Comparing second-order gravitational self-force, numerical relativity and effective one body waveforms from inspiralling, quasi-circular and nonspinning black hole binaries

Abstract

We present the first systematic comparison between gravitational waveforms emitted by inspiralling, quasi-circular and nonspinning black hole binaries computed with three different approaches: second-order gravitational self-force (2GSF) theory, as implemented in the 1PAT1 model; numerical relativity (NR), as implemented by the SXS collaboration; and the effective one body (EOB) formalism, as implemented in the TEOBResumS waveform model. To compare the models we use both a standard, time-domain waveform alignment and a gauge-invariant analysis based on the dimensionless function $Q_{\omega }(\omega )\equiv {\omega }^2/\dot{\omega }$, where $\omega$ is the gravitational wave frequency. We analyse the domain of validity of the 1PAT1 model, deriving error estimates and showing that the effects of the final transition to plunge, which the model neglects, extend over a significantly larger frequency interval than one might expect. Restricting to the inspiral regime, we find that, while for mass ratios $q=m_1/m_2\le 10$ TEOBResumS is largely indistinguishable from NR, 1PAT1 has a significant dephasing $\gtrsim 1$rad; conversely, for $q\gtrsim 100$, 1PAT1 is estimated to have phase errors $<0.1$rad on a large frequency interval, while TEOBResumS develops phase differences $\gtrsim 1$rad with it. Most crucially, on that same large frequency interval we find good agreement between TEOBResumS and 1PAT1 in the intermediate regime $15\lesssim q\lesssim 64$, with $<0.5$rad dephasing between them. A simple modification to the TEOBResumS flux further improves this agreement for $q\gtrsim 30$, reducing the dephasing to $\approx 0.27$rad even at $q=128$. Our results pave the way for the construction of GSF-informed EOB models for both intermediate and extreme mass ratio inspirals for the next generation of gravitational wave detectors.

31 pages, 19 figures, published on Phys. Rev. D

References in corpus (29)

• Laser Interferometer Space Antenna
• An improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors
• Two timescale analysis of extreme mass ratio inspirals in Kerr. I. Orbital Motion
• Modeling the dynamics of tidally-interacting binary neutron stars up to merger
• Faithful Effective-One-Body waveforms of small-mass-ratio coalescing black-hole binaries
• An improved analytical description of inspiralling and coalescing black-hole binaries
• Fourth post-Newtonian effective one-body dynamics
• A new effective-one-body description of coalescing nonprecessing spinning black-hole binaries
• A Horizon Study for Cosmic Explorer: Science, Observatories, and Community
• Tidal effects in binary neutron star coalescence
• Improved effective-one-body description of coalescing nonspinning black-hole binaries and its numerical-relativity completion
• High-accuracy numerical simulation of black-hole binaries: Computation of the gravitational-wave energy flux and comparisons with post-Newtonian approximants
• Analytic modelling of tidal effects in the relativistic inspiral of binary neutron stars
• Binary black hole merger in the extreme mass ratio limit
• Gravitational-wave energy flux for compact binaries through second order in the mass ratio
• Nonrotating black hole in a post-Newtonian tidal environment
• Extreme Mass-Ratio Inspirals in the Effective-One-Body Approach: Quasi-Circular, Equatorial Orbits around a Spinning Black Hole
• A new gravitational wave generation algorithm for particle perturbations of the Kerr spacetime
• Binary black hole merger in the extreme-mass-ratio limit: a multipolar analysis
• Gravitational Self-Force Correction to the Innermost Stable Circular Equatorial Orbit of a Kerr Black Hole
• A new analytic representation of the ringdown waveform of coalescing spinning black hole binaries
• The second RIT binary black hole simulations catalog and its application to gravitational waves parameter estimation
• Binary black hole coalescence in the extreme-mass-ratio limit: testing and improving the effective-one-body multipolar waveform
• Spinning test-body orbiting around a Kerr black hole: circular dynamics and gravitational-wave fluxes
• Horizon-absorption effects in coalescing black-hole binaries: An effective-one-body study of the non-spinning case
• Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasi-circular and nonspinning black hole binaries II: the large-mass-ratio case
• Analytic determination of the eight-and-a-half post-Newtonian self-force contributions to the two-body gravitational interaction potential
• Quasi-5.5PN TaylorF2 approximant for compact binaries: point-mass phasing and impact on the tidal polarizability inference
• The antikick strikes back: recoil velocities for nearly-extremal binary black hole mergers in the test-mass limit

Cited by in corpus (1)

• Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasi-circular and nonspinning black hole binaries II: the large-mass-ratio case