  We compare the CO(1-0) and H$\alpha$ kinematics in 34 nearby galaxies,
selected from the ALMaQUEST and EDGE-CALIFA surveys. We use 3-D Barolo, a 3D
tilted ring model, to derive the CO and H$\alpha$ rotation curves. Before
comparing rotation curves in the 34 nearby galaxies, we found systematics
between the MaNGA and the CALIFA data using eight MaNGA-CALIFA overlapping
galaxies. We assume the rotation curves based on the MaNGA data are accurate
and made the corresponding correction to the CALIFA data. Our result shows that
$\sim$56% (19/34) of our galaxies present slower H$\alpha$ rotation curves
compared to the CO rotation curves, with a median value of 6.5 km/s. The
remaining galaxies (15/34) show consistent CO-H$\alpha$ rotation velocity
within uncertainties. As a result, the Ha rotation may underestimate the total
dynamical mass by ~6% for a circular velocity of 200 km/s (the median value in
our sample). Furthermore, the velocity difference between the CO and H$\alpha$
rotation velocity is found to correlate with the velocity dispersion difference
between CO and H$\alpha$, suggesting that the gas pressure plays a role in the
velocity discrepancy. After incorporating the effect of pressure support due to
the turbulent gas motion to our sample, the median value of the velocity
differences decreases to 1.9 km/s, which in turn reduces the underestimation of
dynamical mass to $\sim$2%. Finally, we also investigate the role that the
extra-planar diffuse ionized gas (eDIG) plays in the CO-H$\alpha$ velocity
discrepancy.
