Scattering of gravitational waves by the weak gravitational fields of lens objects

Takahashi, Ryuichi; Suyama, Teruaki; Michikoshi, Shugo

doi:10.1051/0004-6361:200500140

Cited by 37 publications

(42 citation statements)

References 14 publications

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“…; x) / exp i!jx À x s j ð Þ /jx À x s j. Including the effect of U on the first order (Born approximation), the gravitationally lensed wave at the observer is given by Takahashi et al (2005),…”

Section: Gravitationally Lensed Waveformmentioning

confidence: 99%

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Amplitude and Phase Fluctuations for Gravitational Waves Propagating through Inhomogeneous Mass Distribution in the Universe

Takahashi¹

2006

ApJ

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When a gravitational wave (GW) from a distant source propagates through the universe, its amplitude and phase change due to gravitational lensing by the inhomogeneous mass distribution. We derive the amplitude and phase fluctuations and calculate these variances in the limit of a weak gravitational field of density perturbation. If the scale of the perturbation is smaller than the Fresnel scale $100 pc ( f /mHz) À1/2 ( f is the GW frequency), the GW is not magnified due to the diffraction effect. The rms amplitude fluctuation is 1%-10% for f > 10 À10 Hz, but it is reduced to less than 5% for a very low frequency of f < 10 À12 Hz. The rms phase fluctuation in the chirp signal is $10 À3 rad at the LISA frequency band (10 À5 to 10 À1 Hz). Measurements of these fluctuations will provide information about the matter power spectrum on the Fresnel scale $100 pc. Subject headingg s: gravitational lensing -gravitational waves -large-scale structure of universe

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Section: Gravitationally Lensed Waveformmentioning

confidence: 99%

“…Recently, Macquart (2004) and Takahashi et al (2005) have suggested that if the scale of the density perturbation k À1 is smaller than the Fresnel scale r F $ (kr s ) 1/2 (k is the wavelength), the wave effects become important. This condition is rewritten as k À1 < 100 pc( f /mHz) À1/2 (r s /10 Gpc) 1/2 .…”

Section: Introductionmentioning

confidence: 99%

Amplitude and Phase Fluctuations for Gravitational Waves Propagating through Inhomogeneous Mass Distribution in the Universe

Takahashi¹

2006

ApJ

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“…When the wavelength of the gravitational wave is much larger than, the object's size and the wave travels near the object, the wave may no longer be separated from the background and wave scattering occurs (see e.g Takahashi et al (2005)…”

mentioning

confidence: 99%

Search for Gravitational Lensing Signatures in LIGO-Virgo Binary Black Hole Events

Hannuksela

Haris

et al. 2019

ApJL

173

190

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We search for signatures of gravitational lensing in the binary black hole events detected by Advanced LIGO and Virgo during their first two observational runs. In particular, we look for three effects: 1) evidence of lensing magnification in the individual signals due to galaxy lenses, 2) evidence of multiple images due to strong lensing by galaxies, 3) evidence of wave optics effects due to point-mass lenses. We find no compelling evidence of any of these signatures in the observed gravitational wave signals. However, as the sensitivities of gravitational wave detectors improve in the future, detecting lensed events may become quite likely.

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“…Including the effect of U on the first order (Born approximation), the gravitationally lensed wave at the observer is given by (Takahashi et al 2005)…”

Section: Gravitationally Lensed Waveformmentioning

confidence: 99%

“…Recently, suggested by Macquart (2004) and Takahashi, Suyama & Michikoshi (2005), if the scale of the density perturbation k −1 is smaller than the Fresnel scale r F ∼ (λr s ) 1/2 (λ is the wavelength), the wave effects become important. This condition is rewritElectronic address: takahasi@th.nao.ac.jp…”

Section: Introductionmentioning

confidence: 99%

Amplitude and Phase Fluctuations for Gravitational Waves Propagating through Inhomogeneous Mass Distribution in the Universe

Takahashi

2006

AIP Conference Proceedings

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When a gravitational wave (GW) from a distant source propagates through the universe, its amplitude and phase change due to gravitational lensing by the inhomogeneous mass distribution. We derive the amplitude and phase fluctuations, and calculate these variances in the limit of a weak gravitational field of density perturbation. If the scale of the perturbation is smaller than the Fresnel scale ∼ 100pc(f /mHz) −1/2 (f is the GW frequency), the GW is not magnified due to the diffraction effect. The rms amplitude fluctuation is 1 − 10% for f > 10 −10 Hz, but it is reduced less than 5% for a very low frequency of f < 10 −12 Hz. The rms phase fluctuation in the chirp signal is ∼ 10 −3 radian at LISA frequency band (10 −5 − 10 −1 Hz). Measurements of these fluctuations will provide information about the matter power spectrum on the Fresnel scale ∼ 100 pc.

show abstract

Scattering of gravitational waves by the weak gravitational fields of lens objects

Cited by 37 publications

References 14 publications

Amplitude and Phase Fluctuations for Gravitational Waves Propagating through Inhomogeneous Mass Distribution in the Universe

Amplitude and Phase Fluctuations for Gravitational Waves Propagating through Inhomogeneous Mass Distribution in the Universe

Search for Gravitational Lensing Signatures in LIGO-Virgo Binary Black Hole Events

Amplitude and Phase Fluctuations for Gravitational Waves Propagating through Inhomogeneous Mass Distribution in the Universe

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