Schematic overview of the STA and MTA parts of the pipeline. The input to STA consists of the normalised observed spectra and the template parameters. If ReDetermineApHotStars is applied (see Sect. 3), the template parameters are updated. The template parameters are then used to select the corresponding synthetic spectrum; this is converted into a template and used to derive the cross-correlation functions and the radial velocity for each transit. The MTA part of the pipeline takes the time series of transit radial velocities (for bright stars, i.e., grvs_mag ≤ 12 mag), or the time series of the transit cross-correlation functions (for faint stars, i.e., grvs_mag > 12 mag) to determine the stellar radial velocity.