Sachs–Wolfe effect
E844092
The Sachs–Wolfe effect is a cosmological phenomenon in which gravitational potential fluctuations imprint temperature anisotropies on the cosmic microwave background radiation, especially on large angular scales.
All labels observed (1)
| Label | Occurrences |
|---|---|
| Sachs–Wolfe effect canonical | 1 |
Statements (46)
| Predicate | Object |
|---|---|
| instanceOf |
cosmological effect
ⓘ
physical phenomenon ⓘ |
| abbreviation | SW effect NERFINISHED ⓘ |
| affects |
CMB temperature anisotropies
ⓘ
cosmic microwave background NERFINISHED ⓘ |
| cause |
gravitational potential fluctuations
ⓘ
metric perturbations in the early universe ⓘ |
| component |
integrated Sachs–Wolfe effect
NERFINISHED
ⓘ
ordinary Sachs–Wolfe effect NERFINISHED ⓘ |
| cosmologicalParameterSensitivity |
Hubble parameter H_0
ⓘ
dark energy density parameter Ω_Λ ⓘ matter density parameter Ω_m ⓘ |
| dependsOn |
evolution of gravitational potentials along the line of sight
ⓘ
gravitational potential at last scattering surface ⓘ |
| describedIn | Sachs and Wolfe 1967 paper NERFINISHED ⓘ |
| dominantOn | angular scales larger than a few degrees ⓘ |
| field |
astrophysics
ⓘ
cosmology ⓘ general relativity NERFINISHED ⓘ |
| mathematicalForm | temperature fluctuation proportional to gravitational potential divided by c squared ⓘ |
| mechanism |
gravitational redshift of photons
ⓘ
time dilation in gravitational potentials ⓘ |
| namedAfter |
Arthur Michael Wolfe
NERFINISHED
ⓘ
Rainer Kurt Sachs NERFINISHED ⓘ |
| observationalEvidence |
cross-correlation of CMB with galaxy surveys
ⓘ
large-angle CMB temperature maps ⓘ |
| observedBy |
COBE satellite
NERFINISHED
ⓘ
Planck satellite NERFINISHED ⓘ WMAP satellite NERFINISHED ⓘ |
| occursOn | large angular scales on the sky ⓘ |
| relatedConcept |
cosmic horizon
ⓘ
gravitational redshift ⓘ photon geodesics in curved spacetime ⓘ recombination epoch ⓘ |
| relatedTo |
cosmic microwave background anisotropy power spectrum
ⓘ
inflationary cosmology ⓘ large-scale structure of the universe ⓘ primordial density perturbations ⓘ ΛCDM model NERFINISHED ⓘ |
| scale | super-horizon scales at recombination ⓘ |
| signature | enhanced CMB power at low multipoles ⓘ |
| theoreticalBasis | linear perturbation theory in general relativity ⓘ |
| usedFor |
constraining primordial power spectrum
ⓘ
probing dark energy via integrated Sachs–Wolfe effect ⓘ testing cosmological models ⓘ |
| yearProposed | 1967 ⓘ |
Referenced by (1)
Full triples — surface form annotated when it differs from this entity's canonical label.