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A three-component Stackel model of the Galaxy, including the bulge, disk, andhalo, is constructed. Parameter estimates of the potential are obtained as aresult of fitting the model rotation curve to azimuthal velocities found fromdata on trigonometric parallaxes and spatial velocities of masers. The fittingmethod takes into account the measurement and natural dispersions of azimuthalvelocities and uses an algorithm for excluding objects with excessiveresiduals. In order to obtain more uniform samples, the objects were dividedinto two groups: masers associated with high-mass star forming regions andmasers of other types. A significant kinematic inhomogeneity of these groupswas identified and taken into account: the azimuthal velocity dispersion is$\sigma_{0,1}=4.3\pm 0.4$~km\,s$^{-1}$, in the first group and$\sigma_{0,2}=15.2\pm1.3$~km\,s$^{-1}$ in the second. After constructing themodel of the Galactic-plane potential, it was generalized to the entire spaceunder the assumption of the existence of a third quadratic integral of motion.When reconstructing the Galactic rotation curve in detail, the used algorithmgives an analytical expression for the Stackel potential, which significantlysimplifies the task of constructing the Galaxy's phase density model in theStackel approximation. In order to make the Stackel model more realistic, oneneeds to develop methods of direct account of data on the vertical distributionof density in the Galaxy.

Three-component Stackel model of the Galaxy based on the rotation curve from maser data