All Figures

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4267F1.ps}\end{figure}$ Figure 1: Multiplicity function of LCLGs showing the fraction of groups in systems with at least 2 members as a function of the neighbourhood radius. Bold lines: solid line - slice $\delta = -3^{\circ }$ , dotted line - slice $\delta = -6^{\circ }$ , dashed line - slice $\delta = -12^{\circ }$ . Thin lines: solid line: slice $\delta = -39^{\circ }$ , dotted line - slice $\delta = -42^{\circ }$ , and dashed line - slice $\delta = -45^{\circ }$ . Note the difference between the slice $\delta = -6^{\circ }$ and other slices.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{H4267F2.ps}\end{figure}$ Figure 2: The angle between the line-of-sight and the large semiaxes of the LCLG superclusters (Table 1). The diagonal corresponds to the uniform distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4267F3.ps}\end{figure}$ Figure 3: The distribution of Abell clusters (open circles), Las Campanas Loose Groups (triangles) and LCRS galaxies (stars) in the region of the supercluster SCL126 along line-of-sight, with shape ellipses. Open circles denote Abell clusters, triangles - LCLGs, stars - LCRS galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{H4267F4a.ps}\par\vspace*{2mm} \includegraphics[width=7.8cm,clip]{H4267F4b.ps}\end{figure}$ Figure 4: The distribution of Abell clusters and Las Campanas loose groups in the region of the supercluster SCL48 (the Horologium-Reticulum supercluster) in supergalactic YX (upper panel) and YZ (lower panel) coordinates in Mpc. Filled circles denote Abell clusters, open circles - LCLGs from the slice $\delta = -39^{\circ }$ , crosses - LCLGs from the slice $\delta = -42^{\circ }$ , and $\times$ 's - LCLGs from the slice $\delta = -45^{\circ }$ . The Abell numbers of the richest Abell clusters in this supercluster are given (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4267F5.ps}\end{figure}$ Figure 5: The rms line-of-sight velocities of loose groups in Abell superclusters against the distances from the nearest Abell cluster in a supercluster. The open circle represents LCLG-12 163, that is located at an end of a filament centred on an Abell cluster from SCL119.
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In the text

$\begin{figure} \par\includegraphics[width=14.8cm,clip]{H4267F6a.ps}\par\includegraphics[width=15.4cm,clip]{H4267F6b.ps}\end{figure}$ Figure 6: Upper panel: the Abell clusters in equatorial coordinates. Filled circles show the Abell clusters located in superclusters of richness 8 and more members, open circles mark the Abell clusters in less rich superclusters. Solid lines show the location of the LCRS slices, dashed lines - the location of the Dominant Supercluster Plane. Lower panels show intersections of supercluster ellipsoids with the LCRS slices
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{H4267F7.ps}\end{figure}$ Figure 7: Luminosities of LCRS loose groups from superclusters of Abell clusters (filled circles) and from systems without Abell clusters (open circles) (in units of solar luminosity $h^{-2}~L_{\odot}$ ) versus the distances of the groups (in h^-1 Mpc).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4267F8.ps}\end{figure}$ Figure 8: Maximum relative densities in superclusters (Table 1) versus the distance of a supercluster. Filled circles correspond to superclusters of Abell clusters, open circles - to systems without Abell clusters.
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In the text

Figure 9: The slice delta = -3 degrees

In the text

Figure 10: The slice delta = -6 degrees

In the text

Figure 11: The slice delta = -12 degrees

In the text

Figure 12: The slice delta = -39 degrees

In the text

Figure 13: The slice delta = -42 degrees

In the text

Figure 14: The slice delta = -45 degrees

In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{H4267F2.ps}\end{figure}$	Figure 2: The angle between the line-of-sight and the large semiaxes of the LCLG superclusters (Table 1). The diagonal corresponds to the uniform distribution.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4267F3.ps}\end{figure}$	Figure 3: The distribution of Abell clusters (open circles), Las Campanas Loose Groups (triangles) and LCRS galaxies (stars) in the region of the supercluster SCL126 along line-of-sight, with shape ellipses. Open circles denote Abell clusters, triangles - LCLGs, stars - LCRS galaxies.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4267F5.ps}\end{figure}$	Figure 5: The rms line-of-sight velocities of loose groups in Abell superclusters against the distances from the nearest Abell cluster in a supercluster. The open circle represents LCLG-12 163, that is located at an end of a filament centred on an Abell cluster from SCL119.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{H4267F7.ps}\end{figure}$	Figure 7: Luminosities of LCRS loose groups from superclusters of Abell clusters (filled circles) and from systems without Abell clusters (open circles) (in units of solar luminosity $h^{-2}~L_{\odot}$ ) versus the distances of the groups (in h^-1 Mpc).
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4267F8.ps}\end{figure}$	Figure 8: Maximum relative densities in superclusters (Table 1) versus the distance of a supercluster. Filled circles correspond to superclusters of Abell clusters, open circles - to systems without Abell clusters.
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