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Title:
Refined Estimates of Carbon Abundances for Carbon-Enhanced Metal-Poor Stars
Authors:
Rossi, S.; Placco, V. M.; Beers, T. C.; Marsteller, B.; Kennedy, C. R.; Sivarani, T.; Masseron, T.; Plez, B.
Affiliation:
AA(Department of Astronomy, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, University of Sa~o Paulo, Brazil, Rua do Mata~o 1226, Cidade Universitária, Sa~o Paulo, SP, 05508-090), AB(Department of Astronomy, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, University of Sa~o Paulo, Brazil, Rua do Mata~o 1226, Cidade Universitária, Sa~o Paulo, SP, 05508-090), AC(Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824-1116, USA), AD(Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824-1116, USA), AE(Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824-1116, USA), AF(Department of Physics & Astronomy, CSCE: Center for the Study of Cosmic Evolution, and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824-1116, USA), AG(Department of Astronomy, Ohio State University, Columbus, OH 43210, USA), AH(GRAAL, Université Montpellier II, CNRS, 34095, Montpellier, France)
Publication:
FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 154-156 (2008). (AIPC Homepage)
Publication Date:
03/2008
Origin:
AIP
PACS Keywords:
Population II stars, Galactic halo, Abundances, chemical composition, Star formation, Spectroscopy and spectrophotometry
DOI:
10.1063/1.2905526
Bibliographic Code:
2008AIPC..990..154R

Abstract

We present results from a refined set of procedures for estimation of the metallicities ([Fe/H]) and carbon abundance ratios ([C/Fe]) based on a much larger sample of calibration objects (on the order of 500 stars) then were available to Rossi et al. (2005), due to a dramatic increase in the number of stars with measurements obtained from high-resolution analyses in the past few years. We compare results obtained from a new calibration of the KP and GP indices with that obtained from a custom set of spectral synthesis based on MOOG. In cases where the GP index approaches saturation, it is clear that only spectral synthesis achieve reliable results.
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