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Black hole ringdown: the importance of overtones

Giesler, Matthew and Isi, Maximiliano and Scheel, Mark A. and Teukolsky, Saul A. (2019) Black hole ringdown: the importance of overtones. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20190911-124456116

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Abstract

It is possible to infer the mass and spin of the remnant black hole from binary black hole mergers by comparing the ringdown gravitational wave signal to results from studies of perturbed Kerr spacetimes. Typically these studies are based on the fundamental quasinormal mode of the dominant ℓ=m=2 harmonic. By modeling the ringdown of accurate numerical relativity simulations, we find that the fundamental mode alone is insufficient to recover the true underlying mass and spin, unless the analysis is started very late in the ringdown. Including higher overtones associated with this ℓ=m=2 harmonic resolves this issue, and provides an unbiased estimate of the true remnant parameters. Further, including overtones allows for the modeling of the ringdown signal for all times beyond the peak strain amplitude, indicating that the linear quasinormal regime starts much sooner than previously expected. A model for the ringdown beginning at the peak strain amplitude can exploit the higher signal-to-noise ratio in detectors, reducing uncertainties in the extracted remnant quantities. Tests of the no-hair theorem should consider incorporating overtones in the analysis.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1903.08284arXivDiscussion Paper
ORCID:
AuthorORCID
Isi, Maximiliano0000-0001-8830-8672
Additional Information:The authors thank Vijay Varma for many valuable discussions. We also thank Katerina Chatziioannou and Leo Stein for useful comments. M.G. and M.S. are supported by the Sherman Fairchild Foundation and NSF grants PHY-1708212 and PHY-1708213 at Caltech. M.I. is a member of the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. M.I. is supported by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51410.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. S.T. is supported in part by the Sherman Fairchild Foundation and by NSF Grants PHY-1606654 and ACI-1713678 at Cornell. Computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech. Computation were also performed on the Nemo computing cluster at the University of Wisconsin-Milwaukee, supported by NSF Grant PHY-1626190. This paper carries LIGO document number LIGO-P1900076.
Group:LIGO, TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-1708212
NSFPHY-1708213
NSFPHY-0757058
NASA Hubble FellowshipHST-HF2-51410.001-A
NASANAS5-26555
NSFPHY-1606654
NSFACI-1713678
NSFPHY-1626190
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentP1900076
Record Number:CaltechAUTHORS:20190911-124456116
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190911-124456116
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98575
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:11 Sep 2019 23:28
Last Modified:03 Oct 2019 21:42

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