Sachs-Wolfe effect

The non-integrated Sachs-Wolfe effect is caused by gravitational redshift occurring at the surface of last scattering.

Sachs-Wolfe effect Level 5.

Voids can produce a cooler region than surrounding sightlines from the late-time integrated Sachs-Wolfe effect.

Together with Rainer Kurt Sachs, he authored the Sachs-Wolfe effect.

Such a void would affect the observed CMB via the integrated Sachs-Wolfe effect.

White, Martin, and Wayne Hu, The Sachs-Wolfe effect.

Alternatively, Zwicky proposed a kind of Sachs-Wolfe Effect explanation for the redshift distance relation:

Aguiar, Paulo, and Paulo Crawford, Sachs-Wolfe effect in some anisotropic models.

Sam LaRoque, The Integrated Sachs-Wolfe Effect.

This so-called late-time Integrated Sachs-Wolfe effect (ISW) is a direct signal of dark energy in a flat universe.

He and Arthur Michael Wolfe were the authors of the Sachs-Wolfe effect, which concerns a property of the Cosmic microwave background radiation.

On large angular scales, temperature fluctuations in the cosmic microwave background radiation (CMBR) are produced by the Sachs-Wolfe effect at the end of recombination.

Voids appear to have a correlation with observed temperature of the Cosmic Microwave Background (CMB) due to the Sachs-Wolfe effect.

His contributions include joint work on the Sachs-Wolfe effect and the Ehlers-Geren-Sachs theorem, both of which deal with the Cosmic Microwave Background Radiation.

As the Sachs-Wolfe effect is only significant if the Universe is dominated by radiation or Dark energy, the existence of voids is significant in providing physical evidence for dark energy.

At recombination these scales were larger than the Hubble radius, and because microphysical processes can act only on scales less than the Hubble radius, these fluctuations must have been produced by the Sachs-Wolfe effect.

The "early-time" ISW occurs immediately after the (non-integrated) Sachs-Wolfe effect produces the primordial CMB, as photons course through density fluctuations while there is still enough radiation around to affect the Universe's expansion.

These measurements are expected to provide further confirmation of the theory as well as information about cosmic inflation, and the so-called secondary anisotropies, such as the Sunyaev-Zel'dovich effect and Sachs-Wolfe effect, which are caused by interaction between galaxies and clusters with the cosmic microwave background.

Gravitational blueshift contributes to cosmic microwave background (CMB) anisotropy via the Sachs-Wolfe effect: when a gravitational well evolves while a photon is passing, the amount of blueshift on approach will differ from the amount of gravitational redshift as it leaves the region.

The Sachs-Wolfe effect, named after Rainer Kurt Sachs and Arthur Michael Wolfe, is a property of the cosmic microwave background radiation (CMB), in which photons from the CMB are gravitationally redshifted, causing the CMB spectrum to appear uneven.