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We quantify the mass-dependent mode suppression in Fig. 3 by  showing the relative number of suppressed stars (those below the dashed  line in Fig. 2) in narrow mass intervals.   We see no suppressed stars below 1.1\msol, 1.1\msun,  while above this threshold there is first a gradual increase followed by a rapid increase above approximately  1.5\msol, 1.5\mun,  and a drop beyond 2.0\msol. 2.0\msun.  The onset of suppression beyond 1.1\msol, 1.1\msun,  coincides with the mass above which stars are thought to form convective cores during their hydrogen-core  burning phase[REF].  We believe this shows evidence for the establishment of