Gravity wave-induced polarization of the cosmic microwave background radiation

Ng, Ka Lok; Ng, Kin-Wang

doi:10.1086/175717

Cited by 16 publications

(11 citation statements)

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“…semi-analytical discussions of the problem (see, e. g. [134,135,136]). The polarization decomposition leading to Eqs.…”

Section: Different Parametrizations Of the Full Equationmentioning

confidence: 99%

Stochastic backgrounds of relic gravitons: a theoretical appraisal

Giovannini

2010

PMC Phys A

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Stochastic backgrounds or relic gravitons, if ever detected, will constitute a prima facie evidence of physical processes taking place during the earliest stages of the evolution of the plasma. The essentials of the stochastic backgrounds of relic gravitons are hereby introduced and reviewed. The pivotal observables customarily employed to infer the properties of the relic gravitons are discussed both in the framework of the ΛCDM paradigm as well as in neighboring contexts. The complementarity between experiments measuring the polarization of the Cosmic Microwave Background (such as, for instance, WMAP, Capmap, Quad, Cbi, just to mention a few) and wide band interferometers (e.g. Virgo, Ligo, Geo, Tama) is emphasized. While the analysis of the microwave sky strongly constrains the low-frequency tail of the relic graviton spectrum, wide-band detectors are sensitive to much higher frequencies where the spectral energy density depends chiefly upon the (poorly known) rate of post-inflationary expansion.

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“…semi-analytical discussions of the problem (see, e. g. [134,135,136]). The polarization decomposition leading to Eqs.…”

Section: Different Parametrizations Of the Full Equationmentioning

confidence: 99%

Stochastic backgrounds of relic gravitons: a theoretical appraisal

Giovannini

2010

PMC Phys A

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“…Such calculations for the CMB power spectra from density perturbations were developed in a series of pioneering papers from 1970 until the late 1980s (93,113,(160)(161)(162)(163)(164)(165), and these calculations have been refined extensively in the post-COBE era. Similar calculations can also be carried out for the CMB power spectra from gravitational waves (80,82,112,(166)(167)(168)(169)(170)(171)(172).…”

Section: Cosmic Microwave Background Tests Of Inflationmentioning

confidence: 97%

THECOSMICMICROWAVEBACKGROUND ANDPARTICLEPHYSICS

Kamionkowski

Kosowsky

1999

Annu. Rev. Nucl. Part. Sci.

165

146

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In forthcoming years, connections between cosmology and particle physics will become increasingly important with the advent of a new generation of cosmic microwave background (CMB) experiments. Here, we review a number of these links. Our primary focus is on new CMB tests of inflation. We explain how the inflationary predictions for the geometry of the Universe and primordial density perturbations will be tested by CMB temperature fluctuations, and how the gravitational waves predicted by inflation can be pursued with the CMB polarization. The CMB signatures of topological defects and primordial magnetic fields from cosmological phase transitions are also discussed. Furthermore, we review current and future CMB constraints on various types of dark matter (e.g. massive neutrinos, weakly interacting massive particles, axions, vacuum energy), decaying particles, the baryon asymmetry of the Universe, ultra-high-energy cosmic rays, exotic cosmological topologies, and other new physics.

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“…In the space of the hyperfine sublevels of the 1s state, the perturbation due to resonant scattering is similar to the Hamiltonian of Eq. (7). The relevant terms are those with the intermediate state (labeled by the index n in Eq.…”

Section: Appendix C: Depolarization Due To Lyman-α Scatteringmentioning

confidence: 99%

Detecting primordial gravitational waves with circular polarization of the redshifted 21 cm line. I. Formalism

2018

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We propose a new method to measure the tensor-to-scalar ratio r using the circular polarization of the 21 cm radiation from the pre-reionization epoch. Our method relies on the splitting of the F ¼ 1 hyperfine level of neutral hydrogen due to the quadrupole moment of the cosmic microwave background (CMB). We show that unlike the Zeeman effect, where M F ¼ AE1 have opposite energy shifts, the CMB quadrupole shifts M F ¼ AE1 together relative to M F ¼ 0. This splitting leads to a small circular polarization of the emitted 21 cm radiation. In this paper (Paper I in a series on this effect), we present calculations on the microphysics behind this effect, accounting for all processes that affect the hyperfine transition. We conclude with an analytic formula for the circular polarization from the Dark Ages as a function of prereionization parameters and the value of the remote quadrupole of the CMB. We also calculate the splitting of the F ¼ 1 hyperfine level due to other anisotropic radiation sources and show that they are not dominant. In a companion paper (Paper II) we make forecasts for measuring the tensor-to-scalar ratio r using future radio arrays.

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Gravity wave-induced polarization of the cosmic microwave background radiation

Cited by 16 publications

References 0 publications

Stochastic backgrounds of relic gravitons: a theoretical appraisal

Stochastic backgrounds of relic gravitons: a theoretical appraisal

THECOSMICMICROWAVEBACKGROUND ANDPARTICLEPHYSICS

Detecting primordial gravitational waves with circular polarization of the redshifted 21 cm line. I. Formalism

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