Strong lensing as a giant telescope to localize the host galaxy of gravitational wave event

Yu, Hai; Zhang, Pengjie; Wang, F. Y.

doi:10.1093/mnras/staa1952

Cited by 39 publications

(32 citation statements)

References 48 publications

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“…These standard sirens are known to be self-calibrating, since these do not rely on a cosmic distance ladder. In order to get the redshift information of a GW event, and so place them on the luminosity distance-redshift (D L − z) relation, an accompanying electromagnetic signal is needed (see for instance Oguri 2016;Ding et al 2019;The LIGO Scientific Collaboration et al 2019;Mukherjee et al 2020;Yu, Zhang & Wang 2020, and references therein for other redshift measurement techniques in the case of dark standard sirens). Such a relation is clearly necessary for the reconstruction of the late-time cosmological expansion of the Universe, and has also been E-mail: amitra@lpnhe.in2p3.fr employed to constrain various cosmological parameters of modified theories of gravity.…”

mentioning

confidence: 99%

Cosmology with the Einstein telescope: No Slip Gravity model and redshift specifications

Mitra

Mifsud

Mota

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The Einstein Telescope and other third generation interferometric detectors of gravitational waves are projected to be operational post 2030. The cosmological signatures of gravitational waves would undoubtedly shed light on any departure from the current gravitational framework. We here confront a specific modified gravity model, the No Slip Gravity model, with forecast observations of gravitational waves. We compare the predicted constraints on the dark energy equation of state parameters $w_0^{}-w_a^{}$, between the modified gravity model and that of Einstein gravity. We show that the No Slip Gravity model mimics closely the constraints from the standard gravitational theory, and that the cosmological constraints are very similar. The use of spectroscopic redshifts, especially in the low–redshift regime, lead to significant improvements in the inferred parameter constraints. We test how well such a prospective gravitational wave dataset would function at testing such models, and find that there are significant degeneracies between the modified gravity model parameters, and the cosmological parameters that determine the distance, due to the gravitational wave dimming effect of the modified theory.

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mentioning

confidence: 99%

Cosmology with the Einstein telescope: No Slip Gravity model and redshift specifications

Mitra

Mifsud

Mota

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…As the magnification is vital in the localization and follow-up cosmography of strongly lensed GWs (e.g. Sereno et al 2011;Hannuksela et al 2020;Yu et al 2020), if 𝜇 m significantly deviates from 1, microlensing might contaminate the signal to a degree that would affect these studies. Figure 6 gives the effective magnification as a function of the micro impact parameter 𝜂 m ∈ [0.1, 1.0]𝜃 m and mass of microlens 𝑚 ∈ [0, 100]M .…”

Section: Demagnification For the Microlensed Type 2 Imagementioning

confidence: 99%

“…Recently, searches for GW lensing using LIGO and Virgo data have also started (Hannuksela et al 2019;Li et al 2019a;McIsaac et al 2020;Pang et al 2020;Dai et al 2020;Liu et al 2020;Collaboration & Collaboration 2021), and many of the detection methodologies have been outlined in recent years (Cao et al 2014;Lai et al 2018;Christian et al 2018;Hannuksela et al 2019;Li et al 2019a;McIsaac et al 2020;Pang et al 2020;Hannuksela et al 2020;Dai et al 2020;Liu et al 2020;Wang et al 2021b;Lo & Magana Hernandez 2021;Janquart et al 2021a,b). If observed, lensed GWs could enable studies spanning the domains of fundamental physics, astrophysics, and cosmology Sereno et al (2011); Baker & Trodden (2017); Fan et al (2017); Liao et al (2017); Lai et al (2018); Liao (2019); Cao et al (2019); Li et al (2019b); Hou et al (2020); Mukherjee et al (2020a,b); Goyal et al (2020); Diego (2020); Hannuksela et al (2020); Yu et al (2020); Oguri & Takahashi (2020); Cremonese et al (2021); Finke et al (2021).…”

Section: Introductionmentioning

confidence: 99%

Microlensing of type II gravitational-wave macroimages

Yeung¹,

Cheung²,

Gais³

et al. 2021

Preprint

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Gravitational lensing describes the bending of the trajectories of light and gravitational waves due to the gravitational potential of a massive object. Strong lensing by galaxies can create multiple images with different overall amplifications, arrival times, and image types. If, furthermore, the gravitational wave encounters a star along its trajectory, microlensing will take place. Our previous research studied the effects of microlenses on strongly-lensed type I images. We extend our research to type II strongly-lensed images to complete the story. Our results are broadly consistent with prior work by other groups. As opposed to being magnified, the type II images are typically demagnified. Moreover, the type II images produce larger mismatches than type I images. Similar to our prior work, we find that the wave optics effects significantly suppress microlensing in the stellar-mass limit. We also discuss the implication of our results for a particularly promising method to use strong lensing to detect microlensing. In the future, it will be crucial to incorporate these microlensed waveforms in gravitational-wave lensing searches.

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“…In the case of doubly imaged GWs, there are two pieces of information immediately accessible to us from the GWs: the time delay between the images and the flux ratio of the images (Sereno et al 2011;Yu et al 2020). However, these two pieces of information alone will not significantly constrain the lensing system as the time delay is degenerate with the lens mass distribution, and the alignment of lens and source on the sky.…”

Section: Introductionmentioning

confidence: 99%

Localizing merging black holes with sub-arcsecond precision using gravitational-wave lensing

Hannuksela

Collett

Çalışkan

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The current gravitational-wave localization methods rely mainly on sources with electromagnetic counterparts. Unfortunately, a binary black hole does not emit light. Due to this, it is generally not possible to localize these objects precisely. However, strongly lensed gravitational waves, which are forecasted in this decade, could allow us to localize the binary by locating its lensed host galaxy. Identifying the correct host galaxy is challenging because there are hundreds to thousands of other lensed galaxies within the sky area spanned by the gravitational-wave observation. However, we can constrain the lensing galaxy’s physical properties through both gravitational-wave and electromagnetic observations. We show that these simultaneous constraints allow one to localize quadruply lensed waves to one or at most a few galaxies with the LIGO/Virgo/Kagra network in typical scenarios. Once we identify the host, we can localize the binary to two sub-arcsec regions within the host galaxy. Moreover, we demonstrate how to use the system to measure the Hubble constant as a proof-of-principle application.

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Strong lensing as a giant telescope to localize the host galaxy of gravitational wave event

Cited by 39 publications

References 48 publications

Cosmology with the Einstein telescope: No Slip Gravity model and redshift specifications

Cosmology with the Einstein telescope: No Slip Gravity model and redshift specifications

Microlensing of type II gravitational-wave macroimages

Localizing merging black holes with sub-arcsecond precision using gravitational-wave lensing

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