The hangup effect in unequal mass binary black hole mergers and further
  studies of their gravitational radiation and remnant properties
  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 $1/7\leq q\leq1$ and
individual spins covering the parameter space $-0.95\leq\alpha_{1,2}\leq0.95$
with one runs with spins of $\pm0.95$. 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
$\vec{S}_{hu}=(1+\frac12\frac{m_2}{m_1})\vec{S}_1+(1+\frac12\frac{m_1}{m_2})\vec{S}_2$.
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.
