Astronomy & Astrophysics

All Figures

$\begin{figure} \par {\includegraphics[width=14cm,clip]{0552fig1.ps} } \end{figure}$ Figure 1: VLA H I channel maps of NGC 4569. The central velocity of each channel is indicated in the upper part of each panel. The HPBW ( $31''\times 39''$ ) is plotted in the lower left corner of the first channel. The contours are in steps of $3\sigma =1.5$ mJy/beam beginning at 1.5 mJy/beam.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{0552fig2.ps} } \end{figure}$ Figure 2: Solid line: Effelsberg spectrum of the central position. Dashed line: integrated VLA spectrum. Dotted line: 3 $\sigma$ noise level of the Effelsberg spectrum. The radial velocities are relative to the systemic velocity of NGC 4569.
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In the text

$\begin{figure} \par {\includegraphics[width=6.6cm,clip]{0552fig3.ps} } \end{figure}$ Figure 3: H I moment maps of NGC 4569. Upper panel: column density. The contour steps are from 1 to $9 \times 1.3\times 10^{20}$ cm^-2. Middle panel: velocity field. Contour levels are from -440 to -40 km s^-1 in steps of 20 km s^-1. Lower panel: velocity dispersion. Contour levels are from 1 to $9 \times 8.3$ km s^-1.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{0552fig4.ps} } \end{figure}$ Figure 4: Contours: H I column density. The contour levels are the same as in Fig. 3. Greyscale: B band DSS image. The contrast is chosen such that the whole disk extent becomes visible.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0552fig5.ps} } \end{figure}$ Figure 5: Solid lines: Effelsberg 100-m spectra of the five 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 Effelsberg spectra. Radial velocities are given relative to the systemic velocity of NGC 4569.
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In the text

$\begin{figure} \par {\includegraphics[width=17cm,clip]{0552fig6.ps} } \end{figure}$ Figure 6: Evolution of the model stellar (1st and 3rd column) and gas disk (2nd and 4th column). The major axis position angle and inclination of NGC 4569 are ${\rm PA}=23^{\circ }$ and $i=62^{\circ }$ , 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 $\rho v_{\rm gal}^{2}$ . The galaxy passes the cluster core at 0 Myr. The time to the core passage is marked at the top of each panel.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{0552fig7.ps} } \end{figure}$ Figure 7: Comparison snapshot of the gas distribution of NGC 4569 for the case of ongoing ram pressure stripping. Left panel: the disk seen face-on. Right panel: view of the disk using the observed position angle and inclination of NGC 4569. The arrow indicates the direction of the wind, i.e. opposite to the galaxy's motion.
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In the text

$\begin{figure} \par {\includegraphics[width=6.8cm,clip]{0552fig8.ps} } \end{figure}$ Figure 8: Initial gas velocity field. The disk is truncated at a radius of 5 kpc.
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In the text

$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{0552fig9.ps} } \end{figure}$ Figure 9: Model H I spectrum for ongoing ram pressure stripping.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0552fig10.ps} } \end{figure}$ Figure 10: Model spectra corresponding to our offset H I observations (Fig. 5) for ongoing stripping.
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In the text

$\begin{figure} \par {\includegraphics[width=6.5cm,clip]{0552fig11.ps} } \end{figure}$ Figure 11: Model moment maps for ongoing ram pressure stripping. Upper panel: gas distribution in arbitrary units. The relative contours are the same as in Fig. 3. Middle panel: velocity field. The contours are the same as in Fig. 3. Lower panel: velocity dispersion. The contours are the same as in Fig. 3.
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In the text

$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{0552fig12.ps} } \end{figure}$ Figure 12: Model H I spectrum for a past ram pressure stripping event.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0552fig13.ps} } \end{figure}$ Figure 13: Model spectra corresponding to our offset H I observations (Fig. 5) for a past ram pressure stripping event.
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In the text

$\begin{figure} \par {\includegraphics[width=6cm,clip]{0552fig14.ps} } \end{figure}$ Figure 14: Model moment maps for a past ram pressure stripping event. Upper panel: gas distribution in arbitrary units. The relative contours are the same as in Fig. 3. Middle panel: velocity field. The contours are the same as in Fig. 3. Lower panel: velocity dispersion. The contours are the same as in Fig. 3.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{0552fig15.ps} } \end{figure}$ Figure 15: Three dimensional view of the data cubes. The RA-Dec plane is perpendicular to the image plane, and the velocity axis is the vertical axis. a) H I observations. b) Unperturbed gas disk. c) Ongoing ram pressure stripping. d) Past ram pressure stripping event.
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In the text

