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The Hamburg/ESO R-process Enhanced Star survey (HERES): Abundances

Published online by Cambridge University Press:  23 December 2005

P. S. Barklem ,
N. Christlieb ,
T. C. Beers ,
V. Hill ,
J. Holmberg ,
B. Marsteller ,
S. Rossi ,
F.-J. Zickgraf  and
M. S. Bessell
P. S. Barklem
Affiliation:
Department of Astronomy and Space Physics, Uppsala University, Box 515, S 751-20 Uppsala, Sweden email: [email protected]
N. Christlieb
Affiliation:
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
T. C. Beers
Affiliation:
Department of Physics and Astronomy and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI 48824 USA
V. Hill
Affiliation:
GEPI, Observatoire de Paris Meudon, F-92125 Meudon Cedex, France
J. Holmberg
Affiliation:
Astronomical Observatory, NBIfAFG, Juliane Meries Vej 30, 2100 Copenhagen, Denmark Nordic Optical Telescope Scientific Association, Apartado 474, ES-38 700 Santa Cruz de La Palma, Spain Tuorla Observatory, Väisäläntie 20, FI-21500 Piikkiö, Finland
B. Marsteller
Affiliation:
Department of Physics and Astronomy and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI 48824 USA
S. Rossi
Affiliation:
Departamento de Astronomia, IAG, Universidade de São Paulo, Rua do Matão 1226, 05508-900 São Paulo - SP, Brazil
F.-J. Zickgraf
Affiliation:
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
M. S. Bessell
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd, Weston, ACT 2611, Australia
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Abstract

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We present the results of analysis of “snapshot” spectra (i.e., R=20,000 and S/N=50 per pixel) of 253 metal-poor halo stars $-3.8<$[Fe/H]$<-1.5$ obtained in the HERES survey. The spectra are analysed using an automated line profile analysis method based on the Spectroscopy Made Easy (SME) codes of Valenti & Piskunov (1996). Elemental abundances of moderate precision (absolute r.m.s. errors of order 0.25 dex) have been obtained for 22 elements, C, Mg, Al, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Zn, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, and Eu, where detectable. The results are presented and discussed, particularly trends and scatter in the abundance distributions.

Keywords

Stars abundances – stars Population II – Galaxy abundances – Galaxy evolution – Galaxy halo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 201 - 206
Copyright
© 2005 International Astronomical Union