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6◦ displayed as a function of right ascension. Each plot shows the second difference in mK after binning into 1◦ bins. A running mean has been subtracted from each scan. Long scans are displayed modulo 360◦ . reached was not very high as the integration time at each declination was limited. 6◦ Declination data. The long term baseline drifts are still apparent at this stage. After the baseline has been removed using the maximum entropy technique the data was stacked together and compared with the expected signals (see Chapter 7).

5 GHz, 53 GHz and 90 GHz. The frequencies were chosen to overlap the expected minimum in Galactic foreground emission. Each radiometer pair have two independent receivers (denoted by A and B) that measure the difference in the level of CMB in beams of FWHM 7◦ separated by 60◦ in the sky. 1) the sum and difference between the A and B are calculated. The sum maps, which enhance any signal present in both A and B, give an estimate of the fluctuations present in the CMB while the difference maps, which remove any consistent signal, gives a measure of the instrumental noise.

The Far Infrared Absolute Spectrophotometer (FIRAS) measured the CMB spectrum between 1 cm and 100 µm. The results from FIRAS showed the CMB to have a black body spectrum that was correct to 1 part in 104 , the most accurate black body known to science. 010 K at 95% confidence (see Mather et al 1994). The Differential Microwave Background Radiometer (DMR) maps the fluctuations in the CMB over the full sky. 5. 5 GHz, 53 GHz and 90 GHz. The frequencies were chosen to overlap the expected minimum in Galactic foreground emission.

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