Резюме: The halos of galaxies are prime snooping grounds for clues to their formation histories: clues such as the distribution of dark matter and the orbits of baryons. The currently accepted cosmological paradigm, the LambdaCDM model, has been successful in describing the formation and evolution of structures in the Universe, however, there remain many observational discrepancy on scales of galaxies and galaxy clusters. In the Local Group, the spatial distribution, kinematics, and abundances of resolved halo stars provide a powerful probe of their host galaxies' formation histories, however, in more distant systems, including even the nearest early-type galaxies, such field star studies are not yet feasible, but an alternative is the use of globular clusters. Results from the kinematics of planetary nebulae indicate that many ordinary ellipticals show scant trace of their expected dark matter halos and there may be a dynamical difference between the halos of such ellipticals. There are suggestions that the difference corresponds to a bimodality in dark matter content between bright, boxy, slowly rotating ellipticals and faint, disky, fast rotating ellipticals. Kinematical studies of globular cluster systems around elliptical galaxies are well established, but the few galaxies mostly near the center of high density cluster environments are probed and it is not yet clear whether the apparent bimodality is a reflection of galaxy type or environment. In this talk, i review the dark matter halo properties for a few elliptical galaxies and their implications on Lambda CDM and MOND scenario.