Overview of BAF-type main-sequence stars with derived values for the near-core rotation rate f_rot,i and the surface rotation rate f_rot,o. The bottom figure is a zoom-in of the top figure. For most stars, the values are consistent with rigid rotation within 1σ. The observational signature of differential surface-to-core rotation becomes stronger when the star is slowly rotating, and/or in a binary system. The stars with values from the literature were taken from (Kurtz et al. 2014; Saio et al. 2015; Triana et al. 2015; Moravveji et al. 2016; Murphy et al. 2016; Schmid & Aerts 2016; Guo et al. 2017; Kallinger et al. 2017; Sowicka et al. 2017).