of masses indicated in Table \[table\]. Notice that our study covers over one and a half decades in the host-halo mass of SDSS-DR6 galaxies.

(130,498) (0,0) (7,173) (7,340)

As we demonstrated in the previous section both, the large scale structure and alignments surrounding galaxies, can be studied using the projected correlation function, $\omega(\sigma)$, measured in terms of the projected separation, $\sigma$. We now apply this method to our samples of edge-on galaxies, and compare the outcome from using tracers in the direction parallel and perpendicular to the inferred angular momentum, to detect differences between the structure along these two directions.

The projected correlation functions are calculated using galaxies in a given subsample, cross-correlated to the full spectroscopic SDSS-DR6 catalogue. As in the 2-dimensional analysis carried out in the numerical simulations, we calculate the cross-correlation for edge-on galaxies selected so that $b/a<0.7$. Note that in the numerical simulation we used an angle between the halo angular momentum and the line of sight of $60^o$, which in the case of a perfect thin disk is equivalent to $b/a=0.5$, but is larger for a thick disk as is the case of the intrinsic shapes of spiral galaxies or flattened ellipsoids (Padilla & Strauss, 