Visibility and phase variations in the Hα, Brγ, and He i emission lines obtained from the high-spectral-resolution CHARA/VEGA and VLTI/AMBER observations obtained in 2010 (blue line and circles). The best-fit kinematic-model for this dataset is over-plotted as a red line. The black dotted line (upper right figure) corresponds to an Hα profile taken from the BeSS database and used to determine the real line EW.