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Galaxy clusters' structure, dominated by dark matter, is traced by membergalaxies in the optical and hot intra-cluster medium (ICM) in X-rays. Wecompare the radial distribution of these components and determine themass-to-light ratio vs. system mass relation.  We use 14 clusters from the REXCESS sample which is representative ofclusters detected in X-ray surveys. Photometric observations with the WideField Imager on the 2.2m MPG/ESO telescope are used to determine the numberdensity profiles of the galaxy distribution out to $r_{200}$. These arecompared to electron density profiles of the ICM obtained using XMM-Newton, anddark matter profiles inferred from scaling relations and an NFW model.  While red sequence galaxies trace the total matter profile, the blue galaxydistribution is much shallower. We see a deficit of faint galaxies in thecentral regions of massive and regular clusters, and strong suppression ofbright and faint blue galaxies in the centres of cool-core clusters,attributable to ram pressure stripping of gas from blue galaxies in highdensity regions of ICM and disruption of faint galaxies due to galaxyinteractions. We find a mass-to-light ratio vs. mass relation within $r_{200}$of $\left(3.0\pm0.4\right) \times 10^2\,h\,\mathrm{M}_{\odot}\,\mathrm{L}_{\odot}^{-1}$ at$10^{15}\,\mathrm{M}_{\odot}$ with slope $0.16 \pm 0.14$, consistent with mostprevious results.

Optical and X-ray profiles in the REXCESS sample of galaxy clusters