[Previous] | [Session 40] | [Next]
E.K. Grebel (U. Wash)
Comparative properties of young star clusters in the Magellanic Clouds are discussed. The isochrone-based age distribution of about 200 young star clusters in the Small Magellanic Cloud shows a pronounced peak at ~100 Myr and a second, smaller peak at ~200 Myr, similar to the broad peak around 100--200 Myr in the age distribution of LMC clusters. N-body simulations suggest that the last close LMC/SMC encounter was ~200 Myr ago, and that the last perigalacticon occurred ~100 Myr ago, coincident with the common peaks in the cluster age distribution. The enhanced cluster formation rate been triggered by these events. The implications of the absence of an SMC cluster age concentration at log(t)~9.1 as seen in the LMC are discussed. The cluster formation rate is compared to the field star formation rate in both Clouds.
If the author provided an email address or URL for general inquiries, it is a
s follows:
http://www.astro.washington.edu/grebel/