A catalogue of galaxies up to magnitude 
has been built applying the
algorithms described in Slezak et al. (1988) to automatic scans of
POSSII plates, thanks to the MAMA facilities;
this catalogue included the coordinates of galaxies within
a radius of one degree from each cluster centre.
Selected galaxies have been observed
at the 193 cm telescope of the Observatoire de Haute-Provence, using the
Carelec spectrograph in long slit mode (Lemaitre et al. 1990).
The choice of the grating represented a compromise between good resolution and reasonable exposure time, and was also constrained
by the wavelength range suited for
line identification at low-redshift (
.
The dispersion was 260 Å/mm,
corresponding to 
Å/pixel with the CCD TK512 
pixels of
m), and with the slit aperture of 1 '' the spectral resolution was
8 Å.
The following results are based on four observing
runs (7 nights each one) in April and September 1993,
and in April and May 1994.
Unfortunately more than half of the nights were lost for bad weather
conditions.
The exposure time was 45 minutes; two exposures were taken for faint objects. Wavelength calibrations were done using an He lamp and an Ar lamp before each exposure. Standard stars were observed each night (HD 102494, HD 171232, HD 112299, HD 140913). We obtained the spectra of about 8/10 objects per night. Usually we obtained one spectrum per exposure, but in some cases, for instance when sampling the core of rich clusters, we rotated the spectrograph in order to get simultaneously the spectra of a few objects. At the end, we have collected 93 spectra with a sufficient signal-to-noise ratio to allow a good redshift determination. Data reduction was carried out with IRAF, using the MULTIRED package. MULTIRED is an integrated multi-slit spectra reduction task (Le Fèvre et al. 1995) which allows to process raw 2D spectra CCD frames (with one or several spectra) into bias/flat/sky corrected 2D spectra and wavelength calibrated 1D spectra. Radial velocities have been determined using the cross-correlation technique (Tonry & Davis 1979) implemented in the RVSAO package (developed at the Smithsonian Astrophysical Observatory).
Finding charts for each cluster are displayed in Fig. 1 (click here). They cover
square regions extracted
from the Space Telescope Science Institute Digital Sky Survey
around the position of the cluster in the Abell/ACO
catalogue (
for A1413, A1781 and A2457).
An identifying number is displayed to the right of each target.
Figure 1: a) to l): Finding charts for our nearby sample of clusters:
a) A195, b) A1035, c) A1045, d) A1126, e) A1413,
f) A1468, g) A1781, h) A1831, i) A2034, j) A2245,
k) A2312, l) A2457.
These frames are extracted from the Digital Sky Survey
Velocity measurements are listed in Table 1 (click here). The columns are as follows:
Column (1): Abell cluster number (Abell et al. 1989);
Column (2): identification number of each target galaxy in
the cluster as shown in the finding charts; Columns (3) and (4): right
ascension and declination (J2000.0) of the target galaxy;
Column (5): best estimate of the radial velocity resulting from
the cross-correlation technique;
Column (6): estimated error;
Column (7): other published measurement of the radial velocity.
The subscript 
indicates that
the measurement refers to the emission line velocity.
Table 1: Heliocentric redshifts for galaxies
Table 1: continued
