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%[MAYBE REMOVE NEXT PARAGRAPH AND PUT INFO IN FIG2 CAPTION OR MAYBE NOT GIVE REASON]  We restrict our analysis to stars with \numax\ larger than 50\muhz\  and masses below 2.1\msol, to ensure it includes only red giants that do  not burn helium in their cores [ref Stello2013Mosser2014Montalban201?].   %A cross matching of our sample with samples of known classification [REF  %Stello2013,Mosser2014] we found only XX helium-core burning stars in our  %sample (all with \numax below 70\muhz), which were removed.  %Because the proposed theory for the suppression has only been developed for  %hydrogen-shell burning stars, we remove helium-core burning stars from our  %sample. We ensure that by looking only at stars with \numax\ larger than 50\muhz\  %and masses below 2.1\msol[ref Stello2013Mosser2014Montalban201?].   %The proposed theory for the suppression has only been developed for  %hydrogen-shell burning stars, and we restrict our analysis to those by  %looking only at stars with \numax\ between 50 and 240\muhz\ and masses  %below 2.1\msol[ref Stello2013Mosser2014Montalban201?]   In Fig. 2 we show the power ratio between dipole and radial modes (the  dipole mode visibility, $V^2$) for about 3500 red giants. It is striking  how the stars form two distinct branches that gradually merge as the stars  evolve towards lower \numax. This trend is also evident in Fig.1. Most  stars fall on the `normal' upper branch of visibilities around 1.5 in  agreement with previous results [ref Mosser2012LargeKepler].   The agreement with the theoretically predicted location of the  suppressed branch (black curve) show strong support for an almost 100\%  dissipative loss of mode energy in the core, and hence a gradually  decreasing suppression arising from a weaker coupling between acoustic waves   in the envelope and gravity waves in the core when the stars evolve  to larger \numax[ref theory paper].   Interestingly, with this large stellar sample we can separate the stars by   mass into the five panels of Fig.2, which clearly shows that the relative  population on the lower branch (suppressed stars) is strongly mass dependent.