### Abstract

The tails of gravitational waves result from the non-linear interaction between the usual quadrupole radiation generated by an isolated system (with total mass - energy M), and the static monopole field associated with M. Their contributions to the field at large distances from the system include a particular effect of modulation of the phase in the Fourier domain, having M as a factor and depending on the frequency as . In this paper we investigate the level at which this tail effect could be detected in future laser interferometric detectors. We consider a family of matched filters of inspiralling compact binary signals, allowing for this effect and parametrized by a family of independent 'test' parameters including M. Detecting the effect is equivalent to attributing, by optimal signal processing, a non-zero value to M. The error bar in the measurement of M is computed by analytical and numerical methods as a function of the optimal signal-to-noise ratio (SNR). We find that the minimal values of the SNR for detection of the tail effect at the level range from to for neutron-star binaries (depending on the type of noise in the detector and on our a priori knowledge of the binary), and from to for a black-hole binary with . It is argued that some of these values, at least for black-hole binaries, could be achieved in future generations of detectors, following the currently planned VIRGO and LIGO detectors.

Original language | English (US) |
---|---|

Article number | 020 |

Pages (from-to) | 2807-2831 |

Number of pages | 25 |

Journal | Classical and Quantum Gravity |

Volume | 11 |

Issue number | 11 |

DOIs | |

State | Published - Dec 1 1994 |

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### All Science Journal Classification (ASJC) codes

- Physics and Astronomy (miscellaneous)

### Cite this

*Classical and Quantum Gravity*,

*11*(11), 2807-2831. [020]. https://doi.org/10.1088/0264-9381/11/11/020

}

*Classical and Quantum Gravity*, vol. 11, no. 11, 020, pp. 2807-2831. https://doi.org/10.1088/0264-9381/11/11/020

**Signal analysis of gravitational wave tails.** / Blanchet, Luc; Sathyaprakash, B. S.

Research output: Contribution to journal › Article

TY - JOUR

T1 - Signal analysis of gravitational wave tails

AU - Blanchet, Luc

AU - Sathyaprakash, B. S.

PY - 1994/12/1

Y1 - 1994/12/1

N2 - The tails of gravitational waves result from the non-linear interaction between the usual quadrupole radiation generated by an isolated system (with total mass - energy M), and the static monopole field associated with M. Their contributions to the field at large distances from the system include a particular effect of modulation of the phase in the Fourier domain, having M as a factor and depending on the frequency as . In this paper we investigate the level at which this tail effect could be detected in future laser interferometric detectors. We consider a family of matched filters of inspiralling compact binary signals, allowing for this effect and parametrized by a family of independent 'test' parameters including M. Detecting the effect is equivalent to attributing, by optimal signal processing, a non-zero value to M. The error bar in the measurement of M is computed by analytical and numerical methods as a function of the optimal signal-to-noise ratio (SNR). We find that the minimal values of the SNR for detection of the tail effect at the level range from to for neutron-star binaries (depending on the type of noise in the detector and on our a priori knowledge of the binary), and from to for a black-hole binary with . It is argued that some of these values, at least for black-hole binaries, could be achieved in future generations of detectors, following the currently planned VIRGO and LIGO detectors.

AB - The tails of gravitational waves result from the non-linear interaction between the usual quadrupole radiation generated by an isolated system (with total mass - energy M), and the static monopole field associated with M. Their contributions to the field at large distances from the system include a particular effect of modulation of the phase in the Fourier domain, having M as a factor and depending on the frequency as . In this paper we investigate the level at which this tail effect could be detected in future laser interferometric detectors. We consider a family of matched filters of inspiralling compact binary signals, allowing for this effect and parametrized by a family of independent 'test' parameters including M. Detecting the effect is equivalent to attributing, by optimal signal processing, a non-zero value to M. The error bar in the measurement of M is computed by analytical and numerical methods as a function of the optimal signal-to-noise ratio (SNR). We find that the minimal values of the SNR for detection of the tail effect at the level range from to for neutron-star binaries (depending on the type of noise in the detector and on our a priori knowledge of the binary), and from to for a black-hole binary with . It is argued that some of these values, at least for black-hole binaries, could be achieved in future generations of detectors, following the currently planned VIRGO and LIGO detectors.

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UR - http://www.scopus.com/inward/citedby.url?scp=21844488465&partnerID=8YFLogxK

U2 - 10.1088/0264-9381/11/11/020

DO - 10.1088/0264-9381/11/11/020

M3 - Article

AN - SCOPUS:21844488465

VL - 11

SP - 2807

EP - 2831

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

SN - 0264-9381

IS - 11

M1 - 020

ER -