Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj....100..849b&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 100, Sept. 1990, p. 849-883. Research supported by Michigan State University and Alf
Astronomy and Astrophysics
Astronomy
65
Abundance, Calcium, K Lines, Metallicity, Stellar Composition, Calibrating, Color-Magnitude Diagram, Globular Clusters, Spectral Line Width, Stellar Atmospheres, Stellar Spectrophotometry, Visible Spectrum
Scientific paper
A method for estimating the stellar metal abundances is proposed which compares measures of the equivalent width of a single feature in moderate resolution (1 A) optical spectra of stars, the Ca II K line at 3933 A, with models of the predicted line strength as a function of the broadband B-V color and Fe/H. The approach is capable of providing estimates of stellar metallicity over the range -4.5 to -1.0 with a scatter of about 0.15 dex for dwarfs and giants in the color range 0.33-0.85. For cooler stars, with B-V in the range 0.85-1.1, the scatter may be as large as 0.19 dex. The calibration of the Ca II K index with Fe/H is discussed, and average radial velocities and abundances are presented for several galactic globular clusters.
Beers Timothy C.
Kage Julie A.
Preston George W.
Shectman Stephen A.
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