along the major axis which made the rotation curve symmetric or as symmetric as possible (with similar amplitudes for the receding and approaching sides). This freedom with the Fabry-Perot data was, in fact, one reason why it was possible to construct fairly well behaved rotation curves even when the velocity maps were highly peculiar due to localized non-circular motions. The values for $\vert$$\Delta_{kin-cont}$$\vert$ varied from zero to six arcseconds.

Our conclusion is that the velocity fields of compact group galaxies are, in several cases, significantly affected by non-circular motions, local asymmetries and misalignments between the kinematic and stellar axes. A fine tuning of map parameters (center, inclination and position angle of the velocity fields) and an average of the velocities over a large sector of the galaxy are needed to derive reliable rotation curves and representative values of V$_{max}$.

A few other comparisons with data from R1991 and N2000 are exemplified in Fig. 3. In all cases we plot rotation curves resulting from a cut through the Fabry-Perot data, using the parameters given by the author’s (photometric parameters). An important point becomes clear when inspecting Fig. 3, especially Figs. 3a, 3b and 3f. In these cases the rotation curves derived 