the sky. Then, one can calculate the cross-correlation function for neighbors in the projected direction parallel and perpendicular to the direction of the angular momentum of the centre galaxies, in redshift slices around them, assuming all these neighbors to be at the same distance than the centre galaxy. This slice needs to be defined so that it avoids projecting large amounts of foreground and background structures while still allowing enough numbers of neighbors to obtain good statistics.

In order to assess whether the alignments found in the previous subsection are identifiable in observational catalogues analised this way, we reproduce the procedure mentioned in the previous paragraph in our analysis of the numerical simulation which consists on projecting the structure onto the plane of the sky, assuming all objects within $\Delta v=750$km/s from the centre haloes to be exactly at the same distance from the observer.

Therefore we only use information from two cartesian coordinates in the simulation, $x$ and $y$, and transform the third, $z$, into a velocity component by multiplying $z$ by the Hubble Constant and adding the $z$ component of the peculiar velocity. In order to complete the emulation of redshift space effects suffered by observational surveys, we 