  Existing long-slit spectral data for edge-on spiral galaxies suggesting that
their Diffuse Ionized Gas (DIG) halos rotate slower than their underlying disks
are summarized. An attempt to characterize lagging halos using a model of
purely ballistic disk-halo flow is discussed, with the result that the model
fails badly for the lagging halo of NGC 891, but is somewhat more successful
for NGC 5775. New two-dimensional kinematic data on the DIG halo of NGC 4302
are presented, along with a preliminary analysis of its rotation.
Two-dimensional data on NGC 5775 and a preliminary analysis of its halo
rotation is discussed by Heald et al. (this volume). The halo of NGC 4302 shows
clear signs of lagging on its approaching side, but also strong indications of
peculiar kinematics. The kinematics of the receding side are more complex.
