I have provided a brief review of the formation of the first stars and their radiative, chemical, and mechanical feedback that affects subsequent structure and galaxy formation. Over the past decade, many groups have used numerical simulations to study these astrophysics events in the first billion years of the universe. Currently, the general consensus is that Population III stars are still very massive with a characteristic mass of tens M with an unknown fraction in binaries. The prospect of Population III binaries is exciting, and their impact on the universe prior to reionization, such as pre-ionization from X-rays, will be addressed in future studies. To summarize, the radiation from Population III expels most of the gas from the host halos, creating gas-poor halos that cannot form stars for 10-50 Myr. The SNe from the first stars enriches the first galaxies to a nearly uniform ~ 10-3 Z, and ultimately leads to the demise of this unique population of stars. The gas depletion, IGM pre-heating, and chemical enrichment all have a lasting impact on the formation of the first galaxies. Hopefully we can utilize these imprints to disentangle Population III stellar properties from the most distant galaxies in the universe.