AB Dor is the nearest identified moving group .
As with other such groups , the age is important for understanding of several key questions .
It is important , for example , in establishing the origin of the group and also in comparative studies of the properties of planetary systems , eventually surrounding some of the AB Dor group members , with those existing in other groups .
For AB Dor two rather different estimates for its age have been proposed : a first one , of the order of 50 Myr , by Zuckerman and coworkers from a comparison with Tucana / Horologium moving group and a second one of about 100 - 125 Myr by Luhman and coworkers from color-magnitude diagrams ( CMD ) .
Using this last value and the closeness in velocity space of AB Dor and the Pleiades galactic cluster , Luhman and coworkers suggested coevality for these systems .
Because strictly speaking such a closeness does not still guarantee coevality , here we address this problem by computing and comparing the full 3D orbits of AB Dor , Pleiades , \alpha Persei and IC 2602 .
The latter two open clusters have estimated ages of about 85 - 90 Myr and 50 Myr .
The resulting age 119 \pm 20 Myr is consistent with AB Dor and Pleiades being coeval .
Our solution and the scenario of open cluster formation proposed by Kroupa and collaborators suggest that the AB Dor moving group may be identified with the expanding subpopulation ( Group I ) present in this scenario .
We also discuss other related aspects as iron and lithium abundances , eventual stellar mass segregation during the formation of the systems and possible fraction of debris discs in AB Dor group .