deletions | additions       diff --git a/section_Methods_Results_The_R__.tex b/section_Methods_Results_The_R__.tex  index 9fa33b7..25445c0 100644  --- a/section_Methods_Results_The_R__.tex  +++ b/section_Methods_Results_The_R__.tex 
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\rm y = 1 - a~ exp \left[-\left(\frac{|\lambda-\lambda_0|}{b}\right)^{c}\right]  \end{equation}  and the parameters of these lines clearly differentiate between the populations. Unfortunately, we do not have observations of the H$\gamma$ or H$\delta$ line, only the H$\epsilon$ and H$\zeta$ line. To determine whether we can use the better resolved  H$\epsilon$ line as a similar discriminator, we first assemble a sub-population of BHB, BS, and MS drawn from the catalog presented in \cite{Xue_2008}, selected to be brighter than 16th magnitude in g. These targets have already been fit, and classified, but to test our method we refit the H$\gamma$ line in the SDSS DR10 spectra using Equation \ref{sersic}. We find that we can indeed reproduce the bifurcation. We then apply this same fitting procedure to the H$\epsilon$ line. The results for both fits are shown in Figure \ref{hgammahepsilon}. The H$\epsilon$ line fit Sersi\'c parameters b and c do not as clearly delineate between BHB and BS stars, but the differentiation is still quite clearly in place. We then apply this same fit to our VLT/FLAMES spectrum of USNO-A0600-15865535, and overplot the b and c parameters. USNO-A0600-15865535 isvery  clearly a BHB star. BHB stars have the useful property of being rather accurate standard candles. Using the color $g-r = -0.21$, we can measure the absolute magnitude of the star to be $M_g = 0.64$, using the values from \cite{Xue_2008} (these values are originally reported in \cite{Sirko_2004} with a typographical error). This gives USNO-A0600-15865535 a distance of 5.2 kpc, with distance  errors for BHB stars typically quoted at 10\%.