The upper panel shows the best-fitting binary rv curves for our observations of μ¹ Sco, with the residuals plotted below. The excursions of the stronger primary lines are slightly less than those of the secondary. The former appear consistent with the random scatter in the individual measures of less ∼12 km s⁻¹ amplitude. The lower panel shows our fitting to the rv data assembled by vAM (2010). Again we notice a comparable scatter in the residuals, relating to the difficulties of locating the few, very broad and shallow lines.