  This paper is a continuation of our recent paper devoted to refining the
parameters of three component (bulge, disk, halo) axisymmetric model Galactic
gravitational potentials differing by the expression for the dark matter halo
using the velocities of distant objects. In all models the bulge and disk
potentials are described by the Miyamoto-Nagai expressions. In our previous
paper we used the Allen-Santill'an (I), Wilkinson--Evans (II), and
Navarro-Frenk-White (III) models to describe the halo. In this paper we use a
spherical logarithmic Binney potential (model IV), a Plummer sphere (model V),
and a Hernquist potential (model VI) to describe the halo. A set of present-day
observational data in the range of Galactocentric distances R from 0 to 200 kpc
is used to refine the parameters of the listed models, which are employed most
commonly at present. The model rotation curves are fitted to the observed
velocities by taking into account the constraints on the local matter density
and the vertical force . Model VI looks best among the three models considered
here from the viewpoint of the achieved accuracy of fitting the model rotation
curves to the measurements. This model is close to the Navarro-Frenk-White
model III refined and considered best in our previous paper, which is shown
using the integration of the orbits of two globular clusters, Lynga 7 and NGC
5053, as an example.
