Details
| Original language | English |
|---|---|
| Article number | 023016 |
| Number of pages | 14 |
| Journal | Physical Review D |
| Volume | 109 |
| Issue number | 2 |
| Publication status | Published - 10 Jan 2024 |
Abstract
We investigate the prospect of performing a null test of binary black hole (BBH) nature using spin-induced quadrupole moment (SIQM) measurements. This is achieved by constraining a deviation parameter (δκ) related to the parameter (κ) that quantifies the degree of deformation due to the spin of individual binary components on leading (quadrupolar) spin-induced moment. Throughout the paper, we refer to κ as the SIQM parameter and δκ as the SIQM-deviation parameter. The test presented here extends the earlier SIQM-based null tests for BBH nature by employing waveform models that account for double spin-precession and higher modes. We find that waveform with double spin-precession gives better constraints for δκ, compared to waveform with single spin-precession. We also revisit earlier constraints on the SIQM-deviation parameter for selected GW events observed through the first three observing runs (O1-O3) of LIGO-Virgo detectors. Additionally, the effects of higher-order modes on the test are also explored for a variety of mass-ratio and spin combinations by injecting simulated signals in zero-noise. Our analyses indicate that binaries with mass-ratio greater than three and significant spin precession may require waveforms that account for spin-precession and higher modes to perform the parameter estimation reliably.
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Nuclear and High Energy Physics
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In: Physical Review D, Vol. 109, No. 2, 023016, 10.01.2024.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Effect of double spin-precession and higher harmonics on spin-induced quadrupole moment measurements
AU - Divyajyoti,
AU - Krishnendu, N. V.
AU - Saleem, Muhammed
AU - Colleoni, Marta
AU - Vijaykumar, Aditya
AU - Arun, K. G.
AU - Mishra, Chandra Kant
N1 - Funding Information: We thank Michalis Agathos for his useful comments on the manuscript. D. J. thanks Sayantani Datta, Pankaj Saini, and Sajad A. Bhat for useful discussions. We thank Anuradha Gupta, Archisman Ghosh, and Ish Gupta for the review of the waveform code, and Pankaj Saini and Sijil Jose for help with the review readiness. N. V. K. acknowledges the support from the Science and Engineering Research Board (SERB), Government of India, through the National Post Doctoral Fellowship Grant (Reg. No. PDF/2022/000379). M. S. acknowledges the support from the National Science Foundation with Grants No. PHY-1806630, PHY-2010970, and PHY-2110238. A. V. is supported by the Department of Atomic Energy, Government of India, under Project No. RTI4001. A. V. also acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC) (funding reference number 568580). K. G. A. acknowledges support from the Department of Science and Technology and the Science and Engineering Research Board (SERB) of India via Swarnajayanti Fellowship Grant No. DST/SJF/PSA-01/2017-18 and Core Research Grant No. CRG/2021/004565. K. G. A. also acknowledges support from the Infosys Foundation. C. K. M. acknowledges the support of SERB’s Core Research Grant No. CRG/2022/007959. M. C. acknowledges funding from the Spanish Agencia Estatal de Investigación, Grant No. IJC2019-041385. Computations were performed on the CIT cluster provided by the LIGO Laboratory. N. V. K. acknowledges Max Planck Computing and Data Facility computing cluster Cobra for early stages of the work. We acknowledge National Science Foundation Grants PHY-0757058 and PHY-0823459. This material is based upon work supported by NSF’s LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. We used the following software packages: lals uite , bilby , bilby _ pipe , p y cbc , n um p y , pes ummary , m atplotlib , seaborn , jupyter , dynesty , and corner . This document has LIGO preprint No. LIGO-P2300337 .
PY - 2024/1/10
Y1 - 2024/1/10
N2 - We investigate the prospect of performing a null test of binary black hole (BBH) nature using spin-induced quadrupole moment (SIQM) measurements. This is achieved by constraining a deviation parameter (δκ) related to the parameter (κ) that quantifies the degree of deformation due to the spin of individual binary components on leading (quadrupolar) spin-induced moment. Throughout the paper, we refer to κ as the SIQM parameter and δκ as the SIQM-deviation parameter. The test presented here extends the earlier SIQM-based null tests for BBH nature by employing waveform models that account for double spin-precession and higher modes. We find that waveform with double spin-precession gives better constraints for δκ, compared to waveform with single spin-precession. We also revisit earlier constraints on the SIQM-deviation parameter for selected GW events observed through the first three observing runs (O1-O3) of LIGO-Virgo detectors. Additionally, the effects of higher-order modes on the test are also explored for a variety of mass-ratio and spin combinations by injecting simulated signals in zero-noise. Our analyses indicate that binaries with mass-ratio greater than three and significant spin precession may require waveforms that account for spin-precession and higher modes to perform the parameter estimation reliably.
AB - We investigate the prospect of performing a null test of binary black hole (BBH) nature using spin-induced quadrupole moment (SIQM) measurements. This is achieved by constraining a deviation parameter (δκ) related to the parameter (κ) that quantifies the degree of deformation due to the spin of individual binary components on leading (quadrupolar) spin-induced moment. Throughout the paper, we refer to κ as the SIQM parameter and δκ as the SIQM-deviation parameter. The test presented here extends the earlier SIQM-based null tests for BBH nature by employing waveform models that account for double spin-precession and higher modes. We find that waveform with double spin-precession gives better constraints for δκ, compared to waveform with single spin-precession. We also revisit earlier constraints on the SIQM-deviation parameter for selected GW events observed through the first three observing runs (O1-O3) of LIGO-Virgo detectors. Additionally, the effects of higher-order modes on the test are also explored for a variety of mass-ratio and spin combinations by injecting simulated signals in zero-noise. Our analyses indicate that binaries with mass-ratio greater than three and significant spin precession may require waveforms that account for spin-precession and higher modes to perform the parameter estimation reliably.
UR - http://www.scopus.com/inward/record.url?scp=85182363547&partnerID=8YFLogxK
U2 - 10.48550/arXiv.2311.05506
DO - 10.48550/arXiv.2311.05506
M3 - Article
AN - SCOPUS:85182363547
VL - 109
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 2
M1 - 023016
ER -