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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, for example 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.   Through our the observation of our data, we note that an increase in the separation between quasar pairs may lead to a decrease in the accretion rate, perhaps leading to an increase in the luminosity of the AGN. in the same breath we note that \cite{Liu_2012} states that AGN pairs experience higher black hole accretion, as measured by their radio luminosities - this is compared to samples of single AGNs which were matched to the pair samples in redshift and host-galaxy stellar mass. We also observe (in Figure 12) that the errors seem to be overlapping for three out of five of our bins (i.e. there not much difference between these bins), which might suggest that the value near $10^{24}$ is $10^{24} W Hz^{-1}$is  an outlier. The errors are also very small which might suggest that there is a significant difference between the observed luminosities of our binned data- this is especially apparent when we compare very low separation and very high separation data (refer to Figure 12). lastly 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 clearly seen in Figure 10. For these 24 data points, we note that only 8 out of 24 have pair projected separations that are approximately 60 kpc and above. From Figure 11, We see that the detection of of quasars in each bin is significantly higher than the typical fraction of radio detection. There does not seem to be any significant trend from bin to bin as the bin error bars largely overlap. The error seems to decrease with an increase in projected separation because the number of points increases.