The Rotation Curves and Three-Dimensional Kinematics of the MilkyWay from Gaia DR3

We investigate the fundamental kinematic parameters of stellar motions in the Milky Way using a statistical sample of 27,485,720 stars with measured three-dimensional velocities from the Gaia DR3 catalogue. From these data, we determine the local solar velocity (U⊙,V⊙,W⊙)=10.5±0.7,14.5±0.9,7.33±0.1km/s, the average orbital velocity V0=228±4km/s and the circular velocity Vc=234±4km/s, at the radius R⊙. Next, within the range of 3−14 kpc, we derive the Galactic rotation curve Vc(R) and determine the average spherical components of the stellar velocities as functions of both Galactocentric radius R and distance from the Galactic plane Z. Two-dimensional R−Z maps of these components reveal a complex three-dimensional kinematic structure. In particular, the pattern observed at R≲5kpc can be associated with the influence of the Galactic bar. To facilitate the description of the observations, we employ a simplified axisymmetric Monte Carlo model with several free parameters that reproduces the main kinematic trends.