REVIEW 13 cited by
Accurate waveforms for eccentric, aligned-spin binary black holes: The multipolar effective-one-body model SEOBNRv5EHM
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
The measurement of orbital eccentricity in gravitational-wave (GW) signals will provide unique insights into the astrophysical origin of binary systems, while ignoring eccentricity in waveform models could introduce significant biases in parameter estimation and tests of General Relativity. Upcoming LIGO-Virgo-KAGRA observing runs are expected to detect a subpopulation of eccentric signals, making it vital to develop accurate waveform models for eccentric orbits. Here, employing recent analytical results through the third post-Newtonian order, we develop SEOBNRv5EHM: a new time-domain, effective-one-body, multipolar waveform model for eccentric binary black holes with spins aligned (or antialigned) with the orbital angular momentum. Besides the dominant (2,2) mode, the model includes the (2,1), (3,3), (3,2), (4,4) and (4,3) modes. We validate the model's accuracy by computing its unfaithfulness against 99 (28 public and 71 private) eccentric numerical-relativity (NR) simulations, produced by the Simulating eXtreme Spacetimes Collaboration. Importantly, for NR waveforms with initial GW eccentricities below 0.5, the maximum (2,2)-mode unfaithfulness across the total mass range 20-200 $M_\odot$ is consistently below or close to $1 \%$, with a median value of $ \sim 0.02 \% $, reflecting an accuracy improvement of approximately an order of magnitude compared to the previous-generation SEOBNRv4EHM and the state-of-the-art TEOBResumS-Dal\'i eccentric model. In the quasi-circular-orbit limit, SEOBNRv5EHM is in excellent agreement with the highly accurate SEOBNRv5HM model. The accuracy, robustness, and speed of SEOBNRv5EHM make it suitable for data analysis and astrophysical studies. We demonstrate this by performing a set of recovery studies of synthetic NR-signal injections, and parameter-estimation analyses of the events GW150914 and GW190521, which we find to have no eccentricity signatures.
Forward citations
Cited by 13 Pith papers
-
High-Post-Newtonian-Order Dynamics Induced by Tail-of-Tail Interactions: The Non-Geodesic Terms
The authors compute tail-of-tail contributions to the effective-one-body Q potential through p_r^12 and derive new second-order self-force redshift predictions for eccentric binaries.
-
Constraints on Line-of-Sight Acceleration from O1-O4
All known compact binary mergers show line-of-sight accelerations consistent with zero under a new time-domain Doppler-shift model, with current detectors only sensitive to high-acceleration scenarios.
-
Unified remnant models for aligned-spin, precessing, and eccentric binary black hole mergers
New analytic fits, gwModelRemS/P, predict remnant mass, spin, luminosity, and kick for black hole mergers from equal mass to q=1000, with a neural-flow model for precessing kicks.
-
Impact of eccentricity and higher-modes on neutron star-black hole parameter estimation
Eccentric NSBH signals like GW200105 contain much more information about masses, mass ratio, and effective spin per unit SNR than circular signals, but not about sky position or distance.
-
Assessing the waveform systematics from parameter estimation to population inference with eccentricity
Eccentric waveform-model differences, small per event, accumulate across the GWTC-4 catalog and alter inferred redshift evolution and effective-spin population distributions.
-
Impact of numerical-relativity waveform calibration on parametrized post-Einsteinian tests
NR late-inspiral calibration systematics in IMRPhenomD produce false ppE GR violations at O5 SNRs ≳60; an uncertainty-aware baseline restores consistency with GR up to SNR 330.
-
Advancing the Effective-One-Body Framework in the Test-Mass Limit
SEOB-TML cuts dephasing by up to an order of magnitude in the test-mass limit by Q-factorizing the flux (including horizon absorption) and by modeling mode mixing with extracted QNM coefficients.
-
Accelerated Sequential Posterior Inference via Reuse for Gravitational-Wave Analyses
ASPIRE reuses old posterior samples via normalizing flows and sequential Monte Carlo to produce unbiased posteriors and evidences under new models, cutting likelihood evaluations 4-10x.
-
Chase Orbits, not Time: A Scalable Paradigm for Long-Duration Eccentric Gravitational-Wave Surrogates
Eccentric inspiral waveforms are modeled against mean anomaly rather than time, yielding an order-of-magnitude compression and a 2.77e6 M surrogate that is ~20x faster to evaluate.
-
Improved post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries
The paper presents pyEFPE, a validated and publicly available frequency-domain post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries, with up to about a fifteen-fold speedup.
-
Testing the nature of GW200105 by probing the frequency evolution of eccentricity
GW200105's recovered eccentricity as a function of frequency is consistent with the general-relativistic decay law at 68% confidence, supporting the eccentric-orbit interpretation.
-
Potential science with GW250114 -- the loudest binary black hole merger detected to date
This simulation study forecasts that GW250114 can reveal measurable orbital eccentricity, decisive ringdown overtones, and tight black hole area theorem constraints.
-
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.
Discussion (0). Continue with ORCID to comment.