Gas kinematics are an important part of the planet formation process. Turbulence influences planetesimal growth and migration from the scale of submicron dust grains through gas-giant planets. Radio observations of resolved molecular line emission can directly measure this non-thermal motion and, taking advantage of the layered chemical structure of disks, different molecular lines can be combined to map the turbulence throughout the vertical extent of a protoplanetary disk. Here we present ALMA observations of three molecules (DCO(3-2), C18O(2-1) and CO(2-1)) from the disk around HD 163296. We are able to place stringent upper limits (v turb s , , s , and , and s for CO(2-1), C18O(2-1), and DCO(3-2) respectively), corresponding to α ≲ 3 × 10-3, similar to our prior limit derived from CO(3-2). This indicates that there is little turbulence throughout the vertical extent of the disk, contrary to theoretical predictions based on the magnetorotational instability and gravitoturbulence. In modeling the DCO emission, we also find that it is confined to three concentric rings at 65.7 ± 0.9 au, {149.9}-0.7 0.5 {au}, and 259 ± 1 au, indicative of a complex chemical environment.
