All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.
hub Mixed citations
Pompili et al
Mixed citation behavior. Most common role is background (67%).
31
Pith papers citing it
Background
67% of classified citations
abstract
We present SEOBNRv5HM, a more accurate and faster inspiral-merger-ringdown gravitational waveform model for quasi-circular, spinning, nonprecessing binary black holes within the effective-one-body (EOB) formalism. Compared to its predecessor, SEOBNRv4HM, the waveform model i) incorporates recent high-order post- Newtonian results in the inspiral, with improved resummations, ii) includes the gravitational modes (l, |m|) = (3, 2), (4, 3), in addition to the (2, 2), (3, 3), (2, 1), (4, 4), (5, 5) modes already implemented in SEOBNRv4HM, iii) is calibrated to larger mass-ratios and spins using a catalog of 442 numerical-relativity (NR) simulations and 13 additional waveforms from black-hole perturbation theory, iv) incorporates information from second-order gravitational self-force (2GSF) in the nonspinning modes and radiation-reaction force. Computing the unfaithfulness against NR simulations, we find that for the dominant (2, 2) mode the maximum unfaithfulness in the total mass range $10-300 M_{\odot}$ is below $10^{-3}$ for 90% of the cases (38% for SEOBNRv4HM). When including all modes up to l = 5 we find 98% (49%) of the cases with unfaithfulness below $10^{-2} (10^{-3})$, while these numbers reduce to 88% (5%) when using SEOBNRv4HM. Furthermore, the model shows improved agreement with NR in other dynamical quantities (e.g., the angular momentum flux and binding energy), providing a powerful check of its physical robustness. We implemented the waveform model in a high-performance Python package (pySEOBNR), which leads to evaluation times faster than SEOBNRv4HM by a factor 10 to 50, depending on the configuration, and provides the flexibility to easily include spin-precession and eccentric effects, thus making it the starting point for a new generation of EOBNR waveform models (SEOBNRv5) to be employed for upcoming observing runs of the LIGO-Virgo-KAGRA detectors.
hub tools
citation-role summary
background 10
method 5
citation-polarity summary
representative citing papers
All gravitational-wave binaries analyzed through O4a are consistent with zero line-of-sight acceleration, measured with a new time-domain Doppler method applicable to any waveform model.
Bayesian analysis of GW230627 and GW250114 finds no deviation from GR at 4PN and 4.5PN orders, setting the first empirical baseline with 90% intervals of order O(1)-O(10).
New frequency-domain models IMRPhenomXHM_NSBH, SEOBNRv5HM_ROM_NRTidalv3_NSBH, and IMRPhenomXPHM_NSBH bring higher-order modes and tidal effects to fast NSBH waveform templates.
SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.
The gwNRHME framework constructs a multi-modal non-spinning eccentric gravitational waveform surrogate by modulating quasi-circular models with universal eccentric functions, achieving median mismatches of ~9e-5 against 156 NR waveforms.
Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dynamical parameters.
Closed-form Sommerfeld factor via EFT connection matrix with analytic O(G^10) magnitude and phase for l=0,1,2 waves, plus a new RG equation for radiative multipole moments that improves waveform resummation beyond tail logarithms.
A universal anomalous dimension for multipole moments in GR is derived via two EFT methods and applied to resum short-distance logarithmic tails in binary gravitational waveforms.
A mixture-model framework for combining gravitational-wave tests of General Relativity yields Bayes factors of 10-20 favoring GR, substantially lower than existing methods that assume uniform deviations across events.
Near-identity averaging transformations applied to osculating orbital elements reduce the computational cost of eccentric EOB inspirals by up to two orders of magnitude while maintaining accuracy for moderate to large eccentricities at NNLO.
SEOBNRv6EHM reduces parameter biases for eccentric binaries versus prior models and shows mild support for eccentricity in five catalog events plus comparable unbound fits for three high-mass events.
SPRING framework propagates pre-merger information into spectral-level ringdown inference, improving Bayesian support for an agnostic two-damped-sinusoid model on GW250114 by ΔlnB ~5-10 while keeping remnant posteriors consistent with IMR estimates.
FluxMC integrates flow matching with parallel tempering MCMC to converge in under five hours on high-fidelity IMRPhenomHM waveforms for massive black hole binaries, where standard methods fail after hundreds of hours and produce two to three orders of magnitude higher distributional error.
