$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f01.ps} \end{figure}$ Figure 1: The wedge diagram of the Coma Supercluster galaxies in the declination interval $18^{\circ }<\delta <32^{\circ }$ . Members are divided between late-type (large circles, filled if observed in HI) and early-type (E-S0a: empty squares). Empty triangles mark foreground and background galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f02.ps} \end{figure}$ Figure 2: The sky projection of Coma Supercluster members (including the "homunculus legs'' HL). Spirals are represented by circles (filled if observed in H I) and E-S0a objects by empty squares.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f03.ps} \end{figure}$ Figure 3: The late-type Coma Supercluster members (including HL) coded according to their H I deficiency parameter: Def $_{\rm HI} \leq 0.5$ (empty circles); Def $_{\rm HI} > 0.5$ (filled circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{f04.ps} \end{figure}$ Figure 4: The projected distribution about the X-ray center of the Coma cluster of the H I deficiency of Late-type Supercluster detected (dots) and undetected (triangles) members (excluding HL). Large circles represent averages in bins of 0.5 $^\circ$ (1 $^\circ$ ). One $\sigma$ errorbars are given.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{f05.ps} \end{figure}$ Figure 5: The correlation between log $M_{\rm HI}$ and $B_{\rm T}^\circ$ for Sa-Sb (filled circles), Sbc-Sc (empty circles), Scd-Im-BCD (filled squares). The direct fit (solid line), the inverse fit (dashed) (obtained considering all Hubble types), and the relation used in Paper I (dotted) are given.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{f06.ps} \end{figure}$ Figure 6: The MHI function for the members of the Coma+A1367 clusters (solid) and for the non-cluster Supercluster members (dotted). The optical (log $M_{\rm HI}=9.3~M_\odot$ ) and radio (log $M_{\rm HI} =9.0~M_\odot$ ) completeness limits are drawn.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{f07.ps}\end{figure}$ Figure A.1: H I spectra of the tentatively detected galaxies in the Coma Supercluster.

In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{f08.ps}\end{figure}$ Figure A.2: H I spectra of the tentatively detected galaxies in the Virgo cluster.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f01.ps} \end{figure}$	Figure 1: The wedge diagram of the Coma Supercluster galaxies in the declination interval $18^{\circ }<\delta <32^{\circ }$ . Members are divided between late-type (large circles, filled if observed in HI) and early-type (E-S0a: empty squares). Empty triangles mark foreground and background galaxies.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f02.ps} \end{figure}$	Figure 2: The sky projection of Coma Supercluster members (including the "homunculus legs'' HL). Spirals are represented by circles (filled if observed in H I) and E-S0a objects by empty squares.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f03.ps} \end{figure}$	Figure 3: The late-type Coma Supercluster members (including HL) coded according to their H I deficiency parameter: Def $_{\rm HI} \leq 0.5$ (empty circles); Def $_{\rm HI} > 0.5$ (filled circles).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{f04.ps} \end{figure}$	Figure 4: The projected distribution about the X-ray center of the Coma cluster of the H I deficiency of Late-type Supercluster detected (dots) and undetected (triangles) members (excluding HL). Large circles represent averages in bins of 0.5 $^\circ$ (1 $^\circ$ ). One $\sigma$ errorbars are given.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{f05.ps} \end{figure}$	Figure 5: The correlation between log $M_{\rm HI}$ and $B_{\rm T}^\circ$ for Sa-Sb (filled circles), Sbc-Sc (empty circles), Scd-Im-BCD (filled squares). The direct fit (solid line), the inverse fit (dashed) (obtained considering all Hubble types), and the relation used in Paper I (dotted) are given.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{f06.ps} \end{figure}$	Figure 6: The MHI function for the members of the Coma+A1367 clusters (solid) and for the non-cluster Supercluster members (dotted). The optical (log $M_{\rm HI}=9.3~M_\odot$ ) and radio (log $M_{\rm HI} =9.0~M_\odot$ ) completeness limits are drawn.
Open with DEXTER