All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4473F1.eps}} \end{figure}$ Figure 1: Optical image of the pair NGC 3718 (to the west) and NGC 3729 (to the east). Taken from the DSS service.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4473F2corr.eps}} \end{figure}$ Figure 2: Optical image of NGC 3718. Taken from the DSS survey.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics[clip]{H4473F3.eps}\end{turn}} \end{figure}$ Figure 3: A map of the pointing coordinates, observed at the two observing runs. The respective observed frequencies are marked as: black diamonds (CO(1-0)), red crosses (CO(2-1)) and blue squares (HCN(1-0)).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F4.eps}\end{turn}} \end{figure}$ Figure 4: Global CO(1-0) spectrum, obtained by summing up all individual spectra, measured at the positions given in Fig. 3. The intensity scale is in units of $T_{\rm A}^*$ (K). To compare the global CO spectrum with the global HI spectrum, the latter is also shown as a solid line. The corresponding data are published in Schwarz (1985). The antenna temperature scale in the plot describes only the CO data.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4473F5corr.eps}} \end{figure}$ Figure 5: Integrated line intensity map of CO(1-0) with linear contour lines (steps: $0.25~{\rm K}~\mbox{km~s$^{-1}$ }$ ). The observations were carried out in November 1999 at the IRAM 30 m telescope. The map is overlaid with an optical image of the galaxy, taken from the DSS survey. The cross indicates the optical center and the beamsize is presented in the upper left corner.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4473F6corr.eps}} \par\end{figure}$ Figure 6: Integrated intensity map of CO(2-1). The contours correspond to 0.2, 0.4, 0.6 times K km s^-1. The cross indicates the optical center. The map is convolved to the 21 $^{\prime \prime }$ resolution of the corresponding CO(1-0) observation, as indicated in the upper left corner.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{0}\includegraphics[clip]{H4473F7corr.eps}\end{turn}} \end{figure}$ Figure 7: The position-velocity-diagram of NGC 3718, obtained in ${\rm CO}_{1-0}$ along the major axis, with linear-scale contours. The cross indicates the optical center of the galaxy and the resolution is indicated by the pv-beam in the lower left corner.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics[clip]{H4473F8.eps}\end{turn}} \end{figure}$ Figure 8: The CO(1-0) spectrum in the center. Vertical scale is $T_{\rm A}^*$ (K). The solid line shows a Gauss fit, with $I_{\rm CO(1{-}0)}=3.11$ K km s^-1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics[clip]{H4473F9.eps}\end{turn}} \end{figure}$ Figure 9: The CO(2-1) spectrum in the center. Vertical scale is $T_{\rm A}^*$ (K). The solid line shows a Gauss fit, with $I_{\rm CO(2{-}1)}=1.99$ K km s^-1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F10.eps}\end{turn}} \end{figure}$ Figure 10: NGC 3718 has the same ratio of FIR to HCN luminosity as ULIRGs (black triangles) and normal spirals (red squares). NGC 5128 (blue asterisk) and the Milky Way (green cross) are shown for comparison as well. The blue circle shows the upper limit of $L_{\rm {HCN}}$ for NGC 3718. All data except our own are taken from Solomon et al. (1992).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F11.eps}\end{turn}} \end{figure}$ Figure 11: Comparison of the fraction of dense gas to the star formation efficiency (Solomon et al. 1992). Symbols are the same as in Fig. 10.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{0}\includegraphics{H4473F12.eps}\end{turn}} \end{figure}$ Figure 12: The modeled integrated CO(1-0) line intensity shown with linear-scale contours.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4473F13.eps}} \end{figure}$ Figure 13: The upper panel shows the rotation curve v(r) used to model NGC 3718, in the lower panel the corresponding tilting-angles $\omega (r)$ are plotted.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{0}\includegraphics{H4473F14.eps}\end{turn}} \end{figure}$ Figure 14: The modeled pv-diagram along the major axis of the integrated line-intensity. A linear contour-scale is shown.