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2 Sample and observations

Our present sample consists of 24 early-type galaxies, with 20 ellipticals and four S0s, and one spiral. There is only one object in common with the preceding papers of the series: NGC 4318, which appeared in Paper II; this duplicate measurement has been included in the present work for comparison purposes. Relevant catalog elements are presented in the first 10 columns of Table 1. The Es have ellipticities corresponding to classes between $\simeq$ E1 and $\simeq$ E5, and the S0s are moderately to highly flattened. The distances are in the range of $\simeq 10$ to $\simeq 74$ Mpc (for $H_0={\rm 75 \, km \, s^{-1} \, 
Mpc^{-1}}$). These objects are intrinsically bright (-22.0< MB < -18.0), except for NGC 4239 and NGC 4318, which are significantly fainter.

The observations have been secured at the 1.93-m telescope of the Observatoire de Haute-Provence, equipped with the CARELEC long-slit spectrograph. The selected setup provided a spectral range of either $\simeq 900$ Å (with a dispersion of 1.8 Å per pixel at $\lambda=5200$ Å, i.e. 104 km s-1), or $\simeq 450$ Å (with a dispersion of 0.9 Å per pixel, i.e. 52 km s-1). The slit width, projected onto the plane of the sky, was 2.2''.

In February, October, November 1992, and in March 1993, four observing runs totalling nine clear nights allowed us to collect one or two spectra on these 25 galaxies. For 20 of them, the slit was positioned on the major axis. For NGC 2872, paired with the spiral NGC 2874, the slit was oriented along the direction linking the two objects, and we included the central velocity dispersion of NGC 2874 in Table 1. For IC 4051, NGC 2476, and NGC 3605, the adequate PA values were unfortunately missing in our files, and we adopted either arbitrary values (0 or $90^\circ $), or old, unaccurate determinations.

The atmospheric conditions were variable, with a seeing disk between 1.5'' and 3.5'' (FWHM) for most objects, but up to $\simeq 6''$ for three of them. The log of the observations is given in Table 1, which is proposed in electronic form only.


  
Table 1: Catalog elements and kinematical results

\begin{tabular}
{l@{\hspace{0.2cm}}r@{\hspace{0.3cm}}r@{\hspace{0.3cm}}
 r@{\hsp...
 ...8 \pm 32 $\space & $ 105 \pm 29 $\space & 
$ 10 $\space \\  
\hline\end{tabular}
Notes. Col. (2): morphological type (from the LEDA database - status: LEDA1996); Cols. (3), (4): coordinates, from Prugniel & Simien (1997: hereafter PS97), except for NGC 2874 (from LEDA); Col. (5): $B_{\rm T}$, integrated blue magnitude, corrected for Galactic extinction and k term (from PS97, except for NGC 2874 and NGC 3245: from LEDA); Col. (6): MB, absolute B magnitude (for a distance modulus from PS97, corresponding to $H_0={\rm 75 \, km \, s^{-1} \, 
Mpc^{-1}}$; except for NGC 2874 and NGC 3245: from LEDA); Col. (7): $r_{\rm e}$, effective radius, in arcsec (from PS97, except for NGC 2874 and NGC 3245: from Prugniel & Héraudeau 1998); Col. (8): $\epsilon$, ellipticity; Col. (9): PA, position angle of major axis, in degrees (North through East, to $180\hbox{$^\circ$}$); Col. (10): reference for $\epsilon$ and PA, 1= Djorgovski (1985), 2= Michard & Marchal (1993), 3= LEDA; Col. (11): $v_{\rm hel}$, heliocentric radial velocity, in kms-1; Col. (12): $\sigma_0$, central velocity dispersion, in kms-1; Col. (13): $V_{\rm max}$, maximum rotation velocity, in kms-1 (the > sign indicates that the rotation is still rising at the outermost point, or that the PA of the slit was inclined with respect to the major axis); Col. (14): $r_{\rm max}$, the radius at which $V_{\rm max}$ was measured, in arcsec.


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