Volume 569, September 2014
|Number of page(s)||14|
|Section||Numerical methods and codes|
|Published online||01 October 2014|
Determining stellar atmospheric parameters and chemical abundances of FGK stars with iSpec⋆
1 Univ. Bordeaux, LAB, UMR 5804, 33270 Floirac, France
2 CNRS, LAB, UMR 5804, 33270 Floirac, France
3 Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden
4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
Received: 4 April 2014
Accepted: 26 June 2014
Context. An increasing number of high-resolution stellar spectra is available today thanks to many past and ongoing extensive spectroscopic surveys. Consequently, the scientific community needs automatic procedures to derive atmospheric parameters and individual element abundances.
Aims. Based on the widely known SPECTRUM code by R.O. Gray, we developed an integrated spectroscopic software framework suitable for the determination of atmospheric parameters (i.e., effective temperature, surface gravity, metallicity) and individual chemical abundances. The code, named iSpec and freely distributed, is written mainly in Python and can be used on different platforms.
Methods. iSpec can derive atmospheric parameters by using the synthetic spectral fitting technique and the equivalent width method. We validated the performance of both approaches by developing two different pipelines and analyzing the Gaia FGK benchmark stars spectral library. The analysis was complemented with several tests designed to assess other aspects, such as the interpolation of model atmospheres and the performance with lower quality spectra.
Results. We provide a code ready to perform automatic stellar spectral analysis. We successfully assessed the results obtained for FGK stars with high-resolution and high signal-to-noise spectra.
Key words: stars: atmospheres / stars: abundances / methods: data analysis
The code is available via http://www.blancocuaresma.com/s/
© ESO, 2014
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