### Abstract

General relativity's no-hair theorem states that isolated astrophysical black holes are described by only two numbers: mass and spin. As a consequence, there are strict relationships between the frequency and damping time of the different modes of a perturbed Kerr black hole. Testing the no-hair theorem has been a long-standing goal of gravitational-wave astronomy. The recent detection of gravitational waves from black hole mergers would seem to make such tests imminent. We investigate how constraints on black hole ringdown parameters scale with the loudness of the ringdown signal - subject to the constraint that the postmerger remnant must be allowed to settle into a perturbative, Kerr-like state. In particular, we require that - for a given detector - the gravitational waveform predicted by numerical relativity is indistinguishable from an exponentially damped sine after time tcut. By requiring the postmerger remnant to settle into such a perturbative state, we find that confidence intervals for ringdown parameters do not necessarily shrink with louder signals. In at least some cases, more sensitive measurements probe later times without necessarily providing tighter constraints on ringdown frequencies and damping times. Preliminary investigations are unable to explain this result in terms of a numerical relativity artifact.

Original language | English |
---|---|

Article number | 102004 |

Journal | Physical Review D |

Volume | 96 |

Issue number | 10 |

DOIs | |

Publication status | Published - 1 Jan 2017 |

### Cite this

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*Physical Review D*, vol. 96, no. 10, 102004. https://doi.org/10.1103/PhysRevD.96.102004

**Challenges for testing the no-hair theorem with current and planned gravitational-wave detectors.** / Thrane, Eric; Lasky, Paul D.; Levin, Yuri.

Research output: Contribution to journal › Article › Research › peer-review

TY - JOUR

T1 - Challenges for testing the no-hair theorem with current and planned gravitational-wave detectors

AU - Thrane, Eric

AU - Lasky, Paul D.

AU - Levin, Yuri

PY - 2017/1/1

Y1 - 2017/1/1

N2 - General relativity's no-hair theorem states that isolated astrophysical black holes are described by only two numbers: mass and spin. As a consequence, there are strict relationships between the frequency and damping time of the different modes of a perturbed Kerr black hole. Testing the no-hair theorem has been a long-standing goal of gravitational-wave astronomy. The recent detection of gravitational waves from black hole mergers would seem to make such tests imminent. We investigate how constraints on black hole ringdown parameters scale with the loudness of the ringdown signal - subject to the constraint that the postmerger remnant must be allowed to settle into a perturbative, Kerr-like state. In particular, we require that - for a given detector - the gravitational waveform predicted by numerical relativity is indistinguishable from an exponentially damped sine after time tcut. By requiring the postmerger remnant to settle into such a perturbative state, we find that confidence intervals for ringdown parameters do not necessarily shrink with louder signals. In at least some cases, more sensitive measurements probe later times without necessarily providing tighter constraints on ringdown frequencies and damping times. Preliminary investigations are unable to explain this result in terms of a numerical relativity artifact.

AB - General relativity's no-hair theorem states that isolated astrophysical black holes are described by only two numbers: mass and spin. As a consequence, there are strict relationships between the frequency and damping time of the different modes of a perturbed Kerr black hole. Testing the no-hair theorem has been a long-standing goal of gravitational-wave astronomy. The recent detection of gravitational waves from black hole mergers would seem to make such tests imminent. We investigate how constraints on black hole ringdown parameters scale with the loudness of the ringdown signal - subject to the constraint that the postmerger remnant must be allowed to settle into a perturbative, Kerr-like state. In particular, we require that - for a given detector - the gravitational waveform predicted by numerical relativity is indistinguishable from an exponentially damped sine after time tcut. By requiring the postmerger remnant to settle into such a perturbative state, we find that confidence intervals for ringdown parameters do not necessarily shrink with louder signals. In at least some cases, more sensitive measurements probe later times without necessarily providing tighter constraints on ringdown frequencies and damping times. Preliminary investigations are unable to explain this result in terms of a numerical relativity artifact.

UR - http://www.scopus.com/inward/record.url?scp=85037107949&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.96.102004

DO - 10.1103/PhysRevD.96.102004

M3 - Article

AN - SCOPUS:85037107949

VL - 96

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 10

M1 - 102004

ER -