Upper panels: residuals from the Keplerian fit in Dataset E (black diamonds), after the empirical color-effect correction; (top). The dispersion outside the transit is 28 cm/s. The solid red line shows the best fit of the Rossiter-McLaughlin anomaly with . The residuals to the Keplerian + RM fit over the entire sequence yield a dispersion of 28 cm/s (bottom). Vertical dashed lines indicate the times of mid-transit, first, and fourth contacts. Lower panels: residuals from the Keplerian fit after the DRS standard color-effect correction (top). The dispersion outside the transit is 43 cm/s. The dashed red line shows the best fit of the Rossiter-McLaughlin anomaly with , in agreement with the best-fit obtained after the empirical correction (solid red line as in the upper panels). The DRS-corrected residuals to the Keplerian + RM fit over the entire sequence yield a dispersion of 39 cm/s (bottom). Thus, both the Keplerian fit and the RM fit are better when using the empirical correction rather than the DRS correction.