We have analysed the kinematics of a sample of 114 hot subdwarf stars .
For 2/3 of the stars , new proper motions , spectroscopic and photometric data are presented .
The vast majority of the stars show a kinematic behaviour that is similar to that of Thick Disk stars .
Some stars have velocities rather fitting to solar , i.e .
Thin Disk , kinematics .
About \sim 15 objects have orbital velocities which differ considerably from those of Disk stars .
These are members of the Galactic Halo .
We investigated the velocity dispersions and calculated the orbits .
Most stars feature orbits with disk character ( eccentricity of less than 0.5 ) , a few reach far above the Galactic plane and have very eccentric orbits ( eccentricity of more than 0.7 ) .
The intermediate eccentricity range is poorly populated .
This seems to indicate that the ( Thick ) Disk and the Halo are kinematically disjunct .
Plotting a histogram of the orbit data points along z 
leads to the z -distance probability distribution of the star ; doing this for the whole sample leads to the z -distance probability distribution of the sample .
The logarithmic histogram shows two slopes , each representing the scale height of a population .
The disk component has a scale height of 0.9 ( \pm 0.1 ) kpc , which is consistent with earlier results and is similar to that of the Thick Disk .
The other slope represents a component with a scale height \sim 7 kpc , a much flatter gradient than for the disk component .
This shows that the vast majority of the sdBs are disk stars , but a Halo minority is present , too .
The kinematic history and population membership of the sdB stars on the whole is different from that of the cooler HBA stars , which are predominantly or even exclusively Halo objects .
This leads to the question , whether the Halo sdB stars are of similar origin as the HBA stars , or whether their kinematical behaviour possibly represents another origin , such as infalling stellar aggregates or inner disk events .