期刊
PHYSICAL REVIEW LETTERS
卷 115, 期 3, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.115.031102
关键词
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资金
- NSF [PHY-1208881, PHY-1305682, PHY-0960291]
- NASA [NNX12AN10G]
- NSERC of Canada
- Canada Chairs Program
- Canadian Institute for Advanced Research
- Simons Foundation
- Sherman Fairchild Foundation
- NSF at Cornell [PHY-1306125, AST-1333129]
- NSF at Caltech [PHY-1440083, AST-1333520]
- NSF XSEDE network [TG-PHY990007N]
- Cal State Fullerton
- Canada Foundation for Innovation under the Compute Canada
- Government of Ontario, Ontario Research Fund-Research Excellence
- University of Toronto
We present the first numerical-relativity simulation of a compact-object binary whose gravitational waveform is long enough to cover the entire frequency band of advanced gravitational-wave detectors, such as LIGO, Virgo, and KAGRA, for mass ratio 7 and total mass as low as 45.5 M-circle dot. We find that effective-one-body models, either uncalibrated or calibrated against substantially shorter numerical-relativity waveforms at smaller mass ratios, reproduce our new waveform remarkably well, with a negligible loss in detection rate due to modeling error. In contrast, post-Newtonian inspiral waveforms and existing calibrated phenomenological inspiral-merger-ringdown waveforms display greater disagreement with our new simulation. The disagreement varies substantially depending on the specific post-Newtonian approximant used.
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