4. Presentation of the results

Determinations of the heliocentric radial velocity , of , and of (together with the corresponding radius ) are listed in Table 3 (click here). The V(r) and profiles are presented in Fig. 1 (click here), and also in Table 4, which is proposed in electronic form only. Beginning with the present paper, we adopt for the position angle PA the following convention: for , r<0 corresponds to the eastern side of the galaxy, for , r<0 corresponds to the western side; and for , r<0 is to the North. Tables 1 (click here) through 4 are available from the CDS.

    
Figure 1: Profiles of rotation velocities and velocity dispersions

Our results are summarized as follows:

• We have measured the central velocity dispersion for 24 E and S0 galaxies.
• For 21 galaxies in our sample, we have been able to determine the and V(r) profiles along the major axis and, for five of them, along the minor axis as well. For 12 of these objects, the profiles extend beyond the effective radius. Whenever possible (for 17 galaxies), we have determined the maximum rotation velocity : this parameter was still unavailable for six of these objects.
• For a few galaxies, we note secondary peaks in the velocity dispersion, which are likely the result of a strongly non-gaussian LOSVD (line-of-sight velocity distribution); the most striking example is NGC 2768.

   

(1) (2) (3) (4) (5)

N0499 12

N0584 25

N0680 15

N0890 20

N0990 10

N1016 ...

N1023 55

N1060 ...

N1175 22

N1209 18

N1521 10

N1573 ...

N1653 12

N1726 20

N2314 15

N2340 20

N2549 35

N2685 35

N2732 31

N2768 72

N7332 38

N7457 22

N7778 15

N7785 22

Notes:
column (2): , heliocentric radial velocity, in kms^-1;
column (3): , central velocity dispersion, in kms^-1;
column (4): , maximum rotation velocity, in kms^-1;
column (5): , the radius at which has been measured, in arcsec.

Acknowledgements

We are indebted to the telescope operators at the Observatoire de Haute-Provence for their continuous support. We are pleased to thank B. Germain for his help during one of the observing runs, G. Rau for his search of the archives, and G. Busarello, the referee, for his comments. We have made use of the Lyon-Meudon Extragalactic Database supplied by the LEDA team.