from the 2-D maps extend beyond the long-slit ones, which is also another reason for the discrepant values of derived V$_{max}$, using these two different techniques, Fabry-Perot or long-slit. We should have in mind, however, that an over/underestimation of the inclination leads to an over/underestimation of the extension of the rotation curves.

Another point we should note is that the rotation curves derived by Fabry-Perot spectroscopy are much more well behaved in the sense that more often the two sides of the curves approximately agree and they are either flat or rising in the last measured point. In fact, we have no example of galaxy with a rotation curve that drops in both sides as one would expect in the Keplerian case.

Results
=======

Table 1 summarizes the main parameters for each galaxy. In columns (1) and (2) we show the identification and length of semi-major axis of the galaxy as given by Hickson (1993). The morphological classification for the galaxies taken from Hickson (1993) and from NED are given in columns (3) and (4) respectively . The values for the total B magnitudes of the galaxies, listed in column (5), B$_{Tcor}$, were obtained from the B$_T$ listed in Hickson 