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(abridged) We want to provide further evidence of the origin of the proposedstellar members of Chamaeleon and to identify interlopers from the foreground\epsilon Cha and \eta Cha associations. To this aim, we compile lists ofspectroscopically confirmed members of Chamaeleon I and II, \epsilon Cha and\eta Cha, and of background objects in the same line of sight. Using VirtualObservatory tools, we cross-match these lists with the UCAC3 catalogue to getthe proper motions of the objects. In the vector point diagram, we identify thedifferent moving groups, and use this information to study the membership ofproposed candidate members of the associations from the literature. For thoseobjects with available radial velocities, we compute their Galactic spacevelocities. We look for correlations between the known properties of theobjects and their proper motions. The members of the dark clouds exhibitclearly different proper motions from those of the foreground associations andof the background stars. The data suggest that Chamaeleon II could havedifferent dynamical properties from Chamaeleon I. Although the two foregroundclusters \epsilon and \eta Chamaeleontis constitute two different proper motiongroups, they have similar spatial motions, which are different from the spatialmotion of Chamaeleon I. On the other hand, the space motions of the ChamaeleonII stars look more similar to those of the foreground clusters than to theChamaeleon I stars, but the numbers are low. Hence, with the available data itis unclear to what extent the stellar populations in both clouds are physicallyconnected to each other. We find no correlations between the proper motions andthe properties of the objects in either of the clouds.

Proper motions of young stars in Chamaeleon. I. A Virtual Observatory study of spectroscopically confirmed members