Surrogate model for gravitational wave signals from non-spinning, comparable- to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity

Abstract

We present a reduced-order surrogate model of gravitational waveforms from non-spinning binary black hole systems with comparable to large mass-ratio configurations. This surrogate model, \texttt{BHPTNRSur1dq1e4}, is trained on waveform data generated by point-particle black hole perturbation theory (ppBHPT) with mass ratios varying from 2.5 to 10,000. \texttt{BHPTNRSur1dq1e4} extends an earlier waveform model, \texttt{EMRISur1dq1e4}, by using an updated transition-to-plunge model, covering longer durations up to 30,500 $m_1$ (where $m_1$ is the mass of the primary black hole), includes several more spherical harmonic modes up to $\ell =10$, and calibrates subdominant modes to numerical relativity (NR) data. In the comparable mass-ratio regime, including mass ratios as low as $2.5$, the gravitational waveforms generated through ppBHPT agree surprisingly well with those from NR after this simple calibration step. We also compare our model to recent SXS and RIT NR simulations at mass ratios ranging from $15$ to $32$, and find the dominant quadrupolar modes agree to better than $\approx 10^{-3}$. We expect our model to be useful to study intermediate-mass-ratio binary systems in current and future gravitational-wave detectors.

20 pages, 15 figures

References in corpus (24)

• Can environmental effects spoil precision gravitational-wave astrophysics?
• An improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors
• Intermediate and Extreme Mass-Ratio Inspirals -- Astrophysics, Science Applications and Detection using LISA
• Two timescale analysis of extreme mass ratio inspirals in Kerr. I. Orbital Motion
• Observational evidence for intermediate-mass black holes
• Gravitational wave snapshots of generic extreme mass ratio inspirals
• Validating the effective-one-body model of spinning, precessing binary black holes against numerical relativity
• A 400 solar mass black hole in the Ultraluminous X-ray source M82 X-1 accreting close to its Eddington limit
• Towards adiabatic waveforms for inspiral into Kerr black holes: I. A new model of the source for the time domain perturbation equation
• Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: comparable mass, nonspinning case
• Accelerated gravitational-wave parameter estimation with reduced order modeling
• The influence of the hydrodynamic drag from an accretion torus on extreme mass-ratio inspirals
• Gravitational-wave observations of binary black holes: Effect of non-quadrupole modes
• Towards adiabatic waveforms for inspiral into Kerr black holes: II. Dynamical sources and generic orbits
• Environmental Effects for Gravitational-wave Astrophysics
• Testing Chern-Simons Modified Gravity with Gravitational-Wave Detections of Extreme-Mass-Ratio Binaries
• On the coexistence of stellar-mass and intermediate-mass black holes in globular clusters
• Forced motion near black holes
• Gravitational waves from Extreme Mass Ratio Inspirals in non-pure Kerr spacetimes
• Binary black hole merger gravitational waves and recoil in the large mass ratio limit
• Targeted large mass ratio numerical relativity surrogate waveform model for GW190814
• Intermediate-mass-ratio-inspirals in the Einstein Telescope: I. Signal-to-noise ratio calculations
• Numerical-relativity validation of effective-one-body waveforms in the intermediate-mass-ratio regime
• Testing Chern-Simons modified gravity with observations of extreme-mass-ratio binaries

Cited by in corpus (3)

• Waveform accuracy and systematic uncertainties in current gravitational wave observations
• Survey of gravitational wave memory in intermediate mass ratio binaries
• Success of the small mass ratio approximation during the final orbits of binary black hole simulations