All Figures

Figure 1: The left panel shows the absolute magnitudes of galaxies, as well as magnitudes of the luminosity window, M1 and M2, for the slice. The right panel gives the luminosities (weights) of galaxies as a function of distance for the same slice. In the left panel black symbols mark the absolute magnitudes of observed galaxies, the upper and lower strips with gray symbols show the absolute magnitude limit M1 and M2. In the right panel gray symbols show the observed luminosities of galaxies, black symbols are for total luminosities corrected for the unobserved part of the luminosity range.

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In the text

	Figure 2: The luminosity density field of the LCRS slices smoothed with a  h-1Mpc Gaussian filter. Open circles denote positions of Abell clusters located within boundaries of slices. In some cases an Abell cluster consists of several subclusters, in these cases only rich subclusters are marked. The observer is located at the coordinates (x,y)=(0,0).
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In the text

	Figure 3: The density field of the LCRS slices smoothed with a  h-1Mpc Gaussian filter. The location of slices as in Fig. 2. Densities are reduced to a sheet of constant thickness.
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In the text

	Figure 4: The luminosity density of the LCRS slices as a function of distance. The left panel shows Northern slices, the right panel shows Southern slices.
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In the text

	Figure 5: The luminosities of DF-clusters as a function of distance. The upper panels show the distribution for the DF-clusters, the lower panels for the LCRS loose groups; the left panels show Northern slices, the right panels show Southern slices. The idential trend in different slices is clearly seen. The less well sampled slice is highlighted with larger symbols.
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In the text

	Figure 6: Total luminosities of the DF-clusters (upper panels) and the LCRS loose groups (lower panels) as a function of the global relative density . The left panels show Northern slices, the right panels show Southern slices.
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In the text

	Figure 7: Total luminosities of DF-clusters as a function of the global relative density ; clusters are divided into 3 distance classes: , , and  h-1Mpc, shown in the lower, middle and upper panels, respectively. The left panels show Northern slices, the right panels show Southern slices.
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In the text

Figure 8: The left panel shows the distribution of luminosities of DF-clusters (the cluster luminosity function) in the LCRS slices. The right panel shows the LCRS loose group luminosity functions. For comparison we show the cluster luminosity function for the SDSS Northern slice (Paper I), and the LCRS loose group mass function according to Heinämäki et al. (2003) reduced by mass-to-luminosity value M/L=600 (open circles).

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In the text

	Figure 9: The confidence regions for the Schechter function parameters and . The upper panel shows the 1, 2, and 3 confidence regions for the total sample and the lower panel - the 2 regions for individual samples. Note that the scales in the panels are different. The confidence regions in the lower panel are marked by the slice number in their centres.
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In the text

	Figure 10: The cluster luminosity selection function, determined by two methods. The solid line shows the selection function found in this paper using Eq. (4). Dots give the selection function as found in Paper I using two sets of parameters of the Schechter function.
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In the text

Figure 11: Properties of the LCRS density field superclusters as a function of the threshold density, , that separates superclusters (high-density regions) and voids (low-density regions). The upper panel shows the number of superclusters, N, the middle panel shows the area of the largest supercluster (in units of the total area covered by superclusters), and the lower panel shows the size (either in the x or y direction, whatever is larger) of the largest supercluster.

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In the text

	Figure 12: Total luminosities of DF-superclusters, determined by summing luminosities of DF-clusters, , and by integrating luminosity inside the threshold density contour, .
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In the text

	Figure 13: Characteristic density profiles in superclusters of the slice. For each peak density profiles are given in the x and y directions (in  h-1Mpc). The supercluster identification is shown according to Table 4.
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In the text

	Figure 14: The total luminosities of the DF-superclusters in the LCRS slices at different distances from the observer.
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In the text

	Figure 15: Total luminosities of the DF-superclusters versus the number of DF-clusters in a supercluster (supercluster richness). Filled circles: DF-superclusters which belong to the superclusters of Abell clusters, empty circles: DF-superclusters that do not belong to the Abell superclusters (see Tables 4, 5 and text).
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In the text