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We explore the phenomenon commonly known as halo assembly bias, whereby darkmatter halos of the same mass are found to be more or less clustered when asecond halo property is considered, for halos in the mass range $3.7 \times10^{11} \; h^{-1} \mathrm{M_{\odot}} - 5.0 \times 10^{13} \; h^{-1}\mathrm{M_{\odot}}$. Using the Large Suite of Dark Matter Simulations(LasDamas) we consider nine commonly used halo properties and find that aclustering bias exists if halos are binned by mass or by any other haloproperty. This secondary bias implies that no single halo property encompassesall the spatial clustering information of the halo population. The mean valuesof some halo properties depend on their halo's distance to a more massiveneighbor. Halo samples selected by having high values of one of theseproperties therefore inherit a neighbor bias such that they are much morelikely to be close to a much more massive neighbor. This neighbor bias largelyaccounts for the secondary bias seen in halos binned by mass and split byconcentration or age. However, halos binned by other mass-like properties stillshow a secondary bias even when the neighbor bias is removed. The secondarybias of halos selected by their spin behaves differently than that for otherhalo properties, suggesting that the origin of the spin bias is different thanof other secondary biases.

Spatial Clustering of Dark Matter Halos: Secondary Bias, Neighbor Bias, and the Influence of Massive Neighbors on Halo Properties