Mass-to-Luminosity Ratio and Its Correlation To Dark Matter Distributions Across Different Galaxy Types

Dark matter is believed to play a pivotal role in the structure and dynamics of galaxies. Unlike ordinary matter, dark matter does not emit light or energy or interact with electromagnetic forces. This study explores dark matter distribution in galaxies and compares various galaxy types. We utilize the Spitzer Photometry & Accurate Rotation Curves database, focusing on latetype and early-type galaxies, including Blue Compact Dwarf, Lenticular, Small Magellanic, Tight Spirals, Loose Spirals, Irregular Spirals, and Elliptical galaxies. Using centripetal acceleration and Newton’s Law of Universal Gravitation, we derive a galaxy-mass equation within a certain radius. Luminosity within a given radius is graphed through conversions from the database. Results indicate that the mass-to-luminosity ratio generally increases with radius across all galaxy types, suggesting an intertwined relationship between mass, luminosity, and dark matter distribution. The increasing mass-to-luminosity ratio with radius implies that all galaxies tend to have more mass relative to their luminosity as we move further from the center. This supports the idea that dark matter becomes more prominent in the outer areas of the galaxy, forming a dark matter halo and exerting gravitational forces on visible matter to influence the structure of the galaxy. Our results imply that dark matter is a significant part of galaxies.