  Recent simulations of the densest portion of the Corona Borealis supercluster
(A2061, A2065, A2067, and A2089) have shown virtually no possibility of
extended gravitationally bound structure without inter-cluster matter (Pearson
& Batuski). In contrast, recent analyses of the dynamics found that the
clusters had significant peculiar velocities towards the supercluster centroid
(Batiste & Batuski). In this paper we present the results of a thorough
investigation of the CSC: we determine redshifts and virial masses for all 8
clusters associated with the CSC; repeat the analysis of Batiste & Batuski with
the inclusion of A2056 and CL1529+29; estimate the mass of the supercluster by
applying the virial theorem on the supercluster scale (e.g. Small et al.), the
caustics method (e.g. Reisenegger et al.), and a new procedure using the
spherical collapse model (SCM) with the results of the dynamical analysis
(SCM+FP); and perform a series of simulations to assess the likelihood of the
CSC being a gravitationally bound supercluster. We find that the mass of the
CSC 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, with
the 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-cluster
mass, there is likely extended bound structure in the CSC. Our results suggest
that A2056, A2061, A2065, A2067, and A2089 form a gravitationally bound
supercluster.
