Institution(s): 1. University of Virginia
The Magellanic Clouds offer the opportunity to study star formation at reduced metallicity with no distance ambiguity and minimal line-of-sight confusion. They are arguably unique in that it is observationally tractable to analyze entire galaxies (e.g. our surveys with Spitzer and Herschel) simultaneously with critical subparsec physics, especially using ALMA and HST (1"~0.25pc). I will discuss the effects of the massive cluster R136 on star formation within 100pc in 30 Doradus, and on the formation of new star clusters in N159, a separate region 600pc to the south. These represent two different evolutionary states: 30 Doradus a more evolved cluster in which current star formation has potentially been significantly affected by the previous generations, and N159 a significantly younger region in which massive clusters may still form in the future. Cluster-forming clumps near R136 analyzed with ALMA contain both massive YSOs and low-mass pre-main-sequence stars revealed by HST. Although diffuse molecular gas is photodissociated, the cluster-forming clumps do not have dramatically different properties from parsec-sized clumps in less active Milky Way regions. Cluster-forming clumps and filaments in N159 also contain a rich pre-main-sequence population which we can now relate to the clump-scale dense gas distribution.