Residuals from the linear fit described by Eq. (4) for the selected Kepler pulsators used in Fig. 1. The distribution of modes with (k, m) = (0, 1), ν > 1, and observed frequency above 0.35 d⁻¹ is shown in dark grey, wile the distribution of all dominant modes with amplitude ≥4 mmag is shown in light grey. The full, dashed, and dotted lines indicate the same relation and confidence intervals as those in Fig. 1.