Searching For Alpha-poor Stars In The Galactic Halo

Details Searching For Alpha-poor Stars In The Galactic Halo Searching For Alpha-poor Stars In The Galactic Halo

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21110317f&link_type=abstract

American Astronomical Society, AAS Meeting #211, #103.17; Bulletin of the American Astronomical Society, Vol. 39, p.922

Astronomy and Astrophysics

Astronomy

Scientific paper

It has been known for more than 40 years that metal-poor stars have chemical compositions that are enriched by alpha-elements (e.g., Mg, Si, S, Ca and possibly Ti). These elements are overabundant by a factor of roughly two compared with the Fe-peak elements. A few striking exceptions have been discovered in recent years, such as BD+80 245, G4-36, CS 22966-043 and HE 1424-0241. Similarly low-alpha abundance patterns are also seen in the Sagittarius dSph galaxy. However, we know almost nothing about what the true occurance frequency of these alpha-poor stars is and how they form. We are conducting the first homogeneous spectroscopic survey of suspected metal poor ([Fe/H]<=-0.75) and alpha-poor ([Mg/Fe]<=+0.2) stars in the Galactic halo. We are obtaining high resolution, high signal-to-noise data with the 2dCoude spectrograph of the McDonald Observatory 2.7m telescope. The goal of this survey is to derive atmospheric parameters Teff, log g and metallicity in a consistent way, and then to perform a detailed analysis of the elemental abundance ratios, in particular the abundances of neutron-capture and alpha-elements. Here we present the preliminary results of this search. This work is supported by NSF grant AST-0607708.

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