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Identifying Fe I Levels from Stellar Spectra
Published online by Cambridge University Press: 18 July 2017
Abstract
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The spectrum of the Fe I atom is critical to many areas of astrophysics and beyond. Measurements of the energies of its high-lying levels remain seriously incomplete. Here we update the work by Peterson & Kurucz (2015) to identify such levels using new and archival high-resolution absorption-line UV and optical spectra of stars whose warm temperatures favor Fe I lines. Our GO-14161 Hubble program will obtain UV spectra for four metal-poor turnoff stars, archive them at ASTRAL, and draw from them the new identifications of 250 – 500 Fe I levels.
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- Copyright © International Astronomical Union 2017
References
Carpenter, K. G. & Ayres, T. R.
2015, in 18th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, eds. van Belle, G. and Harris, H. C., p. 1041Google Scholar
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