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The density field in the outskirts of dark matter halos is discontinuous dueto a caustic formed by matter at its first apocenter after infall. In thispaper, we present an algorithm to identify the "splashback shell" formed bythese apocenters in individual simulated halos using only a single snapshot ofthe density field. We implement this algorithm in the code SHELLFISH (SHELLFinding In Spheroidal Halos) and demonstrate that the code identifiessplashback shells correctly and measures their properties with an accuracy of$<5\%$ for halos with more than 50,000 particles and mass accretion rates of$\Gamma_\textrm{DK14}>0.5$. Using SHELLFISH, we present the first estimates forseveral basic properties of individual splashback shells, such as radius,$R_\textrm{sp}$, mass, and overdensity, and provide fits to the distribution ofthese quantities as functions of $\Gamma_\textrm{DK14}$, $\nu_\textrm{200m}$,and $z.$ We confirm previous findings that $R_\textrm{sp}$ decreases withincreasing $\Gamma_\textrm{DK14}$, but we show that independent of accretionrate, it also decreases with increasing $\nu_\textrm{200m}$. We also study the3D structures of these shells and find that they generally have non-ellipsoidaloval shapes. We find that splashback radii estimated by SHELLFISH are$20\%-30\%$ larger than those estimated in previous studies from stackeddensity profiles at high accretion rates. We demonstrate that the latter arebiased low due to the contribution of high-mass subhalos to these profiles andshow that using the median instead of mean density in each radial bin mitigatesthe effect of substructure on density profiles and removes the bias.

Splashback Shells of Cold Dark Matter Halos