A framework using scale separation in the Isaacson description defines observable gravitational memory rise for compact binary coalescences, providing a basis for hypothesis testing in LISA data.
GW250114 data constrains GR deviations in merger amplitude to 10% and frequency to 4% at 90% CL, with first bounds on the (4,4) mode frequency at 6%.
Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.
GW250114 data confirm the remnant is consistent with a Kerr black hole and bound the dominant quadrupolar mode frequency to within a few percent of the GR prediction, with constraints tighter than prior multi-event catalogs.
BHPTNRSur2dq1e3 is a new surrogate model for spinning intermediate-mass-ratio black hole binary gravitational waves, constructed from ppBHPT training data with domain decomposition for retrograde modes and calibrated to NR simulations.
Bayesian inference on LVK O1-O3 events with eccentric aligned-spin waveforms yields log10 Bayes factors of 1.77-4.75 favoring eccentricity for GW200129, GW190701 and GW200208_22, and >99.5% probability that at least one of 57 events is eccentric under an astrophysically motivated rate prior.
An idealized Gaussian model demonstrates that single-event correlations inflate uncertainties in population correlations and that catalog-wide correlated biases can be misread as population correlations.
Outlines a Schwinger-Keldysh path-integral framework that derives worldline equations of motion and computes weak-field gravitational waveforms independently for unspecified relativistic orbits.
Hybrid SPA-plus-FFT frequency-domain version of SEOBNRv5THM for quasi-circular spin-aligned BNS systems matches time-domain baseline accuracy while cutting computational cost for long signals.
Hierarchical Bayesian inference on GWTC-5.0 constrains the memory enhancement factor to 0.26 with large uncertainties consistent with the GR value of 1 and forecasts that 2000 detections are needed for a 1σ constraint away from zero.
citing papers explorer
-
Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries
All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.
-
Constraints on Line-of-Sight Acceleration from O1-O4
All gravitational-wave binaries analyzed through O4a are consistent with zero line-of-sight acceleration, measured with a new time-domain Doppler method applicable to any waveform model.
-
Tests of general relativity at the fourth post-Newtonian order with GW230627 and GW250114
Bayesian analysis of GW230627 and GW250114 finds no deviation from GR at 4PN and 4.5PN orders, setting the first empirical baseline with 90% intervals of order O(1)-O(10).
-
Fast gravitational waveform models for quasi-circular coalescences of neutron star--black hole binaries
New frequency-domain models IMRPhenomXHM_NSBH, SEOBNRv5HM_ROM_NRTidalv3_NSBH, and IMRPhenomXPHM_NSBH bring higher-order modes and tidal effects to fast NSBH waveform templates.
-
Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM
SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.
-
Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions
The gwNRHME framework constructs a multi-modal non-spinning eccentric gravitational waveform surrogate by modulating quasi-circular models with universal eccentric functions, achieving median mismatches of ~9e-5 against 156 NR waveforms.
-
Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms
Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dynamical parameters.
-
Gravitational Sommerfeld Effects: Formalism, Renormalization, and Perturbation to $O(G^{10})$
Closed-form Sommerfeld factor via EFT connection matrix with analytic O(G^10) magnitude and phase for l=0,1,2 waves, plus a new RG equation for radiative multipole moments that improves waveform resummation beyond tail logarithms.
-
Resummation of Universal Tails in Gravitational Waveforms
A universal anomalous dimension for multipole moments in GR is derived via two EFT methods and applied to resum short-distance logarithmic tails in binary gravitational waveforms.
-
Testing General Relativity with GWTC-4.0 through mixture models
A mixture-model framework for combining gravitational-wave tests of General Relativity yields Bayes factors of 10-20 favoring GR, substantially lower than existing methods that assume uniform deviations across events.
-
Efficient Eccentric Effective-One-Body Dynamics via Near-Identity Averaging Transformations
Near-identity averaging transformations applied to osculating orbital elements reduce the computational cost of eccentric EOB inspirals by up to two orders of magnitude while maintaining accuracy for moderate to large eccentricities at NNLO.
-
Eccentric and unbound compact binaries in the LIGO-Virgo-KAGRA catalog: parameter estimation and waveform systematics with SEOBNRv6EHM
SEOBNRv6EHM reduces parameter biases for eccentric binaries versus prior models and shows mild support for eccentricity in five catalog events plus comparable unbound fits for three high-mass events.
