$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8057fi2a.eps}\hspace*{1cm} \includegraphics[width=5.5cm,clip]{8057fi2b.eps}\end{figure}$ Figure 2: Left: graphical representation of a perfect S-warp ( $S\ne 0$ , U=0). Right: graphical representation of a perfect U-warp ( $U\ne 0$ , S=0). North (higher declination) is up, south is down. ``i'' stands for the inclination between the line ``centre of void''-galaxy and the rotation axis of the galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{8057fi3a.eps}\hspace*{1cm} \includegraphics[width=5.8cm,clip]{8057fi3b.eps}\end{figure}$ Figure 3: Dependence of $\overline {S}$ and $\overline {U}$ on i predicted by the theory. Solid line: expected trend if the warps were produced by intergalactic winds flowing radially outwards in the void, according to expressions (8) and (9), normalized to a maximum height of one. Dashed line: $\cos i$ .
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{8057fi4a.ps}\\ \vspace*{2... ...c.eps}\hspace*{0.5cm} \includegraphics[width=4cm,clip]{8057fi4d.eps}\end{figure}$ Figure 4: Warp curves and contour maps of three selected galaxies ( up); and 5-filters combined SDSS images of them ( down), 50 $^{\prime \prime } \times 50^{\prime \prime }$ . The isophotes are equidistant (in units of n*3 $\sigma$ equiv. to a step of +0.75 mag/arcsec²) starting at a level of about 3 $\sigma$ above the sky background. Left: $RA=234.8898^\circ$ , $\delta =+3.2352^\circ$ (J2000), S-warped. Centre: $RA=131.4264^\circ$ , $\delta =+51.2122^\circ$ (J2000), U-warped downwards. Right: $RA =226.3795^\circ$ , $\delta =+57.4142^\circ$ (J2000), negligible warp.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8057fi5a.eps}\hspace*{1cm} \includegraphics[width=5.5cm,clip]{8057fi5b.eps}\end{figure}$ Figure 5: Dependence of S and U on the inclination i in the observational data (stars). The squares with error bars represent the average in bins of i of 30 degrees.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8057fig1.ps}\end{figure}$	Figure 1: Graphical representation of the warp measurement.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8057fi2a.eps}\hspace*{1cm} \includegraphics[width=5.5cm,clip]{8057fi2b.eps}\end{figure}$	Figure 2: Left: graphical representation of a perfect S-warp ( $S\ne 0$ , U=0). Right: graphical representation of a perfect U-warp ( $U\ne 0$ , S=0). North (higher declination) is up, south is down. ``i'' stands for the inclination between the line ``centre of void''-galaxy and the rotation axis of the galaxy.
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$\begin{figure} \par\includegraphics[width=5.8cm,clip]{8057fi3a.eps}\hspace*{1cm} \includegraphics[width=5.8cm,clip]{8057fi3b.eps}\end{figure}$	Figure 3: Dependence of $\overline {S}$ and $\overline {U}$ on i predicted by the theory. Solid line: expected trend if the warps were produced by intergalactic winds flowing radially outwards in the void, according to expressions (8) and (9), normalized to a maximum height of one. Dashed line: $\cos i$ .
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8057fi5a.eps}\hspace*{1cm} \includegraphics[width=5.5cm,clip]{8057fi5b.eps}\end{figure}$	Figure 5: Dependence of S and U on the inclination i in the observational data (stars). The squares with error bars represent the average in bins of i of 30 degrees.
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