Journal
PHYSICAL REVIEW D
Volume 95, Issue 4, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.95.044028
Keywords
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Funding
- Sherman Fairchild Foundation
- NSF [PHY-1404569, PHY-1606654, AST-1333129, PHY-1307489, PHY-1606522]
- NSERC of Canada
- Ontario Early Researcher Awards Program
- Canada Research Chairs Program
- Canadian Institute for Advanced Research
- Canada Foundation for Innovation (CFI) under Compute Canada
- Government of Ontario
- Ontario Research Fund (ORF)-Research Excellence
- University of Toronto
- Canada Foundation for Innovation (CFI)
- Ministere de l'Economie, de l'Innovation et des Exportations du Quebec (MEIE)
- RMGA
- Fonds de recherche du Quebec-Nature et Technologies (FRQ-NT)
- Research Corporation for Science Advancement [PHY-1429873]
- Cal State Fullerton
- STFC [ST/N005430/1] Funding Source: UKRI
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1333129] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1429873, 1404569] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1606522, 1306125, 1606654] Funding Source: National Science Foundation
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We improve the accuracy of the effective-one-body (EOB) waveforms that were employed during the first observing run of Advanced LIGO for binaries of spinning, nonprecessing black holes by calibrating them to a set of 141 numerical-relativity (NR) waveforms. The NR simulations expand the domain of calibration toward larger mass ratios and spins, as compared to the previous EOBNR model. Merger-ringdown waveforms computed in black-hole perturbation theory for Kerr spins close to extremal provide additional inputs to the calibration. For the inspiral-plunge phase, we use a Markov-chain Monte Carlo algorithm to efficiently explore the calibration space. For the merger-ringdown phase, we fit the NR signals with phenomenological formulae. After extrapolation of the calibrated model to arbitrary mass ratios and spins, the (dominant-mode) EOBNR waveforms have faithfulness-at design Advanced-LIGO sensitivity-above 99% against all the NR waveforms, including 16 additional waveforms used for validation, when maximizing only on initial phase and time. This implies a negligible loss in event rate due to modeling for these binary configurations. We find that future NR simulations at mass ratios greater than or similar to 4 and double spin greater than or similar to 0.8 will be crucial to resolving discrepancies between different ways of extrapolating waveform models. We also find that some of the NR simulations that already exist in such region of parameter space are too short to constrain the low-frequency portion of the models. Finally, we build a reduced-order version of the EOBNR model to speed up waveform generation by orders of magnitude, thus enabling intensive data-analysis applications during the upcoming observation runs of Advanced LIGO.
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