Kicking gravitational wave detectors with recoiling black holes
  Binary black holes emit gravitational radiation with net linear momentum
leading to a retreat of the final remnant black hole that can reach up to
$\sim5,000$ km/s. Full numerical relativity simulations are the only tool to
accurately compute these recoils since they are largely produced when the black
hole horizons are about to merge and they are strongly dependent on their spin
orientations at that moment. We present eight new numerical simulations of BBH
in the hangup-kick configuration family, leading to the maximum recoil. Black
holes are equal mass and near maximally spinning
($|\vec{S}_{1,2}|/m_{1,2}^2=0.97$). Depending on their phase at merger, this
family leads to $\sim\pm4,700$ km/s and all intermediate values of the recoil
along the orbital angular momentum of the binary system. We introduce a new
invariant method to evaluate the recoil dependence on the merger phase via the
waveform peak amplitude used as a reference phase angle and compare it with
previous definitions.
  We also compute the mismatch between these hangup-kick waveforms to infer
their observable differentiability by gravitational wave detectors, such as
advanced LIGO, finding currently reachable signal-to-noise ratios, hence
allowing for the identification of highly recoiling black holes having
otherwise essentially the same binary parameters.
