  Determining the internal kinematics of a galaxy from planetary nebulae (PN)
is usually a two step process in which the candidate PN are first identified in
a target galaxy and then, in a follow up run, spectra are obtained. We have
implemented a new technique in which two dispersed images at the wavelength of
the [OIII] emission line at 5007A are combined to yield positions, magnitudes
and velocities of the PN population in a single step. A reduction in observing
time of about a factor 2 is attainable. We present here the proof-of-principle
results.
