Using state-of-the-art dynamical simulations of globular clusters , including radiation reaction during black hole encounters and a cosmological model of star cluster formation , we create a realistic population of dynamically-formed binary black hole mergers across cosmic space and time .
We show that in the local universe , 10 % of these binaries form as the result of gravitational-wave emission between unbound black holes during chaotic resonant encounters , with roughly half of those events having eccentricities detectable by current ground-based gravitational-wave detectors .
The mergers that occur inside clusters typically have lower masses than binaries that were ejected from the cluster many Gyrs ago .
Gravitational-wave captures from globular clusters contribute 1-2 Gpc ^ { -3 } yr ^ { -1 } to the binary merger rate in the local universe , increasing to \gtrsim 10 Gpc ^ { -3 } yr ^ { -1 } at z \sim 3 .
Finally , we discuss some of the technical difficulties associated with post-Newtonian scattering encounters , and how care must be taken when measuring the binary parameters during a dynamical capture .