Quantitative Analysis of the Spectrum of the B3 Abundance Standard iota Herculis

Details Quantitative Analysis of the Spectrum of the B3 Abundance Standard iota Herculis Quantitative Analysis of the Spectrum of the B3 Abundance Standard iota Herculis

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542707p&link_type=abstract

American Astronomical Society, AAS Meeting #215, #427.07; Bulletin of the American Astronomical Society, Vol. 42, p.343

Astronomy and Astrophysics

Astrophysics

Scientific paper

Iota Herculis is an ultrasharp-lined B3IV star that historically has been considered as an abundance standard for the early B stars. New abundances of the lighter and Fe group elements have been determined with the aid of high resolution spectral data from HST/STIS and the Dominion Astrophysical Observatory. The HST spectra were obtained with the STIS E140M and E230M gratings and cover the region 1160-2350 A with a 2-pixel spectral resolution that varies from 0.03-0.08 A. The DAO spectral atlas covers 3820-5350 A in the second order with a 2-pixel resolution 0.072 A. We compare theoretical spectra computed from the NLTE code TLUSTY/SYNSPEC (I. Hubeny & T. Lanz, ApJ, 439,875,1995) and the LTE code ATLAS9/SYNTHE (R. Kurucz, 1993, CD-ROMs 13 & 18) with the observations. The model parameters adopted for the star are Teff = 17,500 K, log g = 3.75, Vturb = 0 km/s, and vsin i = 5 km/s. Solar abundances appear to prevail for the lighter elements but the abundances of Fe group elements are 0.1-0.3 dex below the solar values given by Asplund, Grevesse, & Sauval (2005). In general the NLTE calculations fit the observations better, especially for lines formed high in the atmosphere such as the C I lines near 1260 A. The detailed analysis of the spectrum of this standard star not only allows one to determine the abundances in the atmosphere of a typical field B star but also presents the opportunity to assess the accuracy of atomic parameters for UV lines and find astrophysical f-values.
The authors appreciate support from NASA and STScI grants NAG5-11802 and GO-09848. SJA was a guest observer at DAO.

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