Equivalent widths for Fe-group lines in field and cluster metal poor stars

Details Equivalent widths for Fe-group lines in field and cluster metal poor stars Equivalent widths for Fe-group lines in field and cluster metal poor stars

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26as...86..269g&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 86, no. 2, Dec. 1990, p. 269-298.

Astronomy and Astrophysics

Astrophysics

5

Error Analysis, Giant Stars, Globular Clusters, Iron, Spectral Line Width, Stellar Composition, Charge Coupled Devices, Metallicity, Signal To Noise Ratios

Scientific paper

Abundances of Fe-group elements in field and cluster metal poor stars have been presented in Gratton and Sneden (1990). Presented here is a tabulation of the equivalent widths used in that paper. Errors in these equivalent widths are + or - 2 mA for field stars (observed at a resolution of 50,000 and S/N of 150 or less), and + or - 10 mA in cluster giants (observed at a resolution of 20,000 and S/N of 100 or less). These errors are mainly due to uncertainties (about 1-1.5) in the location of the continuum level.

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