deletions | additions       diff --git a/section_Results_subsection_Enhanced_radio__.tex b/section_Results_subsection_Enhanced_radio__.tex  index b627172..92f44a3 100644  --- a/section_Results_subsection_Enhanced_radio__.tex  +++ b/section_Results_subsection_Enhanced_radio__.tex 
...
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 decreases the accretion rate, thus the luminosity of the core increases.   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. 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.