Effective-one-body model for black-hole binaries with generic mass ratios and spins
Creators
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1.
University of Maryland, College Park
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2.
Cornell University
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3.
California Institute of Technology
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4.
California State University, Fullerton
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5.
Canadian Institute for Theoretical Astrophysics
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6.
Canadian Institute for Advanced Research
Abstract
Gravitational waves emitted by black-hole binary systems have the highest signal-to-noise ratio in LIGO and Virgo detectors when black-hole spins are aligned with the orbital angular momentum and extremal. For such systems, we extend the effective-one-body inspiral-merger-ringdown waveforms to generic mass ratios and spins calibrating them to 38 numerical-relativity nonprecessing waveforms produced by the SXS Collaboration. The numerical-relativity simulations span mass ratios from 1 to 8, spin magnitudes up to 98% of extremality, and last for 40 to 60 gravitational-wave cycles. When the total mass of the binary is between 20 and 200M_⊙, the effective-one-body nonprecessing (dominant mode) waveforms have overlap above 99% (using the advanced-LIGO design noise spectral density) with all of the 38 nonprecessing numerical waveforms, when maximizing only on initial phase and time. This implies a negligible loss in event rate due to modeling. We also show that—without further calibration— the precessing effective-one-body (dominant mode) waveforms have overlap above 97% with two very long, strongly precessing numerical-relativity waveforms, when maximizing only on the initial phase and time.
Additional Information
© 2014 American Physical Society. Received 12 November 2013; published 13 March 2014. A. B., T. H., Y. P., and A. T. acknowledge partial support from NSF Grants No. PHY-0903631 and No. PHY- 1208881. A. B. also acknowledges partial support from NASA Grant No. NNX12AN10G. T. H. and A. T. also acknowledge support from the Maryland Center for Fundamental Physics. A. M. and H. P. gratefully acknowledge support from NSERC of Canada, the Canada Chairs Program, and the Canadian Institute for Advanced Research. M. B., D. H., and L. K. gratefully acknowledge support from the Sherman Fairchild Foundation, and from NSF Grants No. PHY-1306125 and No. PHY-1005426 at Cornell. M. S., B. S., N. T., and A. Z. acknowledge support from the Sherman Fairchild Foundation and from NSF Grants No. PHY-106881, No. PHY-1005655, and No. DMS-1065438 at Caltech. G. L. acknowledges partial support from NSF Grant No. PHY-1307489. Simulations used in this work were computed with the SPEC code [29]. Computations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291, on the NSF XSEDE network under Grant No. TG-PHY990007N, on the Orca cluster supported by Cal State Fullerton, and on the GPC supercomputer at the SciNet HPC Consortium [30]. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund–Research Excellence, and the University of Toronto.Attached Files
Published - PhysRevD.89.061502.pdf
Submitted - 1311.2544v1.pdf
Files
1311.2544v1.pdf
Additional details
Identifiers
- Eprint ID
- 45187
- Resolver ID
- CaltechAUTHORS:20140424-093721400
Related works
- Describes
- http://arxiv.org/abs/1311.2544 (URL)
Funding
- NSF
- PHY-0903631
- NSF
- PHY-1208881
- NASA
- NNX12AN10G
- Maryland Center for Fundamental Physics
- NSERC (Canada)
- Canada Chairs Program
- Canadian Institute for Advanced Research
- Sherman Fairchild Foundation
- NSF
- PHY-1306125
- NSF
- PHY-1005426
- NSF
- PHY-106881
- NSF
- PHY-1005655
- NSF
- DMS-1065438
- NSF
- PHY-1307489
Dates
- Created
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2014-04-24Created from EPrint's datestamp field
- Updated
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2021-11-10Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Physics Department