Redshift prior dependence on redshift ζ and apparent galaxy magnitude for two different templates (upper and lower panel). The inset panels show the template spectra. The two templates were selected arbitrarily from the optimised template set (see Fig. 8) and serve as examples. The priors are arbitrarily normalised. The decrease of prior towards redshift zero is because of the volume prior, while the decrease at larger redshifts is due to the luminosity function prior. The differences in spectral templates affect the higher redshift end due to different k-corrections. The slight deviation from a smooth prior is caused by the features (e.g. emission lines) in the spectral templates.