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F15.eps}\end{turn}} \end{figure}$ Figure 15: The plot shows the curve of nodes of our model (solid line), discussed in Sect. 4. In our model the warp starts at 20'', as one can see in Fig. 13. Furthermore the errorbars are indicating the corresponding values of the HI-rings (Schwarz 1985) in the same frame of reference.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4473F1.eps}} \end{figure}$	Figure 1: Optical image of the pair NGC 3718 (to the west) and NGC 3729 (to the east). Taken from the DSS service.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4473F2corr.eps}} \end{figure}$	Figure 2: Optical image of NGC 3718. Taken from the DSS survey.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics[clip]{H4473F3.eps}\end{turn}} \end{figure}$	Figure 3: A map of the pointing coordinates, observed at the two observing runs. The respective observed frequencies are marked as: black diamonds (CO(1-0)), red crosses (CO(2-1)) and blue squares (HCN(1-0)).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4473F5corr.eps}} \end{figure}$	Figure 5: Integrated line intensity map of CO(1-0) with linear contour lines (steps: $0.25~{\rm K}~\mbox{km~s$^{-1}$ }$ ). The observations were carried out in November 1999 at the IRAM 30 m telescope. The map is overlaid with an optical image of the galaxy, taken from the DSS survey. The cross indicates the optical center and the beamsize is presented in the upper left corner.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4473F6corr.eps}} \par\end{figure}$	Figure 6: Integrated intensity map of CO(2-1). The contours correspond to 0.2, 0.4, 0.6 times K km s^-1. The cross indicates the optical center. The map is convolved to the 21 $^{\prime \prime }$ resolution of the corresponding CO(1-0) observation, as indicated in the upper left corner.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{0}\includegraphics[clip]{H4473F7corr.eps}\end{turn}} \end{figure}$	Figure 7: The position-velocity-diagram of NGC 3718, obtained in ${\rm CO}_{1-0}$ along the major axis, with linear-scale contours. The cross indicates the optical center of the galaxy and the resolution is indicated by the pv-beam in the lower left corner.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics[clip]{H4473F8.eps}\end{turn}} \end{figure}$	Figure 8: The CO(1-0) spectrum in the center. Vertical scale is $T_{\rm A}^*$ (K). The solid line shows a Gauss fit, with $I_{\rm CO(1{-}0)}=3.11$ K km s^-1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics[clip]{H4473F9.eps}\end{turn}} \end{figure}$	Figure 9: The CO(2-1) spectrum in the center. Vertical scale is $T_{\rm A}^*$ (K). The solid line shows a Gauss fit, with $I_{\rm CO(2{-}1)}=1.99$ K km s^-1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F10.eps}\end{turn}} \end{figure}$	Figure 10: NGC 3718 has the same ratio of FIR to HCN luminosity as ULIRGs (black triangles) and normal spirals (red squares). NGC 5128 (blue asterisk) and the Milky Way (green cross) are shown for comparison as well. The blue circle shows the upper limit of $L_{\rm {HCN}}$ for NGC 3718. All data except our own are taken from Solomon et al. (1992).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F11.eps}\end{turn}} \end{figure}$	Figure 11: Comparison of the fraction of dense gas to the star formation efficiency (Solomon et al. 1992). Symbols are the same as in Fig. 10.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{0}\includegraphics{H4473F12.eps}\end{turn}} \end{figure}$	Figure 12: The modeled integrated CO(1-0) line intensity shown with linear-scale contours.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{H4473F13.eps}} \end{figure}$	Figure 13: The upper panel shows the rotation curve v(r) used to model NGC 3718, in the lower panel the corresponding tilting-angles $\omega (r)$ are plotted.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{0}\includegraphics{H4473F14.eps}\end{turn}} \end{figure}$	Figure 14: The modeled pv-diagram along the major axis of the integrated line-intensity. A linear contour-scale is shown.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\begin{turn}{-90}\includegraphics{H4473F15.eps}\end{turn}} \end{figure}$	Figure 15: The plot shows the curve of nodes of our model (solid line), discussed in Sect. 4. In our model the warp starts at 20'', as one can see in Fig. 13. Furthermore the errorbars are indicating the corresponding values of the HI-rings (Schwarz 1985) in the same frame of reference.
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