Discuss the practical pros and cons of disentangling vs. naive coadding vs. low-S/N individual spectra for EBs with different flux ratios. (Or maybe this discussion is better suited to the previous section?)

Present plots of regions potentially sensitive to magnetic activity - Ca H&K, Ca II triplet, and possibly Halpha. (Forget the Fe lines shown in some of the sample plots below). Best way to quantitatively report differences in line profiles? Discuss whether these three regions correlate with each other as activity indicators, or not, and why. Compare also to photometric measures of activity for these stars \citet{gau14}.