To derive the fundamental atmospheric parameters of a solar-type star (effective temperature, surface gravity, metallicity), I use two widely used methods.
- The Equivalent Width method
This method is based on the measurement of the EW of selected Fe I & Fe II lines and by imposing ionization and excitation balance. For a description of the method, take a look at this practical guide. I have been working on the optimization of the iron line lists to provide more precise parameters. For stars with effective temperature below 5200K, you can use the line list of Tsantaki et al. (2013) and for the hotter stars the extended line list of Sousa et al. (2008).
- The spectral synthesis technique
To derive spectroscopic parameters for solar-type stars with high rotation, I use the spectral synthesis package Spectroscopy Made Easy (SME). Below you can find the line list I use in Tsantaki et al. (2014) in SME readable format. The atomic parameters are derived after solar calibration.