Modern observations of astrophysical spectra are in many cases of higher quality than those observed within a laboratory setting. This can result in inaccurate conclusions being drawn. Accurate measurements of spectral line wavelengths and oscillator strengths are required particularly for use in stellar models and chemical abundance calculations, and in surveys such as Gaia-ESO or APOGEE and future surveys. Laboratory astrophysicists aim to measure and improve the atomic data most useful for astronomers, for light and heavy elements across the spectrum, from IR to vacuum-UV (VUV).

Atomic data of iron-group elements are important due to their high abundance and line-rich spectra. Lanthanides are under study as their line-rich spectra overwhelms at sites of r-process production. Our high-resolution Fourier Transform Spectrometry (FTS) group at Imperial College London has, supported by STFC, been providing accurate atomic data for use in astrophysics.

Recent results include new Fe I oscillator strengths for use in Galactic surveys (Belmonte et al. 2017), and 1130 wavelengths and transition probabilities of parity-forbidden Lines for Mn II (Liggins et al. 2021). The first high-resolution measurements of UV transition wavelengths of Cr III are being used as wavelength standards (Smillie et al. 2008). There has been an order of magnitude improvement in atomic data for Co III (Smillie et al. 2016) and in the accuracy of energy levels and transition wavelengths for Mn II (Liggins et al. 2021) and Ni II (Clear, PhD, Imperial College, 2018). Analysis of hyperfine structure of Co II lines has led to the determination of A constants for 292 levels (Ding and Pickering, 2020).

Using new spectra recorded, analysis is underway for accurate wavelengths and atomic energy levels in Mn I and Fe III. The investigation into the spectrum of Neodymium, with a focus on Nd III, has also begun. We welcome data requests!