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Frequency of Carbon Stars among Extremely Metal-poor Stars

Cohen, Judith G. and Shectman, Stephen and Thompson, Ian and McWilliam, Andrew and Christlieb, Norbert and Meléndez, Jorge and Zickgraf, Franz-Josef and Ramírez, Solange and Swenson, Amber (2005) Frequency of Carbon Stars among Extremely Metal-poor Stars. Astrophysical Journal, 633 (2). L109-L112. ISSN 0004-637X. doi:10.1086/498502.

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We demonstrate that there are systematic scale errors in the [Fe/H] values determined by the Hamburg/ESO Survey (HES; and by inference by the HK survey in the past) for certain extremely metal-poor, highly C-enhanced giants. The consequences of these scale errors are that (1) the fraction of carbon stars at extremely low metallicities has been overestimated in several papers in the recent literature, (2) the number of extremely metal-poor stars known is somewhat lower than has been quoted in the recent literature, and (3) the yield for extremely metal-poor stars by the HES is somewhat lower than is stated in the recent literature. A preliminary estimate for the frequency of carbon stars among the giants in the HES sample with -4 < [Fe/H] < -2.0 dex is 7.4% ± 2.9%; adding an estimate for the C-enhanced giants with [C/Fe] > 1.0 dex without detectable C_2 bands raises the fraction to 14% ± 4%. We rely on the results of an extensive set of homogeneous, detailed abundance analyses of stars expected to have [Fe/H] ≤ -3.0 dex selected from the HES to establish these claims. We have found that the Fe metallicity of the cooler (T_(eff) ≾ 5200 K) C stars as derived from spectra taken with HIRES at Keck are a factor of ~10 higher than those obtained via the algorithm used by the HES project to analyze the moderate-resolution follow-up spectra, and this algorithm is identical to that used until very recently by the HK survey. This error in the Fe abundance estimate for C stars arises from a lowering of the emitted flux in the continuum bandpasses of the KP index (Ca II λ3933) and, particularly, the HP2 (Hδ) index used to estimate [Fe/H] due to absorption from strong molecular bands.

Item Type:Article
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URLURL TypeDescription Paper
Cohen, Judith G.0000-0002-8039-4673
Christlieb, Norbert0000-0002-4043-2727
Meléndez, Jorge0000-0002-4933-2239
Additional Information:© 2005 The American Astronomical Society. Received 2005 March 29; accepted 2005 October 4; published 2005 October 21. Based in part on observations obtained at the W. M. Keck Observatory, which is operated jointly by the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The entire Keck/HIRES user community owes a huge debt to the many other people who have worked to make the Keck Telescope and HIRES a reality and who operate and maintain the Keck Observatory. J. G. C. and J. M. are grateful for partial support from NSF grant AST-0205951. J. G. C. is grateful for support from the Ernest Fullam Award of the Dudley Observatory that helped initiate this work. The work of N. C. and F.-J. Z. is supported by Deutsche Forschungsgemeinschaft (grants Ch 214-3 and Re 353/44). N. C. acknowledges support through a Henri Chretien International Research Grant administered by the American Astronomical Society.
Funding AgencyGrant Number
Dudley ObservatoryUNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)Ch 214-3
Deutsche Forschungsgemeinschaft (DFG)Re 353/44
American Astronomical SocietyUNSPECIFIED
Subject Keywords:Galaxy: abundances—Galaxy: halo—stars: carbon
Issue or Number:2
Record Number:CaltechAUTHORS:20190522-080209202
Persistent URL:
Official Citation:Judith G. Cohen et al 2005 ApJ 633 L109
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95681
Deposited By: Tony Diaz
Deposited On:22 May 2019 22:36
Last Modified:16 Nov 2021 17:14

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