We observed the selected clusters with EFOSC at the Cassegrain focus of the ESO 3.6 m telescope at La Silla (30 Sept.- 2 Oct. 1989). We obtained images of the fields with EFOSC; then, we selected the objects and we prepared the masks for multi-object spectroscopy with PUMA (Soucail et al. 1987). Three masks were employed for A 3889, two masks for Cl 0053-37, and one for A 3663. Integration times were 3600 s. The finding charts of all galaxies with measured redshift are given in Figs. 1-3.
Figure 1: Cl 0053-37: finding chart (in this as in the following finding
charts, west is on the left and north is on the top).
This cluster was considered part of the ACO poor cluster S0102;
Abell et al. (1989) noticed it as a "curious linear concentration".
B is a background galaxy at 
Figure 2: A 3889: finding chart. F1 and F2 are two foreground galaxies at
; S indicates a star
Figure 3: A 3663: finding chart
The spectroscopic observations were accomplished using EFOSC in MOS mode, with the B300 grism (which gives a dispersion of 230 Å/mm). The RCA SID 006 EX Hi-Res. CCD detector (ESO CCD #8) was used in binned mode (see also Dupin et al. 1987; Giraud 1988; Soucail et al. 1988, for details on the MOS technique). The B300 grism gives a resolution of 7 Å per pixel over a spectral range between 3600 and 7200 Å; the effective range depends however on the position of the galaxy on the CCD. Spectra were wavelength calibrated using a He-Ar lamp.
Data reduction was performed using the ESO package MIDAS. Spectra were reduced in the standard way, by bias subtraction and flat-fielding of the science frame. Central columns with high S/N ratio were coadded, cosmic rays removed, then the object spectra were wavelength calibrated using a He-Ar lamp and sky subtracted. Usually for each galaxy spectrum we had a sky spectrum taken in a nearby position on the mask; when this was not the case (because of geometrical constraints on the masks in order to avoid overlapping of spectra) we used a mean sky spectrum.
As discussed by Garilli et al. (1991), cross-correlation techniques
are not so effective when spectra are obtained through
holes with EFOSC in MOS mode. To assure homogeneity of
results, for all spectra (obtained with holes or slits)
lines were identified and their centers were determined
semi-automatically using a series of MIDAS routines.
The good S/N ratio of the spectra allowed us easy identification and precise
measurements of the line centers.
At least 4 lines were used for each spectrum;
the Balmer lines (from 
to 
),
the CaII H & K lines,
the G-band, the magnesium blend B were the most common absorption features.
In Tables 2-4, for each galaxy we report
in the first column a number which allows identification
on the finding charts, in the second and third columns
right ascension and declination (J2000) as measured on
Digitized Sky Survey scans, in the fourth column
the measured heliocentric velocity, in the sixth column its internal error
(estimated as the standard deviation of the velocities of individual lines),
and in the seventh column the redshift (in the transformation from redshift
to velocity we used c = 299792.5 km s
).
| No. | RA (J2000) | DEC (J2000) | V |  | Redshift | Note |
| 1 | 00:56:10.23 | -37:34:07.9 | 51570 | 282 | 0.17202 | |
| 2 | 00:56:09.22 | -37:33:59.5 | 50799 | 51 | 0.16945 | |
| 3 | 00:56:07.07 | -37:33:49.4 | 51628 | 138 | 0.17221 | |
| 4 | 00:56:09.71 | -37:33:39.9 | 50709 | 120 | 0.16915 | |
| 5 | 00:56:01.49 | -37:33:31.6 | 49315 | 111 | 0.16450 | |
