Fig. 5
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Simulated spectra of the J = 3−2 CO line for TWA 7 for the no wind case (solid), and wind (dash-dotted) cases. Along with the moment-0 image of the disk, one can identify that the wind profile is not Keplerian but it is even more clearly visible on the moment-1 images in Fig. 7 (because the velocity structure changes significantly).
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