The Chemical Abundances of New Extremely Metal-Poor Giants with [Fe/H] < -3.0

Details The Chemical Abundances of New Extremely Metal-Poor Giants with [Fe/H] < -3.0 The Chemical Abundances of New Extremely Metal-Poor Giants with [Fe/H] < -3.0

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21925213r&link_type=abstract

American Astronomical Society, AAS Meeting #219, #252.13

Astronomy and Astrophysics

Astrophysics

Scientific paper

Extremely metal-poor (EMP) stars with [Fe/H] < -3.0 observable in the Galactic halo and thick disk today are believed to be the second-generation stars born out of those materials that were slightly chemically polluted by the extinct, metal-free first stars. If true, these oldest surviving stars with the lowest metal abundances are astrophysical laboratories that may shed essential light on the origins and evolution of the chemical elements and on the formation of the Milky Way.
In order to newly discover field metal-deficient stars in the inner halo of the Galaxy, the Purdue Ultra Metal-Poor Star Survey (PUMPSS) program was conducted. Candidate metal-poor stars were initially selected utilizing the photometric data of the GALEX and the 2MASS, and subsequent medium- and high-resolution spectroscopy were carried out for the identification of true metal-poor giant stars and detailed chemical abundance analyses, respectively. We present an overview of the PUMPSS program and the results of the abundance analysis for high-dispersion spectra of EMP giant stars taken at the KPNO 4m telescope.
We acknowledge support for this work from NASA grants 07-ADP07-0080 and 05-GALEX05-27.

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