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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.   From Figure 9 we observe as the pair velocity decreases -because of the closer interaction of the quasar pairs- the redshift (and thus the luminosity) increases. This is because accretion onto SMBHs releases energy that drives outflows which correlates to high luminosities seen in Figure 12.We further observe that as the separation between quasar pairs increases, the accretion rate, thus the luminosity of the core increases.  Figure 11 shows the distribution of quasar pair with reference to projected pair separation. The averages of each of our bins is significantly higher than the typical fraction of radio detections in SDSS-selected quasars. There also seems to be no significant difference from bin to bin as the error in all our bins overlaps. Error seems to decrease with an increase in projected separation because the number of points increases - refer to figure 11. The distribution of data points in Figure 10 indicate that we observe smaller wavelengths from the quasar pair as the separation between the quasars increases. \cite{Liu_2011} noted that we have only 24 quasar pairs with redshift larger than 0.16 ,this is cleary seen in Figure 10. From Figure 11, we observe that as the separation between quasar pairs decreases the accretion rate, thus the luminosity of the core increases.