The Abundances of Metal-poor Stars in the Outer Halo of the Milky Way

Details The Abundances of Metal-poor Stars in the Outer Halo of the Milky Way The Abundances of Metal-poor Stars in the Outer Halo of the Milky Way

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21340714l&link_type=abstract

American Astronomical Society, AAS Meeting #213, #407.14; Bulletin of the American Astronomical Society, Vol. 41, p.204

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present a program measuring the abundance ratios of stars in the outer halo of the Milky Way. Using the metal-poor candidates from SDSS-SEGUE and follow-up spectra with ESI on Keck we efficiently measure metallicity, alpha-ratio abundances, and certain neutron-capture abundance ratios for stars out to distances of about 30 kpc, thereby placing them in situ in the outer halo (Carollo et al. 2007). By studying metal-poor stars in this relatively unexplored region we can look for evidence of different star formation environments which can provide a important constraint on current Galaxy formation scenarios (e.g., Bullock & Johnston 2005), and potentially discover interesting individual stars. In an initial sample of 25 stars, we have already discovered one new highly r-process-enhanced metal-poor star and a new type of very metal-poor star with a unique [Ca/Mg] of 1.2. In terms of the larger sample, we are also seeing hints of a different alpha-element population, possible evidence of varied star formation environments in the outer halo. DKL acknowledges the support from the NSF grant AST-0802292 through the Astronomy and Astrophysics Postdoctoral Fellowship program.

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