  The Hercules Supercluster consists of the Abell clusters 2147, 2151, and
2152. Previous studies of the kinematics have been confounded by the difficulty
of correctly assigning galaxies to the individual clusters, which are not
well-separated. Our study has a total of 468 available velocities for galaxies
in the region, 175 of them new. 414 galaxies are in the supercluster, about
three times the number used in the previous supercluster study. We verify the
existence of the three individual clusters and compute their individual
dynamical parameters. We investigate several techniques for assigning galaxy
membership to clusters in this crowded field. We use the KMM mixture-modeling
algorithm to separate the galaxies into clusters; we find that A2152 has a
higher mean velocity than previous studies have reported. A2147 and A2152 also
have lower velocity dispersions: 821(+68)(-55) and 715(+81)(-61) km/s. The
assignment of galaxies to either A2152 or A2147 requires velocity and position
information. We study the kinematics of the supercluster using the two-body
formalism of Beers, Geller, and Huchra (1982) and conclude that A2147 and A2151
are probably bound to each other, and that the supercluster as a whole may also
be bound. The mass of the supercluster, if bound, is $(7.6\pm2.0)\times 10^{15}
h^{-1} M_{\sun}$; with the supercluster luminosity, $(1.4\pm0.2) \times 10^{13}
h^{-2} L_{\sun}$, this yields Omega = 0.34\pm0.1$.
