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Fig. 5


Left panel: Keplerian model (red) using an iterative inversion method to fit the velocity profile of the AS 205 A CO v = 1–0 P(8) line (black). Right panel: the excitation temperature as a function of radius needed to create the modeled lines. The models in the upper panels include extended emission out to 30 AU, a stellar mass of 1.4 M, an inclination of 25° and ΔVmod = 3 km s-1. The models in the lower panels include emission out to 10 AU, a stellar mass of 1.0 M, an inclination of 22° and an increased ΔVmod = 7 km s-1.

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