Radial velocities for all 4 stars in Table 5 are in agreement with Harris (1996) value within 3 errors. Hence, V10, V21, V50 and V51 are likely cluster members.
Radial velocities for all 4 stars in Table 5 are in agreement withHarris (1996) value within 3 errors. Hence, V10, V21, V50 and V51 arelikely cluster members.