English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Catalog of Chromium, Cobalt, and Nickel Abundances in Globular Clusters and Dwarf Galaxies

MPS-Authors

Kirby,  Evan N.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Xie,  Justin L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Guo,  Rachel
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kovalev,  Mikhail
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bergemann,  Maria
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Kirby, E. N., Xie, J. L., Guo, R., Kovalev, M., & Bergemann, M. (2018). Catalog of Chromium, Cobalt, and Nickel Abundances in Globular Clusters and Dwarf Galaxies. The Astrophysical Journal Supplement Series, 237.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CCD2-8
Abstract
We present measurements of the abundances of chromium, cobalt, and nickel in 4113 red giants, including 2277 stars in globular clusters (GCs), 1820 stars in the Milky Way’s dwarf satellite galaxies, and 16 field stars. We measured the abundances from mostly archival Keck/DEIMOS medium-resolution spectroscopy with a resolving power of R ̃ 6500 and a wavelength range of approximately 6500-9000 Å. The abundances were determined by fitting spectral regions that contain absorption lines of the elements under consideration. We used estimates of temperature, surface gravity, and metallicity that we previously determined from the same spectra. We estimated systematic error by examining the dispersion of abundances within mono-metallic GCs. The median uncertainties for [Cr/Fe], [Co/Fe], and [Ni/Fe] are 0.20, 0.20, and 0.13, respectively. Finally, we validated our estimations of uncertainty through duplicate measurements, and we evaluated the accuracy and precision of our measurements through comparison to high-resolution spectroscopic measurements of the same stars. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.