  A planet embedded in a protoplanetary disk produces a gap by disk-planet
interaction. It also generates velocity perturbation of gas, which can also be
observed as deviations from the Keplerian rotation in the channel map of
molecular line emission, called kinematic planetary features. These observed
signatures provide clues to determine the mass of the planet. We investigated
the features induced by the planet with an inclined orbit through
three-dimensional hydrodynamic simulations. We found that a smaller planet,
with the inclination being $\sim 10^{\circ}$ -- $20^{\circ}$, can produce
kinematic features as prominent as those induced by the massive coplanar
planet. Despite the kinematic features being similar, the gap is shallower and
narrower as compared with the case in which the kinematic features are formed
by the coplanar planet. We also found that the kinematic features induced by
the inclined planet were fainter for rarer CO isotopologues because the
velocity perturbation is weaker at the position closer to the midplane, which
was different in the case with a coplanar massive planet. This dependence on
the isotopologues is distinguished if the planet has the inclined orbit. We
discussed two observed kinematic features in the disk of HD 163296. We
concluded that the kink observed at 220 au can be induced by the inclined
planet, while the kink at 67 au is consistent to that induced by the coplanar
planet.
