The high-resolution echelle spectra presented here were obtained by us during several observing runs with the 4.2 m William Herschel Telescope (WHT) at La Palma Observatory, using the Utrecht Echelle Spectrograph (UES) mounted on a Nasmith focal station. A description of the WHT/UES is given by Unger (1992). In addition, we analysed also different WHT/UES observational campaigns retrieved from La Palma Data Archive (Zuiderwijk et al. 1994).
In Table 1 (click here) we give a summary of WHT/UES observations,
for each observing run we list the date, the observer, the CCD detector,
the number of echelle orders included,
the central wavelength (
),
the wavelength range covered (
) and the range
of reciprocal dispersion achieved (/pixel) from the first to the last
echelle orders. The echelle grating used in all these runs was the E31.
The interorder spacing was too small to perform a good sky subtraction.
Sky contamination is only significant for the few faint very-late M-type
stars of this library (VB 8 and VB 10).
As can be seen in Table 1, the spectra cover
the spectral range from 4800 to 10600
with spectral resolution (
pixels) ranging
from 0.19 to 0.09 ,
corresponding to 
.
However, as the CCD chips we have used were smaller than
the echelle orders, we did not get a full recording of the different orders.
The gaps between the adjacent recorded orders got larger towards longer
wavelengths, as can be seen in
Tables 2 (click here) to 5 (click here),
where we give for each observing run the wavelength range and the
spectral lines of interest in each echelle order.
The spectra have been extracted using the standard
reduction procedures in the IRAF
package (bias subtraction,
flat-field division, and optimal extraction of the spectra).
The wavelength calibration was obtained by taking
spectra of a Th-Ar.
Finally, the spectra have been normalized by
a polynomial fit to the observed continuum.
Table 1: Summary of WHT/UES observations
(published only electronically at CDS)
Table 2: UES spectral orders (Jul.-93)
(published only electronically at CDS)
Table 3: UES spectral orders (Dec.-93)
(published only electronically at CDS)
Table 4: UES spectral orders (Apr.-94, Mar.-95, Jun.-95)
(published only electronically at CDS)
Table 5: UES spectral orders (Nov.-94)
(published only electronically at CDS)