deletions | additions       diff --git a/subsection_The_Liu_Quasar_Pair__.tex b/subsection_The_Liu_Quasar_Pair__.tex  index b76628e..5759243 100644  --- a/subsection_The_Liu_Quasar_Pair__.tex  +++ b/subsection_The_Liu_Quasar_Pair__.tex 
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The velocity offset – removes chance superpositions. ${100h_{70}}^{-1}$ is the Hubble constant, which accounts for /is a measure of the expansion rate of the Universe ( more details in \cite{Huchra_1992}). \citet{Liu_2011} further observes that most pairs with separation greater than 100 kpc are found to be closely separated but not interacting with one another. Selecting those with separation less than 100 kpc helps remove these points that are not a part of our sample space. The separation between merging AGN is a few galactic diameters for the average galaxy.  \cite{Liu_2011} further Justifies the use a LOS velocity offset $ \Delta v < 600 km s^{-1}$ km/s$  as a method to further refine the desired sample space. Plotting the distribution of $\Delta v$ of AGN pairs (Figure 2 provided in \cite{Liu_2011}) shows us that that most AGN pairs in the catalogue are found within the $300 ≲ \Delta v < 600 km s^{-1} $interval. /s$ interval.  Even so, \citet{Liu_2011} further states that $Delta v$ range within which the pair is still interacting depends on the environment – there could be a chance that some data point were erroneously cut from the sample, however, the combined LOS velocity offset, projected separation and visual inspection (discussed below) aim to minimize this. Visual inspection of SDSS images for spectroscopically selected images further removes 34 AGN pairs from the parent sample. This means that strongly interacting AGN pairs can have $\Delta v$ very large.