deletions | additions       diff --git a/Stellar atmosphere model.tex b/Stellar atmosphere model.tex  index 054c1bd..69f78ad 100644  --- a/Stellar atmosphere model.tex  +++ b/Stellar atmosphere model.tex 
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\section{Stellar atmosphere model}\label{atm}  \subsection{Spectral disentangling}\label{disentangle}  Before the two stars' atmospheres can be modeled, it is necessary to extract each star's spectrum from the observed binary spectrum. spectra.  While the location of a set of absorption lines in wavelength space is the only requirement for radial velocity studies, using an atmosphere model to measure $T_{\rm{eff}}$, $\log g$, and metallicity for each star requires precise equivalent widths of particular absorption lines. To accomplish this, we use the FDBinary tool \citep{ili04} on the spectral window 5402--6750 \AA. Following the approach in \citet{bec14}, we break the window into 26 pieces that each span about 10 \AA. FDBinary does not require a template spectrum, and instead uses the orbital parameters of a binary system to separate spectra in Fourier space. We use orbital parameters from a preliminary set of photodynamical models, which are later refined with stellar atmosphere models (see Section \ref{model}).