All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4396_f1.ps}} \end{figure}$ Figure 1: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data. Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4388 ( $v_{\rm sys}=2524$ km s^-1).
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics[clip]{H4396_f2.eps}} \end{figure}$ Figure 2: Solid lines: Effelsberg 100-m spectra of the four off-center positions. Their locations with respect to the galaxy center are marked on top of each panel. Dashed line: synthesized VLA spectra which only show H I disk emission. Dotted line: 3 $\sigma$ noise levels of the 100-m spectra. Velocities are given relative to the systemic velocity of NGC 4388.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{H4396_f3.ps}} \end{figure}$ Figure 3: Evolution of the model stellar and gas disk. The disk is seen face-on and rotates counter-clockwise. The arrow indicates the direction of ram pressure, i.e. it is opposite to the galaxy's velocity vector. The size of the arrow is proportional to $\rho v_{\rm gal}^{2}$ . The galaxy passes the cluster core at 0 Myr. The time to the core passage is marked at the top of the panels. (An animation of the temporal evolution is available at http://www.edpsciences.org).
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{H4396_f4.ps}} \end{figure}$ Figure 4: Evolution of the model stellar and gas disk. The position and inclination angle of NGC 4388 ( $\rm PA=90^{\rm o}$ , $i=85^{\rm o}$ ) are used. The arrow indicates the direction of ram pressure, i.e. it is opposite to the galaxy's velocity vector. The size of the arrow is proportional to $\rho v_{\rm gal}^{2}$ . The galaxy passes the cluster core at 0 Myr. The time to the core passage is marked at the top of the panels. (An animation of the temporal evolution is available at http://www.edpsciences.org).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4396_f5.ps}} \end{figure}$ Figure 5: ISM radial velocity as a function of the projected distance to the galaxy center.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{H4396_f6.ps}} \end{figure}$ Figure 6: Left panel: stellar distribution as contours, gas distribution as greyscales. Only gas with a local density greater than $\sim$ 30 cm^-3 is shown. For clarity the greyscales are inverted, i.e. dark regions correspond to low column density gas. Right panel: model velocity field. Dashed lines mark positive, solid lines negative velocity contours. The velocities range between -200 km s^-1 and 260 km s^-1. The contour stepsize is 20 km s^-1.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{H4396_f7.ps}} \end{figure}$ Figure 7: Left panel: model 100-m spectrum at the central (C) position. Right panel: model 100-m spectrum at the northeastern (NE) position. Velocities are given relative to the systemic velocity of NGC 4388.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4396_f1.ps}} \end{figure}$	Figure 1: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data. Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4388 ( $v_{\rm sys}=2524$ km s^-1).
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$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics[clip]{H4396_f2.eps}} \end{figure}$	Figure 2: Solid lines: Effelsberg 100-m spectra of the four off-center positions. Their locations with respect to the galaxy center are marked on top of each panel. Dashed line: synthesized VLA spectra which only show H I disk emission. Dotted line: 3 $\sigma$ noise levels of the 100-m spectra. Velocities are given relative to the systemic velocity of NGC 4388.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4396_f5.ps}} \end{figure}$	Figure 5: ISM radial velocity as a function of the projected distance to the galaxy center.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{H4396_f7.ps}} \end{figure}$	Figure 7: Left panel: model 100-m spectrum at the central (C) position. Right panel: model 100-m spectrum at the northeastern (NE) position. Velocities are given relative to the systemic velocity of NGC 4388.
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