a member. We find that 2M0355 overlaps within 1$\sigma$ of the range in UVW values for probable members of AB Doradus.

To examine the likelihood of 2M0355’s membership in nearby moving groups, we determine the $\chi^{2}$ probability for several known stellar groups within 75pc. We include a field star model and nearby moving group parameters from @Malo12 and supplement with the parameters for the Ursa Major, Hyades, and Carina Near groups. For most groups, we adopt the centroid positions and dispersions calculated by @Malo12, however we use velocity estimates either calculated by us or from the recent literature, where we split the uncertainties in the centroid velocities from their 1D intrinsic velocity dispersions [^6].

We first determine a $\chi^{2}$ probability that estimates the percentage of real members of a given group expected to have $\chi^{2}$ values higher than that of 2M0355–allowing for 2M0355’s observational errors and the estimated intrinsic velocity spread and spatial distribution of group members. Then we calculate a “final" probability, normalizing by the sum of the individual (marginal) star-group probabilities. At this time, equal weights are assigned to the field star and individual group models (further refinement would be beyond the focus of this study).

The initial 