2 Observations

The observations have been performed with the 2.5 m DuPont telescope at the Las Campanas Observatory, Chile, during the nights of 7-9 December, 1996. The multi-fiber spectrograph from Shectman (1989) has been used. The field of view is $1.5\times1.5$ degree. The aperture size of each fiber is 2 arcsec in diameter on the sky. The fibers were connected with a Boller & Chivens spectrograph coupled to a 2DFrutti detector (2DF). With a blaze angle of $9^\circ45\hbox{$^\prime$}$ we got a spectral range of 3800 Å - 6800 Å. The spectra are projected to a $1520\times1024$ pixel area, with a dispersion of $\simeq$ 2-3 Å$\cdot$pixel^-1 and a final resolution of $\simeq$5 Å.

From our catalog 125 galaxies brighter than V = 20.0 mag were selected. Accurate positions have been obtained by using reference stars from the Guide Star Catalog. Astrometric solutions yielded positions with accuracies better than $0\hbox{$.\!\!^{\prime\prime}$}3$.In addition, three bright dE, Ns have been included from the FCC (Ferguson 1989), namely FCC 188, FCC 222, and FCC 274. Their positions are not as accurate as those of the CCD sample. Small positional deviations for these objects resulted in quite low signal-to-noise spectra despite the high central surface brightnesses of their nuclei. The whole sample was divided in two sets of positions in order to avoid overlaps in the fiber configuration. In spite of this, 13 positions could not be taken. About 20 to 30 fibers per set were positioned as sky fibers to random positions in the field. The integration times of the first and second set were 4 hours and 4.5 hours respectively. For the wavelength calibration comparison HeNe spectra have been obtained at the two positions before and after the long integrations. Additionally, long flatfield exposures have been taken. We have chosen different grating angles between $8\hbox{$^\circ$}45\hbox{$^\prime$}$ and $10\hbox{$^\circ$}45\hbox{$^\prime$}$ to get an homogenous illumination of the whole spectral range.