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An Improved Metallicity Calibration with UBV Photometry

Published online by Cambridge University Press:  02 January 2013

S. Karaali ,
S. Bilir ,
S. Ak ,
E. Yaz  and
B. Coşkunoğlu
S. Karaali*
Affiliation:
Beykent University, Faculty of Science and Letters, Department of Mathematics and Computer, Beykent Ayazağa Campus, 34398, Istanbul, Turkey
S. Bilir
Affiliation:
Istanbul University, Faculty of Sciences, Department of Astronomy and Space Sciences, 34119, Istanbul, Turkey
S. Ak
Affiliation:
Istanbul University, Faculty of Sciences, Department of Astronomy and Space Sciences, 34119, Istanbul, Turkey
E. Yaz
Affiliation:
Istanbul University, Faculty of Sciences, Department of Astronomy and Space Sciences, 34119, Istanbul, Turkey
B. Coşkunoğlu
Affiliation:
Istanbul University, Faculty of Sciences, Department of Astronomy and Space Sciences, 34119, Istanbul, Turkey
*
CCorresponding author. Email: karsa@istanbul.edu.tr
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Abstract

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We used the data of 701 stars covering the colour index interval 0.32 < B − V ≤ 1.16, with metallicities −1.76 ≤ [Fe/H]≤+0.40 dex. The data were taken from the PASTEL catalogue and estimated metallicity-dependent guillotine factors, which provide a more accurate metallicity calibration. We reduced the metallicities of 11 different authors to the metallicities of Valenti & Fischer (2005), and thus obtained a homogeneous set of data which increased the accuracy of the calibration, i.e. [Fe/H]= −14.316δ20.6 − 3.557δ0.6+0.105. Comparison of the metallicity residuals for two sets of data based on the metallicity-dependent guillotine factors with the ones obtained via metal-free guillotine factors shows that metallicities estimated by means of the new guillotine factors are more accurate than the other ones. This advantage can be used in the metallicity gradient investigation of the Galactic components, i.e. thin disc, thick disc, and halo.

Keywords

stars: abundancesstars: metallicity calibrationstars: metal poor
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 28 , Issue 2 , 2011 , pp. 95 - 106
Copyright
Copyright © Astronomical Society of Australia 2011

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