Orbital and photometric decomposition of FCC 167. Left panel: orbit distribution in the phase space of circularity λ_Z vs. intrinsic radius r, as derived from the best-fitting orbit-superposition model shown in Fig. 8. Grey-scale colours indicate the orbital density in phase space. The horizontal dashed lines separate stars in highly-circular cold thin-disc orbits (λ_Z > 0.7) from those following dynamically warm thick-disc motions (0.2 < λ_Z < 0.7) and those in the non-rotating bulge and stellar halo (λ_Z ~ 0). Right panel:stellar surface-density profiles of FCC 167. The grey lines trace the profiles of a classical exponential disc and Sérsic bulge as derived from a standard bulge-disc decomposition, whereas the blue, orange, and red lines follow the projected surface brightness of the dynamically cold, warm (thick disc), and hot (bulge) components, respectively.