Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832302a&link_type=abstract
American Astronomical Society, AAS Meeting #218, #323.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
We derived the elemental abundances of the sharp-lined B3IV star iota Herculis from high quality optical region spectra (Δλ/λ = 67000, signal-to-noise ≥ 750) obtained with the long camera of the coude spectrograph of the 1.22-m telescope of the Dominion Astrophysical Observatory, Victoria, BC. Canada. The 4096 pixel long SITe4 CCD was used. Generally, two or three one-hour spectra of the same region taken on the same night were co-added to increase the S/N. Twenty-one central wavelength settings covered the entire spectrum (λλ3827-8976) where the desired S/N could be obtained. The regions selected were not seriously affected by telluric lines were not observed.
The spectrum was measured using the REDUCE family of programs of Graham Hill. H I, He I, C II, C III, N I, N II, O I, O II, Ne I, Mg II, Al II, Al III, Si II, Si III, P II, P III, S II, S III, Ar II, Fe II, Fe III, and Ni II lines are used to derive the elemental abundances in an LTE fine analysis using Kurucz's ATLAS9 and WIDTH9 programs. Lines of additional species might be present. Initial estimates of the effective temperature, surface gravity, and microturbulence are 17400 K, 3.85 dex, and 1.9 km s-1, respectively. The He/H ratio is found to be near solar as are the other derived abundances. However, abundances of the same element derived from two species can be different. This probably indicates that some adjustments of these parameters and non-LTE physics are needed to get ionization equilibrium. In addition to our fine analysis we performed a synthesized spectra analysis to refine the results.
SJA and AFG are Guest Observers at the Dominion Astrophysical Observatory.
Adelman Saul J.
Farr A.
Gulliver A.
Hill Gary
Peters Geraldine
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