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In astronomy, dark matter is an invisible and hypothetical form of matter that does not interact with light or other electromagnetic radiation.Dark matter is implied by gravitational effects which cannot be explained by general relativity unless more matter is present than can be observed.
[27] [28] Rubin's results were confirmed over subsequent decades, [1] and became the first persuasive results supporting the theory of dark matter, initially proposed by Fritz Zwicky in the 1930s. [1] [12] [29] This data was confirmed by radio astronomers, the discovery of the cosmic microwave background, and images of gravitational lensing.
The second class are those which try to find voids via the geometrical structures in the dark matter distribution as suggested by the galaxies. [29] The third class is made of those finders which identify structures dynamically by using gravitationally unstable points in the distribution of dark matter. [30]
Dark matter is called ‘dark’ because it’s invisible to us and does not measurably interact with anything other than gravity. It could be interspersed between the atoms that make up the Earth ...
The peaks contain interesting physical signatures. The angular scale of the first peak determines the curvature of the universe (but not the topology of the universe). The next peak—ratio of the odd peaks to the even peaks—determines the reduced baryon density. [68] The third peak can be used to get information about the dark-matter density ...
Unlike dark matter, ordinary matter can lose energy by many routes, which means that as it collapses, it can lose the energy which would otherwise hold it apart, and collapse more quickly, and into denser forms. Ordinary matter gathers where dark matter is denser, and in those places it collapses into clouds of mainly hydrogen gas.
The third component, the dark matter, was detected indirectly by the gravitational lensing of background objects. In theories without dark matter, such as modified Newtonian dynamics (MOND), the lensing would be expected to follow the baryonic matter; i.e. the X-ray gas. However, the lensing is strongest in two separated regions near (possibly ...
During the 1980s, most research focused on cold dark matter with critical density in matter, around 95% CDM and 5% baryons: these showed success at forming galaxies and clusters of galaxies, but problems remained; notably, the model required a Hubble constant lower than preferred by observations, and observations around 1988–1990 showed more ...