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The Frequency of Carbon Rich Stars Among Extremely Metal Poor Stars

Published online by Cambridge University Press:  23 December 2005

Judith G. Cohen
Affiliation:
Palomar Observatory, MC 105-24, California Institute of Technology, Pasadena, CA 91125, email: jlc@astro.caltech.edu
Stephen Shectman
Affiliation:
Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101
Ian Thompson
Affiliation:
Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101
Andrew McWilliam
Affiliation:
Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101
Norbert Christlieb
Affiliation:
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg
Jorge Melendez
Affiliation:
Palomar Observatory, MC 105-24, California Institute of Technology, Pasadena, CA 91125, email: jlc@astro.caltech.edu
Franz-Josef Zickgraf
Affiliation:
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg
Solange Ramírez
Affiliation:
Spitzer Science Center, MC 100-22, California Institute of Technology, Pasadena, CA 91125
Amber Swenson
Affiliation:
Palomar Observatory, MC 105-24, California Institute of Technology, Pasadena, CA 91125, email: jlc@astro.caltech.edu
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Abstract

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We discuss the fraction of carbon stars (C-stars) and of C-enhanced stars among samples of candidate extremely metal poor (EMP: [Fe/H] $\le -3.0$ dex) stars selected from the Hamburg/ESO Survey (HES), obtaining a total for C-rich stars with [C/Fe] $\ge$ +1.0 dex of 14.4$\pm4$%. We also present the key results of detailed abundance analyses of a sample of 14 C-stars selected in this way.

Type
Contributed Papers
Copyright
© 2005 International Astronomical Union

Footnotes

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.