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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig1.eps} \end{figure}$ Figure 1: Deep Effelsberg 100-m H I spectra of the NGC 4388 H I plume. The spectrum centered on the galaxy is labeled with a "G''. We clearly detect H I line emission is 4 positions: in NGC 4388 and in 3 positions to the north west of the galactic disk. These positions are labeled with "tail''. The spatial separation between two spectra corresponds to the beamsize (9.3'). We were not able to obtain proper spectra for two positions north west of the galaxy. In the corresponding boxes we have replaced the spectra by a solid line.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig2.eps} \end{figure}$ Figure 2: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data (Crowl et al. 2005). Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4402 ( $v_{\rm sys}=235$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig3.eps} \end{figure}$ Figure 3: 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 (Crowl et al. 2005), 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 4402.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig4.eps} \end{figure}$ Figure 4: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: CO(1-0) spectrum from Vollmer et al. (2005) in arbitrary units. Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4438 ( $v_{\rm sys}=-70$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig5.eps} \end{figure}$ 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. Dotted line: 3 $\sigma$ noise levels of the Effelsberg spectra. Radial velocities are given relative to the systemic velocity of NGC 4438.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig6.eps} \end{figure}$ Figure 6: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data (Vollmer et al. in prep.). Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4501 ( $v_{\rm sys}=2281$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig7.eps} \end{figure}$ Figure 7: 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 Effelsberg spectra. Radial velocities are given relative to the systemic velocity of NGC 4501.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig8.eps} \end{figure}$ Figure 8: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data of Kenney et al. (2004). Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4522 ( $v_{\rm sys}=2324$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig9.eps} \end{figure}$ Figure 9: 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 (Kenney et al. 2004), 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 4522.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig2.eps} \end{figure}$	Figure 2: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data (Crowl et al. 2005). Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4402 ( $v_{\rm sys}=235$ km s^-1).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig4.eps} \end{figure}$	Figure 4: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: CO(1-0) spectrum from Vollmer et al. (2005) in arbitrary units. Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4438 ( $v_{\rm sys}=-70$ km s^-1).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig5.eps} \end{figure}$	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. Dotted line: 3 $\sigma$ noise levels of the Effelsberg spectra. Radial velocities are given relative to the systemic velocity of NGC 4438.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig6.eps} \end{figure}$	Figure 6: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data (Vollmer et al. in prep.). Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4501 ( $v_{\rm sys}=2281$ km s^-1).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig7.eps} \end{figure}$	Figure 7: 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 Effelsberg spectra. Radial velocities are given relative to the systemic velocity of NGC 4501.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6302fig8.eps} \end{figure}$	Figure 8: Solid line: Effelsberg 100-m spectrum of the central position. Dashed line: spectrum of the VLA data of Kenney et al. (2004). Dotted line: 3 $\sigma$ noise level of the 100-m spectrum. Heliocentric velocities are given relative to the systemic velocity of NGC 4522 ( $v_{\rm sys}=2324$ km s^-1).
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