Astronomy & Astrophysics

All Figures

$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{h4735f1.eps}} \end{figure}$ Figure 1: Sketch of the parameters used for characterizing the dimensions of the 3C 48 host. The lengths (L1, L2) are measured along the longest extension of the host body (PA $\approx 4\hbox {$^\circ $ }$ for the observations, PA $\approx 19\hbox {$^\circ $ }$ for the simulations), the widths (W1, W2) are measured perpendicular to this. The curvature of the tail is traced along maximum intensity (right panel) by angle-distance-vectors $(\alpha _i,d_i)$ .
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In the text

$\begin{figure}\resizebox{17cm}{!}{\includegraphics{h4735f2.eps}} \end{figure}$ Figure 2: Two different projections of the same simulation snapshot after 461.1 Myr. The left panel shows the projection for which the merger remnant looks like the "Antennae'', the right panel shows the projection for which the remnant looks like the 3C 48 host. The coordinate planes indicate the respective tilt of the orbital plane (x-y). See text for a detailed description.
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In the text

$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{h4735f3.eps}} \end{figure}$ Figure 3: Contour plot of the surface brightness of the 3C 48 look-alike. Length units are fixed in arcsec by positioning the four slits A, B, C, G used by Canalizo & Stockton (2000). The small inset shows a magnified view on the still separated density peaks of the merging bulges.
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In the text

$\begin{figure}\resizebox{18cm}{!}{\includegraphics{h4735f4.eps}} \end{figure}$ Figure 4: Comparison of the observed and simulated line-of-sight velocities $v_{\rm LOS}$ along the four slits A, B, C, G. Offsets are measured in the direction indicated by the arrows in Fig. 3. Dots represent the average velocities of the 3C 48 look-alike. The area enclosed by $v_{\rm LOS}+\Delta v_{\rm LOS}$ and $v_{\rm LOS}-\Delta v_{\rm LOS}$ (dashed histograms) corresponds to the confidence region of the stellar line-of-sight velocities measured for the 3C 48 host. These data are taken from Fig. 1 and Table 2 in Canalizo & Stockton (2000).
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In the text

$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{h4735f5.eps}} \end{figure}$ Figure 5: Comparison of the curvature of the northwestern tidal tail of the 3C 48 host (solid line) and its look-alike (dashed line).
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In the text

$\begin{figure}\resizebox{17cm}{!}{\includegraphics{h4735f2.eps}} \end{figure}$	Figure 2: Two different projections of the same simulation snapshot after 461.1 Myr. The left panel shows the projection for which the merger remnant looks like the "Antennae'', the right panel shows the projection for which the remnant looks like the 3C 48 host. The coordinate planes indicate the respective tilt of the orbital plane (x-y). See text for a detailed description.
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$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{h4735f3.eps}} \end{figure}$	Figure 3: Contour plot of the surface brightness of the 3C 48 look-alike. Length units are fixed in arcsec by positioning the four slits A, B, C, G used by Canalizo & Stockton (2000). The small inset shows a magnified view on the still separated density peaks of the merging bulges.
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$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{h4735f5.eps}} \end{figure}$	Figure 5: Comparison of the curvature of the northwestern tidal tail of the 3C 48 host (solid line) and its look-alike (dashed line).
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