Computer Science
Scientific paper
Jul 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9396w&link_type=abstract
HST Proposal ID #9396
Computer Science
Hst Proposal Id #9396
Scientific paper
Massive young star clusters are found in large numbers within the mergers of massive, gas-rich disk galaxies. The most outstanding and well studied case is in the nearby merging Antennae pair {Whitmore and colleagues}. These systems may give us our best hope to see directly the way in which globular clusters formed in the uniquely gas-rich protogalactic era of the universe. But, even in the Antennae, the many hundreds of young clusters have a median mass which is still 5 to 10 times smaller than the characteristic mass 3 * 10^5 M_odot that characterizes normal, old-halo globular clusters. To find objects closer to the mass range of ``true'' protoglobular clusters, we need mergers which are still more gas-rich than the Antennae and in which the gas has been collected into more massive GMCs. Two excellent candidates are Arp 220 and Arp 299, both of which are undergoing extremely high star formation rates and have > 10^10 M_odot of molecular hydrogen compressed into their central few kpc. With the ACS High Resolution Camera we will obtain deep UBVI imaging of the active central regions of these galaxies, allowing us to trace the luminosities, colors, masses, and ages of the young star clusters within them.
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