Abstract
Synthetic stellar spectra are extensively used for many different applications in astronomy, from determining atomic parameters of new observed stars to the study of the stellar populations of galaxies. One of the inputs for the codes that generate these synthetic spectra are atomic and molecular line lists, which contain the atomic parameters of the absorption lines that should appear in each spectrum. Although these lists contain million of lines, very few of them were actually measured in laboratory. The consequence is that for many lines the errors in the parameters can be as large as 200%. Besides that, we do not know all the lines that appear in the stars. Even for the Sun, our closest and most studied star, the synthetic spectra misses many lines. This is one of the main reasons we still cannot reproduce the spectrum of observed stars. In this project we will develop a careful strategy to compare the synthetic and observed spectrum of the Sun to try to identify and quantify the lines still missing in the models. We will also try to identify lines with large errors in the atomic parameters, as for example, lines in which the central wavelength is wrong.
