  The splashback radius ($R_{\rm sp}$) of dark matter halos has recently been
detected using weak gravitational lensing and cross-correlations with galaxies.
However, different methods have been used to measure $R_{\rm sp}$ and to assess
the significance of its detection. In this paper, we use simulations to study
the precision and accuracy to which we can detect the splashback radius with 3D
density, 3D subhalo, and weak lensing profiles. We study how well various
methods and tracers recover $R_{\rm sp}$ by comparing it with the value
measured directly from particle dynamics. We show that estimates of $R_{\rm
sp}$ from density and subhalo profiles correspond to different percentiles of
the underlying $R_{\rm sp}$ distribution of particle orbits. At low accretion
rates, a second caustic appears and can bias results. Finally, we show that
upcoming lensing surveys may be able to constrain the splashback-accretion rate
relation directly.
