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Cosmic voids are the vast empty spaces between filaments (the largest-scale structures in the Universe), which contain very few, or no, galaxies. They were first discovered in 1978 during a pioneering study by Stephen Gregory and Laird A. Thompson at the Kitt Peak National Observatory.〔Freedman, R.A., & Kaufmann III, W.J. (2008). Stars and galaxies: Universe. New York City: W.H. Freeman and Company.〕 These zones have less than one-tenth of the average density of matter abundance that is considered typical for the observable Universe. Voids typically have a diameter of 11 to 150 megaparsecs; particularly large voids, defined by the absence of rich superclusters, are sometimes called "supervoids". Voids located in high-density environments are smaller than voids situated in low-density spaces of the universe. Voids are believed to have been formed by baryon acoustic oscillations in the Big Bang—collapses of mass followed by implosions of the compressed baryonic matter. Starting from initially small anisotropies due to quantum fluctuations in the early Universe, the anisotropies grew larger in scale over time. Regions of higher density collapsed more rapidly under gravity, eventually resulting in the large-scale, foam-like structure or “cosmic web” of voids and galaxy filaments seen today. Voids appear to correlate with the observed temperature of the cosmic microwave background (CMB), due to the Sachs–Wolfe effect. Colder regions correlate with voids, whereas hotter regions correlate with filaments, because of gravitational redshifting. As the Sachs–Wolfe effect is only significant if the Universe is dominated by radiation or dark energy, the existence of voids is significant in providing physical evidence for dark energy. == Large-scale structure == The structure of our Universe can be broken down into components that can help describe the characteristics of individual regions of the cosmos. These are the main structural components of the cosmic web: * Voids – vast regions with very low cosmic mean densities, usually larger than 10 megaparsecs (Mpc) in diameter. * Walls – the regions that contain the typical cosmic mean density of matter abundance. Walls can be further broken down into two smaller structural features: * * Clusters – highly concentrated zones where walls meet and intersect, adding to the effective size of the local wall. * * Filaments – the branching arms of walls that can stretch for tens of megaparsecs. Voids have a mean density less than tenth of the average density of the universe. This serves as a working definition even though there is no single agreed upon definition of what constitutes a void. The matter density value used for describing the cosmic mean density is usually based on a ratio of the number of galaxies per unit volume rather than the total mass of the matter contained in a unit volume. 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「Void (astronomy)」の詳細全文を読む スポンサード リンク
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