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The 162 pages that link to Cosmic microwave background, each with the reason it gives.

• Gravitational waveCompared with: It is a radiation background measured in light, distinct from a stochastic gravitational-wave background.

• Radio frequency interferenceCompared with: It is a genuine cosmic signal, not contamination, despite occupying similar frequencies.

• Vesto SlipherCompared with: It provides independent evidence for cosmic history, unlike Slipher’s optical galaxy spectra.

• Planck unitsCompared with: Its measured conditions are far below Planck scales, limiting direct access to that regime.

• Cosmic infrared backgroundCompared with: It is another diffuse cosmic background, but originates from the early universe rather than galaxies.

• Cosmic dustCompared with: Foreground emission from Galactic dust can obscure precise measurements of its primordial polarization.

• Cosmic neutrino backgroundCompared with: Photons decoupled much later than neutrinos, leaving a warmer and directly observed background.

• Static universeCompared with: Its existence and properties support an evolving hot universe, not Einstein’s static picture.

• Zone of AvoidanceCompared with: Its foreground-emission mask is a related but distinct sky-obscuration problem.

• Atacama Large Millimeter/submillimeter ArrayCompared with: ALMA can measure small-scale variations in this background, although it is not primarily a CMB observatory.

• Black dwarfCompared with: For an immense future interval, even a cooled remnant would remain warmer than this cosmic background.

• IC 342/Maffei GroupCompared with: Foreground Milky Way emission in this direction also complicates observations of the microwave background.

• Sandra FaberCompared with: It probes early cosmic conditions, complementing Faber’s focus on the later growth of galaxies and structure.