New FeII energy levels from stellar spectra (Castelli+, 2010)

Details New FeII energy levels from stellar spectra (Castelli+, 2010) New FeII energy levels from stellar spectra (Castelli+, 2010)

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ycat..35209057c&link_type=abstract

VizieR On-line Data Catalog: J/A+A/520/A57. Originally published in: 2010A&A...520A..57C

Physics

Atomic Physics

Atomic Physics, Line Profiles, Models: Atmosphere, Spectroscopy, Stars: Peculiar

Scientific paper

FeII lines in the 3800-8000Å region, produced by transitions to the FeII subconfigurations (3P)4f, (3H)4f, (3F)4f, and (3G)4f are given in Tables 6, 7, 8, and 9, respectively. Only lines with loggf>=-1.5 are listed. Most of these lines can be observed in the UVES spectrum of HR 6000 and have allowed us to identify more than 50% of the previously unidentified lines (Castelli & Hubrig, 2007A&A...475.1041C).
(4 data files).

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