Method one: by combining a sampling parameter related to an isolating integral of the stellar motion, an optimisation of
the mixture approach, and a maximisation of the partition entropy for the constituent populations of the stellar sample.
Method two: by segregating into different kinematical components in terms of the stellar orbital parameters.
Method three: by approaching a maximum entropy velocity distribution to samples selected in terms of stellar eccentricity
Working samples: HIPPARCOS and Geneva-Copenhagen survey catalog.
Results: kinematical characterisation of large-scale structures, such as thin disc, thick disc and halo, and identification of
small-scale structures, such as moving groups in the solar neighbourhood.
Consequences: confirmation of the Titius-Bode-like law for radial velocity dispersions and explanation of the apparent
vertex deviation of the disc from the swinging of two major kinematic groups around the LSR, by predicting a continuously
changing orientation of the disc pseudo ellipsoid.
CitacióCubarsi, R. [et al.]. Three kinematical methods to identify local galactic structures. A: DYNAMICS AND EVOLUTION OF DISC GALAXIES. "27th Annual Pushchino Conference". Moscou: 2010.