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and Cosmology

Extragalactic Astronomy and Cosmology: An Introduction

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8.6 Angular Fluctuations of the Cosmic Microwave Background<br />

343<br />

Fig. 8.27. In 2000, two groups published the results of their<br />

CMB observations, BOOMERANG <strong>and</strong> MAXIMA. This<br />

figure shows the BOOMERANG data. On the left, the temperature<br />

distributions at 90 GHz, 150 GHz, <strong>and</strong> 240 GHz are<br />

displayed, while the lower right panel shows that at 400 GHz.<br />

The three small circles in each panel denote the location of<br />

known strong point sources. The two upper panels on the right<br />

show the differences of temperature maps obtained at two different<br />

frequencies, e.g., the temperature map obtained with<br />

the 90-GHz data minus that obtained from the 150-GHz data.<br />

These difference maps feature considerably smaller fluctuations<br />

than the individual maps. This is compatible with the<br />

idea that the major fraction of the radiation originates in the<br />

CMB <strong>and</strong> not, e.g., in Galactic radiation which has a different<br />

spectral distribution <strong>and</strong> would thus be more prominent in the<br />

difference maps. Only the region within the dashed rectangle<br />

was used in the original analysis of the temperature fluctuations,<br />

in order to avoid boundary effects. The fluctuation<br />

spectrum computed from the difference maps is compatible<br />

with pure noise<br />

indications of the presence of the second Doppler peak<br />

were found.<br />

In April 2001, refined CMB anisotropy measurements<br />

from three experiments were released,<br />

BOOMERANG, MAXIMA, <strong>and</strong> DASI. For the former<br />

two, the observational data were the same as in the year<br />

before, but improved analysis methods were applied;<br />

in particular, a better instrumental calibration was obtained.<br />

The resulting temperature fluctuation spectrum<br />

is presented in Fig. 8.28, demonstrating that it was now<br />

possible to determine the locations of the first three<br />

Doppler peaks.<br />

The status of measurements of the CMB anisotropy<br />

as of the end of 2002 is shown in Fig. 8.29. In the lefth<strong>and</strong><br />

panel, the results of numerous experiments are<br />

plotted individually. The panel on the right shows the<br />

weighted mean of these experiments. Although it might<br />

not be suspected at first sight, the results of all experiments<br />

shown on the left are compatible with each<br />

other. With that we mean that the individual measure-

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