Effective-one-body model for black-hole binaries with generic mass ratios and spins

By A. Taracchini, A. Buonanno, Yi Pan, T. Hinderer, M. Boyle, Daniel A. Hemberger, Lawrence E. Kidder, G. Lovelace, A. Mroué, Harald P. Pfeiffer and 4 more. Physical Review D, 2013

325 citations recorded by the source corpus.

Gravitational waves emitted by black-hole binary systems have the highest signal-to-noise ratio in LIGO and Virgo detectors when black-hole spins are aligned with the orbital angular momentum and extremal. For such systems, we extend the effective-one-body inspiral-merger-ringdown waveforms to generic mass ratios and spins calibrating them to 38 numerical-relativity nonprecessing waveforms produced by the SXS Collaboration. The numerical-relativity simulations span mass ratios from 1 to 8, spin magnitudes up to 98% of extremality, and last for 40 to 60 gravitational-wave cycles. When the total mass of the binary is between 20 and 200M_⊙, the effective-one-body nonprecessing (dominant mode) waveforms have overlap above 99% (using the advanced-LIGO design noise spectral density) with all of the 38 nonprecessing numerical waveforms, when maximizing only on initial phase and time. This implies a negligible loss in event rate due to modeling. We also show that—without further calibration— the precessing effective-one-body (dominant mode) waveforms have overlap above 97% with two very long, strongly precessing numerical-relativity waveforms, when maximizing only on the initial phase and time.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/782264220dcef35ea5219be77d961a3ff8177638

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Citations in the corpus

A Future Percent-level Measurement of the Hubble Expansion at Redshift 0.8 with Advanced LIGO (2019, background): “Using parameterized models of these waveforms (Taracchini et al. 2014; Khan et al. 2016; Bohé et al. 2017; Chatziioannou et al. 2017), it will be possible to measure the detector-frame masses with ~20% uncertainty and luminosity distances (Hogg 1999) with ~50% uncertainty for a source near the…”
THE RATE OF BINARY BLACK HOLE MERGERS INFERRED FROM ADVANCED LIGO OBSERVATIONS SURROUNDING GW150914 (2016, methodology): “…correspond to BBH systems with spins aligned with the orbital angular momentum and are generated using the effective one body (EOB) formalism (Taracchini et al. 2014; Pürrer 2016); in nature we would never expect perfect spin alignment, but nevertheless the EOB waveforms are a good fit to…”
Dynamical Tides in General Relativity: Effective Action and Effective-One-Body Hamiltonian (2016, methodology): “For instance, in the case of spinning black holes, different proposals exist [60, 61].”
Properties of the Binary Neutron Star Merger GW170817 (2018, methodology): “PhenomDNRT is based on an aligned-spin point-particle model [76,77] calibrated to untuned EOB waveforms [90] and NR hybrids [76,77].”
2-OGC: Open Gravitational-wave Catalog of Binary Mergers from Analysis of Public Advanced LIGO and Virgo Data (2019, methodology): “We use the spinning effective-onebody model (SEOBNRv4) for templates corresponding to mergers with (redshifted, detector frame) total mass m1 + m2 > 4M (Taracchini et al. 2014; Bohé et al. 2016).”
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “…albeit differently: IMRPhenomPv2(Hannam et al. 2014; Husa et al. 2016; Khan et al. 2016), which includes an effective representation(Schmidt et al. 2015) of precession effects, and SEOBNRv3(Pan et al. 2014; Taracchini et al. 2014; Babak et al. 2017), which incorporates all spin degrees of freedom.”
1-OGC: The First Open Gravitational-wave Catalog of Binary Mergers from Analysis of Public Advanced LIGO Data (2018, methodology): “For binaries with total mass greater than 4Me, we use the spinning effective-one-body model (SEOBNRv4;Taracchini et al. 2014; Bohé et al. 2016) as template gravitational waveforms.”