  We use 3-D K Means clustering to characterize galaxy substructure in the
Abell 2146 cluster of galaxies (z = 0.2343). This method objectively
characterizes the cluster's substructure using projected position and velocity
data for 67 galaxies within a 2.305 Mpc circular region centered on the
clusters optical center. The optimal number of substructures is found to be 4.
Four distinct substructures with RMS velocity typical of galaxy groups or low
mass subclusters, when compared to cosmological simulations of galaxy cluster
formation, suggests that Abell 2146 is in the early stages of formation. We
utilize this disequilibrium, that is so prevalent in galaxy clusters at all
redshifts, to construct a radial mass distribution. Substructures are bound but
not virialized. This method is in contrast to previous kinematical analyses,
which have assumed virialization, and ignored the ubiquitous clumping of
galaxies. The best fitting radial mass profile is much less centrally
concentrated than the well known NFW profile, indicating that the dark matter
dominated mass distribution is flatter pre-equilibrium, becoming more centrally
peaked in equilibrium through merging of substructure.
