Iron abundances from optical FeIII absorption lines in B-type stellar spectra

H.M.A. Thompson, F. P. Keenan, P. L. Dufton, C. Trundle, R. S. I. Ryans, P. A. Crowther

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Abstract

The role of optical FeIII absorption lines in B-type stars as iron abundance diagnostics is considered. To date, ultraviolet Fe lines have been widely used in B-type stars, although line blending can severely hinder their diagnostic power. Using optical spectra, covering a wavelength range ~3560-9200Å, a sample of Galactic B-type main-sequence and supergiant stars of spectral types B0.5 to B7 are investigated. A comparison of the observed FeIII spectra of supergiants, and those predicted from the model atmosphere codes TLUSTY [plane-parallel, non-local thermodynamic equilibrium (LTE)], with spectra generated using SYNSPEC (LTE), and CMFGEN (spherical, non-LTE), reveal that non-LTE effects appear small. In addition, a sample of main-sequence and supergiant objects, observed with the Fiber-fed Extended Range Optical Spectrograph (FEROS), reveal LTE abundance estimates consistent with the Galactic environment and previous optical studies. Based on the present study, we list a number of FeIII transitions which we recommend for estimating the iron abundance from early B-type stellar spectra.
Original languageEnglish
Pages (from-to)729-740
JournalMonthly Notices of the Royal Astronomical Society
Volume383
DOIs
Publication statusPublished - Jan 2008

ASJC Scopus subject areas

  • Space and Planetary Science

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