2001ApJ...554..857G

We use the two-point correlation function in redshift space, ξ(s), to study the clustering of the galaxies and groups of the Nearby Optical Galaxy (NOG) sample, which is a nearly all-sky (|b|>20°), complete, magnitude-limited sample of ∼7000 bright and nearby optical galaxies (cz≤6000 km.s^–1). The correlation function of galaxies is well described by a power law, ξ(s)=(s/s₀)^–γ, with slope γ∼1.5 and s₀∼6.4 h^–1 Mpc (on scales 2.7-12 h^–1 Mpc), in substantial agreement with previous results of several redshift surveys of optical galaxies. Splitting NOG into different morphological subsamples, we confirm the existence of morphological segregation between early- and late-type galaxies (out to 20 h^–1 Mpc), and, in particular, we find a gradual decreasing of the strength of clustering from the S0 galaxies to the late-type spirals on intermediate scales (around 5 h^–1 Mpc). The relative bias factor between early- and late-type galaxies appears to be substantially constant with scale. Furthermore, luminous galaxies turn out to be more clustered than dim galaxies. The luminosity segregation, which is significant for both early- and late-type objects, starts to become appreciable only for galaxies brighter than M_B~-19.5+5logh (∼0.6L^*) and is independent of scale. The NOG groups identified with the hierarchical and percolation algorithms show similar clustering properties, with a degree of clustering that is intermediate between galaxies and clusters. The group correlation functions are characterized by s₀-values ranging from ∼8 h^–1 Mpc (for groups with at least three members) to ∼10 h^–1 Mpc (for groups with at least five members). The degree of group clustering depends on the physical properties of groups. Specifically, groups with greater velocity dispersions, sizes, and masses tend to be more clustered than those with lower values of these quantities.