Kicking gravitational wave detectors with recoiling black holes

Abstract

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 $\sim 5,000$ 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 $\sim \pm 4,700$ 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.

10 pages, 6 figures

References in corpus (27)

• Large Merger Recoils and Spin Flips From Generic Black-Hole Binaries
• Total recoil: the maximum kick from nonspinning black-hole binary inspiral
• Towards models of gravitational waveforms from generic binaries II: Modelling precession effects with a single effective precession parameter
• The LIGO Open Science Center
• Spin Flips and Precession in Black-Hole-Binary Mergers
• High-spin binary black hole mergers
• Remnant mass, spin, and recoil from spin aligned black-hole binaries
• Reducing phase error in long numerical binary black hole evolutions with sixth order finite differencing
• Observable Signatures of a Black Hole Ejected by Gravitational Radiation Recoil in a Galaxy Merger
• Gravitational Wave Recoil and the Retention of Intermediate Mass Black Holes
• Effective potentials and morphological transitions for binary black-hole spin precession
• Gravitational recoil: signatures on the massive black hole population
• Recoiling black holes: electromagnetic signatures, candidates, and astrophysical implications
• Effects of gravitational-wave recoil on the dynamics and growth of supermassive black holes
• Remnant of binary black-hole mergers: New simulations and peak luminosity studies
• Foundations of multiple black hole evolutions
• The second RIT binary black hole simulations catalog and its application to gravitational waves parameter estimation
• The numerical relativity breakthrough for binary black holes
• Black hole kicks as new gravitational wave observables
• A practical formula for the radiated angular momentum
• Perturbative extraction of gravitational waveforms generated with Numerical Relativity
• Recoiling Supermassive Black Holes: a search in the Nearby Universe
• Modeling maximum astrophysical gravitational recoil velocities
• Extreme recoils: impact on the detection of gravitational waves from massive black hole binaries
• The nonspinning binary black hole merger scenario revisited
• New insights on the recoiling/binary black hole candidate J0927+2943 via molecular gas observations
• Evolutions of Nearly Maximally Spinning Black Hole Binaries Using the Moving Puncture Approach

Cited by in corpus (25)

• Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo
• The Third RIT binary black hole simulations catalog
• Extracting the Gravitational Recoil from Black Hole Merger Signals
• Remnant Black Hole Kicks and Implications for Hierarchical Mergers
• Formation of the largest galactic cores through binary scouring and gravitational wave recoil
• The growth of intermediate mass black holes through tidal captures and tidal disruption events
• Inferring the gravitational wave memory for binary coalescence events
• Universal features of gravitational waves emitted by superkick binary black hole systems
• A unified accretion disc model for supermassive black holes in galaxy formation simulations: method and implementation
• Amplification of superkicks in black-hole binaries through orbital eccentricity
• Investigating the effect of in-plane spin directions for Precessing BBH systems
• Anomalies in the gravitational recoil of eccentric black-hole mergers with unequal mass ratios
• Adapted gauge to small mass ratio binary black hole evolutions
• The Search for Binary Supermassive Black Holes Amongst Quasars with Offset Broad Lines Using the Very Long Baseline Array
• Adding equatorial-asymmetric effects for spin-precessing binaries into the SEOBNRv5PHM waveform model
• Dynamics and spin alignment in massive, gravito-turbulent circumbinary discs around supermassive black hole binaries
• Inconsistent black hole kick estimates from gravitational-wave models
• Merging timescale for supermassive black hole binary in interacting galaxy NGC 6240
• Testing general relativity via direct measurement of black hole kicks
• Hypercompact stellar clusters: morphological renditions and spectro-photometric models
• Revisiting the relationship of black-hole kicks and multipole asymmetries
• Where Have All the Little Red Dots Gone? Supermassive Black Hole Binary Dynamics and its Impact on Galaxy Properties
• Observability of spin precession in the presence of a black-hole remnant kick
• Adapted gauge to a quasilocal measure of the black holes recoil
• Evidence of large recoil velocity from a black hole merger signal