Example BP/RP spectrophotometry. The spectra have been normalized to have the same number of photon counts over the spectral bands plotted. (This does not yield the same area under each spectrum as plotted – against wavelength – due to the nonlinear dispersion.) Except for the emission line stars, all spectra are noise-free synthetic spectra. Several examples of each type of object are shown in each panel (the line colours are arbitrary). The galaxies are for a range of types, all with zero redshift and zero Galactic extinction. The quasar spectra cover a range of emission line strengths, continuum slopes and redshifts. In the ultra cool dwarf panel six spectra are shown with T_eff ranging from 500–3000 K in steps of 500 K for log g = 5 dex. The top-right panel shows five emission line sources: Herbig Ae, PNe, T Tauri, WN4/WCE, dMe. The lack of red flux for these sources is a result of the input spectra used not spanning the full BP/RP wavelength range. The bottom row shows normal stars, in which just one parameter varies in each panel. From left to right these are: T_eff ∈  {3000,4000,5000,6000,7000,8500,10   000,12   000,15   000,20   000} K; A₀ ∈  {0.0,0.1,0.5,1.0,2.0,3.0,5.0,7.0,10.0} mag; [Fe/H] ∈  {−2.5, −1.5, −0.5, +0.5} dex; log g ∈  {0,2.5,4,5.5} dex. The other parameters are held constant as appropriate at T_eff = 5000 K, A₀ = 0 mag, [Fe/H] = 0 dex, log g = 4.0 dex. A common photon count scale is used in all the panels of the bottom row. The cooler/redder stars are those with increasingly more flux in the red part of the spectrum in the two lower left panels.