We quantify the mass dependence in Fig. 3 by showing the relative number of dipole-suppressed stars (those below the dashed line in Fig. 2) in narrow mass intervals. We see no suppression in red giants below 1.1\(\mathrm{M}_\odot\), which coincides with the mass below which they did not have convective cores during the core-hydrogen-burning phase \citep{Kippenhahn_1990}. The onset of magnetic suppression above this threshold suggests that at least some of those stars had convectively driven magnetic dynamos in their cores during the core-hydrogen-burning (main-sequence) phase. This is supported by 3D hydrodynamical modeling of these stars \citep{Brun_2005}. Red giants no longer contain convective cores, leading us to conclude that the strong magnetic fields in suppressed oscillators are the remnants of the fields produced by core dynamos during the main sequence.