Cross-correlation templates introduced in this work prior to continuum subtraction and broadening, derived from model spectra of the atmosphere of WASP-121 b. The chemical abundances of the atoms assume chemical equilibrium with elemental abundances equivalent to a metallicity of 20× solar and a temperature of 2000 K. The templates include all atoms with atomic number up to 40 for which line absorption is significant in the HARPS wavelength range (387.4–690.9 nm) under these conditions, as well as the H₂O, SH, TiO and VO molecules. SH is included as a byproduct of sulphur photo-chemistry, with a disequilibrium abundance profile artifically set to match the profile presented in Evans et al. (2018). The profile is parametrised as having a VMR of 10⁻⁴ for pressureshigher than 10⁻⁵ bar, and zero at lower pressures. Note that for clarity, the scale of the y-axis of the molecular absorption spectra is a factor of 2 smaller than the atoms. Also note that the absorption lines of SH are expected to be significantly weaker than those of the atomic metals. Templates of ionic species (Ti II, Cr II and Fe II) are adopted from the analysis of Hoeijmakers et al. (2019), calculated for the atmosphere of KELT-9 b with a temperature of 4000 K and solar metallicity.