$0.3\le z\le 2.9$, whereas for a model with $\Omega_{M}=0.3$ and $\Omega_{\Lambda}=0.7$ the clustering signal shows a marginal increase at high redshift. Here $\Omega_{M}$ and $\Omega_{\Lambda}$ are the mass and cosmological constant density contribution, respectively, to the total density of the universe.

The observed behavior of the QSO clustering can be explained within the linear theory and a typical bias model. The theoretical interpretation of the picture drawn by 2QZ is a result of the combination of many ingredients and their degeneracies: the bias factor, the ratio between the masses of black hole and dark matter halo, the life-time of QSOs, the efficiency and the mass accretion rate.

To add new insights in the modeling and interpretation, one has to consider the constraints from the luminosity function (LF) or/and to enlarge the redshift domain toward lower or higher redshifts. For these reasons, we have started a project, the AERQS, to find bright AGN in the local universe, removing present uncertainties about the properties of the local QSO population and setting the zero point for clustering evolution. For the general aims of the AERQS Survey and its detailed presentation \[see @GC2000 [@DSS2k2]\].

The goal of this paper is to analyze the clustering 