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Litmus Test for Cosmic Hemispherical Asymmetry in the Cosmic Microwave Background B-Mode Polarization.

Physical review letters·2016

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Updated: May 14, 2026

The Generation of Higher-order Laguerre-Gauss Optical Beams for High-precision Interferometry

The Generation of Higher-order Laguerre-Gauss Optical Beams for High-precision Interferometry

Published on: August 12, 2013

New window into stochastic gravitational wave background.

Aditya Rotti¹, Tarun Souradeep

¹IUCAA, Post Bag 4, Ganeshkhind, Pune 411007, India. aditya@iucaa.ernet.in

Physical Review Letters

|February 2, 2013

Summary

A stochastic gravitational wave background (SGWB) can lens cosmic microwave background (CMB) photons. Analyzing CMB polarization, particularly B modes, offers a path to detect SGWB and constrain its energy density.

Area of Science:

Cosmology
Astrophysics
Gravitational Wave Astronomy

Background:

A stochastic gravitational wave background (SGWB) is predicted by various cosmological models.
This SGWB can gravitationally lens cosmic microwave background (CMB) photons, affecting their polarization.

Purpose of the Study:

To correct existing literature for CMB polarization power spectra modifications due to gravitational wave lensing.
To explore the potential of using CMB measurements to constrain the energy density of an SGWB.

Main Methods:

Analyzing modifications to CMB polarization power spectra caused by weak gravitational lensing from SGWB.
Investigating the mixing of E-mode and B-mode polarization power spectra.
Utilizing current data from QUAD, WMAP, and ACT experiments.

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Last Updated: May 14, 2026

The Generation of Higher-order Laguerre-Gauss Optical Beams for High-precision Interferometry

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Published on: August 12, 2013

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Main Results:

Gravitational wave lensing distorts all four CMB power spectra, most notably mixing E-mode and B-mode polarization.
Current CMB temperature anisotropy power spectra provide the most stringent constraints on SGWB energy density (Ω(GW)).

Conclusions:

Future improvements in B-mode polarization upper limits will yield more stringent bounds on Ω(GW).
Detection of B-mode polarization exceeding predictions from large-scale structure lensing could indicate the presence of an SGWB.