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In cosmology, baryon acoustic oscillations (BAO) are regular, periodic fluctuations in the density of the visible baryonic matter of the universe. In the same way that supernova provide a "standard candle" for astronomical observations,〔 〕 BAO matter clustering provides a "standard ruler" for length scale in cosmology.〔 〕 The length of this standard ruler (~490 million light years in today's universe〔 〕) can be measured by looking at the large scale structure of matter using astronomical surveys.〔 BAO measurements help cosmologists understand more about the nature of dark energy (which causes the apparent slight acceleration of the expansion of the universe) by constraining cosmological parameters.〔 ==The early universe== The early universe consisted of a hot, dense plasma of electrons and baryons (protons and neutrons). Photons (light particles) traveling in this universe were essentially trapped, unable to travel for any considerable distance before interacting with the plasma via Thomson scattering.〔 〕 As the universe expanded, the plasma cooled to below 3000 K—a low enough energy such that the electrons and protons in the plasma could combine to form neutral hydrogen atoms. This recombination happened when the universe was around 379,000 years old, or at a redshift of .〔 Photons interact to a much lesser degree with neutral matter, therefore at recombination the universe suddenly became transparent to photons, allowing them to decouple from the matter and free-stream through the universe.〔 Technically speaking, the mean free path of the photons became on the order of the size of the universe. The cosmic microwave background (CMB) radiation is light that was emitted after recombination that is only now reaching our telescopes. Therefore when we look at Wilkinson Microwave Anisotropy Probe (WMAP) data, we are looking back in time to see an image of the universe when it was only 379,000 years old.〔 WMAP indicates (Figure 1) a smooth, homogeneous universe with density anisotropies of 10 parts per million.〔 However, when we observe the universe today we find large structure and density fluctuations. Galaxies, for instance, are a million times more dense than the universe's mean density.〔 The current belief is that the universe was built in a bottom-up fashion, meaning that the small anisotropies of the early universe acted as gravitational seeds for the structure we see today. Overdense regions attract more matter, whereas underdense regions attract less, and thus these small anisotropies we see in the CMB became the large scale structures we observe in the universe today. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「baryon acoustic oscillations」の詳細全文を読む スポンサード リンク
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