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TEOBResumS: assessment of consistent next-to-quasicircular corrections and post-adiabatic approximation in multipolar binary black holes waveforms
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abstract
The use of effective-one-body (EOB) waveforms for black hole binaries analysis in gravitational-wave astronomy requires faithful models and fast generation times. A key aspect to achieve faithfulness is the inclusion of numerical-relativity (NR) informed next-to-quasicircular corrections(NQC), dependent on the radial momentum, to the waveform and radiation reaction. A robust method to speed up the waveform generation is the post-adiabatic iteration to approximate the solution of the EOB Hamiltonian equations. In this work, we assess the performances of a fast NQC prescription in combination to the post-adiabatic method for generating multipolar gravitational waves. The outlined approach allows a consistent treatment of NQC in both the waveform and the radiation-reaction, does not require iterative procedures to achieve high faithfulness, and can be efficiently employed for parameter estimation. Comparing to 611 NR simulations, for total mass $10M_\odot\leq M \leq 200M_\odot$ and using the Advanded LIGO noise, the model has EOB/NR unfaithfulness well below $0.01$, with 78.5\% of the cases below $0.001$. We apply the model to the parameter estimation of GW150914 exploring the impact of the new NQC and of the higher modes up to $\ell=m=8$.
Forward citations
Cited by 5 Pith papers
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Advancing the Effective-One-Body Framework in the Test-Mass Limit
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Can Eccentric Binary Black Hole Signals Mimic Gravitational-Wave Microlensing?
Eccentric BBH signals can masquerade as wave-optics microlensing in quasicircular analyses, but eccentric recovery templates break the degeneracy.
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Black-hole - neutron-star mergers: new numerical-relativity simulations and multipolar effective-one-body model with spin precession and eccentricity
A new catalog of 52 numerical-relativity BHNS merger simulations is used to calibrate TEOBResumS-Dalí, an improved effective-one-body waveform model with multipolar ringdown, spin precession, and eccentricity.
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Self-force framework for merger-ringdown waveforms
A phase-space self-force framework is extended through the final plunge to produce merger-ringdown waveforms at leading geodesic order, with stationary-phase and quasinormal-mode approximations both failing near the p...
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Revisiting GW150914 with a non-planar, eccentric waveform model
Using a waveform model that includes both eccentricity and spin precession, the authors confirm GW150914 was a quasi-circular, slowly spinning black hole merger, with eccentricity below 0.08 at 15 Hz.
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