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A bolometer detects absorbed electromagnetic radiation through the resulting change in temperature, often read as a change in electrical resistance. Its response depends on absorbed power, so interpreting an optical spectrum requires accounting for the incident wavelength band and detector calibration.

BOOMERANG's 1998 Antarctic balloon flight scanned a low-dust region with a microwave telescope near $38\mathrm{km}$ and bolometers at $0.3\mathrm{K}$. Ground beam measurements and microwave angular dipole calibration connected signals to sky temperature. Frequency-map and time-split differences tested contamination. The 2000 paper fitted the Cosmic microwave background power spectrum, finding ${\ell }_{\mathrm{peak}}=197\pm 6$ at one standard deviation. Its near-flat-geometry inference used a chosen model family and parameter priors; secondary peaks were not yet established.^[ref]

FIRAS compared sky radiation with an adjustable internal blackbody using an interferometer and cold bolometers. An external blackbody could cover the sky entrance for measurement calibration. The team adjusted the internal temperature to minimize the difference signal.^[ref]

Comparisons across detectors and mirror strokes tested instrumental errors; sky mapping separated Milky Way emission. John C. Mather's lecture reports a final root-mean-square spectral departure of 50 parts per million of peak brightness. This is neither the preliminary 1990 precision nor a relative error in every spectral bin. Calibration drift and nonideal reference emission required correction.^[ref]

The advantage of a null measurement is that a small difference can be resolved without assigning the same absolute precision to a large detector output. Nevertheless, matching an internal reference is meaningful only after its relation to an independently calibrated blackbody has been tested. A bound on departures from a Planck spectrum constrains energy redistribution after thermal equilibrium; it does not require the cosmic microwave background to have exactly the same temperature in every direction.

William Weber Coblentz's primary report describes an electrically heated porcelain cavity wound with platinum ribbon. Mirrors imaged its central radiating diaphragm onto a $0.6\mathrm{mm}$ optical slit; a fluorite optical prism dispersed the beam onto a vacuum bolometer. Galvanometer deflections read the detector response. A resistance standard checked electrical sensitivity, while repeated readings checked stability. Sodium lines fixed the angular zero; a refractive index curve supplied wavelengths and slit-bandwidth corrections. Thermocouples were standardized at freezing points of zinc, antimony and copper. Drying the optical path reduced atmospheric absorption; prism scattering and temperature calibration remained limitations. These were Coblentz's measurements. His extraction of radiation constants assumed the Planck law, so it was not a model-independent proof of the spectral formula.^[ref]

The inference to test is whether corrected spectra taken at independently determined temperatures have their $B_{\lambda }$ maxima at a constant product ${\lambda }_{\max }T$. Comparing raw galvanometer deflections at different optical prism settings would also compare different wavelength widths and optical losses. The response integral in blackbody peak and detector response explains why those corrections belong to the physical inference rather than merely to presentation.