Signal analysis of gravitational wave tails

Luc Blanchet, B. S. Sathyaprakash

Research output: Contribution to journalArticle

49 Citations (Scopus)

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 languageEnglish (US)
Article number020
Pages (from-to)2807-2831
Number of pages25
JournalClassical and Quantum Gravity
Volume11
Issue number11
DOIs
StatePublished - Dec 1 1994

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signal analysis
gravitational waves
detectors
signal to noise ratios
LIGO (observatory)
matched filters
monopoles
neutron stars
signal processing
quadrupoles
modulation
radiation
lasers
interactions

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy (miscellaneous)

Cite this

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title = "Signal analysis of gravitational wave tails",
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.",
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Signal analysis of gravitational wave tails. / Blanchet, Luc; Sathyaprakash, B. S.

In: Classical and Quantum Gravity, Vol. 11, No. 11, 020, 01.12.1994, p. 2807-2831.

Research output: Contribution to journalArticle

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