The AB Dor Moving Group consists of a “ nucleus ” of \sim 10 stars at d \simeq 20 pc , along with dozens of purported “ stream ” members distributed across the sky .
We perform a chemical and kinematic analysis of a subsample of AB Dor stream stars to test whether they constitute a physical stellar group .
We use the NEMO Galactic kinematic code to investigate the orbits of the stream members , and perform a chemical abundance analysis using high resolution spectra taken with the Magellan Clay 6.5-m telescope .
Using a \chi ^ { 2 } test with the measured abundances for 10 different elements , we find that only half of the purported AB Dor stream members could possibly constitute a statistically chemically homogeneous sample .
Some stream members with 3D velocities were hundreds of parsecs from the AB Dor nucleus \sim 10 ^ { 8 } yr ago , and hence were unlikely to share a common origin .
We conclude that the published lists of AB Dor moving group stream members are unlikely to represent the dispersed remnant of a single star formation episode .
A subsample of the stream stars appears to be both statistically chemically homogeneous and in the vicinity of the AB Dor nucleus at birth .
Their mean metallicity is [ Fe/H ] = 0.02 \pm 0.02 dex , which we consider representative for the AB Dor group .
Finally , we report a strong lower limit on the age of the AB Dor nucleus of > 110 Myr based on the pre-MS contraction times for K-type members which have reached the main sequence .