Including mode mixing in a higher-multipole model for gravitational waveforms from nonspinning black-hole binaries
Creators
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1.
International Centre for Theoretical Sciences
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2.
Indian Institute of Science Bangalore
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3.
Washington State University
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4.
University of Cambridge
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5.
Indian Institute of Technology Madras
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6.
California Institute of Technology
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7.
Canadian Institute for Advanced Research
Abstract
As gravitational-wave (GW) observations of binary black holes are becoming a precision tool for physics and astronomy, several subdominant effects in the GW signals need to be accurately modeled. Previous studies have shown that neglecting subdominant modes in the GW templates causes an unacceptable loss in detection efficiency and large systematic errors in the estimated parameters for binaries with large mass ratios. Our recent work [Mehta et al., Phys. Rev. D 96, 124010 (2017)] constructed a phenomenological gravitational waveform family for nonspinning black-hole binaries that includes subdominant spherical harmonic modes (ℓ=2, m=±1), (ℓ=3, m=±3), and (ℓ=4, m=±4) in addition to the dominant quadrupole mode, (ℓ=2, m=±2). In this article, we construct analytical models for the (ℓ=3, m=±2) and (ℓ=4, m= ±3) modes and include them in the existing waveform family. Accurate modeling of these modes is complicated by the mixing of multiple spheroidal harmonic modes. We develop a method for accurately modeling the effect of mode mixing, thus producing an analytical waveform family that has faithfulness greater than 99.6%.
Additional Information
© 2019 American Physical Society. Received 15 February 2019; published 16 July 2019. We are grateful to the SXS Collaboration for making a public catalog of numerical-relativity waveforms. We also thank Emanuele Berti and Michael Boyle for useful discussions and clarifications, Frank Ohme for helpful comments, and Mark Scheel for providing a Cauchy-characteristic extraction SXS waveform for comparison. A. K.M., P. A., and V. V. acknowledge support from the Indo-US Centre for the Exploration of Extreme Gravity funded by the Indo-US Science and Technology Forum (Grant No. IUSSTF/JC-029/2016). N. K. J.-M. acknowledges support from the AIRBUS GroupCorporate Foundation through a chair in "Mathematics of Complex Systems" at the International Centre for Theoretical Sciences (ICTS) and from STFC Consolidator Grant No. ST/L000636/1. Also, this work has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie Grant No. 690904. P. A.'s research was supported by the Max Planck Society through a Max Planck Partner Group at ICTS-TIFR and by the Canadian Institute for Advanced Research through the CIFAR Azrieli Global Scholars program. V. V.'s research was supported by the Sherman Fairchild Foundation, and NSF Grants No. PHY–170212 and No.PHY–1708213 at Caltech.Computations were performed at the ICTS cluster Alice. This document has LIGO preprint number LIGO-P1800203-v6.Attached Files
Published - PhysRevD.100.024032.pdf
Accepted Version - 1902.02731.pdf
Files
1902.02731.pdf
Additional details
Identifiers
- Eprint ID
- 97172
- Resolver ID
- CaltechAUTHORS:20190716-111910657
Related works
- Describes
- https://arxiv.org/abs/1902.02731 (URL)
Funding
- Indo-US Science and Technology Forum
- IUSSTF/JC-029/ 2016
- AIRBUS Group Corporate Foundation
- Science and Technology Facilities Council (STFC)
- ST/L000636/1
- Marie Curie Fellowship
- 690904
- Max Planck Society
- Canadian Institute for Advanced Research (CIFAR)
- Sherman Fairchild Foundation
- NSF
- PHY-170212
- NSF
- PHY-1708213
Dates
- Created
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2019-07-16Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- LIGO
- Other Numbering System Name
- LIGO Document
- Other Numbering System Identifier
- LIGO-P1800203-v6