  We have spectroscopically identified about 100 G-, K- and M-type members of
the Scorpius Centaurus complex. To deduce the age of these young stars we
compare their Li $\lambda$6708 absorption line strengths against those of stars
in the TW Hydrae association and $\beta$ Pictoris moving group. These line
strengths indicate that Sco-Cen stars are younger than $\beta$ Pic stars whose
ages of ~12 Myr have previously been derived from a kinematic traceback
analysis. Our derived age,~10Myr, for stars in the LCC and UCL subgroups of
ScoCen is younger than previously published ages based on the moving cluster
method and upper main sequence fitting. The discrepant ages are likely due to
an incorrect (or lack of) cross-calibration between model-dependent and
model-independent age-dating methods.
