This paper discusses the life and death of massive single stars, focusing on how their final fate depends on their helium core and hydrogen envelope masses at death. The study considers the effects of metallicity on mass loss, which influences the evolution and final outcomes of massive stars. It maps where black holes and neutron stars are likely to form and which types of supernovae are produced as a function of mass and metallicity. The paper also explores the potential for gamma-ray bursts and jet-driven supernovae from rapidly rotating stars. The study uses stellar models from previous research to examine the evolution of massive stars, considering the effects of mass loss, explosion mechanisms, and remnant properties. It discusses how the mass of the helium core determines the explosion mechanism and the type of remnant produced. The hydrogen envelope is crucial for determining the spectrum and light curve of Type II supernovae, while the absence of a hydrogen envelope leads to Type Ib and Ic supernovae. The paper also addresses the role of metallicity in mass loss, noting that lower metallicity stars lose less mass and have larger helium cores and hydrogen envelopes. The effects of metallicity on mass loss are discussed, including the scaling laws for different types of stars. The study also considers the impact of rotation on mass loss and the formation of black holes and neutron stars. The paper concludes that the final fate of massive stars is influenced by their mass, metallicity, and rotation. It suggests that binary systems are more likely to produce gamma-ray bursts and that single stars may only produce a small subset of GRB progenitors at higher metallicities. The study also highlights the importance of considering the initial mass function and the distribution of massive stars in the galaxy. The results suggest that the populations of massive star outcomes may vary with redshift, and that future observations could help test these predictions.This paper discusses the life and death of massive single stars, focusing on how their final fate depends on their helium core and hydrogen envelope masses at death. The study considers the effects of metallicity on mass loss, which influences the evolution and final outcomes of massive stars. It maps where black holes and neutron stars are likely to form and which types of supernovae are produced as a function of mass and metallicity. The paper also explores the potential for gamma-ray bursts and jet-driven supernovae from rapidly rotating stars. The study uses stellar models from previous research to examine the evolution of massive stars, considering the effects of mass loss, explosion mechanisms, and remnant properties. It discusses how the mass of the helium core determines the explosion mechanism and the type of remnant produced. The hydrogen envelope is crucial for determining the spectrum and light curve of Type II supernovae, while the absence of a hydrogen envelope leads to Type Ib and Ic supernovae. The paper also addresses the role of metallicity in mass loss, noting that lower metallicity stars lose less mass and have larger helium cores and hydrogen envelopes. The effects of metallicity on mass loss are discussed, including the scaling laws for different types of stars. The study also considers the impact of rotation on mass loss and the formation of black holes and neutron stars. The paper concludes that the final fate of massive stars is influenced by their mass, metallicity, and rotation. It suggests that binary systems are more likely to produce gamma-ray bursts and that single stars may only produce a small subset of GRB progenitors at higher metallicities. The study also highlights the importance of considering the initial mass function and the distribution of massive stars in the galaxy. The results suggest that the populations of massive star outcomes may vary with redshift, and that future observations could help test these predictions.