A. Jones's Appl of Novel Analysis Tech to Cosmic Microwave Bkd PDF

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0◦ FWHM experiment have been taking data since 1985, 1990 and 1992 respectively. 5◦ ). It is seen that the full area is not covered by all three experiments but they are continually taking new data to build up a well sampled, high sensitivity data set. 8 shows the noise levels per 1◦ bin achieved in this data set. 2. 7: The number of independent measurements in the RA range 161◦ − 250◦ in each of the Tenerife data sets. 8: The noise per beam in µK for each of the Tenerife final stacked scans. Dec.

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). At this frequency and angular scale the experiment is more sensitive to Galactic emission than to the CMB radiation and so this data will be used to put constraints on the Galactic contamination to the 5◦ Tenerife experiments.

Produced for the Bersanelli et al 1996 phase A study. used as a cross–check between the two different types of receiver technologies used. 1. The four lowest frequency channels consist of HEMT radio receivers while the six highest frequency channels are bolometer arrays. This difference in detector technology was chosen to achieve the best sensitivity to the signal and accounts for the apparent discontinuity in the table between the two 100 GHz channel sensitivities. 6 shows an artist’s impression of the Planck Surveyor satellite.

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Appl of Novel Analysis Tech to Cosmic Microwave Bkd Astronomy [thesis] by A. Jones


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