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The most luminous galaxies in the blue passband have a larger correlationamplitude than L* galaxies. They do not appear to be preferentially located inrich clusters or groups, but a significant fraction of them seem to be insystems which include fainter members.We present an analysis of fields centeredon 18 Very Luminous Galaxies (MB < -21) selected from the Southern Sky RedshiftSurvey 2, based on new observations and public data of the 2dF Galaxy RedshiftSurvey; we present also additional data on a CfA VLG and on Arp 127. We findthat all the selected VLGs are physically associated to fainter companions.Moreover, there is a relation between the VLG morphology (early or late) andthe dynamical properties of the system, which reflects the morphology-densityrelation. 6 out of the 18 SSRS2 VLGs are early type galaxies: 2 are in thecenter of rich Abell clusters with velocity dispersion sigma ~600 km/s, and theother 4 are in poor clusters or groups with sigma ~300. The VLG extracted fromthe CfA catalog is also an elliptical in a Zwicky cluster. The remaining 2/3 ofthe sample are late-type VLGs, generally found in poorer systems with a largerspread in velocity dispersion, from ~100 up to ~750 km/s. The low velocitydispersion, late-type VLG dominated systems appear to be the analogous of ourown Local Group. The possibile association of VLG systems to dark matter haloswith mass comparable to rich groups or clusters, as suggested by the comparablecorrelation amplitude, would imply significant differences in the galaxyformation process. This work also shows that observing fields around VLGsrepresents an effective way of identifying galaxy systems which are notselected through other traditional techniques.Comment: 21 pages, A&A, in pres

Nature and environment of Very Luminous Galaxies