The analysis of stellar spectra is vital in the determination of chemical abundances, the understanding of galaxy formation and evolution or the synthesis of the different elements. However, despite the large investment of time and money done to record spectra of astrophysical objects at unprecedented resolution, this work is being hindered by the lack of accurate atomic data. As stellar models are strongly dependent on parameters such as transition probabilities [1], this shortage of data or its poor quality leads to mistaken values of the chemical abundances and stellar ages.

This situation has resulted in an acute need for new measured atomic parameters of matching accuracy and completeness, a task that can be accomplished by using high-resolution Fourier Transform spectroscopy. This technique has evolved dramatically over the past thirty years and nowadays it is able to provide, amongst other parameters, values of transition probabilities with uncertainties as low as 5% (0.02 dex in log(gf)) for strong transitions.

The Fourier Transform Spectroscopy (FTS) Laboratory at Imperial College London is conducting a very fruitful collaboration with the National Institute of Standards and Technology (NIST) and the University of Wisconsin to obtain accurate transition probabilities for many spectral lines needed in surveys such as Gaia-ESO or APOGEE [2-4]. The main aim of this contribution is to encourage further dialogue with astronomers regarding their current necessities of spectroscopic data, as this would help spectroscopists to prioritise present-day needs within the field.