Fig. 6
Best-fit Keplerian rotation model (left panel) and the residuals calculated by subtracting the model from the observed rotation velocity (right panel), shown for 12 CO. The residuals inside a radius of 1.5 times the FWHM of the beam are masked out. In the residuals a spiral Spv is spanning more than one azimuth between ~40 and 180 au.
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