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%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 %power  ratio between dipole and radial modes (the dipole mode visibility, $V^2$) visibility  for about 3600 red giants observed over the first 37 months of the Kepler mission. Our analysis is restricted to stars with \numax\   larger than 50\muhz\ and masses below 2.1\msol, which ensures it includes only red   giants that do not burn helium in their cores \citep{Stello_2013,Mosser_2014}.   %The missing dipole modes in a significant fraction of stars revented us using   %the dipole mode period spacings to select stars in this particular evolution stage  %\citep{Bedding_2011}.   %IF A REFEREEE ASKS IF WE CHECKED OUR SELECTION WORKED  %A comparison with lists of helium core burning stars identified through measured period   %spacings of non-suppressed stars  \citep{Stello_2013,Mosser_2014} revealed only X stars in common with our %sample. They all had \numax\$ < 70\,$\muhz.   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 \citep{Mosser_2011}.   The agreement with the theoretically predicted location of the  suppressed branch (black curve) is remarkable. This curve assumes that all the wave energy leaking into the stellar core is trapped; the decrease of the suppression towards lower \numax\ is a consequence of the increasingly weaker coupling between acoustic waves in the envelope and gravity waves in the core as stars evolve (Fuller et al. 2015). With this large stellar sample we can separate the stars into five different mass intervals represented in Fig.2 from 0.9 to 2.1 times the mass of the Sun, which clearly shows that the relative  population on the lower branch (suppressed stars) is strongly mass dependent.