How much can we trust high-resolution spectroscopic stellar atmospheric parameters?

Abstract

The determination of atmospheric parameters depends on the use of radiative transfer codes (among other elements such as model atmospheres) to compute synthetic spectra and/or derive abundances from equivalent widths. However, it is common to mix results from different surveys/studies where different setups were used to derive the parameters. These inhomogeneities can lead us to inaccurate conclusions. In this work, we studied one aspect of the problem: When deriving atmospheric parameters from high-resolution stellar spectra, what differences originate from the use of different radiative transfer codes?

To appear in the 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun proceeding

Cited by in corpus (2)

• The masses of retired A stars with asteroseismology: Kepler and K2 observations of exoplanet hosts
• Three Hot-Jupiters on the upper edge of the mass-radius distribution: WASP-177, WASP-181 and WASP-183