Left panel: Cartesian velocities of the GUMS sample in the solar neighbourhood. The blue points mark the halo stars, while the underlying density distribution shows all the stars in the sample. One can readily notice that the halo members have distinctly different kinematics compared to the rest of the stars. Middle panel: equivalent velocity distribution calculated assuming v_los = 0 km s⁻¹, for the case when the radial velocities of the stars are not known. The halo stars with v_los close to 0 are not affected by this transformation, while the stars with large v_los values cluster around ṽ_y ~ 200 km s⁻¹. There is still a kinematic distinction between the halo stars and the rest. Right panel: HR diagram, where the symbols are the same as on the left panel. The halo stars have systematically bluer colours, in line with their [Fe/H] distribution.