Kicking gravitational wave detectors with recoiling black holes. (arXiv:1908.04382v1 [gr-qc])

<a href="http://arxiv.org/find/gr-qc/1/au:+Lousto_C/0/1/0/all/0/1">Carlos O. Lousto</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Healy_J/0/1/0/all/0/1">James Healy</a>

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 $simpm4,700$ 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.

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 $simpm4,700$ 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.

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