Comparison to numerical simulations of SMC stellar tidal debris (Besla et al. 2013). Because the orbit is mainly confined to the y–z plane, we choose to compare the x-component of the angular momentum vector, L_x, and R_GAL of simulated particles to the H3 stars (large green circles). We highlight the population of interest with the shaded box in the upper panel and distinguish those particles in the simulation that lie in the leading arm (small red circles) to those in the trailing arm (large blue diamonds). In the lower panel, we compare the distribution on the sky of the simulated particles using the same symbols. Uncertainties in R_GAL account for the potential ∼20% systematic underestimation in distance due to the application of the priors. Uncertainties in L_x do not account for this effect. Using the revised distances drives the location of the H3 stars closer to that of the blue diamonds. Although the bulk of the simulated particles at R_GAL < 80 kpc are either in the body of the SMC or the leading arm, the H3 stars are not entirely without analogs.