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We explore the dynamical structure of the protoplanetary disks surrounding HD163296 and MWC 480 as part of the Molecules with ALMA at Planet Forming Scales(MAPS) large program. Using the $J = 2-1$ transitions of $^{12}$CO, $^{13}$COand C$^{18}$O imaged at spatial resolutions of $\sim 0.^{\prime \prime}15$ andwith a channel spacing of $200$ ${\rm m\,s^{-1}}$, we find perturbations fromKeplerian rotation in the projected velocity fields of both disks($\lesssim\!5\%$ of the local Keplerian velocity), suggestive of large-scale(10s of au in size), coherent flows. By accounting for the azimuthal dependenceon the projection of the velocity field, the velocity fields were decomposedinto azimuthally averaged orthogonal components, $v_{\phi}$, $v_r$ and $v_z$.Using the optically thick $^{12}$CO emission as a probe of the gas temperature,local variations of $\approx\! 3$ K ($\approx\! 5 \%$ relative changes) wereobserved and found to be associated with the kinematic substructures. The MWC480 disk hosts a suite of tightly wound spiral arms. The spirals arms, inconjunction with the highly localized perturbations in the gas velocitystructure (kinematic planetary signatures), indicate a giant planet, $\sim\! 1$$M_{\rm Jup}$, at a radius of $\approx 245$ au. In the disk of HD 163296, thekinematic substructures were consistent with previous studies of Pinte et al.(2018a) and Teague et al. (2018a) advocating for multiple $\sim\! 1$ $M_{\rmJup}$ planets embedded in the disk. These results demonstrate that molecularline observations that characterize the dynamical structure of disks can beused to search for the signatures of embedded planets. This paper is part ofthe MAPS special issue of the Astrophysical Journal Supplement.

Molecules with ALMA at Planet-forming Scales (MAPS XVIII): Kinematic Substructures in the Disks of HD 163296 and MWC 480