deletions | additions       diff --git a/subsubsection_Methods_204_076_29__.tex b/subsubsection_Methods_204_076_29__.tex  index ebe4060..b051416 100644  --- a/subsubsection_Methods_204_076_29__.tex  +++ b/subsubsection_Methods_204_076_29__.tex 
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204.076-29.732 is a very blue ($g-r = -0.21$) source, unresolved in Pan-STARRS imaging, and thus was targeted as a quasar. The R ~ 25000, high SNR spectra subsequently showed it to have very strong H$\epsilon$ and H$\zeta$ at Milky Way rest frame. 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 \cite{Sirko_2004} and later explored by \cite{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]