deletions | additions       diff --git a/Radial Velocities.tex b/Radial Velocities.tex  index 4895d4d..8f93dba 100644  --- a/Radial Velocities.tex  +++ b/Radial Velocities.tex 
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We use a PHOENIX BT-Settl model atmosphere spectrum as a BF template \citep{all03}. This particular model uses \citet{asp09} solar abundance values for a star with $T_{\rm{eff}} = 4800$ K, $\log g = 2.5$, and solar metallicity, selected based on revised KIC values for KIC 9246715\footnote{We later confirm that the RV results are indistinguishable from those measured with a more accurate BF model template ($T_{\rm{eff}} = 5000$ K, $\log g = 3.0$, see Table \ref{table2}).} \citep{hub14.2}. Since the BF handles line broadening between template and target robustly, we do not adjust the resolution of the template.  Using a model template avoids inconsistencies between the optical and IR regime, additional barycentric corrections, spurious telluric line peaks, and uncertainties from a template star's systemic RV. In comparison, we tested the BF with an observation of Arcturus as a template, and found that using a real star template gives BF peaks that are narrower and have larger amplitudes. These qualities may be essential to measure RVs in the situation where a companion star is extremely faint, because the signal from a faint companion may not appear above the noise if the BF peaks are weaker and broader. However, each star contributes roughly equally to  the RVs of both stars in KIC 9246715 appear with similar strength, overall spectrum,  so we choose a model atmosphere template for simplicity. The advantages of using a real star spectrum as a BF template instead of a model will likely be crucial for future work, as most other RG/EBs are composed of a bright RG and relatively faint main sequence companion. For the optical spectra we consider the wavelength range 5400--6700 \AA. This region is chosen because it has a high signal-to-noise ratio and minimal telluric features. For the near-IR APOGEE spectra, we consider the wavelength range 15150--16950 \AA. We smooth the BF with a Gaussian to remove un-correlated, small-scale noise below the size of the spectrograph slit, and then fit Gaussian profiles to measure the location of the BF peaks in velocity space. The geocentric (uncorrected) results from the BF technique are shown for the optical spectra in Figure \ref{fig:bffig}. The results look similar for the near-IR spectra. The final derived radial velocity points with barycentric corrections are presented in Table \ref{table0} and Figure \ref{fig:rvfig}. The radial velocities vary from about $-50$ to $40 \ \rm{km} \ \rm{s}^{-1}$. 
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