Photometric redshift as a function of r-band magnitude for each set of photometric redshifts, from left to right: T80S/S-PLUS, LS-DR9, LS-DR10, and LS-DR10-CBPF. We include the corresponding parent sample (grey circles), the A0085 galaxy cluster candidate members selected from our photometric method (blue), the spectroscopically confirmed members (yellow circles), and the confirmed spectroscopic cluster members and spectroscopic objects within the cluster redshift range (yellow crosses) that were not selected by our method. The solid black line indicates the cluster redshift obtained from the mean spectroscopic redshift distribution, while the dashed lines indicate the cluster spectroscopic redshift lower and upper limits. The bright-faint boundary at m_r = 18.5 is indicated by a vertical dotted line. Adopting different z_phot with their corresponding σ_NMAD curves lead to a different cluster galaxy candidate members selection, specially at fainter magnitudes (m_r ≥ 18.5), where S-PLUS selects more candidates as compared with –z_phot.