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The Chamaeleon star-forming region has been extensively studied in the lastdecades. However, most studies have been confined to the densest parts of theclouds. In a previous paper, we analysed the kinematical properties of thespectroscopically confirmed population of the Chamaeleon I and II clouds. Wenow report on a search for new kinematical candidate members to the ChamaeleonI and II moving groups using available information from public databases andcatalogues. Our candidates were initially selected in an area of 3 deg aroundeach cloud on the basis of proper motions and colours from the UCAC4 Catalog.The SEDs of the objects were constructed using photometry retrieved from theVirtual Observatory and other resources, and fitted to models of stellarphotospheres to derive effective temperatures, gravity values, andluminosities. Masses and ages were estimated by comparison with theoreticalevolutionary tracks in a Hertzprung-Russell diagram. We have identified 51 and14 candidate members to the Chamaeleon I and II moving groups, respectively, ofwhich 17 and 1, respectively, are classified as probable young stars (ages < 20Myr) according to our analysis. Another object in Chamaeleon I located slightlyabove the 1 Myr isochrone is classified as a possible young star. All theseobjects are diskless stars with masses in the range 0.3M-1.4MSun, and agesconsistent with those reported for the corresponding confirmed members. Theytend to be located at the boundaries of or outside the dark clouds, preferablyto the north-east and south-east in the case of Chamaeleon I, and to thenorth-east in the case of Chamaeleon II. We conclude that the kinematicalpopulation of Chamaeleon I and II could be larger and spread over a larger areaof the sky than suggested by previous studies.

Proper motions of young stars in Chamaeleon. II. New kinematical candidate members of Chamaeleon I and II