A Gaussian statistical model of galaxy shapes and radio polarizations yields unbiased, minimum-variance estimators for cosmic shear, intrinsic alignment, and line-of-sight rotation that are accurate to first order.
Weak Lensing On the Celestial Sphere
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
This paper details a description of the pattern of galaxy image distortion over the entire sky caused by the gravitational lensing which is the result of large scale inhomogeneities in our universe. We present a tensor spherical harmonic formalism to describe this pattern, giving many useful formulae. This is applied to density inhomogeneities, where we compute the angular power spectrum of the shear pattern, as well as the noise properties due to finite galaxy sampling and cosmic variance. We show that a detectable level of shear is present for very nearby galaxies, $z\simlt0.2$. For such a shallow sample much of the largest signal-to-noise comes from very large angular scales, $\theta\simgt10^\circ$, although it is in the form of very small shear at a level $\simlt10^{-3}$.
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astro-ph.CO 2years
2026 2representative citing papers
B-mode null tests for UNIONS-3500 cosmic shear pass after galaxy size cuts and stellar masking, with an oscillatory pattern from additive shear bias suppressed by excluding CCD angular scales.
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How to augment cosmic shear measurements with radio polarimetry of galaxies?
A Gaussian statistical model of galaxy shapes and radio polarizations yields unbiased, minimum-variance estimators for cosmic shear, intrinsic alignment, and line-of-sight rotation that are accurate to first order.
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UNIONS-3500 Weak Lensing: II. B-mode validation for cosmic shear
B-mode null tests for UNIONS-3500 cosmic shear pass after galaxy size cuts and stellar masking, with an oscillatory pattern from additive shear bias suppressed by excluding CCD angular scales.