Splashback Shells of Cold Dark Matter Halos

The density field in the outskirts of dark matter halos is discontinuous as a result of a caustic formed by matter at its first apocenter after infall. In this paper, we present an algorithm to identify the "splashback shell" formed by these apocenters in individual simulated halos using only a single snapshot of the density field. We implement this algorithm in the code SHELLFISH (SHELL Finding In Spheroidal Halos) and demonstrate that the code identifies splashback 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(DK14) > 0.5. Using SHELLFISH, we present the first estimates for several basic properties of individual splashback shells, such as radius, R-sp, mass, and overdensity, and provide fits to the distribution of these quantities as functions of Gamma(DK14), nu(200m), and z. We confirm previous findings that R-sp decreases with increasing Gamma(DK14), but we show that, independent of accretion rate, it also decreases with increasing nu(200m). We also study the 3D structures of these shells and find that they generally have non-ellipsoidal oval shapes. We find that splashback radii estimated by SHELLFISH are 20%-30% larger than those estimated in previous studies from stacked density profiles at high accretion rates. We demonstrate that the latter are biased low owing to the contribution of high-mass subhalos to these profiles, and we show that using the median instead of mean density in each radial bin mitigates the effect of substructure on density profiles and removes the bias.