Exploring the Cosmic History of Star Formation, Metallicity Evolution, and Core-Collapse Supernova Rates

Abstract

Research on star formation is essential for understanding galaxy evolution and the universe’s evolution. Astronomers can learn about star formation over time by observing core-collapse supernovae and determining their occurrence rate. Core collapse supernovae are a valuable resource in the investigation of star formation due to the period between the birth of a massive star and the supernova being so brief compared to the cosmic timescale. This thesis explores various aspects related to star formation and core-collapse supernovae rates and their connection to host galaxies. The characteristics of host galaxies are also examined using the core-collapse supernova sample. The study also discusses different models of star formation rate, such as Madau & Dickinson (2014), and compares them. The thesis also addresses highly active galaxies and their star formation and investigates the relationship between metallicity evolution and star formation history across cosmic time. It is observed that metallicity increases over cosmic time and reaches its highest value at present day. This study looks at the rate of nearby core-collapse supernovae, considering both the cumulative and shell volume rates. It also examines the significance of any decrease in this rate using statistical methods, as well as the impact of galaxy orientation and extinction in host galaxies. Additionally, the study calculates the absolute magnitudes of these supernovae. The findings indicate that the rate of core-collapse supernovae decreases at a distance of 16 Mpc. The study also concludes that observed rates of these supernovae need to be adjusted to account for different missing supernova fractions at different redshifts to fit the rates derived from star formation rate models.