Spectroscopy for 58 Be stars in eight open clusters is presented with
measurements of FWHM, 
and values of
EW from H
to H
. This is complemented by the
contemporary photometric data of Paper I. In order to preserve the homogeneity
of the sample, a first examination of the results has been made showing a good
agreement with earlier results of other authors based on higher resolution
data. The spectroscopic behavior of Be stars in clusters is, within our
limited resolution, similar to that of field Be stars. We also present, the
measured EW for the regular B stars also included in our sample.
Our data are in agreement with the relation given by
Dachs et al. (1986), and
slightly modified by Hanuschik et al. (1988), between full widths at half
maximum and equivalent widths (Eq. 2). The data are consistent as well with the
previous finding of some preference for 
(Eq. 5) therefore
placing the rotation field somewhere between the cases of angular momentum
conservation and keplerian, as well as with the already known fact that the
higher the member of the series, the closer it arises to the central star.
Some stars will be rejected in future work: non members of clusters,
members with uncertain values of reddening, Herbig Ae/Be type objects, Blue Stragglers, etc.
Furthermore, we will divide the sample into early Be, late Be and Shell type
objects since some differences seem to exist between their physical
characteristics (Paper I, Slettebak et al. 1992).
Figure 1: 
, 
and 
for stars in NGC 457. Flux has been normalized to continuum level.
Figure 2: 
and 
for stars in NGC 457. HeI is also visible.
Figure 3: a,b) 
, 
and 
for stars in NGC 663.
Figure 4: a,b) 
for stars in NGC 663.
Figure 5: 
and
for stars in
NGC 663. HeI is also visible.
Figure 7: 
, 
and
for Pleiades. Besides the star
number, the date of observation is shown.
Figure 8: 
and
for Pleiades. HeI is also visible.
Figure 9: 
, 
and 
for star 157 in NGC 2323.
Figure 10: 
, 
and 
for stars in NGC 2422.
Figure 11: 
, 
and 
for stars in NGC 7654.
Figure 12: 
and 
for stars in NGC 7654. HeI is also visible.
Figure 13: 
, 
and 
for stars in Cep OB3.
Figure 14: 
for stars in Cep OB3.
Figure 15: Full width at
half maximun for emission lines
vs. equivalent width. Dotted line and
dashed line represent the relationships
for the whole sample and the early type
Be stars respectively. Open circles are
early type Be stars and solid circles
are late type Be stars
Figure 16: Full width at half maximun for
, 
and
emission lines vs. 
.
Dotted lines represent the relationship for
the whole sample while dashed lines
represent the relationship for single
peaked profiles. Open circles and solid
circles represent stars which show single
peaked and double peaked profiles
respectively in our spectra
Figure 17: Velocity
peak separation vs. equivalent width for
Acknowledgements
We would like to acknowledge V. Reglero and J. Busquets for their help with the observations, and B. Payne for his careful reading of the manuscript. The useful suggestions made by the referee Dr. R. Hanuschik helped us to improve the presentation of the paper. We also thank the staff of the Calar Alto Observatory for the kind assistance during the observations. Software and data analysis facilities were provided by Starlink, which is founded by the UK PPARC. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. S.A. acknowledges a research grant from the Conselleria d'Educació i Ciència, Generalitat Valenciana. J.M.T. acknowledges a research grant from the Instituto de Estudios Turolenses (CSIC).
, 
and 
for h & 
Per.