Observing ROSAT sources in an area covering \sim 30 % of the Southern Hemisphere , including the R CrA Association , we found evidences that this nearby association may be much larger than previously thought .
Although in the survey we found many young stars near the R CrA , there are 20 young stars with properties that characterize them as possibly belonging to the R CrA association .
From the nine known members with measured proper motions and radial velocities , we obtain the mean space velocity components for the Association relative to the Sun : ( U , V , W ) = ( -3.8 \pm 1.2 , -14.3 \pm 1.7 , -8.3 \pm 2.0 ) km/s .
The new young stars with similar space velocities are in a projected diameter of \sim 35 ^ { \circ } .
At a distance of \sim 100 pc , this represents a size of \sim 60 pc , similar to the spread in the kinematical distances obtained assuming the above space velocity components .
If the original velocity dispersion during star formation was equal to the dispersion of the velocity vector moduli ( \sim 3 km/s ) , then the age of the association should be \sim 10 Myr to reach this size .
In this way , the classical T Tauri spectroscopic binary V4046 Sgr could be a member of the association .