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Cluster cosmology depends critically on how optical clusters are selectedfrom imaging surveys. We compare the conditional luminosity function (CLF) andweak lensing halo masses between two different cluster samples at fixedrichness, detected within the same volume ($0.1{<}z{<}0.34$) using thered-sequence and halo-based methods. After calibrating our CLF deprojectionmethod against mock galaxy samples, we measure the 3D CLFs by cross-correlatingclusters with SDSS photometric galaxies. As expected, the CLFs of red-sequenceand halo-based finders exhibit redder and bluer populations, respectively. Thered-sequence clusters have a flat distribution of red galaxies at the faintend, while the halo-based clusters host a decreasing faint red and a boostedblue population at the bright end. By comparing subsamples of clusters thathave a match between the two catalogues to those without matches, we discoverthat the CLF shape is mainly caused by the different cluster centroiding.However, the average weak lensing halo mass between the matched and non-matchedclusters are consistent with each other in either cluster sample for halos with$\lambda>30$ (M$_{h}^{WL}{>}1.5\times10^{14}h^{-1}M_{\odot}$). Since the colourpreferences of the two cluster finders are almost orthogonal, such aconsistency indicates that the scatter in the mass-richness relation of eithercluster sample is close to random. Therefore, while the choice of how opticalclusters are identified impacts the satellite content, our result suggests thatit should not introduce strong systematic biases in cluster cosmology, exceptfor the $\lambda<30$ regime.

Satellite Content and Halo Mass of Galaxy Clusters: Comparison between Red-Sequence and Halo-based Optical Cluster Finders