The elemental compositions of resolved stars formed across different epochs document the chemical evolution path of a galaxy. This evolution is shaped by factors such as the galaxy-wide stellar initial mass function (gwIMF), gas infall, and outflows. Analyzing abundance profiles provides insights into estimating these properties in nearby dwarf galaxies and the Milky Way. Our study indicates that dwarf galaxies, characterized by low stellar metallicities and star formation rates, exhibit shallower gwIMF slopes for low-mass stars and steeper slopes for massive stars. Additionally, comparing our results with independent IMF estimation techniques reveals consistent and systematic IMF variations. However, caution is warranted in interpreting gas outflow in galaxy chemical evolution models, as while it serves as a quenching mechanism, other factors such as gas heating and galaxy interaction may also play significant roles.