We present the results of 74 new simulations of nonprecessing spinning black hole binaries with mass ratios q = m _ { 1 } / m _ { 2 } in the range 1 / 7 \leq q \leq 1 and individual spins covering the parameter space -0.95 \leq \alpha _ { 1 , 2 } \leq 0.95 with one runs with spins of \pm 0.95 .
We supplement those runs with 107 previous simulations to study the hangup effect in black hole mergers , i.e .
the delay or prompt merger of spinning holes with respect to non spinning binaries .
We perform the numerical evolution for typically the last ten orbits before the merger and down to the formation of the final remnant black hole .
This allows us to study the hangup effect for unequal mass binaries leading us to identify the spin variable that controls the number of orbits before merger as \vec { S } _ { hu } \cdot { \hat { L } } , where \vec { S } _ { hu } = ( 1 + \frac { 1 } { 2 } \frac { m _ { 2 } } { m _ { 1 } } ) \vec { S } _ { 1 } + ( 1 + \frac { 1 } { 2 } \frac% { m _ { 1 } } { m _ { 2 } } ) \vec { S } _ { 2 } .
We also combine the total results of those 181 simulations to obtain improved fitting formulae for the remnant final black hole mass , spin and recoil velocity as well as for the peak luminosity and peak frequency of the gravitational strain , and find new correlations among them .
This accurate new set of simulations enhances the number of available numerical relativity waveforms available for parameter estimation of gravitational wave observations .