deletions | additions       diff --git a/subsubsection_Methods_204_076_29__.tex b/subsubsection_Methods_204_076_29__.tex  index ef7ef19..2c51cda 100644  --- a/subsubsection_Methods_204_076_29__.tex  +++ b/subsubsection_Methods_204_076_29__.tex 
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\section{Methods}  204.076-29.732 is a bright ($g= 14.2$)  very blue ($g-r = -0.21$) source, unresolved in Pan-STARRS imaging, imaging. Through a combination of overoptimism  and thus clerical errors, it  was targeted as a quasar. quasar candidate behind the circumgalactic medium of M83 in VLT Program ID 097.A-0552(A).  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,