Left panel: rotation profile Ω(r, θ) of 16 Cyg B corresponding to the MAP estimates of Ω0 and Ω1. The dashed line marks the bottom of the convective envelope. Right panel: distribution of the surface rotation rate as a function of the stellar co-latitude. The red shade represent probability densities. They have been normalised with respect to the rotational rate at fixed latitude. The black line marks the mode of the corresponding density, obtained from a Gaussian mixture model. The long-dash line shows the associated 68.3% credible interval. The short-dash line shows the model corresponding to the MAP estimates of Ω0 and Ω1.
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