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

How Accurately Can We Detect the Splashback Radius of Dark Matter Halos and its Correlation With Accretion Rate?