Applications of

Radiative Transfer

to stellar and planetary atmospheres
Tenerife, Spain - 13-17 Nov. 2017

Poster abstract details

Deriving spectroscopic stellar parameters of cool stars from visible and near-infrared CARMENES spectra
David Montes, Emilio Marfil, Hugo M. Tabernero, Jonay I. González Hernández, José A. Caballero, Adrian Kaminski, Andreas Quirrenbach, Pedro J. Amado, Ignasi Ribas, Ansgar Reiners, Walter Seifert


With the aim of using classic spectroscopic methods with high resolution and high signal-to-noise ratio in the NIR spectral window, we made a selection of FGK-type stars observed with CARMENES, the brand-new, ultra-stable, double-channel spectrograph at the Spanish-German 3.5m Calar Alto telescope. These spectra are part of the CARMENES stellar library of high-resolution spectra. In order to apply the EW method to derive the spectroscopic stellar parameters ($T_{eff}$, $\log g$, [Fe/H], $v_{micro}$), imposing iron excitation and ionization balance under the assumption of local thermodynamic equilibrium, we used our code StePar (Tabernero et al. 2012) with newly-compiled iron line lists in the VIS and NIR range covered by CARMENES (from 0.5 $\mu$m to 1.7 $\mu$m). We compiled different line lists for dwarfs and giants, both metal-rich ([Fe/H] > -0.30) and metal-poor (-0.30 < [Fe/H] < -1.50), which allowed us to split the parameter space into four different regions. We tested the stellar parameters thus obtained with some of the Gaia FGK benchmark stars (Jofré et al. 2014, Heiter et al. 2015) included in our sample. We also focused on the differences in the parameter determinations in case only VIS region is taken into consideration. We are also working on line list compilations to derive chemical abundances and extend this analysis to M-type stars.