The Scale-Dependence of Halo Assembly Bias

Abstract

The two-point clustering of dark matter halos is influenced by halo properties besides mass, a phenomenon referred to as halo assembly bias. Using the depth of the gravitational potential well, $V_{\max }$, as our secondary halo property, in this paper we present the first study of the scale-dependence assembly bias. In the large-scale linear regime, $r\ge 10h^{-1}\mathrm{Mpc},$ our findings are in keeping with previous results. In particular, at the low-mass end ($M_{\mathrm{vir}}<M_{\mathrm{coll}}\approx 10^{12.5}{\mathrm{M}}_{\odot }$), halos with high-$V_{\max }$ show stronger large-scale clustering relative to halos with low-$V_{\max }$ of the same mass, this trend weakens and reverses for $M_{\mathrm{vir}}\ge M_{\mathrm{coll}}.$ In the nonlinear regime, assembly bias in low-mass halos exhibits a pronounced scale-dependent "bump" at $500h^{-1}\mathrm{kpc}-5h^{-1}\mathrm{Mpc},$ a new result. This feature weakens and eventually vanishes for halos of higher mass. We show that this scale-dependent signature can primarily be attributed to a special subpopulation of ejected halos, defined as present-day host halos that were previously members of a higher-mass halo at some point in their past history. A corollary of our results is that galaxy clustering on scales of $r\sim 1-2h^{-1}\mathrm{Mpc}$ can be impacted by up to $\sim 15\%$ by the choice of the halo property used in the halo model, even for stellar mass-limited samples.

7 pages, 4 figures, submitted to MNRAS

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