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2003PASP..115..143K - Publ. Astron. Soc. Pac., 115, 143-169 (2003/February-0)
A globular cluster metallicity scale based on the abundance of Fe II.
KRAFT R.P. and IVANS I.I.
Abstract (from CDS):
We find that [Fe/H]IIis correlated linearly with W', the reduced strength of the near-infrared Ca II triplet defined by Rutledge et al., although the actual correlation coefficients depend on the atmospheric model employed. The correlations, limited to the range -2.4<[Fe/H]II←0.7, are as follows:
(1.)[Fe/H]II=0.531W'-3.279 (MARCS),
(2.)[Fe/H]II=0.537W'-3.225 (Kurucz with convective overshooting),
(3.)[Fe/H]II=0.562W'-3.329 (Kurucz without convective overshooting).
We also discuss how to estimate [X/Fe] ratios. We suggest that C, N, and O, as well as elements appearing in the spectrum in the singly ionized state, e.g., Ti, Sc, Ba, La, and Eu, should be normalized to the abundance of Fe II. Other elements, which appear mostly in the neutral state, but for which the dominant species is nevertheless the ionized state, are probably best normalized to Fe I, but uncertainties remain.
Abstract Copyright: ∼
Journal keyword(s): Galaxy: Abundances - Galaxy: Globular Clusters: Individual: Messier Number: M15 - Galaxy: Globular Clusters: Individual: Messier Number: M92 - Galaxy: Globular Clusters: Individual: Messier Number: M13 - Galaxy: Globular Clusters: Individual: Messier Number: M3 - Galaxy: Globular Clusters: Individual: Messier Number: M5 - Stars: Abundances - Stars: Fundamental Parameters
CDS comments: Table A2 : 20C = Cl* NGC 288 CAN 20.
Simbad objects: 170
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