Modeled stellar kinematics of the BGG. Left: V_rms radial profile predicted by the joint lensing and dynamical modeling Img-MP (L/D) (green triangles) from the most-probable model compared to the V_rms measured over the 11 Voronoi bins and their 1σ uncertainties (gray points). The radial position of each resolution element is defined with respect to the BGG centroid. The observed V_rms are consistent with a flat profile, and predicted values are within the 1σ ranges in most bins. Right: predicted V_rms map from model Img-MP (L/D), showing that this model does not fully recover the angular structure of V_rms in Fig. 5.