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GLoW: novel methods for wave-optics phenomena in gravitational lensing
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Wave-optics phenomena in gravitational lensing occur when the signal's wavelength is commensurate to the gravitational radius of the lens. Although potentially detectable in lensed gravitational waves, fast radio bursts and pulsars, accurate numerical predictions are challenging to compute. Here we present novel methods for wave-optics lensing that allow the treatment of general lenses. In addition to a general algorithm, specialized methods optimize symmetric lenses (arbitrary number of images) and generic lenses in the single-image regime. We also develop approximations for simple lenses (point-like and singular isothermal sphere) that drastically outperform known solutions without compromising accuracy. These algorithms are implemented in Gravitational Lensing of Waves (GLoW): an accurate, flexible, and fast code. GLoW efficiently computes the frequency-dependent amplification factor for generic lens models and arbitrary impact parameters in O(1 ms) to O(10 ms) depending on the lens configuration and complexity. GLoW is readily applicable to model lensing diffraction on gravitational-wave signals, offering new means to investigate the distribution of dark-matter and large-scale structure with signals from ground and space detectors.
Forward citations
Cited by 7 Pith papers
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Probing Dark Matter Substructure with Wave-Optics Distortions of Strongly Lensed LISA Gravitational Waves
Simulated four-year-LISA lensed waveforms show fuzzy-dark-matter substructure leaves a frequency-dependent phase residual that distinguishes it from NFW or self-interacting halos with ~60–110 resolved images.
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The diffraction-lensing interpretation of GW231123 with astrophysical priors
GW231123 is better fit by a lower-mass merger diffracted by an isolated ~1000 M_sun lens, but astrophysical priors and a frequentist rate estimate make this lensing interpretation unlikely.
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Across the Universe: GW231123 as a magnified and diffracted black hole merger
GW231123's extreme mass and spins may be explained by a point-mass microlens embedded in a galaxy, reducing the inferred source mass to about 100-180 solar masses.
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Detection of cosmic strings by gravitational wave lensing. Predictions for Einstein Telescope
Simulated cosmic-string lensing of binary black holes predicts Einstein Telescope would detect the events and infer Gµ ≈ 1e-10, though the source geometry is assumed ad hoc.
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Discovering gravitational waveform distortions from lensing: A deep dive into GW231123
GW231123's apparent gravitational-lensing signal has a false-alarm probability around 4σ, so the event cannot be claimed as lensed under the two-image wave-optics model.
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Accelerated inference of microlensed gravitational waves with machine learning
A neural posterior estimator trained on wave-optics-microlensed gravitational-wave signals recovers source and lens parameters and Bayes factors consistent with Bilby, about 10 times faster.
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Multi-band observation of lensed gravitational waves as a probe of small-mass dark matter halos
Using Fisher forecasts, the paper shows that joint ET and DECIGO observations of one lensed gravitational wave can break the degeneracy between lens mass, impact parameter, and halo core size.
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