deletions | additions       diff --git a/sectionResults__subs.tex b/sectionResults__subs.tex  index c37de25..a91c4fd 100644  --- a/sectionResults__subs.tex  +++ b/sectionResults__subs.tex 
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MWC 237 is the closest Be star in the sample with a photometric distance of 95pc. The Altair images show a K=6.4mag companion at an angular separation of 0.85''. and brightness difference of 1.98 mag in K. JHK photometry calibrated relative to the 2MASS magnitudes for the primary gives color indices consistent with spectral type A. The companion is redder than the primary in all colors, most significantly in H-K. For a distance of 95 pc, the physical separation of the two stars is 78 AU.  Although the sample was selected from J82 to include only stars not known to be visual or spectroscopic binaries,  I subsequently found MWC 237 in the CCDM catalog \cite{Dommanget2002} as the visual binary CCDM J15329+3122AB. The source data for the CCDM entry were observed in 1971, at which time the binary separation was $\rho$=0.5" with position angle PA=203$\deg$. The 2009 Gemini data show $\rho$=0.85" and PA=198.5$\deg$. CCDM gives proper motion for the primary component only. If AB is a true binary system, then it shares a common proper motion and the relative position change is due to orbital motion. With two widely spaced measurements of $\rho$ and PA 38 years apart, an estimate of the orbital period and inclination can be made. By fitting an ellipse, centered on the primary, to the two positions along the orbit, the semi-major axis can be measured. Then by assuming the orbit to be circular, the ratio of major to minor axes of the fitted ellipse provides the inclination of the orbital plane to the line of sight. The period of this orbit is given by Kepler's Law (Equation~\ref{eqn:kepler}), (Equation~\ref{eq:kepler}),  using masses for A and B derived from their spectral types and absolute magnitudes. Finally we can test whether the distance traveled by B in the 38 years between measurements is consistent with the orbital solution. \begin{equation}  \label{eqn:kepler} \label{eq:kepler}  \(P = \frac{2\pi a^{3/2}}{\sqrt{G(M+m)}} \)  \end{equation}  G=6.67 $\times$10$^{-11}m^{3}kg^{-1}s^{-2}$