Annu. Rev. Astron. Astrophys. 1980. 18:
489-535 Copyright © 1980 by Annual Reviews. All rights reserved |
Absolute measurements are always difficult. Measurements of the cosmic background radiation (CBR) spectrum are no exception and are further complicated by the fact that it is impossible to modulate the signal, the CBR. The CBR is therefore the residue, what is left over after one has accounted for everything else. The quality of this accounting, the precision and reliability of measurement of the individual terms, determines the value of the observation. The evolution of experiments to measure the CBR spectrum demonstrates this well. Future progress lies in unproved experimental design or operation. in more benign environments which permit reduction of the most uncertain elements in the accounting sum.
Direct measurements of the CBR spectrum fall crudely into two categories: low frequency observations in the Rayleigh-Jeans portion of the spectrum and observations at high frequencies in the region embracing the blackbody peak and into the Wien tail. This categorization results from the different technologies used in the two regions, and differences between the magnitudes of the terrestrial atmospheric emission. The low frequency measurements employ conventional microwave technology - coherent receivers - at sea-level and mountain observing sites while the high frequency observations have been carried out with less well developed infrared techniques - incoherent detectors, broad-band filters, Fourier transform spectrometers - on balloon- and rocket-borne platforms.
As the sub-millimeter technology of coherent receivers, in particular the development of efficient broad-band mixers, improves, the low frequency techniques will be applied to the high frequency region from balloon and aircraft platforms.
Figure 1 outlines the basis of all the low frequency measurements. The individual experiments listed in Table 1 may differ in details, even in some important ones, but nevertheless all consist of the same components: a coherent receiver, a primary absolute reference calibrator, and an antenna The experimental strategy has been to compare the radiation entering the antenna with that of the primary calibrator, the gain of the receiver being determined by either varying the temperature of the primary reference or by injecting a known power into the receiver input.
Figure 1. Schematic diagram of a generic absolute radiometer. |
Properties of primary calibrator | |||||||||||
Receiver | Beam | Thermodynamic | Antenna | ||||||||
f | v | Altitude | noise | width | temperature of | temperature of | p Tp | w Tw | |||
Reference | (cm) | (GHz) | (cm-1) | (km) | (K/Hz1/2) | (deg.) | primary ref | primary ref. | (K) | R | (K) |
Howell & | 73.5 | 0.41 | 0.014 | 1.7±0.2 | |||||||
Shakeshaft 1967 | 0 | - | 15 | 4.2 | 4.19 | - | - | ||||
49.2 | 0.61 | 0.020 | 1.4±0.2 | ||||||||
Penzias & | 21.2 | 1.415 | 0.047 | 0 | - | - | 4.2 | 4.17 | 0.6 | - | - |
Wilson 1967 | |||||||||||
Howell & | 20.7 | 1.41 | 0.048 | 0 | - | 13×15 | 4.2 | 4.17 | 1.7±0.2 | - | - |
