
TY  - JOUR
A1  - Karaali, S. 
A1  - Bilir, S. 
A1  - Karata&#x015F;, Y. 
A1  - Ak, S. G. 
T1  - New Metallicity Calibration Down to [Fe/H] = &minus;2.75 dex
JF  - Publications of the Astronomical Society of Australia
JO  - Publ. Astron. Soc.  Aust.
Y1  - 2003
VL  - 20
IS  - 2
SP  - 165
EP  - 172
KW  - stars: abundances &#8212; stars: metallicity calibration &#8212; stars: metal -poor
UR  - https://doi.org/10.1071/AS02028 
N2  - We have taken 88 dwarfs, covering the colour-index interval 0.37 &#8804; (B&#8211;V)0 &#8804; 1.07 mag, with metallicities &#8211;2.70 &#8804; [Fe/H] &#8804; &#43;0.26 dex, from three different sources for new metallicity calibration. The catalogue of Cayrel de Stroble et al. (2001), which includes 65&#37; 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 &#8216;corner stones&#8217; 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&#176;; (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 &#8211; 2.76&#948; &#8211; 24.04&#948;2 + 30.00&#948;3. 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 &#8804; [Fe/H] &#8804; 0.11 dex. The mean deviation and the mean error in our work are equal to those of Carney (1979), for [Fe/H] &#x2265; &#8211;1.75 dex where Carney&#39;s calibration is valid. 
ER  -

