deletions | additions       diff --git a/Radial Velocities.tex b/Radial Velocities.tex  index 2bd6781..e4fd1da 100644  --- a/Radial Velocities.tex  +++ b/Radial Velocities.tex 
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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 test the BF with an observation of Arcturus as a template, and find 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 overall spectrum here, 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 \revise{with a least-squares technique}  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 $40 \ \rm{km} \ \rm{s}^{-1}$, \revise{with uncertainties on the order of $0.02 \ \rm{km} \  \rm{s}^{-1}$. Uncertainties are assigned based on the error in position from the least-squares best-fit Gaussian to each BF peak.}  \subsection{Comparison with TODCOR}\label{todcor}  To confirm that the BF-extracted radial velocities are accurate, we also use TODCOR \citep{zuc94} to extract radial velocities for the TRES spectra. TODCOR, which stands for two-dimensional cross-correlation, uses a template spectrum from a library with a narrow spectral range (5050--5350 \AA) to make a two-component radial velocity curve for spectroscopic binaries. It is commonly used with TRES spectra for eclipsing binary studies. From the radial velocity curve, TODCOR subsequently calculates an orbital solution. We use the full TODCOR RV extractor + orbital solution calculator for the TRES spectra, and compare this with the TODCOR orbital solution calculator for the combined ARCES, TRES, and APOGEE RV points which were extracted with the BF technique. We find that the two orbital solutions are in excellent agreement. The TODCOR RVs (available for TRES spectra only) are on average $0.22 \pm 0.25 \ \rm{km \ s}^{-1}$ systematically lower than the BF RVs, which we attribute to a physically unimportant difference in RV zeropoint.