Galaxies in Absorption: A Study of Galactic Chemical Evolution Models

Abstract

Deciphering how our Cosmos unfolded from the uncharted 'dark ages' to the present condition governed by vast systems has become one of the most interesting searches of the human imagination. Over the last few decades, with the aid of empirical surveys and computational simulations, we have made considerable strides towards a coherent image of galaxy forming and evolution. However, we have yet to achieve a good understanding of numerous important things, such as the epoch in which the very first galaxies begin to form; the density and temperature of the hydrogen from which these galaxies were born; the morphologies and chemical contents of the early galaxies and the functions performed by star formation and gas flows in the creation of galaxies. In our search to find answers to these issues, essential hints will come from a robust knowledge of the gas properties in and around galaxies at all times. The wide expanse between the stars of the Milky Way and other galaxies is permeated by interstellar gas, which serves as a key component in the ongoing period of star creation from one generation of stars to the next. As a consequence, the properties (especially the chemical makeup) of the 'interstellar medium' (ISM) of the galaxy provide valuable details on the history of star formation and accretion.