deletions | additions       diff --git a/Observations Kepler.tex b/Observations Kepler.tex  index 543c18e..70565b1 100644  --- a/Observations Kepler.tex  +++ b/Observations Kepler.tex 
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\section{Observations}\label{data}  \subsection{\emph{Kepler} light curves}\label{kepler}  Our light curves are from the \emph{Kepler} satellite Space Telescope  in long-cadence mode (one data point every 29.4 minutes), and span 17 quarters---roughly four years---with only occasional gaps. Long-cadence observations over many years are well-suited for red giant asteroseismology, as main sequence stars with convective envelopes oscillate too rapidly to be measured with \emph{Kepler} long-cadence data. When studying long-period eclipsing binaries, it is important to remove instrumental effects in the light curve while preserving the astrophysically interesting signal. In this work, we prioritize preserving eclipses. Our detrending algorithm uses the simple aperture photometry (SAP) long-cadence \emph{Kepler} data for quarters 0--17. First, any observations with NaNs are removed, and observations from different quarters are put onto the same median level so that the eclipses line up. The out-of-eclipse portions of the light curve are flattened, which removes any out-of-eclipse variability. For eclipse modeling, we use only the portions of the light curve that lie within one eclipse duration of the start and end of each eclipse. This differs from the light curve processing needed for asteroseismology, which requires interpolation to achieve evenly spaced observations (no gaps in time) and typically ``fills'' the eclipses to minimize their effect on the power spectrum \citep{gau14}. 
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