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\subsection{Enhanced radio emission in quasar pairs}  By making use of the data provided in Liu et al 2011, we have identified 1 286 quasar pairs from a parent sample of 138 070 data points from the SDSS. This is only $1.8628\%$ of our original data. This The  percentage of AGN pair in our sample  increases to $3.6\%$ after correction for the SDSS' physical limitations are made \cite{Liu_2011}. Our final sample includes only data points that meet selection criteria mentioned the Liu et al quasar pair catalogue section. Most of our quasar pair are close to the lower limit ($z \approx 0.02$). We have only 24 pairs at $z > 0.16$. From figure 8 we observe that much of the data is clustered in the bottom right corner of the figure. This is because of a geometric effect, where the area in an annulus with $ r_{p}$-lower = 50 & $ r_{p}$-higher is much greater than for $ r_{p}$-lower = 0 & $ r_{p}$-higher = 50. We also note that the pair velocity offset seems to increase slightly with a increase in the projected separation. Since the luminosity of FR-I galaxies falls below a threshold luminosity$ 2 \times 10^{25} W Hz^{-1}sr^{−1}$ , we observe from Figure 12 that our sample data can be categorized as FR-I. We have also stated that most FR-II sources are found at redshift ∼ 0.2 − 0.3.