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tokens: ) resolved the molecular line emission from above and below the disk, we could not detect the emission in the southwest of the disk, possibly due to the lower sensitivity and resolution. Figure 3. (a) Peak positions of the SiO v = 1 and 2 J = 1–0 maser emission (gray circle) and the SiO v = 4 J = 11–10 emission (colored circle). (b) Peak positions of the SiO v = 1 and 2 J = 1–0 maser emission (gray circle) and 29 SiO v = 2 J = 11–10 emission (colored cross). The color of the SiO v = 4 and 29 SiO v = 2 emission represents the line-of-sight velocity. The cross at (0, 0) corresponds to the position of Source I (Goddi et al. 2011 ). The 29 SiO v = 2 J = 11–10 emission is mainly found between the eastern and northern arms of the X-shape and also in the vertical structures from the disk, such as blueshifted emission along the eastern arm and high-velocity components near the disk midplane. It confirms that the 29 SiO v = 2 J = 11–10 emission traces the rotating outflow as other SiO line emission (e.g., Plambeck Wright 2016 ; Hirota et al. 2017 ; Ginsburg et al. 2018 ). On the other hand, the v = 4 J = 11–10 emission is only found in a line connecting the base of eastern and northern arms of 43 GHz SiO masers, which resembles the H 2 O emission in Ginsburg et al. ( 2018 ). The morphology and velocity gradient of this line suggests that it traces both the surface of the disk and the base of the outflow. 4.2. The Kinematics of <italic>v</italic> = 4 <italic>J</italic> = 11–10 Line Emission Figure 4 shows the position–velocity diagrams of the SiO v = 4 J = 11–10 and 29 SiO v = 2 J = 11–10 emissions along the axis with the position angle of 140° (Hirota et al. 2014 ). The spatial distribution and the velocity gradients along the major axis of the continuum emission indicate that the SiO v = 4 J = 11–10 emission is related to the rotating disk. However, the absence of the high-velocity components at the central position suggests that the high-frequency SiO line emissions are associated with a rotating ring structure rather than a filled disk. To find the parameters of the ring structure, we fit the observed rotation curve with a simulated rotation curve using a simple model similar to those of Hirota et al. ( 2014 ) and Plambeck Wright ( 2016 ). We assumed a thin, edge-on ring structure in Keplerian rotation around a central star. In each position, the gas with uniform temperature and density emit the optically thin emission. The thermal width of 3 km s −1 was assumed. We set the systemic velocity of 6 km s −1 , which is the central value of the observed velocity range. We simulated the rotation curve for a range of inner radii r in and outer radii r out with central masses ranges of 5 to 15 M ⊙ . As a result, we assess that r in = 12 au, r out = 26 au, and a central mass of 7 M ⊙ for the best parameter. Figure 4. (a) Position–velocity diagram of the SiO v = 4 J = 11–10 emission. The Keplerian velocity curves for 10 M ⊙ (gray) and 15 M ⊙ (black) are