Computer Science
Scientific paper
Jul 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11577w&link_type=abstract
HST Proposal ID #11577. Cycle 17
Computer Science
Scientific paper
We propose to use WFC3 to provide key observations of young star clusters in "The Antennae" {NGC4038/39}. Of prime importance is the WFC3's ability to push the limiting UV magnitude FIVE mag deeper than our previous WFPC2 observations. This corresponds to pushing the limiting cluster mass from 10**5 to 10**3 solar masses for cluster ages 10**8 yrs. In addition, the much wider field of view of the WFC3 IR channel will allow us to map out both colliding disks rather than just the Overlap Region between them. This will be especially important for finding the youngest clusters that are still embedded in their placental cocoons. The extensive set of narrow-band filters will provide an effective means for determining the properties of shocks, which are believed to be a primary triggering mechanism for star formation. We will also use ACS in parallel with WFC3 to observe portions of both the northern and southern tails at no additional orbital cost. Finally, one additional primary WFC3 orbit will be used to supplement exisiting HST observations of the star-forming "dwarf" galaxy at the end of the southern tail. Hence, when completed we will have full UBVI + H_alpha coverage {or more for the main galaxy} of four different environments in the Antennae. In conjunction with the extensive multi-wavelength database we have collected {both HST and ground-based} these observations will provide answers to fundamental questions such as: How do these clusters form and evolve? How is star formation triggered? How do star clusters affect the local and global ISM, and the evolution of the galaxy as a whole? The Antennae galaxies are the nearest example of a major disk-disk merger, and hence may represent our best chance for understanding how mergers form tremendous numbers of clusters and stars, both in the local universe and during galaxy assembly at high redshift.;
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