, to PA from $-40^\circ$ to $+65^\circ$ in increments of $15^\circ$ and no offset. Bottom: the same spectra with the model of the chakram overlaid. Model lines have been exaggerately broadened so the reader can see both the model and the spectra. Note: each frame is 80'' tall and 480 km s^-1 wide. Northern side is up.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1147fg24.eps} %\end{figure}$ Figure 13: The velocity law of gas in the chackram, extracted and interpolated from ESO spectra.
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{1147fg25.eps}\includegraphics[width=8.2cm,clip]{1147fg26.eps} \end{figure}$ Figure 14: Left: Mz 3 model projected on the plane of the sky. Right: transversal view of Mz 3 model, i.e. after a $90^\circ$ rotation around z axis.
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In the text

$\begin{figure} \par\includegraphics[width=3.8cm,height=10.7cm,clip]{1147fg01.eps... ...clip]{1147fg02.eps}\includegraphics[width=5.5cm,clip]{1147fg03.eps} \end{figure}$	Figure 1: Left and Middle: HST and ESO H $\alpha$ +[N II] images. The white bar in the ESO image corresponds to the gap between the 2 CCD of the mosaic camera SUSI2. Right: sketch of Mz 3, showing the various nebular components discussed in the text.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1147fg04.eps} \end{figure}$	Figure 2: Echelle long-slit location display over Mz 3. CTIO slit positions are indicated by black lines, whereas white ones indicate ESO slit positions.
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$\begin{figure} \par\includegraphics[width=2.6cm,height=10cm,clip]{1147fg05.eps}\includegraphics[width=4cm,height=10cm,clip]{1147fg06.eps} \end{figure}$	Figure 3: The [N II] ESO spectrum along the nebular symmetry axis ( $\rm PA=5^\circ$ ), shown with two different contrasts. The association of velocity features with the different nebular components is indicated. Each frame is 100'' along y axis. Left and right frame are 275 and 430 km s^-1, respectively, along xaxis (both frames have the same scale). Northern side is at the top.
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$\begin{figure} \par\includegraphics[width=2.8cm,height=6.5cm,clip]{1147fg07.eps}\includegraphics[width=2.8cm,height=6.5cm,clip]{1147fg08.eps} \end{figure}$	Figure 4: Left: the H $\alpha$ +[N II] HST image of the lobes of Mz 3. Right: adopted model.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{1147fg11.eps} \end{figure}$	Figure 6: Mz 3 STIS central region data fitted to gaussians ( $\Box$ ) and lobes model ( $\times$ ).
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$\begin{figure} \par\includegraphics[width=4cm,clip]{1147fg12.eps}\hspace*{5mm} \includegraphics[width=2.3cm,clip]{1147fg13.eps} \end{figure}$	Figure 7: Left: the H $\alpha$ +[N II] ESO image of Mz 3. Right: the best-fitting model for the columns.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1147fg16.eps}\hspace*{4mm} \includegraphics[width=8cm,clip]{1147fg17.eps} \end{figure}$	Figure 9: Left: the H $\alpha$ +[N II] ESO image of Mz 3. Right: the best-fitting model for the rays.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1147fg20.eps}\includegraphics[width=8cm,clip]{1147fg21.eps} \end{figure}$	Figure 11: Left: the H $\alpha$ +[N II] ESO image of Mz 3. Right: the adopted model for the chakram.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1147fg24.eps} %\end{figure}$	Figure 13: The velocity law of gas in the chackram, extracted and interpolated from ESO spectra.
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$\begin{figure} \par\includegraphics[width=6.1cm,clip]{1147fg25.eps}\includegraphics[width=8.2cm,clip]{1147fg26.eps} \end{figure}$	Figure 14: Left: Mz 3 model projected on the plane of the sky. Right: transversal view of Mz 3 model, i.e. after a $90^\circ$ rotation around z axis.
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