  We report on a detailed kinematic study of the galactic-scale outflow in the
Seyfert galaxy NGC 2992. The TAURUS-2 Imaging Fabry-Perot Interferometer was
used on the Anglo-Australian 3.9-m telescope to derive the two-dimensional
velocity field of the Halpha-emitting gas over the central arcminute of NGC
2992. The complete two-dimensional coverage of the data combined with simple
kinematic models of rotating axisymmetric disks allows us to differentiate the
outflowing material from the line-emitting material associated with the
galactic disk. The kinematics of the disk component out to R = 3.0 kpc are well
modeled by pure circular rotation. The outflow component is distributed into
two wide cones with opening angle of 125 -- 135 degrees and extending 2.8 kpc
(18") on both sides of the nucleus at nearly right angles to the disk kinematic
major axis. The outflow on the SE side of the nucleus is made of two distinct
kinematic components interpreted as the front and back walls of a cone. The
azimuthal velocity gradient in the back-wall component reflects residual
rotational motion which indicates either that the outflowing material was
lifted from the disk or that the underlying galactic disk is contributing
slightly to this component. A single outflow component is detected in the NW
cone. The most likely energy source for this outflow is a hot bipolar thermal
wind powered on sub-kpc scale by the AGN and diverted along the galaxy minor
axis by the pressure gradient of the ISM in the host galaxy. The data are not
consistent with a starburst-driven wind or a collimated outflow powered by
radio jets. (abridged)
