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Detection and characterization of spin-orbit resonances in the advanced gravitational wave detectors era

Afle, Chaitanya and Gupta, Anuradha and Gadre, Bhooshan and Kumar, Prayush and Demos, Nick and Lovelace, Geoffrey and Choi, Han Gil and Lee, Hyung Mok and Mitra, Sanjit and Boyle, Michael and Hemberger, Daniel A. and Kidder, Lawrence E. and Pfeiffer, Harald P. and Scheel, Mark A. and Szilágyi, Béla (2018) Detection and characterization of spin-orbit resonances in the advanced gravitational wave detectors era. Physical Review D, 98 (8). Art. No. 083014. ISSN 2470-0010. http://resolver.caltech.edu/CaltechAUTHORS:20181017-113318542

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Abstract

Spin-orbit resonances have important astrophysical implications as the evolution and subsequent coalescence of supermassive black hole binaries in one of these configurations may lead to low recoil velocity of merger remnants. It has also been shown that black hole spins in comparable mass stellar-mass black hole binaries could preferentially lie in a resonant plane when their gravitational waves (GWs) enter the advanced LIGO frequency band [1]. Therefore, it is highly desirable to investigate the possibility of detection and subsequent characterization of such GW sources in the advanced detector era, which can, in turn, improve our perception of their high mass counterparts. The current detection pipelines involve only nonprecessing templates for compact binary searches whereas parameter estimation pipelines can afford to use approximate precessing templates. In this paper, we test the performance of these templates in detection and characterization of spin-orbit resonant binaries. We use fully precessing time-domain SEOBNRv3 waveforms as well as four numerical relativity (NR) waveforms to model GWs from spin-orbit resonant binaries and filter them through IMRPhenomD, SEOBNRv4 and IMRPhenomPv2 approximants. We find that the nonprecessing approximants IMRPhenomD and SEOBNRv4 recover only ∼70% of injections with fitting factor (FF) higher than 0.97 (or 90% of injections with FF>0.9). This loss in signal-to-noise ratio is mainly due to the missing physics in these approximants in terms of precession and nonquadrupole modes. However, if we use a new statistic, i.e., maximizing the matched filter output over the sky-location parameters as well, the precessing approximant IMRPhenomPv2 performs magnificently better than their nonprecessing counterparts with recovering 99% of the injections with FFs higher than 0.97. Interestingly, injections with Δϕ=180° have higher FFs (Δϕ is the angle between the components of the black hole spins in the plane orthogonal to the orbital angular momentum) as compared to their Δϕ=0° and generic counterparts. This is because Δϕ=180° binaries are not as strongly precessing as Δϕ=0° and generic binaries. This implies that we will have a slight observation bias towards Δϕ=180° and away from Δϕ=0° resonant binaries while using nonprecessing templates for searches. Moreover, all template approximants are able to recover most of the injected NR waveforms with FFs >0.95. For all the injections including NR, the systematic error in estimating chirp mass remains below <10% with minimum error for Δϕ=180° resonant binaries. The symmetric mass-ratio can be estimated with errors below 15%. The effective spin parameter χ_(eff) is measured with maximum absolute error of 0.13. The in-plane spin parameter χ_p is mostly underestimated indicating that a precessing signal will be recovered as a relatively less precessing signal. Based on our findings, we conclude that we not only need improvements in waveform models towards precession and nonquadrupole modes but also better search strategies for precessing GW signals.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/PhysRevD.98.083014DOIArticle
https://journals.aps.org/prd/abstract/10.1103/PhysRevD.98.083014PublisherArticle
https://arxiv.org/abs/1803.07695arXivDiscussion Paper
ORCID:
AuthorORCID
Pfeiffer, Harald P.0000-0001-9288-519X
Additional Information:© 2018 American Physical Society. Received 20 March 2018; published 16 October 2018. We thank Archisman Ghosh and Varun Srivastava for helpful discussions, and Richard O’Shaughnessy for providing valuable comments on the manuscript. C. A. thanks Inter-University Centre for Astronomy and Astrophysics, Pune for the hospitality, where most of the work is done. A. G. acknowledges support from SERB-NPDF Grant (No. PDF/2015/000263), NSF Grants No. AST-1716394 and No. AST-1708146, and the Charles E. Kaufman Foundation of The Pittsburgh Foundation. B. G. acknowledges the support of University Grants Commission (UGC), India. S. M. acknowledges support from the Department of Science & Technology (DST), India provided under the Swarna Jayanti Fellowships scheme. The work done by CSUF authors was supported in part by Grants No. NSF PHY-1307489, No. PHY-1606522, No. PHY-1654359 and No. PHY-1429873 and the computations we did were done on ORCA, a cluster supported in part by Grant No. NSF PHY-1429873, the Research Corporation, and Cal State Fullerton. We gratefully acknowledge support for this research at CITA from NSERC of Canada, the Ontario Early Researcher Awards Program, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research; at Caltech from the Sherman Fairchild Foundation and NSF Grants No. PHY-1404569 and No. AST-1333520; and at Cornell from the Sherman Fairchild Foundation and NSF Grants No. PHY-1606654 and No. ACI-1713678. This research is benefited from a grant awarded to IUCAA by the Navajbai Ratan Tata Trust (NRTT). Numerical calculations were partially carried out through the HPC support program by KISTI to HML in 2016. We are grateful for computational resources provided by the Leonard E Parker Center for Gravitation, Cosmology and Astrophysics at University of Wisconsin-Milwaukee, the Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Hannover, Inter-University Centre for Astronomy and Astrophysics, Pune and LIGO-Caltech. This paper has LIGO document number LIGO-P1500266.
Group:LIGO
Funders:
Funding AgencyGrant Number
Science and Engineering Research Board (SERB)PDF/2015/000263
NSFAST-1716394
NSFAST-1708146
Pittsburgh FoundationUNSPECIFIED
University Grants Commission (India)UNSPECIFIED
Department of Science and Technology (India)UNSPECIFIED
NSFPHY-1307489
NSFPHY-1606522
NSFPHY-1654359
NSFPHY-1429873
Research CorporationUNSPECIFIED
California State University, FullertonUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Ontario Early Researcher Awards ProgramUNSPECIFIED
Canada Research Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-1404569
NSFAST-1333520
NSFPHY-1606654
NSFACI-1713678
Navajbai Ratan Tata TrustUNSPECIFIED
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentP1500266
Record Number:CaltechAUTHORS:20181017-113318542
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20181017-113318542
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:90308
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:18 Oct 2018 13:05
Last Modified:18 Oct 2018 16:33

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