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We analyze the $^{12}$CO $J=3-2$ data cubes of the disks in the exoALMAprogram. 13/15 disks reveal a variety of kinematic substructures in individualchannels: large-scale arcs or spiral arms, localized velocity kinks, and/ormultiple faints arcs that appear like filamentary structures on the disksurface. We find kinematic signatures that are consistent with planet wakes insix disks: AA Tau, SY Cha, J1842, J1615, LkCa 15 and HD 143006. Comparison withhydrodynamical and radiative transfer simulations suggests planets with orbitalradii between 80 and 310\,au and masses between 1 and 5 M$_\mathrm{Jup}$.Additional kinematic substructures limit our ability to place tight constraintson the planet masses. When the inclination is favorable to separate the upperand lower surfaces (near 45$^\mathrm{o}$, i.e. in 7/15 disks), we always detectthe vertical CO snowline and find that the $^{12}$CO freeze-out is partial inthe disk midplane, with a depletion factor of $\approx 10^{-3}$ - $10^{-2}$compared to the warm molecular layer. In these same seven disks, we alsosystematically detect evidence of CO desorption in the outer regions.

exoALMA. X. channel maps reveal complex $^{12}$CO abundance distributions and a variety of kinematic structures with evidence for embedded planets