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1. Dark Matter

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   Observational Evidence and Historical Context
   The earliest concrete evidence for non-luminous matter originated from the rotational dynamics of galaxies. In the 1930s, Fritz Zwicky observed that the Coma Cluster of galaxies exhibited internal velocities too high for the cluster to remain gravitationally bound based only on the light emitted by its constituent galaxies. He termed this unseen component dunkle Materie (dark matter) [2].
   A more systematic study emerged in the 1970s through the work of Vera Rubin an…

2. Galaxy Cluster

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   Composition and Mass Budget
   The total mass of a galaxy cluster ($\text{M}_{\text{cluster}}$) is dominated not by the visible galaxies, but by the unseen components. While early estimations based solely on galaxy velocities suggested a mass discrepancy (Fritz Zwicky, 1933), modern analysis confirms the dominant components are dark matter and the intracluster medium (ICM)/).
   The mass distribution generally follows the [$\Lambda$CDM conco…

3. Non Baryonic Matter

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   Historical Context and Cosmological Necessity
   The initial necessity for postulating the existence of non-baryonic matter arose in the 1930s from observations of galaxy cluster dynamics. Fritz Zwicky, while studying the Coma Cluster, noted that the velocities of galaxies within the cluster were far too high for the cluster to remain gravitationally bound if only the visible luminous matter were considered. He termed this missing gravitational source Dunkle Materie (da…