  Studies of the kinematics of gaseous halos in some spiral galaxies have shown
that the rotational velocity of the gas decreases with height above the
midplane (z). This vertical velocity gradient has been observed in both the
neutral and ionized components of halos. We present imaging Fabry-Perot Halpha
observations of the edge-on galaxy NGC 5775. These observations allow us to
study the variation in the rotation curve (and, to some extent, the radial
profile) of the ionized gas component as a function of z. We have used an
iterative technique to infer the major axis rotation curve from the ionized gas
observations as well as CO data. A preliminary analysis of position-velocity
(PV) diagrams parallel to the major axis implies the presence of a vertical
velocity gradient. The magnitude of this gradient is tentatively found to be ~2
km/s/arcsec, consistent with the results of Rand (2000) and Tullmann et al.
(2000).
