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With the advent of the Gaia data, the unprecedented kinematic census of greatpart of the Milky Way disc will allow us to characterise the local kinematicgroups and new groups in different disc neighbourhoods. First, we show herethat the models predict a stellar kinematic response to the spiral arms and barstrongly dependent on disc position. For example, we find that the kinematicgroups induced by the spiral arm models change significantly if one moves only~ 0.6 kpc in galactocentric radius, but ~ 2 kpc in azimuth. There are more andstronger groups as one approaches the spiral arms. Depending on the spiralpattern speed, the kinematic imprints are more intense in nearby vicinities orfar from the Sun. Secondly, we present a preliminary study of the kinematicgroups observed by RAVE. This sample will allow us, for the first time, tostudy the dependence on Galactic position of the (thin and thick) disc movinggroups. In the solar neighbourhood, we find the same kinematics groups asdetected in previous surveys, but now with better statistics and over a largerspatial volume around the Sun. This indicates that these structures are indeedlarge scale kinematic features.

Kinematic groups across the MW disc: insights from models and from the RAVE catalogue