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Tby making use of the data provided in Koss 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 percentage 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 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 , Figure 9 and 0.3.   From  Figure 10 tell also show 11, we observe  that our data is indeed in as  the FR-I class. separation between quasar pairs decreases the accretion rate, thus the luminosity of the core increases.