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Published online by Cambridge University Press: 12 October 2020
High-resolution stellar spectra are important tools for studying the chemical evolution of the Milky Way Galaxy, tracing the origin of chemical elements, and characterizing planetary host stars. Large amounts of data have been accumulating, in particular in the optical and infrared wavelength regions. The observed spectral lines are interpreted using model spectra that are calculated based on transition data for numerous species, in particular neutral and singly ionized atoms. We rely heavily on the continuous activities of laboratory astrophysics groups that produce high-quality experimental and theoretical atomic data for the relevant transitions. We give examples for the precision with which the chemical composition of stars observed by different surveys can be determined, and discuss future needs from laboratory astrophysics.
and the Gaia-ESO line list group (Karin Lind, Maria Bergemann, Martin Asplund, Paul S. Barklem, Šarunas Mikolaitis, Thomas Masseron, Patrick de Laverny, Laura Magrini, Juliet C. Pickering et al.)