All Figures

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f1a.eps}\includegraphi... ...cm,clip]{1410f1e.eps}\includegraphics[width=5.5cm,clip]{1410f1f.eps}\end{figure}$ Figure 1: Evolution of the gas distribution for the full N-body simulations of run A. The system is seen face-on. The gas is displayed with a logarithm intensity scale.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1410f2.eps}\end{figure}$ Figure 2: Bottom: contours of the gaseous component superimposed on a grayscale representation of the stellar component at t= 470 Myr (simulation A). Top: zoom-out with the contours of the dark matter haloes superimposed. The system is seen edge-on.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{1410f3.eps}\end{figure}$ Figure 3: Contours of the gaseous component superimposed on a grayscale representation of the stellar component at t= 850 Myr (run A). The system is seen face-on.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f4a.eps}\includegraphi... ...cm,clip]{1410f4b.eps}\includegraphics[width=5.5cm,clip]{1410f4c.eps}\end{figure}$ Figure 4: Results of the full N-body simulations of runs B ( left), C ( middle) and D ( right) 50 to 100 Myrs after the periapse (see Table 2). Gas contours are superimposed on the stellar component. All systems are seen face-on.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f5a.eps}\includegraphi... ...cm,clip]{1410f5e.eps}\includegraphics[width=5.5cm,clip]{1410f5f.eps}\end{figure}$ Figure 5: Formation of the TDG progenitors in the simulations carried out with the restricted N-body + rigid haloes code. The evolution of the gas distribution in one of the merging galaxies is presented. The position of the the second galaxy is shown by a star at t= 450 Myr. At earlier times, it is outside the field of view. Self-gravity and energy dissipation in the ISM are included in these simulations. The parameters of the simulation were: mass ratio 1:1, 8% of gas, impact parameter 150 kpc, initial relative velocity 125 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f6a.eps}\includegraphi... ...cm,clip]{1410f6b.eps}\includegraphics[width=5.5cm,clip]{1410f6c.eps}\end{figure}$ Figure 6: Left: TDG gaseous progenitors at t= 345 Myr for the collision shown in Fig. 5. Middle: same simulation suppressing the self-gravity in the gaseous component; right: same simulation suppressing self-gravity and energy dissipation.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{1410f7.eps}\end{figure}$ Figure 7: Response of an annulus of uniformly distributed, kinematically cold, gas clouds to a tidal perturbation.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1410f8.eps}\end{figure}$ Figure 8: Response of an annulus of uniformly distributed gas clouds to a tidal perturbation with DM haloes as extended as ten stellar radii (green solid line) and with DM haloes truncated at three stellar radii (red dashed line). The x-axis corresponds to the azimuth after correction of the differential rotation, so that the tidal tail has a fixed azimuth equal to zero. The radii R have been scaled to the maximum extent of the tidal tail, $R{\rm max}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1410f9.eps}\end{figure}$ Figure 9: Schematic view of the effects of tidal perturbations to a series of concentric annuli of radius R for extended ( left) and truncated ( right) dark matter haloes. The annuli were initially regularly spaced out.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1410f10.eps}\end{figure}$ Figure 10: Amplitude of the radial excursions as a function of the initial radius with DM haloes as extended as ten stellar radii (green solid line) and with DM haloes truncated at three stellar radii (red dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1410f11.eps}\end{figure}$ Figure 11: Plots in the left column correspond to the decay of an extended halo potential ( $f(r)\propto r^{-2}$ ) while those of the right column correspond to a Keplerian decay ( $f(r)\propto r^{-3}$ ) of the tidal field. Similarly, the runs of the top row correspond to a local shape of the tidal field that is Keplerian ( $\lambda _1=-2\lambda _2$ ), while the runs of the bottom row correspond to a local shape of the tidal field corresponding to an isothermal sphere potential ( $\lambda _1=-\lambda _2$ ). By comparing these four plots, one can conclude that it is the relative value of $\lambda _1$ and $\lambda _2$ that primarily determines the arms morphology, i.e. the local shape of the tidal field. The grey levels correspond to the same values on the four plots, and scale with the square root of the surface density. Notice in particular the presence of a diffuse scattered population of test particles in the cases where the tidal potential has a Keplerian shape (top row). The symbols in each panel represent the shape of the tidal field as in Dekel et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f1a.eps}\includegraphi... ...cm,clip]{1410f1e.eps}\includegraphics[width=5.5cm,clip]{1410f1f.eps}\end{figure}$	Figure 1: Evolution of the gas distribution for the full N-body simulations of run A. The system is seen face-on. The gas is displayed with a logarithm intensity scale.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1410f2.eps}\end{figure}$	Figure 2: Bottom: contours of the gaseous component superimposed on a grayscale representation of the stellar component at t= 470 Myr (simulation A). Top: zoom-out with the contours of the dark matter haloes superimposed. The system is seen edge-on.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{1410f3.eps}\end{figure}$	Figure 3: Contours of the gaseous component superimposed on a grayscale representation of the stellar component at t= 850 Myr (run A). The system is seen face-on.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f4a.eps}\includegraphi... ...cm,clip]{1410f4b.eps}\includegraphics[width=5.5cm,clip]{1410f4c.eps}\end{figure}$	Figure 4: Results of the full N-body simulations of runs B ( left), C ( middle) and D ( right) 50 to 100 Myrs after the periapse (see Table 2). Gas contours are superimposed on the stellar component. All systems are seen face-on.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{1410f6a.eps}\includegraphi... ...cm,clip]{1410f6b.eps}\includegraphics[width=5.5cm,clip]{1410f6c.eps}\end{figure}$	Figure 6: Left: TDG gaseous progenitors at t= 345 Myr for the collision shown in Fig. 5. Middle: same simulation suppressing the self-gravity in the gaseous component; right: same simulation suppressing self-gravity and energy dissipation.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{1410f7.eps}\end{figure}$	Figure 7: Response of an annulus of uniformly distributed, kinematically cold, gas clouds to a tidal perturbation.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1410f9.eps}\end{figure}$	Figure 9: Schematic view of the effects of tidal perturbations to a series of concentric annuli of radius R for extended ( left) and truncated ( right) dark matter haloes. The annuli were initially regularly spaced out.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1410f10.eps}\end{figure}$	Figure 10: Amplitude of the radial excursions as a function of the initial radius with DM haloes as extended as ten stellar radii (green solid line) and with DM haloes truncated at three stellar radii (red dashed line).
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