deletions | additions       diff --git a/section_Methods_Results_The_R__.tex b/section_Methods_Results_The_R__.tex  index 79d20d7..3b4ef60 100644  --- a/section_Methods_Results_The_R__.tex  +++ b/section_Methods_Results_The_R__.tex 
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The R $\sim 22700$, high SNR spectra of USNO-A0600-15865535 showed it to have very strong H$\epsilon$ and H$\zeta$ at Milky Way rest frame, and thus was very likely to be a star in the Milky Way, rather than the quasar we had originally attempted to target. Such stars are typically either Blue Horizontal Branch (BHB) stars or Blue Stragglers (BS) stars, though can occasionally be hot main sequence (MS) stars.  To distinguish between these possibilities, we use a modification of the method developed by \citet{Sirko_2004} \citei{Sirko_2004}  and later explored by \citet{Xue_2008}. In these works the shape of the H$\gamma$ and H$\delta$ lines are used to distinguish between these populations. The Balmer lines are fit with a standard Sersi\'c profile, \begin{equation}\label{sersic}  \rm y = 1 - a~ exp \left[-\left(\frac{|\lambda-\lambda_0|}{b}\right)^{c}\right]