Role of input atomic data in spectroscopic analyses of the Sun and metal-poor stars

TL;DR

This paper discusses the critical role of atomic data in spectroscopic analysis of the Sun and metal-poor stars, emphasizing the importance of accurate quantum-mechanical data for modeling stellar atmospheres and line formation.

Contribution

It provides an overview of atomic data requirements for LTE and non-LTE models of late-type stars, highlighting where improved data are needed for transition metals.

Findings

Atomic data are essential for accurate stellar spectroscopic analysis.

Quantum-mechanical calculations form the basis of most atomic data used.

Identifies specific areas where more precise atomic data are required.

Abstract

Analysis of high-resolution stellar spectra relies heavily upon atomic data. These include energy levels, wavelengths, cross-sections for various types of interactions between particles and photons, such as photoionization and collision induced transitions. Quantum-mechanical calculations provide largest part of these data. In this paper I describe atomic data necessary to compute model atmospheres and line formation for the late-type stars both in the assumption of local thermodynamic equilibrium (LTE) and in a more general case of non-LTE. I will focus on transition metals with 21 < Z < 29 and discuss whether (and where) more complete and/or accurate atomic data are necessary.