Our present sample consists of 38 early-type galaxies, with ellipticals and
lenticulars in roughly equal proportions. This set adds up to the 21-object
sample of Paper I; there are four objects in common (NGC 2329, NGC 2332,
NGC 4434 and UGC 3696), whose new measurements
have been included in the present work for comparison purposes. Relevant
catalog elements are presented in Table 1 (click here). The Es have
ellipticities corresponding to classes between 
E0 and E4,
and the S0s are moderately to highly flattened. The distances are in the range
of 
to 
Mpc (for 
). The absolute magnitudes are intermediate (-21.8 < MB < -17.3).
Notes:
Col. (2): morphological type (from the LEDA database);
Cols. (3), (4): coordinates;
Col. (5): 
, heliocentric radial velocity, in kms-1
(from LEDA);
Col. (6): 
, integrated blue magnitude, corrected for Galactic
extinction and k term (as calculated by Prugniel & Simien 1997,
hereafter PS97; except for NGC 2332 and UGC 3792, for which is from LEDA);
Col. (7): -MB, absolute B magnitude (for a distance modulus from PS97,
corresponding to );
Col. (8): 
, effective radius (from PS97), in arcsec;
Col. (9): 
, ellipticity;
Col. (10): PA, position angle of major axis, in degrees (North through East);
Col. (11): reference for and PA, 1= Djorgovski (1985),
2= Michard (1985), 3= LEDA;
Col. (12): 
, central velocity dispersion available in the literature,
from an updated version of the compilation in PS96 (excluding all previous measurements by ourselves),
in kms-1;
Col. (13): 
, maximum rotation velocity available in the
literature, from PS96 (same remarks as for ), in kms-1.
Table 1: Catalog elements
The observations have been secured at the 1.93-m telescope of the
Observatoire de Haute-Provence, equipped with the CARELEC long-slit
spectrograph. In March and June 1995, two observing runs totalling 12 nights
collected spectra on the major axis of the galaxies.
The atmospheric conditions were variable, with a seeing disk between
2'' and 3.5'' (FWHM) for most objects, but up to 
for three of
them. The log of the observations is given in Table 2, which is proposed
in electronic form only.