Detection of a Population of Carbon-enhanced Metal-poor Stars in the Sculptor Dwarf Spheroidal Galaxy*
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Chiti_2018_ApJ_856_142.pdf
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Author(s)
Simon, Joshua D.
Thompson, Ian B.
Shectman, Stephen A.
Mateo, Mario
Bailey, John I.
Crane, Jeffrey D.
Walker, Matthew
Frebel, Anna L.
Chiti, Anirudh
Date Issued
April 2018
Journal
Astrophysical Journal
Publisher
American Astronomical Society
Citation
Chiti, Anirudh et al. “Detection of a Population of Carbon-Enhanced Metal-Poor Stars in the Sculptor Dwarf Spheroidal Galaxy.” The Astrophysical Journal 856, 2 (April 2018): 142 © 2018 The American Astronomical Society
Version
Final published version
Abstract
The study of the chemical abundances of metal-poor stars in dwarf galaxies provides a venue to constrain paradigms of chemical enrichment and galaxy formation. Here we present metallicity and carbon abundance measurements of 100 stars in Sculptor from medium-resolution (R ∼ 2000) spectra taken with the Magellan/Michigan Fiber System mounted on the Magellan-Clay 6.5 m telescope at Las Campanas Observatory. We identify 24 extremely metal-poor star candidates ([Fe/H] < -3.0) and 21 carbon-enhanced metal-poor (CEMP) star candidates. Eight carbon-enhanced stars are classified with at least 2σ confidence, and five are confirmed as such with follow-up R ∼ 6000 observations using the Magellan Echellette Spectrograph on the Magellan-Baade 6.5 m telescope. We measure a CEMP fraction of 36% for stars below [Fe/H] = -3.0, indicating that the prevalence of carbon-enhanced stars in Sculptor is similar to that of the halo (∼43%) after excluding likely CEMP-s and CEMP-r/s stars from our sample. However, we do not detect that any CEMP stars are strongly enhanced in carbon ([C/Fe] > 1.0). The existence of a large number of CEMP stars both in the halo and in Sculptor suggests that some halo CEMP stars may have originated from accreted early analogs of dwarf galaxies.
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/10.3847/1538-4357/AAB663
