deletions | additions       diff --git a/SETTING_UP_FOR_THE_PRESENTATION__.tex b/SETTING_UP_FOR_THE_PRESENTATION__.tex  index aa87b19..b0ec7e5 100644  --- a/SETTING_UP_FOR_THE_PRESENTATION__.tex  +++ b/SETTING_UP_FOR_THE_PRESENTATION__.tex 
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%which ensured a unique mode identification. The region of the power spectrum associated with each spherical degree were set   %to be blah, blah, blah, and blah\% for l=0--3, respectively with the regions centred according to the mode location found by   %the correlation with the model spectrum.   While the normal stars show dipole mode visibilities of about 1.5 1.5,  independent of \numax\ \numax,  %ntegrated power in the dipole modes that is typically about 50\% larger   %than for the radial modes ($V^2\simeq 1.5$)   as usual in Kepler observations \citep{Ballot_2011,Mosser_2011},