In astrophysics, metallicity is a key parameter used to quantify the abundance of elements heavier than hydrogen and helium within a celestial object, such as a star, galaxy, or nebula. This measure is crucial for understanding the chemical enrichment history of the universe, as the formation of heavier elements occurs through stellar processes, including supernovae. A star or region with low metallicity is thought to have formed early in the cosmic timeline, when only primordial elements were available. Conversely, high metallicity indicates that the object has resided in an environment that has undergone multiple generations of star formation and element dispersal. Variations in metallicity are used to study the rates of nucleosynthesis and the overall chemical evolution of cosmic structures.