All the material, except one spectrum, was obtained on CCD receivers at the 193 cm telescope at the Haute Provence Observatory (OHP). The spectrograph used was CARELEC (Lemaitre et al. 1990). The observational data are collected in Table 1 (click here).
| Region | Code | Date |
| 3738 - 4189 | a | 04 - 04 - 93 |
| 3896 - 4335 | b | 25 - 10 - 91 |
| 4285 - 4724 | c | 23 - 10 - 91 |
| 4698 - 5138 | d | 25 - 10 - 91 |
| 6302 - 6724 | e | 23 - 02 - 92 |
| 6973 - 7402 | f | 24 - 10 - 91 |
| 7000 - 7444 | g | 06- 04 - 93 |
| 7570 - 7990 | h | 07 -01 - 90 |
| 7570 - 7994 | i | 29 -12 - 90 |
| 7583 - 8009 | j | 29 - 10 - 91 |
| 7586 - 8027 | k | 16 - 03 - 92 |
| 7613 - 8054 | l | 07 - 04 - 93 |
| 8305 - 8726 | m | 30 - 12 - 90 |
| 8358 - 8792 | n | 31 - 03 - 93 |
| 8360 - 8776 | o | 27 -12 - 90 |
| 8365 - 8785 | p | 21 - 02 - 92 |
| 8370 - 8790 | q | 15 - 11 - 89 |
| 9010 - 9425 | r | 27 - 12 - 90 |
| 9828 - 10232 | s | 18 - 04 - 92 |
| 9837 - 10241 | t | 22 - 02 - 92 |
| 9840 - 10232 | u | 14 - 11 - 89 |
| 3925 - 8060 | v | 07 - 03 - 96 |
For 
A a grating with 1200 lines/mm, blazed at 4000 A was used, providing a
dispersion of 33 A/mm in the first order. For 
A a 1200 lines/mm grating was used,
with a blaze at 7500 A which provides in the first order a dispersion of 33 A/mm; filt er OG
590 was used to cut out the second order.
In 1989 the receiver was an RCA CCD with 
pixels (30 square microns),
providing a resolving power of 1.7 A/mm. From 1990 to 1993 the receiver was a Thomson
CCD with 
pixels, (23 square microns), providing a
resolving power of 1 A. After 1993 the receiver used was a TK 512 CCD,
with 
pixels (27 square microns). The
resolving power was about 1.2 A.
For the wavelength calibration we used Ne, Ar and He lamps. Flat field corrections
were made with a Tungsten lamp mounted in the spectrograph. The slit width used was 300
microns, corresponding to 
on the sky.
The data were reduced with the software package IHAP, developed at ESO and installed at the OHP.
The only spectrum not taken at
the OHP was obtained by Dr. D. Ballereau at the Argentinian Observatory of CASLEO, with
the 215 cm telescope, and generously loaned to the authors. The spectrograph is a REOSC type
Cassegrain, the receiver a CCD TEK, 
pixel, and the resolution 0.45 A/mm at 3700
and 0.72 at 6000 A. The reduction programs were made by M.Chauville from the Paris
Observatory.
As remarked above, the resolving power is of about one Angstroem, which is not very
well suited for radial velocity studies.The smallest equivalent width which can be measured is
of the order of 0.15 A. Since we are working with material obtained under the same conditions
as those for HD 51585 (Jaschek et al. 1996 = Paper I)
we adopt the errors given in that paper
which are of the order of 
%. Furth
ermore, the resolution prevents us also from resolving structures in the line profiles (double
lines for instance) whose separation is less than 75 km/s
in the blue and 40 km/s in the red.