4 Presentation of the results

Determinations of the heliocentric radial velocity cz, of $\sigma_0$, and of $V_{\rm max}$ (together with the radius $r_{\rm max}$ of the measurement range) are listed in the last columns of Table 1. The V(r) and $\sigma(r)$ profiles are presented in Fig. 1, and also in Table 3, which is proposed in electronic form only. Following Papers III and IV, we have adopted a convention for the actual position angle PA of the spectrograph slit (as listed in Table 2): for $0<{\rm PA}<180\hbox{$^\circ$ }$, r<0 corresponds to the eastern side of the galaxy, for $180<{\rm PA}<360\hbox{$^\circ$ }$, r<0 corresponds to the western side, and for ${\rm PA}=0\hbox{$^\circ$ }$, r<0 is to the North. Tables 1 through 3 are available from the CDS.

Figure 1: Profiles of rotation velocities and velocity dispersions

Figure 1: continued

Our results are summarized as follows:

• We have measured the central velocity dispersion $\sigma_0$ for 26 early-type galaxies: these values were still unavailable for five objects. We have also determined the $\sigma(r)$ and V(r) profiles along the major axis and, for most galaxies, we have been able to measure the maximum rotation velocity $V_{\rm max}$: this parameter was still unavailable for 21 of these objects;
• We note several peculiar features. In NGC 1550, the rotation curve is unexplainably distorted; in NGC 1684, a secondary photometric peak is present at $\simeq 6''$ West of the nucleus, where the kinematic profiles are distorted; in NGC 2634, the amount of rotation at PA = $285\hbox{$^\circ$ }$, i.e. close to the minor axis, is similar to that along the major axis.

The data presented here, together whith those of the preceding papers of the series, are available in the HYPERCAT database (Prugniel et al. 1999), at http://www-obs.univ-lyon1.fr/hypercat/.

Acknowledgements

We are endebted to the telescope operators at the Observatoire de Haute-Provence for their help in collecting the data. We thank the referee, Giovanni Busarello, for his careful reading of the first version of the manuscript. We have made use of the Lyon-Meudon Extragalactic Database operated by the LEDA team. We have also made use of the ESO/ST-ECF first Digitized Sky Survey (DSS). The DSS was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166; its images are based on photographic data from the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present form with the permission of these institutions. The National Geographic Society - Palomar Observatory Sky Atlas was made by the California Institute of Technology with grants from the National Geographic Society. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory. The UK Schmidt Telescope was operated by the Royal Observatory Edinburgh, with funding from the UK Science and Engineering Research Council (later the UK Particle Physics and Astronomy Research Council), until 1988 June, and thereafter by the Anglo-Australian Observatory; plates of the Sky Atlas Equatorial Extension are from the UK Schmidt.