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| SEOBNRv4 | |
|---|---|
| Name | SEOBNRv4 |
| Title | SEOBNRv4 |
| Developer | LIGO Scientific Collaboration and Numerical Relativity |
| Released | 2017 |
| Latest release | 2018 |
| Programming language | C, Fortran |
| Operating system | Unix-like |
| Genre | Gravitational-wave waveform model |
SEOBNRv4 is a waveform model used in the analysis of compact-object coalescences detected by the LIGO Scientific Collaboration, Virgo Collaboration, and related observatories. It is an effective-one-body inspiral–merger–ringdown model calibrated to numerical relativity results for quasi-circular, spinning binary black holes, designed for parameter estimation and detection studies in the context of observations such as GW150914, GW151226, and later events. The model interoperates with software ecosystems including LALSuite, PyCBC, and Bilby for Bayesian inference and matched-filter searches.
SEOBNRv4 was developed within collaborations involving researchers associated with Caltech, Massachusetts Institute of Technology, Cardiff University, and groups contributing to LIGO Scientific Collaboration efforts. It builds on the effective-one-body (EOB) approach pioneered by teams around Thibault Damour, Alessandra Buonanno, and others, and specifically extends earlier waveform families used in analyses of events like GW150914 and GW170104. The model targets aligned-spin, non-precessing binaries and aims to capture dynamics across inspiral, merger, and ringdown stages relevant to detectors such as LIGO Hanford Observatory and LIGO Livingston Observatory.
SEOBNRv4 encodes two-body dynamics via an effective Hamiltonian formalism influenced by post-Newtonian results from groups at PN Approximation Research and analytic resummation techniques developed by researchers connected to Institut d'Astrophysique de Paris and Sapienza University of Rome. Radiation reaction is incorporated through factorized waveform multipoles and energy flux prescriptions informed by studies tied to Teukolsky equation approaches and perturbation theory associated with Regge–Wheeler and Zerilli frameworks. The merger–ringdown matching uses complex quasi-normal mode spectra computed for Kerr black holes studied by teams at University of Illinois Urbana–Champaign and Harvard University. Spin effects in SEOBNRv4 adopt calibration choices reflecting results from groups led by Mark Hannam and Achamveedu Gopakumar.
Calibration of SEOBNRv4 involved comparison to large sets of high-accuracy numerical relativity waveforms produced by collaborations such as the Simulating eXtreme Spacetimes (SXS) Collaboration, the Georgia Tech Numerical Relativity Group, and the RIT Numerical Relativity Group. Validation studies benchmarked phase and amplitude against waveforms from simulations associated with Frans Pretorius, Maya code development teams, and efforts at Max Planck Institute for Gravitational Physics (Albert Einstein Institute). Error budgets were assessed using mismatch metrics similar to those applied in analyses of GW170814 and GW170817 to ensure consistency within detector sensitivity bands for Advanced LIGO and Advanced Virgo.
SEOBNRv4 is implemented in the LALSuite library used by the LIGO Scientific Collaboration and is callable from analysis packages including PyCBC, GstLAL, and Bilby for parameter estimation with samplers like LALInference, emcee, and dynesty. The implementation interfaces with waveform infrastructure developed at institutions such as Caltech, MIT, and Cardiff University and is distributed alongside other waveform families like models from the IMRPhenom family produced by collaborations involving Max Planck Institute for Gravitational Physics (Albert Einstein Institute) researchers. Cross-language bindings and performance optimizations leverage community tools maintained by contributors at GitHub and research groups with expertise from University of Cambridge.
SEOBNRv4 offers phase coherence and amplitude fidelity tuned to numerical-relativity standards for mass ratios up to the calibration range and spin magnitudes below the model limits reported by teams at SXS Collaboration and RIT. Typical mismatches against reference simulations were evaluated over frequency bands relevant to Advanced LIGO sensitivity curves developed by engineers at LIGO Laboratory. Computational cost is higher than phenomenological models like IMRPhenomD but optimizations and reduced-order modeling initiatives from groups at Cornell University and University of Birmingham have produced faster surrogates suitable for large-scale parameter estimation campaigns used in studies of events such as GW170729.
SEOBNRv4 has been used for parameter estimation and model selection in published analyses by the LIGO Scientific Collaboration and Virgo Collaboration, informing astrophysical inference on source properties for events including GW150914 and subsequent binary black hole detections cataloged by collaborations involving Nitz (researcher) and B. P. Abbott. The model supports tests of general relativity frameworks explored by groups at Perimeter Institute and Albert Einstein Institute, and it contributes to population studies by teams at Monash University and University of Portsmouth that synthesize results from multiple catalogs.
SEOBNRv4 is limited to aligned-spin, quasi-circular binaries and does not include precession or eccentricity effects developed in waveform families by researchers such as those at Caltech and MIT. Ongoing development efforts aim to extend effective-one-body formalisms to precessing systems, eccentric waveforms, and higher-mode inclusions pursued by collaborations at Cardiff University, RIT, and the SXS Collaboration. Future improvements are expected through continued synergy with numerical relativity groups at Max Planck Institute for Gravitational Physics (Albert Einstein Institute), enhanced calibration datasets from SXS Collaboration, and integration with surrogate-model frameworks developed at Caltech and Cornell University.