Cosmic Microwave Background Radiation
Anisotropies: their Discovery and Utilization
Nobel Lecture, December 8, 2006
by
George F. Smoot iii
Lawrence Berkeley National Laboratory, Space Sciences Laboratory,
Department of Physics, University of California, Berkeley, CA 94720, USA.
1 The Cosmic Background Radiation
Observations of the Cosmic Microwave Background (CMB) temperature anisotropies have revolutionized and continue to revolutionize our understanding of the Universe. The observation of the CMB anisotropies angular power spectrum with its plateau, acoustic peaks, and high frequency damping tail have established a standard cosmological model consisting of a flat (critical density) geometry, with contents being mainly dark energy and dark matter and a small amount of ordinary matter. In this successful model the dark and ordinary matter formed its structure through gravitational instability acting on the quantum fluctuations generated during the very early Inflationary epoch. Current and future observations will test this model and determine its
key cosmological parameters with spectacular precision and confidence.
1.1 Introduction
In the Big Bang theory the CMB Radiation is the relic radiation from the hot primeval fireball that began our observable universe about 13.7 billion years ago. As such the CMB can be used as a powerful tool that allows us to measure the dynamics and geometry of the universe. The CMB was first discovered by Penzias and Wilson at Bell Laboratory in 1964 [1]. They found a persistent radiation from every direction which had a thermodynamic temperature of about 3.2K. At that time, physicists at Princeton (Dicke, Peebles, Wilkinson and Roll) [2] were developing an experiment to measure the relic radiation from the Big Bang theory. Penzias and Wilson’s serendipitous discovery of the CMB opened up the new era of cosmology, beginning the process of transforming it from myth and speculation into a real scientific exploration. According to Big Bang theory, our universe began in a nearly perfect thermal equilibrium state with very high temperature. The universe is dynamic and has been ever
expanding and cooling since its birth. When the temperature of the universe dropped to 3,000 K there were insufficient energetic CMB photons to keep hydrogen or helium atoms ionized. Thus, the primeval plasma of charged nuclei, electrons and photons changed into neutral atoms plus background radiation.
The background radiation could then propagate through space freely, though being stretched by the continuing expansion of the universe, while baryonic matter (mostly hydrogen and helium atoms) could cluster by gravitational attraction to form stars, galaxies and even larger structures. For these structures to form there must have been primordial perturbations in the early matter and energy distributions. The primordial fluctuations of matter density that will later form large scale structures leave imprints in the form of temperature anisotropies in the CMB.
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