After a campaign of spectroscopic identifications at various telescopes, we have completed the sample, which is made up of 392 AGN with redshifts between 0.007 and 2.043. The redshift distributions, shown in Fig. \[histz\], show a peak around $z\sim 0.1$ with an extended tail up to $z=0.4$. Five AGN with $0.6\le z\le 2.04$ are possibly objects magnified by gravitational lensing effects. Table \[aerqs\] summarizes the basic properties of the three sub-samples. The area covered by the AERQS Survey consists of $\sim 14,000$ deg$^2$ at the high Galactic latitudes ($|b_{\rm 
gal}|\ge 30^{\circ}$). The mean values for the completeness and efficiency are 65.7% and 52.3%, respectively.

[cccccccc]{} DSS & $-90\le\delta\le 0$ & $12.60\le B\le 15.13$ & 5660 & 111 & $0.012\le z\le 0.680$ & 0.63\
USNO & $0\le\delta\le +90$ & $13.50\le R\le 15.40$ & 8164 & 209 & $0.034\le   
z\le 2.043$ & 0.68\
GSC & $0\le\delta\le +90$ & $12.50\le   
V\le 14.50$ & 8164 & 72 & $0.007\le z\le 0.573$ & 0.63\

Measuring the Clustering in the AERQS
=====================================

The simplest way to analyze the clustering properties of a homogeneous and complete sample of QSOs is to compute the TPCF, $\xi(r)$, in the redshift space. We choose to calculate $\xi(r)$ for two representative 