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Gas kinematics are an important part of the planet formation process.Turbulence influences planetesimal growth and migration from the scale ofsub-micron dust grains through gas-giant planets. Radio observations ofresolved molecular line emission can directly measure this non-thermal motionand, taking advantage of the layered chemical structure of disks, differentmolecular lines can be combined to map the turbulence throughout the verticalextent of a protoplanetary disk. Here we present ALMA observations of threemolecules (DCO$^+$(3-2), C$^{18}$O(2-1) and CO(2-1)) from the disk around HD163296. We are able to place stringent upper limits ($v_{\rm turb}<$0.06c$_s$,$<$0.05c$_s$ and $<$0.04c$_s$ for CO(2-1), C$^{18}$O(2-1) and DCO$^+$(3-2)respectively), corresponding to $\alpha\lesssim$3$\times$10$^{-3}$, similar toour prior limit derived from CO(3-2). This indicates that there is littleturbulence throughout the vertical extent of the disk, contrary to theoreticalpredictions based on the magneto-rotational instability and gravito-turbulence.In modeling the DCO$^+$ emission we also find that it is confined to threeconcentric rings at 65.7$\pm$0.9 au, 149.9$^{+0.5}_{-0.7}$ au and 259$\pm$1 au,indicative of a complex chemical environment.

A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO$^+$