Abstract
We present a new spectroscopic calibration for a fast estimate of T eff and [Fe/H] for FGK dwarfs and GK giant stars. We used spectra from a joint sample of 708 stars, composed by 451 FGK dwarfs and 257 GK-giant stars with homogeneously determined spectroscopic stellar parameters. We have derived 322 EW line-ratios and 100 FeI lines that can be used to compute T eff and [Fe/H], respectively. We show that these calibrations are effective for FGK dwarfs and GK-giant stars in the following ranges: 4500 K eff , 2.5 , and –0.8 ] . The new calibration has a standard deviation of 74 K for T eff and 0.07 dex for [Fe/H]. We use four independent samples of stars to test and verify the new calibration, a sample of giant stars, a sample composed of Gaia FGK benchmark stars, a sample of GK-giant stars from the DR1 of the Gaia-ESO survey, and a sample of FGK-dwarf stars. We present a new computer code, GeTCal, for automatically producing new calibration files based on any new sample of stars.
Highlights
Deriving accurate and precise stellar parameters is a fundamental aspect of astrophysical studies
The volume of data being produced by large-survey observational programs [2, 4] requires the existence of quick methods to obtain stellar parameters for a diverse range of stellar spectral types
This work aimed to build new Teff and [Fe/H] spectroscopic calibrations for both FGK dwarfs and GK giants improving upon the work of Sousa et al [15], hereafter the So12 calibration
Summary
Deriving accurate and precise stellar parameters is a fundamental aspect of astrophysical studies. In order to determine the mass, radius, and age of stars it is necessary to measure stellar atmospheric parameters, such as effective temperature (Teff ), surface gravity (log g), metallicity ([Fe/H]), and microturbulence(vmic), obtained mainly by spectroscopic or photometric methods (e.g. Casagrande et al [3], Sousa et al [12], Tsantaki et al [20]). The volume of data being produced by large-survey observational programs [2, 4] requires the existence of quick methods to obtain stellar parameters for a diverse range of stellar spectral types
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