SPATIAL-DISTRIBUTION OF STELLAR MASS IN THE LARGE MAGELLANIC CLOUD STAR-CLUSTERS

The stellar mass distributions have been studied in halo regions (radi us ranging from approximately 19 to 94 arcsec) of 5 young Large Magell anic Cloud star clusters. Effects of mass segregation have been observ ed in only NGC 1711. A comparison of cluster age with its relaxation t ime indicates that the observed mass segregation could have taken plac e at the time of star formation. Absence of mass segregation in most o f the clusters may indicate that there is generally no spatial prefere nce for the formation of massive stars. Most of the clusters have simi lar spatial density profiles which follow a power law with indices alm ost-equal-to 3.5. This may indicate slow, but efficient process of sta r formation in the young star clusters of the Large Magellanic Cloud.