Stellar-mass microlensing of gravitational waves

Cheung, Mark Ho-Yeuk; Gais, J.; Hannuksela, O. A.; Li, Tjonnie G. F.

doi:10.1093/mnras/stab579

Cited by 47 publications

(41 citation statements)

References 34 publications

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“…There are also cases where the macrolensing effect induced by the cosmic structures hosting those PBHs, such as galaxies and clusters, may be of importance. And such macrolensing effect can be further influenced by the microlensing effect by individual PBHs at sufficiently large magnification [30,41,45].…”

Section: Introductionmentioning

confidence: 99%

Lensing by primordial black holes: constraints from gravitational wave observations

Wang,

Herrera-Martín,

2021

Preprint

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Primordial black holes (PBHs) have been proposed to explain at least a portion of dark matter.Observations have put strong constraints on PBHs in terms of the fraction of dark matter which they can represent, fPBH, across a wide mass range -apart from the stellar-mass range of 20M⊙ < ∼ MPBH < ∼ 100M⊙. In this paper, we explore the possibility that such PBHs could serve as pointmass lenses capable of altering the gravitational-wave (GW) signals observed from binary black hole (BBH) mergers along their line-of-sight. We find that careful GW data analysis could verify the existence of such PBHs based on the fitting factor and odds ratio analyses. When such a lensed GW signal is detected, we expect to be able to measure the redshifted mass of the lens with a relative error ∆MPBH/MPBH < ∼ 0.3. If no such lensed GW events were detected despite the operation of sensitive GW detectors accumulating large numbers of BBH mergers, it would translate into a stringent constraint of fPBH < ∼ 10 −2 − 10 −5 for PBHs with a mass larger than ∼ 10M⊙ by the Einstein Telescope after one year of running, and fPBH < ∼ 0.2 for PBHs with mass greater than ∼ 50M⊙ for advanced LIGO after ten years of running.

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Section: Introductionmentioning

confidence: 99%

Lensing by primordial black holes: constraints from gravitational wave observations

Wang,

Herrera-Martín,

2021

Preprint

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“…Diffraction signature was searched for in current detected events, but it has yet to be found [22]. It is also predicted that, for GWs within the frequency range of LIGO, diffraction becomes important when the lens mass ranges from 1-100 M ⊙ [4,28,29]. Strong lensing by such small lenses requires a small impact parameter, which places stringent requirement on the alignment of the GW source, the lens and the observer [see, e.g., [30]].…”

Section: Successful Detection Of Gravitational Wave (Gw) Signals From Compact Binary Mergers By the Advanced Lasermentioning

confidence: 99%

Identifying type II strongly lensed gravitational-wave images in third-generation gravitational-wave detectors

Wang

et al. 2021

Phys. Rev. D

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Strong gravitational lensing is a gravitational wave (GW) propagation effect that influences the inferred GW source parameters and the cosmological environment. Identifying strongly lensed GW images is challenging as waveform amplitude magnification is degenerate with a shift in the source intrinsic mass and redshift. However, even in the geometric-optics limit, type II strongly lensed images cannot be fully matched by type I (or unlensed) waveform templates, especially with large binary mass ratios and orbital inclination angles. We propose to use this mismatch to distinguish individual type II images. Using planned noise spectra of Cosmic Explorer, Einstein Telescope and LIGO Voyager, we show that a significant fraction of type II images can be distinguished from unlensed sources, given sufficient SNR (∼30). Incorporating models on GW source population and lens population, we predict that the yearly detection rate of lensed GW sources with detectable type II images is 172.2, 118.2 and 27.4 for CE, ET and LIGO Voyager, respectively. Among these detectable events, 33.1%, 7.3% and 0.22% will be distinguishable via their type II images with a log Bayes factor larger than 10. We conclude that such distinguishable events are likely to appear in the third-generation detector catalog; our strategy will significantly supplement existing strong lensing search strategies.

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“…Similar studies [28,29] find that stellar mass microlenses, embedded in a macromodel potential, can introduce interference distortions in strongly lensed gravitational waves and these effects can be used to constrain the fraction of dark matter in galaxies or clusters. More recently, [30,31] studied the effects of microlensing on GWs, taking into account also phase effects. In [30], PM and singular isothermal ellipsoid (SIE) lenses were considered and the authors stated that, for microlensing features to be notable in GW signal, the strong lensing magnification needs to be substantial.…”

Section: Andmentioning

confidence: 99%

“…In [30], PM and singular isothermal ellipsoid (SIE) lenses were considered and the authors stated that, for microlensing features to be notable in GW signal, the strong lensing magnification needs to be substantial. In [31] the authors use PM and SIS lenses and show that diffraction effects are important when we consider GWs in the LIGO frequency band lensed by objects with masses 100 M . Finally, [18] also considers small phase effects to recognize lensed signal, in this case for LISA sources, and with a large impact parameter, considering only SIS models.…”

Section: Andmentioning

confidence: 99%

Characteristic features of gravitational wave lensing as probe of lens mass model

Cremonese¹,

Mota²,

Salzano³

2021

Preprint

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To recognize gravitational wave lensing events and being able to differentiate between similar lens models will be of crucial importance once one will be observing several lensing events of gravitational waves per year. In this work, we study the lensing of gravitational waves in the context of LISA sources and wave-optics regime. While different papers before ours studied microlensing effects enhanced by simultaneous strong lensing, we focus on frequency (time) dependent phase effects produced by one lens that will be visible with only one lensed image. We will show how, in the interference regime (i.e. when interference patterns are present in the lensed image), we are able to i) distinguish a lensed waveform from an unlensed one, and ii) differentiate between different lens models. In pure wave-optics, on the other hand, the feasibility of the study depends on the SNR of the signal and/or the magnitude of the lensing effect. To achieve these goals we study the phase of the amplification factor of the different lens models and its effect on the unlensed waveform, and we exploit the signal-to-noise calculation for a qualitative analysis.

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Stellar-mass microlensing of gravitational waves

Cited by 47 publications

References 34 publications

Lensing by primordial black holes: constraints from gravitational wave observations

Lensing by primordial black holes: constraints from gravitational wave observations

Identifying type II strongly lensed gravitational-wave images in third-generation gravitational-wave detectors

Characteristic features of gravitational wave lensing as probe of lens mass model

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