The last decade has witnessed an almost explosive growth in the availability of global parameters on early-type galaxies. Photometric and kinematical data on large samples of objects, for example, have led to the discovery of the Fundamental Plane (herafter FP): Faber et al. (1987), Djorgovski & Davis (1987). Since these pioneering works, many more observations have been carried out, either to complete statistically significant samples, or to get better measurements on parameters already available; it should be stressed, indeed, that several subtle physical effects related to the FP barely emerge from the measurement errors, and that their study requires the best possible data.
For the kinematics, the main parameter concerned is still the central velocity
dispersion 
, which accounts for most of the kinetic energy. It is
clear from recent compilations (McElroy 1995; Prugniel &
Simien 1996, hereafter PS96) that its availability is growing, and
that its accuracy is improving.
Recent studies have shown that the role of the rotation, although hardly
dominating in most early-type galaxies, has nevertheless a statistical
significance in the global scaling relations (Busarello et al.
1992; Prugniel & Simien 1994, herafter PS94;
Bender et al. 1994; D'Onofrio et al. 1995a;
Prugniel & Simien 1995). The surveys of the literature show
that measurements of the maximum rotation 
are available on a
modest proportion of early-type galaxies for which 
is known,
although there has been many very recent contributions dealing with more
than a dozen objects (e.g., Bender et al. 1994; Carollo
& Danziger 1994; Fried & Illingworth 1994;
Longo et al. 1994; PS94; D'Onofrio et al. 1995b;
Fisher et al. 1995; Seifert & Scorza 1996).
In PS94 and PS96, we have started to present our measurements of 
and
, as part of the data we have used in our study on kinematical
and stellar-population effects related to the FP. In this paper, we
present the central velocity dispersion for 21 objects, and profiles
of 
and V(r) for 18 objects.
Table 1: Catalog elements
