Abundance Results from the Las Campanas Observatory and McDonald Observatory High-Resolution Metal-Poor Star Survey

Details Abundance Results from the Las Campanas Observatory and McDonald Observatory High-Resolution Metal-Poor Star Survey Abundance Results from the Las Campanas Observatory and McDonald Observatory High-Resolution Metal-Poor Star Survey

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715403r&link_type=abstract

American Astronomical Society, AAS Meeting #217, #154.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We have undertaken a survey to collect high-resolution and high S/N spectra for more than 300 metal-poor stars. The majority of our sample was selected from the HK Survey of Beers, Preston, and Shectman, and nearly all stars with estimated [Fe/H] < -2.5 have been observed with the MIKE spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory. Additional metal-poor targets were selected based on their kinematic properties and observed with the Tull spectrograph on the Smith Telescope at McDonald Observatory. Previous abundance analyses based on high-resolution and high S/N spectra have been performed for only about 20% of the sample. While this sample naturally allows us to reconfirm and expand upon previously-detected low metallicity abundance trends and identify new stars with unique abundance signatures, its real power is the ability to probe chemical dispersion in abundance ratios. We exploit this attribute by performing line-by-line differential abundance analyses for many elements in large numbers of stars at a single metallicity and evolutionary state. This allows us to assess the evolution of the cosmic scatter of the chemistry of the ISM at very early times in the halo of the Galaxy. Generous funding has been provided by the U.S. National Science Foundation (grant AST 09-08978 to C.S.).

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