Other
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mcdg.proc..129d&link_type=abstract
The Magellanic Clouds and Other Dwarf Galaxies, Proceedings of the Bonn/Bochum-Graduiertenkolleg Workshop, held at the Physikzen
Other
Be-Stars, Colour-Magnitude Diagrams, Star Clusters
Scientific paper
We studied in detail the binary cluster candidates SL 538 and NGC 2006. This apparent cluster pair is located in the northwestern part of the large OB association LH 77 in supergiant shell LMC 4. A third star cluster, KMHK 1019, is located within 5' from the double cluster. We derived ages by isochrone fits to colour-magnitude diagrams (CMDs) and found that all three star clusters are (nearly) coeval which makes simultaneous formation likely, possibly all in the same giant molecular cloud. We identified Be star candidates and find the same ratio N(Be)/N(B) for the components of the binary cluster while the amount of Be stars detected in KMHK 1019 and in the surrounding field is considerably lower. Since Be stars are usually rapid rotators this may indicate intrinsically higher rotational velocities in the components of the cluster pair. Also the initial mass function (IMF) derived from the CMDs shows the same slope for both SL 538 and NGC 2006 and is consistent with a Salpeter IMF. We suggest that SL 538 and NGC 2006 are a true binary cluster.
Dieball Andrea
Grebel Eva Katharina
No associations
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