Shakeshaft 1966 | |||||||||||
Penzias & | 7.35 | 4.08 | 0.136 | 0 | - | - | 4.2 | 4.10 | 1.3 | - | - |
Wilson 1965, | |||||||||||
Penzias 1968 | |||||||||||
Roll & | 3.2 | 9.37 | 0.313 | 0 | - | 20 | 4.2 | 3.98 | 2.6±0.35 | - | - |
Wilkinson 1966 | |||||||||||
Stokes et al. 1967 | 3.2 | 9.37 | 0.313 | 3.8 | ~ 1.5 | 4 | 3.77 | 3.55 | 0.16±0.10 | 6±3×10-4 | 0.06±0.02 |
Stokes et al. 1967 | 1.58 | 19.0 | 0.633 | 3.8 | ~ 1.5 | 4 | 3.77 | 3.33 | 0.21±0.08 | 1±0.3×10-3 | 0.04±0.01 |
Welch et al. 1967 | 1.5 | 20.0 | 0.666 | 3.8 | ~ 2 | 12 | 73.6 | 73.12 | 0.42±0.1 | < 4.10-4 | - |
Ewing et al. 1967 | 0.924 | 32.5 | 1.08 | 3.8 | ~ 3 | 20 | 3.78 | 3.056 | 1.0±0.15 | - | 0.06±0.02 |
Wilkinson 1967 | 0.856 | 35.05 | 1.168 | 3.8 | ~ 1.5 | 4 | 3.77 | 2.99 | 0.28±0.11 | 0± + 3×10-4 | 0.06±0.06 |
Puzanov et al. 1968 | 0.82 | 36.6 | 1.22 | 0 | 1.6 | 4 | 77.36 | 76.48 | - | - | - |
Kislyakov et al. 1971 | 0.358 | 83.8 | 2.79 | 3 | 2-4 | 10 | ~ 75.0 | ~ 73.0 | - | - | - |
Boynton et al. 1968 | 0.33 | 90.0 | 3.00 | 3.44 | 1.5 | - | 3.8 | 2.042 | 0.22±0.11 | 3×10-4 | 0.27±0.04 |
Millea et al. 1971 | 3.1 | 3.85 | 2.087 | ||||||||
0.33 | 90.4 | 3.00 | 0.5 | 6.6 | 1.1±0.11 | 3±0.6×10-4 | - | ||||
2.8 | 3.88 | 2.114 | |||||||||
Boynton & | 0.33 | 90.0 | 3.00 | 14.9 | 0.1 | - | 4.2 | 2.405 | 0.22±0.11 | 8±4×10-4 | 0.27±0.04 |
Stokes 1974 | |||||||||||
Properties of antenna | External sourcesa | |||||||
Cosmic background | ||||||||
ant Tant | fgnd Tgnd | atm Tatm | Tgal | Switch | thermodynamic | |||
Reference | (K) | (K) | (K) | (K) | asymmetry | temperature | See note b | |
0.4±0.2 | 0.6±0.4 | 1.3±0.1 | 20.6±2.2 | |||||
Howell & Shakeshaft 1967 | - | 3.7±1.2 | 1,2 | |||||
0.4±0.2 | 0.6±0.4 | 1.95±0.1 | 6.7±0.7 | |||||
Penzias & Wilson 1967 | 0.55 | 2.3 | 0.3 | 0.05 | 3.2±1.0 | - | ||
Howell & Shakeshaft 1966 | 1.3±0.2 | 0.1 | 2.2±0.2 | 0.5±0.2 | - | 2.8±0.6 | 2 | |
Penzias & Wilson 1965, | 0.8±0.4 | 0.1 | 2.3±0.3 | < 0.2 | 0.05 | 3.3±1.0 | 3 | |
Penzias 1968 | ||||||||
Roll & Wilkinson 1966 | 1.08±0.15 | - | 3.0±0.2 | < 0.0015 | 3.8±0.2 | 3.0±0.5 | - | |
Stokes et al. 1967 | 0.08±0.06 | < 0.05 | 1.37±0.1 | - | - | 2.69-0.21+0.16 | 4 | |
Stokes et al. 1967 | 0.15±0.05 | < 0.15 | 4±0.1 | - | - | 2.78-0.17+0.12 | 4 | |
Welch et al. 1967 | 1.9±0.2 | 0.1 | 4±0.2 | - | - | 2.45±1.0 | 5 | |
Ewing et al. 1967 | 0.2±0.06 | 0.03±0.01 | 4.6±0.2 | - | 0.5±0.1 | 3.09±0.26 | 6 | |
Wilkinson 1967 | 0.12±0.04 | < 0.05 | 6.5±0.2 | - | - | 2.56-0.22+0.17 | 4 | |
Puzanov et al. 1968 | - | - | 17.0 | - | - | 3.7±1.0 | 5 | |
Kislyakov et al. 1971 | 5±0.4 | - | 14.7±1.2 | - | - | 2.4±0.7 | - | |
Boynton et al. 1968 | 0.21±0.12 | - | 11.5±0.22 | - | - | 2.46-0.44+0.40 | 4 | |
Millea et al. 1971 | 11.8±0.22 | |||||||
0.21±0.11 | 0.02 | - | - | 2.61±0.25 | - | |||
12.1±~0.4 | ||||||||
Boynton & Stokes 1974 | - | - | 1.21±0.37 | - | - | 2.48-0.54+0.50 | 7 | |
<T> = 2.74±0.087 K | ||||||||
normalized 2 = 0.44 | ||||||||
14 degrees of freedom | ||||||||
FOOTNOTES FOR TABLE 1 | ||||||||
a Atmospheric radiation entries are typical
numbers for a data set.
bNotes:
|