All Figures

$\begin{figure} \par {\includegraphics[width=7.7cm,clip]{4954_f1.ps} } \end{figure}$ Figure 1: Inclination angle between the galactic disk and the ICM wind $i=45^{\circ }$ , $i=60^{\circ }$ , and $i=75^{\circ }$ . Left panels: components of the 3D ICM wind direction as a function of the azimuthal viewing angle $\alpha$ . Right panels: projected wind direction with respect to the galaxy's minor axis (counted counter-clockwise) as a function of $\alpha$ . The arrows indicate the best fit model $\alpha =350^{\circ }$ and the azimuthal viewing angle for a projected wind angle of $-15^{\circ }$ .
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In the text

$\begin{figure} \par {\includegraphics[width=15.3cm,clip]{4954_f2.ps} } \end{figure}$ Figure 2: Model snapshots for different simulations. The ram pressure profile for all simulations is given by Eq. (3). The inclination angle i between the orbital and the galaxy's disk plane and the timestep of the snapshot are varied. Left column: t=0 Myr. Middle column: t=50 Myr. Right column: t=100 Myr. Upper row: $i=45^{\circ }$ . Middle row: $i=60^{\circ }$ . Lower row: $i=75^{\circ }$ .
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In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{4954_f3.ps} } \end{figure}$ Figure 3: Snapshot at t=40 Myr of the simulation with $i=60^{\circ }$ . The azimuthal viewing angle is $\alpha =30^{\circ }$ . Left panel: gas distribution. Right panel: velocity field.
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In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{4954_f4.ps} } \end{figure}$ Figure 4: Snapshots of the simulation using a step function for the temporal ram pressure profile with $i=60^{\circ }$ . The azimuthal viewing angle is $\alpha =350^{\circ }$ .
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In the text

$\begin{figure} \par {\includegraphics[width=4.3cm,clip]{4954_f5.ps} } \end{figure}$ Figure 5: Evolution of the model stellar (1st column) and gas disk (2nd column). The major axis position angle and inclination of NGC 4522 are $\rm PA=214^{\circ }$ and $i=80^{\circ }$ , respectively. The arrow indicates the direction of ram pressure, i.e. it is opposite to the galaxy's velocity vector, and its size is proportional to $\rho v_{\rm gal}^{2}$ . Maximum ram pressure occurs at t=0 Myr. The timestep of each snapshot is marked in each panel showing the stellar disk.
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In the text

$\begin{figure} \par {\includegraphics[width=15.2cm,clip]{4954_f6.ps} } \end{figure}$ Figure 6: Comparison snapshot of the gas distribution of NGC 4522. Left panel: view of the disk using the observed position angle and inclination of NGC 4522. Right panel: the disk seen face-on. The arrow indicates the direction of the wind, i.e. opposite to the galaxy's motion.
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In the text

$\begin{figure} \par {\includegraphics[width=7.4cm,clip]{4954_f7.ps} } \end{figure}$ Figure 7: Stellar (contours) and gas (greyscale) distribution of NGC 4522. Left panel: model. Right panel: H I observations (Kenney et al. 2004).
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In the text

$\begin{figure} \par {\includegraphics[width=13.1cm,clip]{4954_f8.ps} } \end{figure}$ Figure 8: Moment maps of NGC 4522. Left panels: model. Right panels: H I observations (Kenney et al. 2004). The same contouring scheme is used for both model and data. Upper panels: gas distribution; contours spaced by $\sqrt {2}$ . Middle panel: velocity field; contours spaced 10 km s^-1. Lower panel: velocity dispersion; contours: 15, 20, 25, 30, 35, 40, 45 km s^-1.
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In the text

$\begin{figure} \par {\includegraphics[width=15cm,clip]{4954_f9.ps} } \end{figure}$ Figure 9: Major axis position-velocity diagram for the disk (greyscale) and extraplanar (contours) component. Left panel: model. Right panel: H I observations (Kenney et al. 2004). Contour levels are 1, 2, 3, 4, 5, 6 times the peak value.
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In the text

$\begin{figure} \par {\includegraphics[width=9.8cm,clip]{4954_f10.ps} } \end{figure}$ Figure 10: Evolution of the polarized radio continuum emission. Time steps are the same as in Fig. 5. The disk is seen face-on and rotates clockwise. Contours: polarized radio continuum emission. The magnetic field vectors are superimposed onto the gas surface density. The timestep is indicated on top of each snapshot. The assumed beamsize for the polarized radio continuum emission is 20''. The arrow in the last panel indicates the direction of the ram pressure wind.
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In the text

$\begin{figure} \par {\includegraphics[width=15.2cm,clip]{4954_f11.ps} } \par\end{figure}$ Figure 11: Greyscale: H I gas distribution with a resolution of $\sim$ 20''. Contours: polarized radio continuum emission. Left panel: model. The FWHM of the relativistic electron distribution in the radial and vertical directions are 8.3 kpc and 1.2 kpc, respectively. Right panel: observations (Vollmer et al. 2004).
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In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{4954_f3.ps} } \end{figure}$	Figure 3: Snapshot at t=40 Myr of the simulation with $i=60^{\circ }$ . The azimuthal viewing angle is $\alpha =30^{\circ }$ . Left panel: gas distribution. Right panel: velocity field.
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$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{4954_f4.ps} } \end{figure}$	Figure 4: Snapshots of the simulation using a step function for the temporal ram pressure profile with $i=60^{\circ }$ . The azimuthal viewing angle is $\alpha =350^{\circ }$ .
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$\begin{figure} \par {\includegraphics[width=15.2cm,clip]{4954_f6.ps} } \end{figure}$	Figure 6: Comparison snapshot of the gas distribution of NGC 4522. Left panel: view of the disk using the observed position angle and inclination of NGC 4522. Right panel: the disk seen face-on. The arrow indicates the direction of the wind, i.e. opposite to the galaxy's motion.
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$\begin{figure} \par {\includegraphics[width=7.4cm,clip]{4954_f7.ps} } \end{figure}$	Figure 7: Stellar (contours) and gas (greyscale) distribution of NGC 4522. Left panel: model. Right panel: H I observations (Kenney et al. 2004).
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$\begin{figure} \par {\includegraphics[width=13.1cm,clip]{4954_f8.ps} } \end{figure}$	Figure 8: Moment maps of NGC 4522. Left panels: model. Right panels: H I observations (Kenney et al. 2004). The same contouring scheme is used for both model and data. Upper panels: gas distribution; contours spaced by $\sqrt {2}$ . Middle panel: velocity field; contours spaced 10 km s^-1. Lower panel: velocity dispersion; contours: 15, 20, 25, 30, 35, 40, 45 km s^-1.
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$\begin{figure} \par {\includegraphics[width=15cm,clip]{4954_f9.ps} } \end{figure}$	Figure 9: Major axis position-velocity diagram for the disk (greyscale) and extraplanar (contours) component. Left panel: model. Right panel: H I observations (Kenney et al. 2004). Contour levels are 1, 2, 3, 4, 5, 6 times the peak value.
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$\begin{figure} \par {\includegraphics[width=15.2cm,clip]{4954_f11.ps} } \par\end{figure}$	Figure 11: Greyscale: H I gas distribution with a resolution of $\sim$ 20''. Contours: polarized radio continuum emission. Left panel: model. The FWHM of the relativistic electron distribution in the radial and vertical directions are 8.3 kpc and 1.2 kpc, respectively. Right panel: observations (Vollmer et al. 2004).
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