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New Metallicity Calibration Down to [Fe/H] = −2.75 dex

Published online by Cambridge University Press:  05 March 2013

S. Karaali ,
S. Bilir ,
Y. Karataş  and
S. G. Ak
S. Karaali
Affiliation:
Department of Astronomy and Space Sciences, Istanbul University, 34452 Istanbul, Turkey.
S. Bilir
Affiliation:
Department of Astronomy and Space Sciences, Istanbul University, 34452 Istanbul, Turkey.
Y. Karataş*
Affiliation:
Department of Astronomy and Space Sciences, Istanbul University, 34452 Istanbul, Turkey.
S. G. Ak
Affiliation:
Department of Astronomy and Space Sciences, Istanbul University, 34452 Istanbul, Turkey.
*
karsa@istanbul.edu.tr
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Abstract

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We have taken 88 dwarfs, covering the colour-index interval 0.37 ≤ (B–V)0 ≤ 1.07 mag, with metallicities –2.70 ≤ [Fe/H] ≤ +0.26 dex, from three different sources for new metallicity calibration. The catalogue of Cayrel de Stroble et al. (2001), which includes 65% of the stars in our sample, supplies detailed information on abundances for stars with determination based on high-resolution spectroscopy. In constructing the new calibration we have used as ‘corner stones’ 77 stars which supply at least one of the following conditions: (i) the parallax is larger than 10 mas (distance relative to the Sun less than 100 pc) and the galactic latitude is absolutely higher than 30°; (ii) the parallax is rather large, if the galactic latitude is absolutely low and vice versa. Contrary to previous investigations, a third-degree polynomial is fitted for the new calibration: [Fe/H] = 0.10 – 2.76δ – 24.04δ2 + 30.00δ3. The coefficients were evaluated by the least-squares method, without regard to the metallicity of Hyades. However, the constant term is in the range of metallicity determined for this cluster, i.e. 0.08 ≤ [Fe/H] ≤ 0.11 dex. The mean deviation and the mean error in our work are equal to those of Carney (1979), for [Fe/H] ≥ –1.75 dex where Carney's calibration is valid.

Keywords

stars: abundancesstars: metallicity calibrationstars: metal -poor

Information

Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 20 , Issue 2 , 2003 , pp. 165 - 172
Copyright
Copyright © Astronomical Society of Australia 2003

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