CCD images described in the present paper were obtained with
the CASLEO 2.15 m Ritchey-Chrètien telescope, San Juan,
Argentina, and the University of Toronto Southern
Observatory (UTSO) 0.6 m reflector at Las Campanas, Chile.
In both observatories were used Tektronix CCDs with
m pixels (CASLEO) and 
m
pixels (UTSO) with image scales 11.1 and 
respectively.
CASLEO data were obtained during two runs: 1995 march 1-5
and august 22 by CJD and DLF. Images were taken under
photometric conditions and with seeing ranging between 
and 3'' (FWHM).
Imaging observations were carried out by CJD during one run
at UTSO: 1995 June 22-25. Seeing conditions were very good
) and nights were photometric.
We obtained a set of short (200-600 s) exposures for each
galaxy using BVRI filters. Photometric calibration was
achieved using observations of at least 10 standard stars
selected from
Landolt (1983). Estimates of accuracy in the
calibrations are 
mag in B, 
mag in
(B-V),
mag in (V-R) and mag in (R-I).
We have used the usual procedures for reducing images and spectra CCD frames (see Donzelli & Espındola 1996 for details). For this purpose we have used the IRAF package (developed by NOAO) and routines of our own. Table 2 (click here) summarizes observation dates, expositions and telescope used.
| Galaxy | Obs. date | B | V | R | I | Telescope |
| exp.(s) | exp.(s) | exp.(s) | exp.(s) | |||
| ESO 316-G029 | 01/03/95 |  |  |  | | CASLEO 2.15 m |
| NGC 3250E | 02/03/95 | | | | - | CASLEO 2.15 m |
| NGC 3318 | 01/03/95 | | | |
| CASLEO 2.15 m |
| NGC 3378 | 02/03/95 | | | |
| CASLEO 2.15 m |
| ESO 340-G021 | 25/06/95 |  |  |  | | UTSO 0.6 m |
| AM 2054-433 N | 22/06/95 |  | | | | UTSO 0.6 m |
| AM 2054-433 S | 22/06/95 | | | | | UTSO 0.6 m |
| IC 5325 | 26/06/95 | | |
|
| UTSO 0.6 m |
Two-dimensional spectroscopy was carried out with the REOSC
Spectrograph at CASLEO 2.15 m telescope in the runs
described above. The spectrograph has attached the same CCD
used for images. Spectra in the wavelength range of 
were taken through a slit aperture of 
long
and 
wide. We use a 300 line mm-1 grating that
implies a resolution of 3.3 Å. At least three exposures
of 600 s each were obtained for the galaxies with the slit
oriented along the major axis or in the 
direction
centered in the nucleus.
Spectra were wavelength calibrated using comparison lines from a He-Ne-Ar lamp and calibration accuracy was estimated < 15 km s-1.
At least 4 standard stars were observed each night to flux
calibrate the spectra. These stars were selected from the
Catalogue of Southern Spectrophotometric Standards
(Stone &
Baldwin 1983). We estimate an rms of 0.06 magnitudes for
residuals of the system sensitivity function fitting.
Nevertheless, relative fluxes are probably only good to
due to inaccuracies in the continuum subtraction
and deblending technique. Standard data reduction techniques
were used to process the data mainly CCDRED and LONGSLIT
packages in the IRAF package.
All spectra are corrected for galactic absorption using 
values taken from the RC3. Table 3 (click here) lists the observation
date, exposure, and slit orientation for each galaxy.
| Galaxy | Obs. Date | Exp.(s) | Slit Orientation |
| ESO 316-G029 | 04/03/95 | | E-W |
| NGC 3250E | 04/03/95 | | major axis |
| ESO 317-G041 | 05/03/95 |  | major axis |
| NGC 3318 | 04/03/95 | | E-W |
| NGC 3378 | 05/03/95 | | E-W |
| ESO 266-G015 | 05/03/95 | | major axis |
| ESO 340-G021 | 22/08/95 |  | E-W |
| AM 2054-433 N | 22/08/95 | | major axis |
| AM 2054-433 S | 22/08/95 | | major axis |
| IC 5325 | 22/08/95 | | E-W |