| 6 | 00:56:06.41 | -37:33:18.0 | 49754 | 154 | 0.16596 | |
| 7 | 00:55:57.50 | -37:32:51.5 | 46839 | 38 | 0.15624 | |
| 8 | 00:55:58.90 | -37:33:00.7 | 48490 | 50 | 0.16175 | |
| 9 | 00:56:02.76 | -37:33:03.9 | 49588 | 192 | 0.16541 | |
| 10 | 00:56:04.76 | -37:33:00.3 | 50394 | 117 | 0.16810 | |
| 11 | 00:56:04.75 | -37:32:51.0 | 51594 | 84 | 0.17210 | |
| 12 | 00:55:55.59 | -37:32:20.2 | 48514 | 145 | 0.16183 | |
| 13 | 00:55:56.74 | -37:32:35.4 | 49555 | 123 | 0.16530 | |
| 14 | 00:55:57.74 | -37:32:23.4 | 48256 | 101 | 0.16096 | |
| 15 | 00:55:59.32 | -37:32:35.2 | 49041 | 145 | 0.16358 | |
| 16 | 00:55:59.09 | -37:32:18.2 | 48888 | 117 | 0.16307 | |
| 17 | 00:56:01.32 | -37:32:41.9 | 50168 | 187 | 0.16734 | |
| 18 | 00:56:02.45 | -37:32:18.0 | 47381 | 138 | 0.15805 | |
| 19 | 00:56:02.41 | -37:32:05.7 | 49097 | 113 | 0.16377 | |
| 20 | 00:55:56.18 | -37:31:48.3 | 49439 | 14 | 0.16491 | |
| 21 | 00:56:09.54 | -37:31:49.0 | 49863 | 107 | 0.16633 | |
| B | 00:55:55.48 | -37:33:07.8 | 81639 | 20 | 0.27232 | [OII] 3727 Å |
| No. | RA (J2000) | DEC (J2000) | V | | Redshift | |
| 1 | 22:34:44.68 | -30:34:17.9 | 76661 | 176 | 0.25571 | |
| 2 | 22:34:46.33 | -30:33:57.5 | 73228 | 95 | 0.24426 | |
| 3 | 22:34:48.37 | -30:34:19.6 | 78120 | 108 | 0.26058 | |
| 4 | 22:34:50.24 | -30:34:07.7 | 74723 | 260 | 0.24935 | |
| 5 | 22:34:50.80 | -30:34:17.9 | 74479 | 304 | 0.24844 | |
| 6 | 22:34:55.87 | -30:34:13.7 | 76804 | 121 | 0.25619 | |
| 7 | 22:34:54.62 | -30:33:56.7 | 74623 | 85 | 0.24892 | |
| 8 | 22:34:54.42 | -30:33:51.0 | 76641 | 81 | 0.25565 | |
| 9 | 22:34:53.34 | -30:33:42.5 | 73741 | 111 | 0.24597 | |
| 10 | 22:34:54.03 | -30:33:42.3 | 76679 | 69 | 0.25577 | |
| 11 | 22:34:57.43 | -30:33:37.8 | 76210 | 118 | 0.25421 | |
| 12 | 22:34:52.05 | -30:33:28.7 | 74660 | 177 | 0.24904 | |
| 13 | 22:34:51.79 | -30:33:21.9 | 72590 | 107 | 0.24213 | |
| 14 | 22:34:52.32 | -30:32:44.5 | 76696 | 210 | 0.25583 | |
| 15 | 22:34:49.97 | -30:32:18.9 | 75003 | 161 | 0.25018 | |
| 16 | 22:34:50.61 | -30:32:24.0 | 75283 | 53 | 0.25112 | |
| 17 | 22:34:51.01 | -30:32:18.1 | 73928 | 150 | 0.24660 | |
| 18 | 22:34:55.22 | -30:31:53.5 | 74498 | 200 | 0.24850 | |
| 19 | 22:34:47.59 | -30:31:56.8 | 74962 | 139 | 0.25005 | |
| 20 | 22:34:48.87 | -30:31:46.2 | 76783 | 264 | 0.25612 | |
| 21 | 22:34:45.22 | -30:31:38.1 | 74932 | 151 | 0.24995 | |
| 22 | 22:34:46.54 | -30:31:39.8 | 73734 | 172 | 0.24595 | |
| 23 | 22:34:45.77 | -30:31:09.8 | 74692 | 300 | 0.24915 | |
| 24 | 22:34:50.36 | -30:30:47.1 | 76923 | 420 | 0.25659 | |
| F1 | 22:34:50.22 | -30:32:01.9 | 33306 | 148 | 0.11110 | |
| F2 | 22:34:54.20 | -30:31:16.1 | 32862 | 124 | 0.10962 |
| No. | RA (J2000) | DEC (J2000) | V | | Redshift | Note |
| 1 | 20:07:12.44 | -52:36:09.5 | 69709 | 240 | 0.23252 | [OIII] doublet |
| 2 | 20:07:11.49 | -52:35:50.1 | 74040 | 274 | 0.24700 | |
| 3 | 20:07:13.76 | -52:35:27.5 | 72886 | 534 | 0.24312 | |
| 4 | 20:07:06.26 | -52:34:31.0 | 73222 | 189 | 0.24424 | |
| 5 | 20:07:18.47 | -52:33:33.9 | 70035 | 234 | 0.23361 | [OII] 3727 Å |
| B | 20:07:16.75 | -52:34:52.3 | 100076 | 573 | 0.33382 | [OII] 3727 Å |
To test the reliability of our data, we also used the
cross-correlation task XCSAO in IRAF to measure radial velocities
for a few randomly chosen galaxy spectra, adopting two spectra
of K stars as templates. The results are consistent with the
redshifts obtained by line identification.
Furthermore, a comparison of the redshifts
from two spectra of the same galaxy observed in two successive runs
gives a difference of 20 km s, well below the quoted errors.