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Fig. 6


maps of 40 000 kinematic models as a function of vrot 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 vrot and β are indicated with red crosses. In order to highlight the correlation between β and vrot, 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 vrot 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.

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