Establishing the Metallicity Distribution in Normal Giant Ellipticals

Details Establishing the Metallicity Distribution in Normal Giant Ellipticals Establishing the Metallicity Distribution in Normal Giant Ellipticals

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9811h&link_type=abstract

HST Proposal ID #9811

Mathematics

Logic

Hst Proposal Id #9811 Stellar Populations

Scientific paper

NGC 3377 and 3379, the Leo Group ellipticals at d=11 Mpc, are the nearest E galaxies commonly regarded to be structually"normal", and as such, they are keystone objects for understanding the evolution and early star formation history of large ellipticals. The ACS/WFC camera now gives us the ability to obtain the metallicity distribution function {MDF} of their stellar population by direct resolution and photometry of their halo stars. To do this, we will follow the same highly successful techniques we have previously used for NGC 5128 with WFPC2 {V, I} imaging: the {V-I} colors of the brightest red-giant stars are highly sensitive to metallicity, and their locations in the color-magnitude diagram can be used for direct construction of the MDF. This will be a major step forward to understanding the formation history of these cosmologically dominant galaxies.

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