Astron. Astrophys. Suppl. Ser. 134, 489-503
S.C. Keller - P.R. Wood - M.S. Bessell
Send offprint request: S.C. Keller
Mount Stromlo & Siding Spring Observatories, Private Bag, Weston Creek PO, ACT 2611,
Australia
e-mail: stefan@mso.anu.edu.au, wood@mso.anu.edu.au, bessell@mso.anu.edu.au
Received May 26; accepted August 27, 1998
We present the results of a search for Be stars
in six fields centered on the
young clusters NGC 330 and NGC
346 in the SMC, and NGC 1818, NGC 1948,
NGC 2004
and NGC 2100 in the LMC.
Be stars were identified by differencing R band and
narrow-band H CCD images.
Our comparatively large images provide
substantial Be star populations both
within the clusters and in their
surrounding fields. Magnitudes, positions
and finding charts are given for the
224 Be stars found. The fraction of Be
stars to normal B stars within each
cluster is found to vary significantly
although the average ratio is similar to
the average Be to B star ratio found in
the Galaxy. In some clusters, the Be
star population is weighted to magnitudes
near the main sequence turn-off. The
Be stars are redder in V-I than
normal main-sequence stars of similar
magnitude and the redness increases with
increasing H
emission
strength.
Key words: stars: emission-line -- stars: Be -- galaxies: clusters -- galaxies: Magellanic Clouds
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