We have calculated an extensive grid of abundance corrections across dwarf, subgiant and giant stars from solar to metal-poor metalicities for Ba II lines at 4554.0, 4934.1, 5853.7, 6141.7, and 6496.9 Ångstrom.

Scientific relation to ChETEC-INFRA

This application addresses one of the science goals of Work Package 5, Task 5.1 of the ChETEC-INFRA project. Specifically, the production of abundance corrections for various elements on the periodic table for a range of stellar parameters. The details of Task 5.1 can be found in the work package description of the original ChETEC-INFRA proposal. This application concerns the first part of the process to produce these abundance corrections; the computation of population departure coefficients in the atomic structure of atoms. We choose barium as the first element to be investigated.

Astronuclear Abundances (JRA3 / WP5)

This activity pursues the development of new tools for advanced stellar abundance analysis based on state-of-the-art stellar model atmospheres and abundance analysis methodologies. It will provide a pipeline that can serve as a starting point for homogeneous abundance analyses of stars used to constrain the chemical evolution of the Galaxy, and web-based interfaces to enable open access to these data products and tools.


Nuclear astrophysics studies the origin of the chemical elements: from the Big Bang, to stellar burning, and to neutron star mergers. ChETEC-INFRA networks the three types of infrastructures that, together, provide the capabilities needed for this quest: astronuclear laboratories supply reaction data, supercomputer facilities perform stellar structure and nucleosynthesis computations, and telescopes and mass spectrometers collect elemental and isotopic abundance data. – About ChETEC-INFRA.