HIGH-RESOLUTION SPECTROSCOPIC STUDY OF EXTREMELY METAL-POOR STAR CANDIDATES FROM THE SKYMAPPER SURVEY
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Author(s)
Keller, Stefan C.
Casey, Andrew R.
Asplund, Martin
Bessell, Michael S.
Costa, Gary S. Da
Lind, Karin
Marino, Anna F.
Norris, John E.
Schmidt, Brian P.
Tisserand, Patrick
Date Issued
July 2015
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Jacobson, Heather R., Stefan Keller, Anna Frebel, Andrew R. Casey, Martin Asplund, Michael S. Bessell, Gary S. Da Costa, et al. “HIGH-RESOLUTION SPECTROSCOPIC STUDY OF EXTREMELY METAL-POOR STAR CANDIDATES FROM THE SKYMAPPER SURVEY.” The Astrophysical Journal 807, no. 2 (July 9, 2015): 171. © 2015 The American Astronomical Society
Version
Final published version
Abstract
The SkyMapper Southern Sky Survey is carrying out a search for the most metal-poor stars in the Galaxy. It identifies candidates by way of its unique filter set which allows for estimation of stellar atmospheric parameters. The set includes a narrow filter centered on the Ca ii K 3933 Å line, enabling a robust estimate of stellar metallicity. Promising candidates are then confirmed with spectroscopy. We present the analysis of Magellan Inamori Kyocera Echelle high-resolution spectroscopy of 122 metal-poor stars found by SkyMapper in the first two years of commissioning observations. Forty-one stars have [Fe/H] ⩽ -3.0. Nine have [Fe/H] ⩽ -3.5, with three at [Fe/H] ~ -4. A 1D LTE abundance analysis of the elements Li, C, Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Co, Ni, Zn, Sr, Ba, and Eu shows these stars have [X/Fe] ratios typical of other halo stars. One star with low [X/Fe] values appears to be "Fe-enhanced," while another star has an extremely large [Sr/Ba] ratio: >2. Only one other star is known to have a comparable value. Seven stars are "CEMP-no" stars ([C/Fe] > 0.7, [Ba/Fe] < 0). 21 stars exhibit mild r-process element enhancements (0.3 ⩽ [Eu/Fe] < 1.0), while four stars have [Eu/Fe] ⩾ 1.0. These results demonstrate the ability to identify extremely metal-poor stars from SkyMapper photometry, pointing to increased sample sizes and a better characterization of the metal-poor tail of the halo metallicity distribution function in the future.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637X/807/2/171
