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Recent simulations of the densest portion of the Corona Borealis supercluster(A2061, A2065, A2067, and A2089) have shown virtually no possibility ofextended gravitationally bound structure without inter-cluster matter (Pearson& Batuski). In contrast, recent analyses of the dynamics found that theclusters had significant peculiar velocities towards the supercluster centroid(Batiste & Batuski). In this paper we present the results of a thoroughinvestigation of the CSC: we determine redshifts and virial masses for all 8clusters associated with the CSC; repeat the analysis of Batiste & Batuski withthe inclusion of A2056 and CL1529+29; estimate the mass of the supercluster byapplying the virial theorem on the supercluster scale (e.g. Small et al.), thecaustics method (e.g. Reisenegger et al.), and a new procedure using thespherical collapse model (SCM) with the results of the dynamical analysis(SCM+FP); and perform a series of simulations to assess the likelihood of theCSC being a gravitationally bound supercluster. We find that the mass of theCSC is between 0.6 and 12 x 10^{16} h^{-1} M_{sun}. The dynamical analysis,caustics method and the SCM+FP indicate that the structure is collapsing, withthe latter two both indicating a turn around radius of about 12.5 h^{-1} Mpc.Lastly, the simulations show that with a reasonable amount of inter-clustermass, there is likely extended bound structure in the CSC. Our results suggestthat A2056, A2061, A2065, A2067, and A2089 form a gravitationally boundsupercluster.

The Largest Gravitationally Bound Structures: The Corona Borealis Supercluster - Mass and Bound Extent