maps of 40 000 kinematic models as a function of v_rot and β from the fit to VEGA (top panel) and AMBER (bottom panel) differential data. Only these two parameters were varied in a regular step in the intervals shown here. The other parameters are fixed (Table 2). Our results found from the MCMC analysis for v_rot and β are indicated with red crosses. In order to highlight the correlation between β and v_rot, the gray region corresponds to an arbitrary number of models, encompassing about the 5000 best models in both cases. The value of β = −0.5 (Keplerian disk) and our determination for v_rot are marked in dashed black line. Note the strong correlation between the stellar rotational velocity and the disk velocity law exponent in both the cases. Also, note that a Keplerian disk is found from modeling the AMBER data, but not from VEGA.