Spectral energy distribution fits to the sample objects (top of each panel) and residuals to the fits (bottom of each panel). The top panels show the SED fits to a DAO (left column) and a DA (right column) WD that do not show an IR excess. The remaining panels (second row: DAO; third and fourth row: DA) depict objects with a near- and/or mid-IR excess modelled with our best fit TMAP models from Paper I and either a best-fit late-type star model from the PHOENIX grid or one or two blackbody component(s). Dots represent observations from different bands, whereas residuals are shown by crosses. Each colour represents a single survey or mission. The dark purple line shows the best-fit (combined) model. Blue and purple areas show the fluxes from the WD and the cool component, respectively. For clarity, the y axis of all panels are shown in the form f_λ λ³, except for WD 1342+443, WD 2218+706, and WD 2350–706 where f_λ is shown on a logarithmic scale.