deletions | additions       diff --git a/Observations spectra.tex b/Observations spectra.tex  index 243b25a..1a15291 100644  --- a/Observations spectra.tex  +++ b/Observations spectra.tex 
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We have a total of 25 high-resolution spectra from three spectrographs. At many orbital phases, prominent absorption lines show a clear double-lined signature when inspected by eye. We find that KIC 9246715 is an excellent target for obtaining radial velocity curves for both stars in the binary as the stellar flux ratio is close to unity. A long time span of observations was necessary due to the 171.277-day orbital period of the binary and visibility of the \emph{Kepler} field from the observing sites.  \subsubsection{TRES echelle from FLWO}\label{tres}  We obtained 13 high-resolution optical spectra from the Fred Lawrence Whipple Observatory (FLWO) 1.5-m telescope in Arizona using the Tillinghast Reflector Echelle Spectrograph (TRES) from 2012 March through 2013 April. The wavelength range for TRES is 3900--9100 \AA, and theaverage  resolution is 30,000. We reduced for  the data using medium fiber used is 44,000. The spectra were extracted and blaze-corrected with  the freely available standard pipeline\footnote{\url{http://tdc-www.harvard.edu/instruments/tres/reduce.html}}. pipeline developed by \citet{buc10}.  \subsubsection{ARCES echelle from APO}\label{arces}  We also obtained ten high-resolution optical spectra from the Apache Point Observatory (APO) 3.5-m telescope in New Mexico using the Astrophysical Research Consortium Echelle Spectrograph (ARCES) from 2012 June through 2013 September. The wavelength range for ARCES is 3200--10,000 \AA \ with no gaps, and the average resolution is 31,000. We reduced the data using standard echelle reduction techniques and Karen Kinemuchi's ARCES cookbook (private communication)\footnote{\url{http://astronomy.nmsu.edu:8000/apo-wiki/wiki/ARCES\#reduction} - ARC Echelle Spectragraph (ARCES) Data Reduction Cookbook}.  %We found a minor discrepancy ($\sim 0.3$ \AA \ at $7640$ \AA) between different nights' wavelength solutions for some of the earlier spectra, and used telluric features in this wavelength regime to apply small shifts in velocity space when necessary. We subsequently took thorium-argon calibration spectra more frequently which has corrected the problem.  % ^^ the above isn't relevant anymore now that we have section wavelength, below.  \subsubsection{APOGEE spectra from APO}\label{apogee}  We finally obtained two near-IR spectra of KIC 9246715 from the Sloan Digital Sky Survey-III (SDSS-III) Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey \citep{2015arXiv150100963A}. The wavelength range for APOGEE is 1.5--1.7 $\mu$m with a nominal resolution of 22,500. The pair of spectra were reduced with the standard APOGEE pipeline, but not combined. 
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