  We have undertaken a pilot project to measure the rotation velocities of
spiral galaxies in the redshift range 0.18 < z < 0.4 using high dispersion long
slit spectroscopy obtained with the Palomar 5m telescope. One field galaxy and
three cluster objects known to have strong emission lines were observed over
wavelength ranges covering the redshifted lines of [OII], CaII K, H beta, and
[OIII]. Two of the objects show extended line emission that allows the tracing
of the rotation curve in one or more lines. A line width similar to that
obtained with single dish telescopes for the 21-cm HI line observed in lower
redshift galaxies can be derived from the observed H beta, [OII], and [OIII]
emission by measuring a characteristic width from the velocity histogram. These
moderately distant galaxies have much stronger emission lines than typical
low-redshift spirals but they appear to be kinematically similar. Application
of the Tully-Fisher relation suggests that the two galaxies with rotation
curves are intrinsically brighter at R-band than nearby galaxies.
