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The disk around HD 169142 has been suggested to host multiple embeddedplanets due to the range of structures observed in the dust distributions. Weanalyze archival ALMA observations of $^{12} \mathrm{CO \ (2-1)}$, $^{13}\mathrm{CO \ (2-1)}$, and $\mathrm{C}^{18} \mathrm{O \ (2-1)}$ to search forlarge-scale kinematic structures associated with other embedded planets in theouter disk. At 125 au, we identify a coherent flow from the disk surface to themidplane, traced by all three CO isotopologues, and interpret it as ameridional flow, potentially driven by an embedded planet. We use changes inthe rotation speed of the gas to characterize the physical structure acrossthis region, finding that at 125 au the CO emission traces regions of increasedgas pressure, despite being at a surface density minimum. Developing a simpleanalytical model, we demonstrate that the physical structure of the gap canhave non-trivial responses to changes in the surface density, consistent bothwith previous thermo-chemical models, and the conditions inferredobservationally. Applying this technique to a range of sources will allow us todirectly confront theoretical models of gap-opening in protoplanetary disks.

Mapping the 3D Kinematical Structure of the Gas Disk of HD 169142