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?
|Title of host publication||19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CS19)|
|Number of pages||3|
|Publication status||Published - 1 Sep 2016|
- spectroscopy, stars, radiative codes
Blanco-Cuaresma, S., Nordlander, T., Heiter, U., Jofré, P., Masseron, T., Casamiquela, L., Tabernero, H. M., Bhat, S. S., Casey, A. R., Meléndez, J., & Ramírez, I. (2016). How much can we trust high-resolution spectroscopic stellar atmospheric parameters? In 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CS19) (pp. 1-3) https://doi.org/10.5281/zenodo.155115