Top panel: power spectra of angular galaxy clustering (δ_g, in blue) and ARF (δ_z, in red), for a Gaussian redshift bin taken in a DESI-like survey. The bin is centred on z_i = 0.75 and has a standard deviation of σ_z = 0.01. The dashed line shows the term coming from the density kernel , the dotted line shows the part coming from the velocity kernel , and the dot-dashed line shows the cross term . The total C_ℓ power spectra (plain lines) correspond to the sum . Bottom panel: velocity dependence ratio in the power spectrum () over the complete power spectrum, for the angular galaxy clustering (blue line) and for the ARF (red line). This figure shows that ARF are more sensitive to the peculiar velocity of galaxies than angular galaxy clustering, for the same redshift shell.