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|a Frebel, Anna L.
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|a Massachusetts Institute of Technology. Department of Physics
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|a Frebel, Anna L.
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|a Yong, David
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|a Norris, John E.
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|a Bessell, M. S.
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|a Christlieb, N.
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|a Asplund, M.
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|a Beers, Timothy C.
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|a Barklem, P. S.
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|a Ryan, S. G.
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|a The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction
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|a The Most Metal-Poor Stars. III. The Metallicity Distribution Function and Carbon-Enhanced Metal-Poor Fraction
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|b IOP Publishing,
|c 2013-01-22T18:58:57Z.
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|u http://hdl.handle.net/1721.1/76328
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|a We examine the metallicity distribution function (MDF) and fraction of carbon-enhanced metal-poor (CEMP) stars in a sample that includes 86 stars with [Fe/H] ≤ -3.0, based on high-resolution, high signal-to-noise spectroscopy, of which some 32 objects lie below [Fe/H] = -3.5. After accounting for the completeness function, the "corrected" MDF does not exhibit the sudden drop at [Fe/H] = -3.6 that was found in recent samples of dwarfs and giants from the Hamburg/ESO survey. Rather, the MDF decreases smoothly down to [Fe/H] = -4.1. Similar results are obtained from the "raw" MDF. We find that the fraction of CEMP objects below [Fe/H] = -3.0 is 23% ± 6% and 32% ± 8% when adopting the Beers & Christlieb and Aoki et al. CEMP definitions, respectively. The former value is in fair agreement with some previous measurements, which adopt the Beers & Christlieb criterion.
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|t Astrophysical Journal
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