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Metallicity and absolute magnitude calibrations for F-G type main-sequence stars in the Gaia era

  • M. ÇelebiEmail author
  • S. Bilir
  • S. Ak
  • T. Ak
  • Z. F. Bostancı
  • T. Yontan
Original Article
  • 47 Downloads

Abstract

In this study, photometric metallicity and absolute magnitude calibrations were derived using F-G spectral type main-sequence stars in the Solar neighbourhood with precise spectroscopic, photometric and Gaia astrometric data for UBV photometry. The sample consists of 504 main-sequence stars covering the temperature, surface gravity and colour index intervals \(5300< T_{eff} < 7300\) K, \(\log g > 4\) (cgs) and \(0.3<(B-V)_{0}<0.8\) mag, respectively. Stars with relative trigonometric parallax errors \(\sigma _{\pi }/\pi \leq 0.01\) were preferred from Gaia DR2 data for the estimation of their \(M_{V}\) absolute magnitudes. In order to obtain calibrations, \((U-B)_{0}\) and \((B-V)_{0}\) colour indices of stars were preferred and a multi-variable second order equation was used. Calibrations are valid for main-sequence stars in the metallicity and absolute magnitude ranges \(-2<{[\mbox{Fe}/\mbox{H}]}<0.5\) dex and \(2.5< M_{V}<6\) mag, respectively. The mean value and standard deviation of the differences between original and estimated values for the metal abundance and absolute magnitude are \(\langle \Delta {[\mbox{Fe}/\mbox{H}]}\rangle =0.00\pm 0.11\) dex and \(\langle \Delta M_{V} \rangle =0.00\pm 0.22\) mag, respectively. In this work, it has been shown that more precise iron abundance and absolute magnitude values were obtained with the new calibrations, compared to previous calibrations in the literature.

Keywords

Stars: abundances Stars: metallicity calibration Stars: distance 

Notes

Acknowledgements

We thank the anonymous referees for their insightful and constructive suggestions, which significantly improved the paper. This research has made use of the SIMBAD, NASA’s Astrophysics Data System Bibliographic Services and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC3). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  • M. Çelebi
    • 1
    Email author
  • S. Bilir
    • 2
  • S. Ak
    • 2
  • T. Ak
    • 2
  • Z. F. Bostancı
    • 2
  • T. Yontan
    • 1
  1. 1.Institute of Graduate Studies in Science, Programme of Astronomy and Space SciencesIstanbul UniversityIstanbulTurkey
  2. 2.Faculty of Science, Department of Astronomy and Space SciencesIstanbul UniversityIstanbulTurkey

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