et al. (1989), corrected by galactic extinction (Schlegel et al. 1998) and by the extinction due to inclination (Tully et al. 1998). The same corrections were also applied to the magnitudes of the galaxies in the control samples. The velocities listed in (6) are the maximum rotational velocities obtained from the average velocity curves as shown in Fig. 1. In (7) we list vvir, the heliocentric radial velocity of the galaxy, corrected for the local group infall onto Virgo, from the Hyperleda database. The absolute magnitudes in column (8) were obtained from $M=B_{Tcor}-5*LG(vvir/75)$. Finally, in column (9) we marked with a $P$ those galaxies whose velocity fields were considered highly disturbed either by Amram et al. (2003), Plana et al. (2003) or Mendes de Oliveira et al. (1998).

The morphological types are represented in the sample in the following proportion $S0:Sa:Sb:Sc:Sd:Sm:I$=1:2:3:12:3:2:2, with preponderance of the Sc and Scd types (both counted in the Sc bin). We note that two galaxies, HCG 16c and HCG 96d, were classified as “irregular” by Hickson (1993), indicating that they had peculiar morphologies and not that they are truly irregular galaxies. The magnitudes of the galaxies ranged from $M_B$ $\sim$ –18.0 to –22.0 $+$ 5 