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We present a new two-color algorithm, the "Stellar Bump Sequence" (SBS), thatis optimized for robustly identifying candidate high-redshift galaxy clustersin combined wide-field optical and mid-infrared (MIR) data. The SBS algorithmis a fusion of the well-tested cluster red-sequence method of Gladders & Yee(2000) with the MIR 3.6um - 4.5um cluster detection method developed byPapovich (2008). As with the cluster red-sequence method, the SBS identifiescandidate overdensities within 3.6um - 4.5um color slices, which are theequivalent of a rest-frame 1.6um stellar bump "red-sequence". In addition toemploying the MIR colors of galaxies, the SBS algorithm incorporates anoptical/MIR (z' - 3.6um) color cut. This cut effectively eliminates foreground0.2 < z < 0.4 galaxies which have 3.6um - 4.5um colors that are similarly redas z > 1.0 galaxies and add noise when searching for high-redshift galaxyoverdensities. We demonstrate using the z ~ 1 GCLASS cluster sample thatsimilar to the red sequence, the stellar bump sequence appears to be aubiquitous feature of high-redshift clusters, and that within that sample thecolor of the stellar bump sequence increases monotonically with redshift andprovides photometric redshifts accurate to dz = 0.05. We apply the SBS methodin the XMM-LSS SWIRE field and show that it robustly recovers the majority ofconfirmed optical, MIR, and X-ray-selected clusters at z > 1.0 in that field.Lastly, we present confirmation of SpARCS J022427-032354 at z = 1.63, a newcluster detected with the method and confirmed with 12 high-confidencespectroscopic redshifts obtained using FORS2 on the VLT. We conclude with adiscussion of future prospects for using the algorithm.

Discovery of a Rich Cluster at z = 1.63 using the Rest-Frame 1.6um "Stellar Bump Sequence" Method