$\begin{figure} \par {\includegraphics[width=14cm,clip]{0552fig1.ps} } \end{figure}$	Figure 1: VLA H I channel maps of NGC 4569. The central velocity of each channel is indicated in the upper part of each panel. The HPBW ( $31''\times 39''$ ) is plotted in the lower left corner of the first channel. The contours are in steps of $3\sigma =1.5$ mJy/beam beginning at 1.5 mJy/beam.
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$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{0552fig2.ps} } \end{figure}$	Figure 2: Solid line: Effelsberg spectrum of the central position. Dashed line: integrated VLA spectrum. Dotted line: 3 $\sigma$ noise level of the Effelsberg spectrum. The radial velocities are relative to the systemic velocity of NGC 4569.
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$\begin{figure} \par {\includegraphics[width=6.6cm,clip]{0552fig3.ps} } \end{figure}$	Figure 3: H I moment maps of NGC 4569. Upper panel: column density. The contour steps are from 1 to $9 \times 1.3\times 10^{20}$ cm^-2. Middle panel: velocity field. Contour levels are from -440 to -40 km s^-1 in steps of 20 km s^-1. Lower panel: velocity dispersion. Contour levels are from 1 to $9 \times 8.3$ km s^-1.
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$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{0552fig4.ps} } \end{figure}$	Figure 4: Contours: H I column density. The contour levels are the same as in Fig. 3. Greyscale: B band DSS image. The contrast is chosen such that the whole disk extent becomes visible.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0552fig5.ps} } \end{figure}$	Figure 5: Solid lines: Effelsberg 100-m spectra of the five 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 Effelsberg spectra. Radial velocities are given relative to the systemic velocity of NGC 4569.
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$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{0552fig7.ps} } \end{figure}$	Figure 7: Comparison snapshot of the gas distribution of NGC 4569 for the case of ongoing ram pressure stripping. Left panel: the disk seen face-on. Right panel: view of the disk using the observed position angle and inclination of NGC 4569. The arrow indicates the direction of the wind, i.e. opposite to the galaxy's motion.
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$\begin{figure} \par {\includegraphics[width=6.8cm,clip]{0552fig8.ps} } \end{figure}$	Figure 8: Initial gas velocity field. The disk is truncated at a radius of 5 kpc.
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$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{0552fig9.ps} } \end{figure}$	Figure 9: Model H I spectrum for ongoing ram pressure stripping.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0552fig10.ps} } \end{figure}$	Figure 10: Model spectra corresponding to our offset H I observations (Fig. 5) for ongoing stripping.
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$\begin{figure} \par {\includegraphics[width=6.5cm,clip]{0552fig11.ps} } \end{figure}$	Figure 11: Model moment maps for ongoing ram pressure stripping. Upper panel: gas distribution in arbitrary units. The relative contours are the same as in Fig. 3. Middle panel: velocity field. The contours are the same as in Fig. 3. Lower panel: velocity dispersion. The contours are the same as in Fig. 3.
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$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{0552fig12.ps} } \end{figure}$	Figure 12: Model H I spectrum for a past ram pressure stripping event.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0552fig13.ps} } \end{figure}$	Figure 13: Model spectra corresponding to our offset H I observations (Fig. 5) for a past ram pressure stripping event.
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$\begin{figure} \par {\includegraphics[width=6cm,clip]{0552fig14.ps} } \end{figure}$	Figure 14: Model moment maps for a past ram pressure stripping event. Upper panel: gas distribution in arbitrary units. The relative contours are the same as in Fig. 3. Middle panel: velocity field. The contours are the same as in Fig. 3. Lower panel: velocity dispersion. The contours are the same as in Fig. 3.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{0552fig15.ps} } \end{figure}$	Figure 15: Three dimensional view of the data cubes. The RA-Dec plane is perpendicular to the image plane, and the velocity axis is the vertical axis. a) H I observations. b) Unperturbed gas disk. c) Ongoing ram pressure stripping. d) Past ram pressure stripping event.
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