A kinematic method of galactic mapping

A method of analyzing galactic structures by investigating physically similar groups of stars with specific peculiar velocities is presented. A previous kinematic method related spatial densities of stars and velocity distribution parameters; the density determination in regions bounded by short coordinate intervals made it difficult to determine the three dispersion components with equal accuracy. The study of selected velocity stars, representative of physically homogeneous groups reduced the error in the dispersion velocity component ratio of 2.2 from 0.47 to 0.40.