Stellar Archaeology: A Keck Pilot Program on Extremely Metal-poor Stars from the Hamburg/ESO Survey. I. Stellar Parameters
Abstract
In this series of two papers, we present a high-dispersion spectroscopic analysis of eight candidate extremely metal-poor stars selected from the Hamburg/ESO Survey (HES) and of six additional very metal-poor stars. We demonstrate that with suitable vetting using moderate-resolution spectra, the yield of this survey for stars with [Fe/H] ≤ -3.0 dex is very high; three out of the eight stars observed thus far at high resolution from the HES are actually that metal-poor, three more have [Fe/H] ≤ -2.8 dex, and the remainder are only slightly more metal-rich. In preparation for a large-scale effort to mine the HES database for such stars about to get under way, we lay out in this paper the basic principles we intend to use to determine in a uniform way the stellar parameters T_(eff), log g, and reddening.
Additional Information
© 2002 The American Astronomical Society. Received 2001 October 1; accepted 2002 March 26. Based in large 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 NASA. The entire Keck/HIRES user community owes a huge debt to Jerry Nelson, Gerry Smith, Steve Vogt, and many other people who have worked to make the Keck Telescope and HIRES a reality and to operate and maintain the Keck Observatory. We are grateful to the W. M. Keck Foundation for the vision to fund the construction of the W. M. Keck Observatory. The authors wish to extend special thanks to those of Hawai'ian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. We thank T. Gehren and J. Reetz for providing us with Balmer line profiles and making the spectrum investigation utility SIU available to us. We thank the referee, Bruce Carney, for his thoughtful and constructive comments. We thank Sarah Yost, James Chakan, and Hubert Chen for obtaining the BV photometry of BS 17447-0029. T. C. B acknowledges partial support for this work from grants AST 00-98508 and AST 00-98549 from the National Science Foundation.Attached Files
Published - Cohen_2002_AJ_124_470.pdf
Accepted Version - 0204082.pdf
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Additional details
- Eprint ID
- 95699
- Resolver ID
- CaltechAUTHORS:20190522-113647897
- W. M. Keck Foundation
- NASA
- AST 00-98508
- NSF
- AST 00-98549
- NSF
- Created
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2019-05-22Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field