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We quantify the expected observed statistical and systematic uncertainties ofthe escape velocity as a measure of the gravitational potential and total massof galaxy clusters. We focus our attention on low redshift (z < 0.15) clusters,where large and deep spectroscopic datasets currently exist. Utilizing a suiteof Millennium Simulation semi-analytic galaxy catalogs, we find that thedynamical mass, as traced by either the virial relation or the escape velocity,is robust to variations in how dynamical friction is applied to "orphan"galaxies in the mock catalogs (i.e., those galaxies whose dark matter haloshave fallen below the resolution limit). We find that the caustic techniquerecovers the known halo masses (M_200) with a third less scatter compared tothe virial masses. The bias we measure increases quickly as the number ofgalaxies used decreases. For N_gal > 25, the scatter in the escape velocitymass is dominated by projections along the line-of-sight. Algorithmicuncertainties from the determination of the projected escape velocity profileare negligible. We quantify how target selection based on magnitude, color, andprojected radial separation can induce small additional biases into the escapevelocity masses. Using N_gal = 150 (25), the caustic technique has a percluster scatter in ln(M|M_200) of 0.3 (0.5) and bias 1+/-3% (16+/-5%) forclusters with masses > 10^14M_solar at z<0.15.

A Systematic Analysis of Caustic Methods for Galaxy Cluster Masses