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The RCS 2319+00 supercluster is a massive supercluster at z=0.9 comprisingthree optically selected, spectroscopically confirmed clusters separated by <3Mpc on the plane of the sky. This supercluster is one of a few known examplesof the progenitors of present-day massive clusters (10^{15} Msun by z~0.5). Wepresent an extensive spectroscopic campaign carried out on the superclusterfield resulting, in conjunction with previously published data, in 1961 highconfidence galaxy redshifts. We find 302 structure members spanning threedistinct redshift walls separated from one another by ~65 Mpc. The componentclusters have spectroscopic redshifts of 0.901, 0.905 and 0.905. The velocitydispersions are consistent with those predicted from X-ray data, givingestimated cluster masses of ~10^{14.5} - 10^{14.9} Msun. The Dressler-Shectmantest finds evidence of substructure in the supercluster field and afriends-of-friends analysis identified 5 groups in the supercluster, includinga filamentary structure stretching between two cluster cores previouslyidentified in the infrared by Coppin et al. (2012). The galaxy colors furthershow this filamentary structure to be a unique region of activity within thesupercluster, comprised mainly of blue galaxies compared to the ~43-77%red-sequence galaxies present in the other groups and cluster cores. Richnessestimates from stacked luminosity function fits results in average group massestimates consistent with ~10^{13} Msun halos. Currently, 22% of our confirmedmembers reside in >~10^{13} Msun groups/clusters destined to merge onto themost massive cluster, in agreement with the massive halo galaxy fractionsimportant in cluster galaxy pre-processing in N-body simulation merger treestudies.

The structure of the merging RCS 231953+00 Supercluster at z ~ 0.9