-
A pre-merger-informed spectral-level ringdown inference framework for black-hole spectroscopy
SPRING framework propagates pre-merger information into spectral-level ringdown inference, improving Bayesian support for an agnostic two-damped-sinusoid model on GW250114 by ΔlnB ~5-10 while keeping remnant posteriors consistent with IMR estimates.
-
FluxMC: Rapid and High-Fidelity Inference for Space-Based Gravitational-Wave Observations
FluxMC integrates flow matching with parallel tempering MCMC to converge in under five hours on high-fidelity IMRPhenomHM waveforms for massive black hole binaries, where standard methods fail after hundreds of hours and produce two to three orders of magnitude higher distributional error.
-
Toward claiming a detection of gravitational memory
A framework using scale separation in the Isaacson description defines observable gravitational memory rise for compact binary coalescences, providing a basis for hypothesis testing in LISA data.
-
Plunge-Merger-Ringdown Tests of General Relativity with GW250114
GW250114 data constrains GR deviations in merger amplitude to 10% and frequency to 4% at 90% CL, with first bounds on the (4,4) mode frequency at 6%.
-
Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary
Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.
-
Black Hole Spectroscopy and Tests of General Relativity with GW250114
GW250114 data confirm the remnant is consistent with a Kerr black hole and bound the dominant quadrupolar mode frequency to within a few percent of the GR prediction, with constraints tighter than prior multi-event catalogs.
-
Gravitational wave surrogate model for spinning, intermediate mass ratio binaries based on perturbation theory and numerical relativity
BHPTNRSur2dq1e3 is a new surrogate model for spinning intermediate-mass-ratio black hole binary gravitational waves, constructed from ppBHPT training data with domain decomposition for retrograde modes and calibrated to NR simulations.
-
Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA
Bayesian inference on LVK O1-O3 events with eccentric aligned-spin waveforms yields log10 Bayes factors of 1.77-4.75 favoring eccentricity for GW200129, GW190701 and GW200208_22, and >99.5% probability that at least one of 57 events is eccentric under an astrophysically motivated rate prior.
-
Population-level correlations in Bayesian statistics: an illustrative model for gravitational-wave astronomy
An idealized Gaussian model demonstrates that single-event correlations inflate uncertainties in population correlations and that catalog-wide correlated biases can be misread as population correlations.
-
Weak-field waveforms for generic relativistic orbits
Outlines a Schwinger-Keldysh path-integral framework that derives worldline equations of motion and computes weak-field gravitational waveforms independently for unspecified relativistic orbits.
-
Speed and accuracy for long signals: Frequency-domain effective-one-body waveforms for compact binary coalescences
Hybrid SPA-plus-FFT frequency-domain version of SEOBNRv5THM for quasi-circular spin-aligned BNS systems matches time-domain baseline accuracy while cutting computational cost for long signals.
-
Constraining Gravitational Wave Memory with Hierarchical Inference
Hierarchical Bayesian inference on GWTC-5.0 constrains the memory enhancement factor to 0.26 with large uncertainties consistent with the GR value of 1 and forecasts that 2000 detections are needed for a 1σ constraint away from zero.
-
Dynamical quasinormal mode excitation II: propagation and convergence in Schwarzschild
Refined propagation prescription for quasinormal modes excited by plunging particles confirms a bounce radius at r_*=0 and yields accurate reproduction of the post-bounce oscillatory waveform component from first principles.
-
Detectability of Gravitational-Wave Memory with LISA: A Bayesian Approach
Bayesian parameter estimation on simulated LISA data establishes conditions for detecting displacement memory in MBHB events and projects observation rates from population models.
-
Gravitational radiation from hyperbolic orbits: comparison between self-force, post-Minkowskian, post-Newtonian, and numerical relativity results
Self-force calculations of radiated gravitational wave energy from hyperbolic orbits around Schwarzschild black holes agree with post-Minkowskian results for large impact parameters and velocities up to 0.7c, with further comparisons to post-Newtonian and numerical relativity.
-
GW250114: testing Hawking's area law and the Kerr nature of black holes
GW250114 data confirm the remnant black hole ringdown frequencies lie within 30% of Kerr predictions and that the final horizon area is larger than the sum of the progenitors' areas to high credibility.
- Horizon absorption in eccentric precessing binary black hole inspirals and its importance for gravitational wave data analysis
- GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors
- Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects