  Clustering properties of two samples of X-ray selected AGNs are compared with
IR/Optical galactic samples. These are the Einstein Observatory Extended Medium
Sensitivity Survey: EMSS; and a sample of 654 ROSAT detected radio quasars. The
cosmological dipole moment is calculated for these samples, yielding the values
of $b \Omega_o^{-0.6}$. We find this factor to be $0.68 \pm 0.22$ for the EMSS
sample, and $1.02 \pm 0.014$ for the quasars sample. Comparing these values
with that of the IRAS 1.2 Jy sample $(1.95 \pm 0.096)$, suggests that these
AGNs are less clustered than the IRAS galaxies. For each sample there is a
depth at which the amplitude of the dipole growth curve saturates. This
convergence radius $(R_{conv})$ is found to be $\sim 300-400$ h$^{-1}$ Mpc for
the EMSS sample and $\sim 450-500$ h$^{-1}$ Mpc for the ROSAT detected quasars
sample, which suggests that X-ray AGNs have a much deeper contribution to the
Local Group (LG) motion compared to the galaxy and cluster samples. Using the
properties of the angular and spatial correlation functions for these samples,
we find: $b_{IRAS}/b_{quasars} = 3.61 \pm 2.7$; $b_{IRAS}/b_{EMSS}= 8.46 \pm
6.4$ and $b_{quasars} / b_{EMSS} = 2.35 \pm 0.2$. Using Chi-squared
minimisation, we have fitted the angular correlation functions using the
standard power law model of the form: $W(\theta)= A \theta^{-\delta}$, and the
spatial correlation functions using the power law model of the form: $\xi(r)
=(r/r_{0})^{-\gamma}$. For the angular correlation functions, we find $A
\sim0.6$ for the AGN auto-correlations and $A \sim0.2-0.3$ for the AGN-IRAS
galaxy cross-correlations. Also $\delta$ is found to be $~ 0.8-1.1$. In the
spatial correlation analysis, we find $r_{o}\sim3.5-5.1$ $h^{-1}Mpc$ and
$\gamma\sim1.4-1.7$ .
