Colours of Bulges and Discs within Galaxy Clusters and the Signature of Disc Fading on Infall

The origins of the bulge and disc components of galaxies are of primary importance to understanding galaxy formation. Here bulge–disc decomposition is performed simultaneously in B and R bands for 922 bright galaxies in eight nearby (z \u3c 0.06) clusters with deep redshift coverage using photometry from the National Optical Astronomy Observatory (NOAO) Fundamental Plane Survey. The total galaxy colours follow a universal colour–magnitude relation (CMR). The discs of L* galaxies are 0.24 mag bluer in B−R than bulges. Bulges have a significant CMR slope while the CMR slope of discs is flat. Thus the slope of the CMR of the total light is driven primarily (60 per cent) by the bulge CMR, and to a lesser extent (40 per cent) by the change in the bulge‐to‐total ratio as a function of magnitude. The colours of the bulge and disc components do not depend on the bulge‐to‐total ratio, for galaxies with bulge‐to‐total ratios greater than 0.2. While the colours of the bulge components do not depend significantly on environment, the median colours of discs vary significantly, with discs in the cluster centre redder by 0.10 mag than those at the virial radius. Thus while star formation in bulges appears to be regulated primarily by mass‐dependent, and hence presumably internal, processes, that of discs is affected by the cluster environment