Long-slit spectroscopy is entering an era of increased spatial and spectral
resolution and increased sample size. Improved instruments reveal complex:
velocity structure that cannot be, described with a one-dimensional rotati
on curve, yet samples are too numerous to examine each galaxy in detail. Th
erefore, one goal of rotation curve measurement techniques is to flag cases
in which the kinematic structure of the galaxy is more complex than a sing
le-valued curve.
We examine cross-correlation as a technique that is easily automated and wo
rks for low signal-to-noise spectra. We show that the technique yields well
-defined errors which increase when the simple spectral model (template) is
a poor match to the data, flagging those cases for later inspection.
We compare the technique to the more traditional, parametric technique of s
imultaneous emission-line fitting. When the line profile at a single slit p
osition is non-Gaussian, the techniques disagree. For our model spectra wit
h two well-separated velocity components, assigned velocities from the two
techniques differ by up to similar to 52% of the velocity separation of the
model components. However, careful use of the error statistics for either
technique allows one to flag these non-Gaussian spectra.