narrow bins in $\log_{10}(r)$ used to calculate the cross-correlation functions). We acknowledge that traces of covariance will still be present between the 1- and 2-halo term ratios. We present these results in Figure \[fig:rat3d\], where triangles show the 1-halo term ratio between correlation functions for neighbors in the directions perpendicular and parallel to the halo angular momentum; Diamonds correspond to the 2-halo term. The horizontal long dashed line at $\xi_\parallel/\xi_\perp = 1$ corresponds to the isotropic case. The data-points at masses lower than $10^{12}h^{-1}M_{\odot}$ correspond to the small numerical simulation, and show larger errors due to both, the smaller simulated volume, and the lower amplitude of clustering characterising low mass haloes.

As can be seen, the 1-halo term always shows more structure in the direction perpendicular to the angular momentum, and more so for larger masses, whereas the 2-halo term shows a similar behaviour with the possible exception of low mass haloes, whose angular momenta tend to point in the direction of the large-scale structure (although with a low statistical significance). The alignments are detected at about a $5-\sigma$ level for the higher mass halo subsamples drawn from the large simulation. As in the 2-halo regime, low mass haloes show 