Near-core rotation frequency f_rot plotted as a function of dominant mode frequency for Kepler gravity-mode pulsators having an observed amplitude above 4 mmag (f_{dom,  ≥ 4 mmag}) from the samples of Li et al. (2020) and Pedersen et al. (2021). Stars are drawn as γ Dor pulsator if they have T_eff < 8500 K and Π₀ < 0.7 d and as SPB star otherwise. When invisible, the error bars are smaller than the symbol sizes. The linear relation (red line) given by Eq. (4) was computed for the 105 stars having a dominant (k, m) = (0, 1) mode with observed frequency above 0.35 d⁻¹ and with ν > 1 (full symbols). The shaded area shows the 1-σ uncertainty region for this relation. The two pulsators indicated in cyan come from short CoRoT light curves (Degroote et al. 2010; Pápics et al. 2012). As the other open symbols, they were not used in the regression. The dashed (dotted) lines mark the 1-σ confidence interval for f_rot derived from the residuals with respect to the red line, excluding (including) stars with modes having (k, m)≠(0, 1) or ν < 1.