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Dark Matter is a theoretical form of matter that is believed to make up approximately 27% of the mass-energy content of the observable universe. Its existence is inferred through its gravitational effects on visible matter, radiation, and the large-scale structure of the universe. Unlike normal matter, dark matter does not emit, absorb, or reflect any electromagnetic radiation, making it impossible to detect directly using existing instruments and technology. In the context of Physical Cosmology, Dark Matter plays a crucial role in our understanding of the formation and evolution of galaxies and large-scale structures in the universe. It provides the necessary gravitational force to hold together the visible matter in galaxies, allowing them to maintain their stability and rotation. Additionally, simulations of cosmic structure formation suggest that dark matter is essential for explaining the observed distribution of matter on large scales. Astrophysicists and cosmologists study Dark Matter through its indirect effects on observable phenomena such as gravitational lensing, galaxy rotation curves, and the cosmic microwave background radiation. By comparing these observations with theoretical models, researchers can make inferences about the properties of dark matter, such as its mass, distribution, and interactions with other forms of matter and energy. In summary, Dark Matter is a fundamental component of our universe that has profound implications for Physical Cosmology, Astrophysics, and Astronomy. Its elusive nature and far-reaching consequences make it an exciting area of ongoing research and discovery.