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We study a sample of 19 galaxy clusters in the redshift range $0.15<z<0.30$with highly complete spectroscopic membership catalogues (to $K < K^{\ast}(\rmz)+1.5$) from the Arizona Cluster Redshift Survey (ACReS); individualweak-lensing masses and near-infrared data from the Local Cluster SubstructureSurvey (LoCuSS); and optical photometry from the Sloan Digital Sky Survey(SDSS). We fit the scaling relations between total cluster luminosity in eachof six bandpasses (${\it grizJK}$) and cluster mass, finding cluster luminosityto be a promising mass proxy with low intrinsic scatter $\sigma_{\ln L|M}$ ofonly $\sim 10-20$ per cent for all relations. At fixed overdensity radius, theintercept increases with wavelength, consistent with an old stellar population.The scatter and slope are consistent across all wavelengths, suggesting thatcluster colour is not a function of mass. Comparing colour with indicators ofthe level of disturbance in the cluster, we find a narrower variety in thecluster colours of 'disturbed' clusters than of 'undisturbed' clusters. Thistrend is more pronounced with indicators sensitive to the initial stages of acluster merger, e.g. the Dressler Schectman statistic. We interpret this aspossible evidence that the total cluster star formation rate is 'standardised'in mergers, perhaps through a process such as a system-wide shock in theintracluster medium.

Galaxy cluster luminosities and colours, and their dependence on cluster mass and merger state